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Sample records for public eso near-ir

  1. Public Surveys at ESO

    NASA Astrophysics Data System (ADS)

    Arnaboldi, M.; Delmotte, N.; Geier, S.; Hilker, M.; Hussain, G.; Mascetti, L.; Micol, A.; Petr-Gotzens, M.; Rejkuba, M.; Retzlaff, J.

    We provide an overview of the ESO public survey projects being carried out at the ESO survey telescopes, VISTA and VST, on the VLT instruments, UVES, FLAMES and VIMOS, and on the NTT, with SOFI and EFOSC, at the La Silla-Paranal Observatory. We outline the motivations behind these extensive projects, the policies and the facilities supporting these programmes. We illustrate how their data products are validated and published through the ESO Science Archive Facility, in order to make them accessible to the astronomical community. We conclude with an outlook on the future of public surveys at ESO.

  2. The Gaia-ESO Public Spectroscopic Survey

    NASA Astrophysics Data System (ADS)

    Gilmore, G.; Randich, S.; Asplund, M.; Binney, J.; Bonifacio, P.; Drew, J.; Feltzing, S.; Ferguson, A.; Jeffries, R.; Micela, G.; Negueruela, I.; Prusti, T.; Rix, H.-W.; Vallenari, A.; Alfaro, E.; Allende-Prieto, C.; Babusiaux, C.; Bensby, T.; Blomme, R.; Bragaglia, A.; Flaccomio, E.; François, P.; Irwin, M.; Koposov, S.; Korn, A.; Lanzafame, A.; Pancino, E.; Paunzen, E.; Recio-Blanco, A.; Sacco, G.; Smiljanic, R.; Van Eck, S.; Walton, N.; Aden, D.; Aerts, C.; Affer, L.; Alcala, J.-M.; Altavilla, G.; Alves, J.; Antoja, T.; Arenou, F.; Argiroffi, C.; Asensio Ramos, A.; Bailer-Jones, C.; Balaguer-Nunez, L.; Bayo, A.; Barbuy, B.; Barisevicius, G.; Barrado y Navascues, D.; Battistini, C.; Bellas Velidis, I.; Bellazzini, M.; Belokurov, V.; Bergemann, M.; Bertelli, G.; Biazzo, K.; Bienayme, O.; Bland-Hawthorn, J.; Boeche, C.; Bonito, S.; Boudreault, S.; Bouvier, J.; Brandao, I.; Brown, A.; de Bruijne, J.; Burleigh, M.; Caballero, J.; Caffau, E.; Calura, F.; Capuzzo-Dolcetta, R.; Caramazza, M.; Carraro, G.; Casagrande, L.; Casewell, S.; Chapman, S.; Chiappini, C.; Chorniy, Y.; Christlieb, N.; Cignoni, M.; Cocozza, G.; Colless, M.; Collet, R.; Collins, M.; Correnti, M.; Covino, E.; Crnojevic, D.; Cropper, M.; Cunha, M.; Damiani, F.; David, M.; Delgado, A.; Duffau, S.; Edvardsson, B.; Eldridge, J.; Enke, H.; Eriksson, K.; Evans, N. W.; Eyer, L.; Famaey, B.; Fellhauer, M.; Ferreras, I.; Figueras, F.; Fiorentino, G.; Flynn, C.; Folha, D.; Franciosini, E.; Frasca, A.; Freeman, K.; Fremat, Y.; Friel, E.; Gaensicke, B.; Gameiro, J.; Garzon, F.; Geier, S.; Geisler, D.; Gerhard, O.; Gibson, B.; Gomboc, A.; Gomez, A.; Gonzalez-Fernandez, C.; Gonzalez Hernandez, J.; Gosset, E.; Grebel, E.; Greimel, R.; Groenewegen, M.; Grundahl, F.; Guarcello, M.; Gustafsson, B.; Hadrava, P.; Hatzidimitriou, D.; Hambly, N.; Hammersley, P.; Hansen, C.; Haywood, M.; Heber, U.; Heiter, U.; Held, E.; Helmi, A.; Hensler, G.; Herrero, A.; Hill, V.; Hodgkin, S.; Huelamo, N.; Huxor, A.; Ibata, R.; Jackson, R.; de Jong, R.; Jonker, P.; Jordan, S.; Jordi, C.; Jorissen, A.; Katz, D.; Kawata, D.; Keller, S.; Kharchenko, N.; Klement, R.; Klutsch, A.; Knude, J.; Koch, A.; Kochukhov, O.; Kontizas, M.; Koubsky, P.; Lallement, R.; de Laverny, P.; van Leeuwen, F.; Lemasle, B.; Lewis, G.; Lind, K.; Lindstrom, H. P. E.; Lobel, A.; Lopez Santiago, J.; Lucas, P.; Ludwig, H.; Lueftinger, T.; Magrini, L.; Maiz Apellaniz, J.; Maldonado, J.; Marconi, G.; Marino, A.; Martayan, C.; Martinez-Valpuesta, I.; Matijevic, G.; McMahon, R.; Messina, S.; Meyer, M.; Miglio, A.; Mikolaitis, S.; Minchev, I.; Minniti, D.; Moitinho, A.; Momany, Y.; Monaco, L.; Montalto, M.; Monteiro, M. J.; Monier, R.; Montes, D.; Mora, A.; Moraux, E.; Morel, T.; Mowlavi, N.; Mucciarelli, A.; Munari, U.; Napiwotzki, R.; Nardetto, N.; Naylor, T.; Naze, Y.; Nelemans, G.; Okamoto, S.; Ortolani, S.; Pace, G.; Palla, F.; Palous, J.; Parker, R.; Penarrubia, J.; Pillitteri, I.; Piotto, G.; Posbic, H.; Prisinzano, L.; Puzeras, E.; Quirrenbach, A.; Ragaini, S.; Read, J.; Read, M.; Reyle, C.; De Ridder, J.; Robichon, N.; Robin, A.; Roeser, S.; Romano, D.; Royer, F.; Ruchti, G.; Ruzicka, A.; Ryan, S.; Ryde, N.; Santos, N.; Sanz Forcada, J.; Sarro Baro, L. M.; Sbordone, L.; Schilbach, E.; Schmeja, S.; Schnurr, O.; Schoenrich, R.; Scholz, R.-D.; Seabroke, G.; Sharma, S.; De Silva, G.; Smith, M.; Solano, E.; Sordo, R.; Soubiran, C.; Sousa, S.; Spagna, A.; Steffen, M.; Steinmetz, M.; Stelzer, B.; Stempels, E.; Tabernero, H.; Tautvaisiene, G.; Thevenin, F.; Torra, J.; Tosi, M.; Tolstoy, E.; Turon, C.; Walker, M.; Wambsganss, J.; Worley, C.; Venn, K.; Vink, J.; Wyse, R.; Zaggia, S.; Zeilinger, W.; Zoccali, M.; Zorec, J.; Zucker, D.; Zwitter, T.; Gaia-ESO Survey Team

    2012-03-01

    The Gaia-ESO Public Spectroscopic Survey has begun and will obtain high quality spectroscopy of some 100000 Milky Way stars, in the field and in open clusters, down to magnitude 19, systematically covering all the major components of the Milky Way. This survey will provide the first homogeneous overview of the distributions of kinematics and chemical element abundances in the Galaxy. The motivation, organisation and implementation of the Gaia-ESO Survey are described, emphasising the complementarity with the ESA Gaia mission. Spectra from the very first observing run of the survey are presented.

  3. ESO imaging survey: infrared deep public survey

    NASA Astrophysics Data System (ADS)

    Olsen, L. F.; Miralles, J.-M.; da Costa, L.; Madejsky, R.; Jørgensen, H. E.; Mignano, A.; Arnouts, S.; Benoist, C.; Dietrich, J. P.; Slijkhuis, R.; Zaggia, S.

    2006-09-01

    This paper is part of the series presenting the final results obtained by the ESO Imaging Survey (EIS) project. It presents new J and Ks data obtained from observations conducted at the ESO 3.5 m New Technology Telescope (NTT) using the SOFI camera. These data were taken as part of the Deep Public Survey (DPS) carried out by the ESO Imaging Survey program, significantly extending the earlier optical/infrared EIS-DEEP survey presented in a previous paper of this series. The DPS-IR survey comprises two observing strategies: shallow Ks observations providing nearly full coverage of pointings with complementary multi-band (in general {UBVRI}) optical data obtained using ESO's wide-field imager (WFI) and deeper J and Ks observations of the central parts of these fields. Currently, the DPS-IR survey provides a coverage of roughly 2.1 square degrees ( 300 SOFI pointings) in Ks with 0.63 square degrees to fainter magnitudes and also covered in J, over three independent regions of the sky. The goal of the present paper is to briefly describe the observations, the data reduction procedures, and to present the final survey products which include fully calibrated pixel-maps and catalogs extracted from them. The astrometric solution with an estimated accuracy of ⪉0.15 arcsec is based on the USNO catalog and limited only by the accuracy of the reference catalog. The final stacked images presented here number 89 and 272, in J and K_s, respectively, the latter reflecting the larger surveyed area. The J and Ks images were taken with a median seeing of 0.77 arcsec and 0.8 arcsec. The images reach a median 5σ limiting magnitude of JAB˜23.06 as measured within an aperture of 2´´, while the corresponding limiting magnitude in KsAB is 21.41 and 22.16 mag for the shallow and deep strategies. Although some spatial variation due to varying observing conditions is observed, overall the observed limiting magnitudes are consistent with those originally proposed. The quality of the data

  4. Linking Publications and Observations: The ESO Telescope Bibliography

    NASA Astrophysics Data System (ADS)

    Meakins, S.; Grothkopf, U.

    2012-09-01

    Bibliometric studies have become increasingly important in evaluating individual scientists, specific facilities, and entire observatories. In this context, the ESO Library has developed and maintains two tools: FUSE, a full-text search tool, and the Telescope Bibliography (telbib), a content management system that is used to classify and annotate ESO-related scientific papers. The new public telbib interface provides faceted searches and filtering, autosuggest support for author, bibcode and program ID searches, hit highlighting as well as recommendations for other papers of possible interest. It is available at www.eso.org/libraries/telbib.html.

  5. The ESO Public Surveys — Review of Milestones and Completion

    NASA Astrophysics Data System (ADS)

    Arnaboldi, M.; Rejkuba, M.; Retzlaff, J.; Delmotte, N.; Geier, S.; Hanuschik, R.; Hilker, M.; Hummel, W.; Hussain, G.; Ivanov, V. D.; Micol, A.; Mieske, S.; Neeser, M.; Petr-Gotzens, M.; Szeifert, T.

    2013-12-01

    In 2013 the eleven currently ongoing ESO public surveys successfully completed the submission and publication of their science data products via the ESO Science Archive Facility. An overview of the public survey projects in terms of telescope time allocation, observation progress and expected date of completion is presented. The science data products available in the ESO archive and their usage by the astronomical community are discussed with regard to the legacy value and scientific impact of these projects. This overview represents a natural introduction to the special section of the Messenger dedicated to the ESO public survey projects, in which the survey teams present their scientific aims and selected results in a series of dedicated articles.

  6. The Gaia-ESO Large Public Spectroscopic Survey

    NASA Astrophysics Data System (ADS)

    Randich, S.; Gilmore, G.; Gaia-ESO Consortium

    2013-12-01

    The Gaia-ESO Public Spectroscopic Survey has completed about one third of the data taking and continues to acquire high-quality spectroscopy, with both Giraffe and UVES, of representative samples of all Galactic stellar populations, including open clusters — young and old, nearby and distant, interior and exterior to the Sun — and field stars in the Galactic Halo, the thick Disc, the thin Disc and the Galactic Bulge. A large sample of stars in the Solar Neighbourhood, selected to include all possible ages and metallicities, is also being observed with UVES. This will be the first such large internally homogeneous study of the Milky Way stellar populations. Besides the intrinsic range of exciting scientific results, the Gaia-ESO Survey is also a pathfinder for future massive Gaia follow-up. Equally importantly, we are building an ESO-wide community of stellar spectroscopists, sharing, optimising, refining and cross-calibrating complementary approaches, strengths and experience. Internal Science Verification (SV) has started with several results demonstrating the huge potential of the survey and the first release of spectra to ESO has occurred.

  7. Publication of Science Data Products through the ESO archive- Lessons learnt and future evolution

    NASA Astrophysics Data System (ADS)

    Retzlaff, Jörg

    2015-12-01

    Phase 3 denotes the process of preparation, submission, validation and ingestion of science data products for storage in the ESO Science Archive Facility and subsequent publication to the scientific community. We will review more than four years of Phase 3 operations at ESO and we will discuss the future evolution of the Phase 3 system.

  8. The ESO Telescope Bibliography on the Web: Linking Publications and Observations

    NASA Astrophysics Data System (ADS)

    Grothkopf, U.; Delmotte, N.; Leibundgut, B.; Rainer, N.; Treumann, A.

    2004-12-01

    We present a web interface that allows users to keep track of the entire lifetime of VLT (Very Large Telescope) programs: from proposals to observations and publications. It links scientific papers with the observing proposals and archival data, located at the ESO/ST-ECF Science Archive Facility. This service is a prerequisite to the astronomical Virtual Observatory. The interface provides search options by bibliographic details (author, title, journal, publication year etc.) as well as by observatory site, telescope, instrument and program ID. Papers based on ESO observations can also be retrieved through the ADS Abstract Service from where active links to the ESO Archive are provided.

  9. Report on the ESO Workshop ''Rainbows on the Southern Sky: Science and Legacy Value of the ESO Public Surveys and Large Programmes''

    NASA Astrophysics Data System (ADS)

    Arnaboldi, M.; Rejkuba, M.; Leibundgut, B.; Beccari, G.

    2015-12-01

    This was the third ESO workshop on the science from Large Programmes and the second on Public Surveys. By design, this workshop covered all areas of research in observational astronomy, providing a forum for the presentation of the most recent scientific results from these programmes and fostering discussions on the planned developments enabled by large and coherent time allocations on ESO telescopes. Several aspects of the legacy value of such programmes —technological, archival content, access to data, time domain and sociological — were evaluated and set a reference for future developments of ESO services to the community.

  10. RR Lyrae stars in omega Centauri: Near-IR properties and period-luminosity relations

    NASA Astrophysics Data System (ADS)

    Navarrete, C.; Catelan, M.; Contreras Ramos, R.; Gran, F.; Alonso-Garcia, J.

    2016-05-01

    Omega Centauri contains a rich harvest of variable stars. Here we report on a deep, wide-field, near-infrared (IR) variability survey for this cluster, carried out using ESO's 4.1m VISTA telescope. Our time-series data includes more than 180 RR Lyrae light curves in both J and Ks, allowing us to derive an unprecedented homogeneous and complete near-IR catalog of RR Lyrae in the field of omega Cen. Near-IR period-luminosity relations are derived and used to determine an updated (pulsational) distance modulus for the cluster.

  11. The ESO-MIM Star Trek: A broadbased public oriented short interactive exhibition for an introduction to contemporary astrophysics

    NASA Astrophysics Data System (ADS)

    Marco, O.; Miranda, F.

    2005-12-01

    In the course of the European Southern Observatory (ESO) Public Relations work in Chile, we have created a permanent exhibition of astronomy for a broad section of the public in the Museo Interactivo Mirador-MIM (Interactive Museum of science, Chile), a collaboration between ESO and MIM. This Museum is mostly directed towards schoolchildren (7-14 years old), with adult visits at weekends. It is funded by public money and is unique in Chile. We decided to present the most recent questions relative to astronomy, based on pictures taken mostly at ESO observatories, and to skip the basics of astronomy that are taught at school.

  12. ESO takes the public on an astronomical journey "Around the World in 80 Telescopes"

    NASA Astrophysics Data System (ADS)

    2009-03-01

    A live 24-hour free public video webcast, "Around the World in 80 Telescopes", will take place from 3 April 09:00 UT/GMT to 4 April 09:00 UT/GMT, chasing day and night around the globe to let viewers "visit" some of the most advanced astronomical telescopes on and off the planet. The webcast, organised by ESO for the International Year of Astronomy 2009 (IYA2009), is the first time that so many large observatories have been linked together for a public event. ESO PR Photo 13a/09 Map of Participating Observatories ESO PR Photo 13b/09 100 Hours of Astronomy logo Viewers will see new images of the cosmos, find out what observatories in their home countries or on the other side of the planet are discovering, send in questions and messages, and discover what astronomers are doing right now. Participating telescopes include those at observatories in Chile such as ESO's Very Large Telescope and La Silla, the Hawaii-based telescopes Gemini North and Keck, the Anglo-Australian Telescope, telescopes in the Canary Islands, the Southern African Large Telescope, space-based telescopes such as the NASA/ESA Hubble Space Telescope, ESA XMM-Newton and Integral, and many more. "Around the World in 80 Telescopes" will take viewers to every continent, including Antarctica! The webcast production will be hosted at ESO's headquarters near Munich, Germany, with live internet streaming by Ustream.tv. Anyone with a web browser supporting Adobe Flash will be able to follow the show, free of charge, from the website www.100hoursofastronomy.org and be a part of the project by sending messages and questions. The video player can be freely embedded on other websites. TV stations, web portals and science centres can also use the high quality feed. Representatives of the media who wish to report from the "front-line" and interview the team should get in touch. "Around the World in 80 Telescopes" is a major component of the 100 Hours of Astronomy (100HA), a Cornerstone project of the International

  13. Strong Lens Search in the ESO Public Survey KiDS

    NASA Astrophysics Data System (ADS)

    Napolitano, N. R.; Covone, G.; Roy, N.; Tortora, C.; La Barbera, F.; Radovich, M.; Getman, F.; Capaccioli, M.; Colonna, A.; Paolillo, M.; Verdoes Kleijn, G. A.; Koopmans, L. V. E.

    We have started a systematic search for strong lens candidates in the ESO public survey KiDS based on the visual inspection of massive galaxies in the redshift range 0. 1 < z < 0. 5. As a pilot program we have inspected 100 deg2, which overlap with SDSS and where there are known lenses to use as a control sample. Taking advantage of the superb image quality of VST/OmegaCAM, the colour information and accurate model subtracted images, we have found 18 new lens candidates, for which spectroscopic confirmation will be needed to confirm their lensing nature and study the mass profile of the lensing galaxies.

  14. Near-IR imaging of demineralization under sealants

    PubMed Central

    Tom, Henry; Chan, Kenneth H.; Darling, Cynthia L.; Fried, Daniel

    2014-01-01

    Previous studies have shown that near-IR reflectance and transillumination imaging can be used to acquire high contrast images of early caries lesions and composite restorative materials. The aim of the study was to determine the optimum near-IR wavelengths for imaging demineralized areas under dental sealants. Fifteen natural human premolars and molars with occlusal lesions were used in this in vitro study. Images before and after application of sealants were acquired using near-IR reflectance and near-IR transillumination at wavelengths of 1300 nm, 1460 nm, and 1500 – 1700 nm. Images were also acquired using polarization sensitive optical coherence tomography for comparison. The highest contrast for near-IR reflectance was at 1460 nm and 1500 – 1700 nm. These near-IR wavelengths are coincident with higher water absorption. The clear Delton sealant investigated was not visible in either co-polarization or cross-polarization OCT images. The wavelength region between 1500-1700-nm yielded the highest contrast of lesions under sealants for near-IR reflectance measurements. PMID:24817807

  15. Near-IR imaging of demineralization under sealants

    NASA Astrophysics Data System (ADS)

    Tom, Henry; Chan, Kenneth H.; Darling, Cynthia L.; Fried, Daniel

    2014-02-01

    Previous studies have shown that near-IR reflectance and transillumination imaging can be used to acquire high contrast images of early caries lesions and composite restorative materials. The aim of the study was to determine the optimum near-IR wavelengths for imaging demineralized areas under dental sealants. Fifteen natural human premolars and molars with occlusal lesions were used in this in vitro study. Images before and after application of sealants were acquired using near-IR reflectance and near-IR transillumination at wavelengths of 1300 nm, 1460 nm, and 1500 - 1700 nm. Images were also acquired using polarization sensitive optical coherence tomography for comparison. The highest contrast for near- IR reflectance was at 1460 nm and 1500 - 1700 nm. These near-IR wavelengths are coincident with higher water absorption. The clear Delton sealant investigated was not visible in either co-polarization or crosspolarization OCT images. The wavelength region between 1500-1700-nm yielded the highest contrast of lesions under sealants for near-IR reflectance measurements.

  16. Near-IR imaging of occlusal dental decay

    NASA Astrophysics Data System (ADS)

    Buehler, Christopher M.; Fried, Daniel

    2005-03-01

    Dental enamel manifests high transparency in the near-IR. Previous work demonstrated that near-IR light at 1310-nm is ideally suited for the transillumination of interproximal dental caries (dental decay in between teeth) [1]. However, most new dental decay occurs in the pits and fissures of the occlusal (biting) surfaces of posterior teeth. These caries lesions cannot be detected by x-rays during the early stages of decay due to the overlapping topography of the crown of the tooth. In this study, a near-IR imaging system operating at 1310-nm was used to acquire occlusal images by launching the near-IR light into the buccal surface of the tooth just above the gingival margin (gum-line). The near-IR light diffuses through the highly scattering dentin providing uniform back illumination of the enamel of the crowns allowing imaging of the occlusal surfaces. The near-IR images show high contrast between sound and demineralized areas. Demineralization (decay) can be easily differentiated from stains and pigmentation. Moreover, the high transparency of the enamel enables imaging at greater depth for the detection of subsurface decay hidden under the enamel. These early images suggest that the near-IR offers significant advantages over conventional visual, tactile and radiographic caries detection methods.

  17. About The ESO Messenger

    NASA Astrophysics Data System (ADS)

    Kjär, K.

    2000-06-01

    The present Messenger is the hundredth issue to be published. This may be a good moment to look back to the beginning and to the development of this publication. The idea of an internal ESO newsletter was born in the early seventies. Using the words of Professor Blaauw, Director General of ESO at that time and the person who launched The Messenger in its orbit, the purpose of The ESO Messenger should be “first of all, to promote the participation of ESO staff in what goes on in the Organization, especially at places of duty other than our own. Moreover, The Messenger may serve to give the world outside some impression of what happens inside ESO. The need for more internal communication is felt by many of the staff. The dispersion of our resources over several countries in widely separated continents demands a special effort to keep us aware of what is going on at the other establishments...”

  18. ESO Highlights in 2008

    NASA Astrophysics Data System (ADS)

    2009-01-01

    As is now the tradition, the European Southern Observatory looks back at the exciting moments of last year. 2008 was in several aspects an exceptionally good year. Over the year, ESO's telescopes provided data for more than 700 scientific publications in refereed journals, making ESO the most productive ground-based observatory in the world. ESO PR Highlights 2008 ESO PR Photo 01a/09 The image above is a clickable map. These are only some of the press releases issued by ESO in 2008. For a full listing, please go to ESO 2008 page. Austria signed the agreement to join the other 13 ESO member states (ESO 11/08 and 20/08), while the year marked the 10th anniversary of first light for ESO's "perfect science machine", the Very Large Telescope (ESO 16/08 and 17/08). The ALMA project, for which ESO is the European partner, had a major milestone in December, as the observatory was equipped with its first antenna (ESO 49/08). Also the Atacama Pathfinder Experiment (APEX) telescope impressed this year with some very impressive and publicly visible results. Highlights came in many fields: Astronomers for instance used the Very Large Telescope (VLT) to discover and image a probable giant planet long sought around the star Beta Pictoris (ESO 42/08). This is now the eighth extrasolar planet to have been imaged since the VLT imaged the first extrasolar planet in 2004 (three of eight were imaged with VLT). The VLT also enabled three students to confirm the nature of a unique planet (ESO 45/08). This extraordinary find, which turned up during their research project, is a planet about five times as massive as Jupiter. This is the first planet discovered orbiting a fast-rotating hot star. The world's foremost planet-hunting instrument, HARPS, located at ESO's La Silla observatory, scored a new first, finding a system of three super-Earths around a star (ESO 19/08). Based on the complete HARPS sample, astronomers now think that one Sun-like star out of three harbours short orbit, low

  19. Early fire sensing using near-IR diode laser spectroscopy

    NASA Astrophysics Data System (ADS)

    Bomse, David S.; Hovde, D. Christian; Chen, Shin-Juh; Silver, Joel A.

    2002-09-01

    We describe research leading to a trace gas detection system based on optical absorption using near-IR diode lasers that is intended to provide early warning of incipient fires. Applications include "high loss" structures such as office buildings, hospitals, hotels and shopping malls as well as airplanes and manned spacecraft where convention smoke detectors generate unacceptably high false alarm rates. Simultaneous or near-simultaneous detection of several gases (typically carbon dioxide, carbon monoxide, acetylene and hydrogen cyanide) provides high sensitivity while reducing the chance of false alarms. Continuous measurement of carbon dioxide concentrations also provides an internal check of instrument performance because ambient levels will not drop below ~350 ppm.

  20. X-shooter near-IR spectrograph arm realisation

    NASA Astrophysics Data System (ADS)

    Navarro, Ramon; Elswijk, Eddy; Tromp, Niels; ter Horst, Rik; Horrobin, Matthew; Vernet, Joel; Finger, Gert; Groot, Paul; Kaper, Lex

    2008-07-01

    X-shooter is a new high-efficiency spectrograph observing the complete spectral range of 300-2500 nm in a single exposure, with a spectral resolving power R>5000. The instrument will be located at the Cassegrain focus of one of the VLT UTs and consists of three spectrographs: UV, VIS and Near-IR. This paper addresses the design, hardware realization and performance of the Near-IR spectrograph of the X-Shooter instrument and its components. Various optical, mechanical and cryogenic manufacturing and verification techniques are discussed. The cryogenic performance of replicated light weight gratings is presented. Bare aluminium mirrors are produced and polished to optical quality to preserve high shape accuracy at cryogenic conditions. Their manufacturing techniques and performance are both discussed. The cryogenic collimator and dispersion boxes, on which the optical components are mounted, feature integrated baffles for improved stiffness and integrated leaf springs to reduce tension on optical components, thereby challenging 5 axis simultaneous CNC milling capabilities. ASTRON Extreme Light Weighting is used for a key component to reduce the flexure of the cryogenic system; some key numbers and unique manufacturing experience for this component are presented. The method of integrated system design at cryogenic working temperatures and the resulting alignment-free integration are evaluated. Finally some key lab test results for the complete NIR spectrograph are presented.

  1. ESO imaging survey. Deep public survey: Multi-color optical data for the Chandra Deep Field South

    NASA Astrophysics Data System (ADS)

    Arnouts, S.; Vandame, B.; Benoist, C.; Groenewegen, M. A. T.; da Costa, L.; Schirmer, M.; Mignani, R. P.; Slijkhuis, R.; Hatziminaoglou, E.; Hook, R.; Madejsky, R.; Rité, C.; Wicenec, A.

    2001-11-01

    This paper presents multi-passband optical data obtained from observations of the Chandra Deep Field South (CDF-S), located at alpha ~ 3h 32m, delta ~ -27o 48'. The observations were conducted at the ESO/MPG 2.2 m telescope at La Silla using the 8kx8k Wide-Field Imager (WFI). This data set, taken over a period of one year, represents the first field to be completed by the ongoing Deep Public Survey (DPS) being carried out as a part of the ESO Imaging Survey (EIS) project. This paper describes the optical observations, the techniques employed for un-supervised pipeline processing and the general characteristics of the final data set. Image processing has been performed using multi-resolution image decomposition techniques adapted to the EIS pipeline. The automatic processing steps include standard de-bias and flat-field, automatic removal of satellite tracks, de-fringing/sky-subtraction, image stacking/mosaicking and astrometry. Stacking of dithered images is carried out using pixel-based astrometry which enables the efficient removal of cosmic rays and image defects, yielding remarkably clean final images. The final astrometric calibration is based on a pre-release of the GSC-II catalog and has an estimated intrinsic accuracy of la 0.10 arcsec, with all passbands sharing the same solution. The paper includes data taken in six different filters (U'UBVRI). The data cover an area of about 0.25 square degrees reaching 5sigma limiting magnitudes of U'AB=26.0, UAB=25.7, BAB=26.4, VAB=25.4, RAB=25.5 and IAB= 24.7 mag, as measured within a 2 x FWHM aperture. The optical data covers an area of ~ 0.1 square degrees for which moderately deep observations in two near-infrared bands are also available, reaching 5sigma limiting magnitudes of JAB ~ 23.4 and KAB ~ 22.6. The current optical/infrared data also fully encompass the region of the deep X-ray observations recently completed by the Chandra telescope. The optical data presented here, as well as the infrared data released

  2. Near-IR Photometry of Nova Del 2013

    NASA Astrophysics Data System (ADS)

    Cass, C. A.; Carlon, L. R.; Corgan, T. D.; Dykhoff, A. D.; Gehrz, D. R.; Shenoy, P. D.

    2013-08-01

    Subjects: Infra-Red, Nova We report Near-IR photometry of Nova Del 2013 taken with the 0.76-m infrared telescope at the University of Minnesota's O'Brien Observatory (Marine on St. Croix, Minnesota, USA). RIJHKLM photometry were obtained on August 21.17 and 23.13 UT using an AsSi bolometer. Vega (alpha Lyrae) was used as the standard star. Our photometry show: August 21.17 UT: R = 5.1 +/- 0.1, I = 4.6 +/- 0.1, J = 4.6 +/- 0.1, H = 4.1 +/- 0.1, K = 3.9 +/- 0.1, L = 2.7 +/- 0.2, M = +2.2 +/- 0.2.

  3. Near-IR Spectral Variability of Young Stars

    NASA Astrophysics Data System (ADS)

    Zajac, Stephanie; Eisner, J. A.; Rudolph, A.

    2011-01-01

    Young stars (such as T Tauri and Herbig Ae/Be sources) exhibit photometric variability across the electromagnetic spectrum, including in the visible and infrared regions. Time-variable mass accretion rates may cause some of the observed variability, although other mechanisms such as starspots or structural changes in the circumstellar disks, provide alternative explanations. Spectroscopic observations provide a means to probe accretion via diagnostic emission lines, and to probe the ratio of stellar-to-circumstellar flux via veiling of stellar absorption lines. While spectroscopic variability in the optical range has been previously investigated, variability in the near-IR has not been explored as thoroughly. We have undertaken a project to track the spectral variability of young stars in the near-IR. Using the 90-inch Bok telescope on Kitt Peak, we observed about 40 young stars with FSPEC during two five-night runs separated by one month. As this project continues, in order to extend the timescales covered by our data, we will survey the same targets under similar circumstances in the summer of 2011. Ultimately, we hope to follow a sample of about 100 young stars with five-night observing runs every month of the year. Here we present initial results showing Brackett gamma Hydrogen line emission for several sources. We show that the emission line luminosity varies, and we use this variability to constrain the mass accretion rate with time for the observed objects. We acknowledge the NSF for funding under Award No. AST-0847170, a PAARE Grant for the Calfornia-Arizona Minority Partnership for Astronomy Research and Education (CAMPARE).

  4. ESO Highlights in 2008

    NASA Astrophysics Data System (ADS)

    2009-01-01

    As is now the tradition, the European Southern Observatory looks back at the exciting moments of last year. 2008 was in several aspects an exceptionally good year. Over the year, ESO's telescopes provided data for more than 700 scientific publications in refereed journals, making ESO the most productive ground-based observatory in the world. ESO PR Highlights 2008 ESO PR Photo 01a/09 The image above is a clickable map. These are only some of the press releases issued by ESO in 2008. For a full listing, please go to ESO 2008 page. Austria signed the agreement to join the other 13 ESO member states (ESO 11/08 and 20/08), while the year marked the 10th anniversary of first light for ESO's "perfect science machine", the Very Large Telescope (ESO 16/08 and 17/08). The ALMA project, for which ESO is the European partner, had a major milestone in December, as the observatory was equipped with its first antenna (ESO 49/08). Also the Atacama Pathfinder Experiment (APEX) telescope impressed this year with some very impressive and publicly visible results. Highlights came in many fields: Astronomers for instance used the Very Large Telescope (VLT) to discover and image a probable giant planet long sought around the star Beta Pictoris (ESO 42/08). This is now the eighth extrasolar planet to have been imaged since the VLT imaged the first extrasolar planet in 2004 (three of eight were imaged with VLT). The VLT also enabled three students to confirm the nature of a unique planet (ESO 45/08). This extraordinary find, which turned up during their research project, is a planet about five times as massive as Jupiter. This is the first planet discovered orbiting a fast-rotating hot star. The world's foremost planet-hunting instrument, HARPS, located at ESO's La Silla observatory, scored a new first, finding a system of three super-Earths around a star (ESO 19/08). Based on the complete HARPS sample, astronomers now think that one Sun-like star out of three harbours short orbit, low

  5. Near-IR imaging toward a puzzling young stellar object precessing jet

    NASA Astrophysics Data System (ADS)

    Paron, S.; Fariña, C.; Ortega, M. E.

    2016-10-01

    Aims: The study of jets that are related to stellar objects in formation is important because it enables us to understand the history of how the stars have built up their mass. Many studies currently examine jets towards low-mass young stellar objects, while equivalent studies toward massive or intermediate-mass young stellar objects are rare. In a previous study, based on 12CO J = 3-2 and public near-IR data, we found highly misaligned molecular outflows toward the infrared point source UGPS J185808.46+010041.8 (IRS) and some infrared features suggesting the existence of a precessing jet. Methods: Using near-IR data acquired with Gemini-NIRI at the JHKs broad- and narrowbands centered on the emission lines of [FeII], H2 1-0 S(1), H2 2-1 S(1), Brγ, and CO 2-0 (bh), we studied the circumstellar environment of IRS with an angular resolution between 0.̋35 and 0.̋45. Results: The emission in the JHKs broadbands shows in great detail a cone-shaped nebula extending to the north-northeast of the point source, which appears to be attached to it by a jet-like structure. In the three bands the nebula is resolved in a twisted-shaped feature composed of two arc-like features and a bow-shock-like structure seen mainly in the Ks band, which strongly suggests the presence of a precessing jet. An analysis of proper motions based on our Gemini observations and UKIDSS data additionally supports the precession scenario. We present one of the best-resolved cone-like nebula that is most likely related to a precessing jet up to date. The analysis of the observed near-IR lines shows that the H2 is collisionally excited, and the spatially coincidence of the [FeII] and H2 emissions in the closer arc-like feature suggests that this region is affected by a J shock. The second arc-like feature presents H2 emission without [FeII], which suggests a nondissociated C shock or a less energetic J shock. The H2 1-0 S(1) continuum-subtracted image reveals several knots and filaments at a larger

  6. Near-IR spectral evolution of dusty starburst galaxies

    NASA Astrophysics Data System (ADS)

    Lançon, Ariane; Rocca-Volmerange, Brigitte

    1996-11-01

    We propose a multicomponent analysis of starburst galaxies, based on a model that takes into account the young and evolved stellar components and the gas emission, with their respective extinction, in the frame of a coherent dust distribution pattern. Near-IR signatures are preferentially investigated, in order to penetrate as deep as possible into the dusty starburst cores. We computed the 1.4-2.5 μm spectra of synthetic stellar populations evolving through strong, short timescale bursts of star formation (continuum and lines, R ≃ 500). The evolution model is specifically sensitive to cool stellar populations (AGB and red supergiant stars). It takes advantage of the stellar library of Lançon & Rocca-Volmerange (1992) [A&ASS, 96, 593], observed with the same instrument (FTS/CFHT) as the analysed galaxy sample, so that the instrumental effects are minimised. The main near-IR observable constraints are the molecular signatures of CO and H2O and the slope of the continuum, observed over a range exceptionally broad for spectroscopic data. The H - K colour determined from the spectra measures the intrinsic stellar energy distribution but also differential extinction, which is further constrained by optical emission line ratios. Other observational constraints are the near-IR emission lines (Brγ, He I 2.06 μm, [Fe II] 1.64 μm, H2 2.12 μm) and the far-IR luminosity. The coherence of the results relies on the interpretation in terms of stellar populations from which all observable properties are derived, so that the link between the various wavelength ranges is secured. The luminosity LK is used for the absolute calibration. We apply this approach to the typical spectrum of the core of NGC 1614. Consistent solutions for the starburst characteristics (star-formation rate, IMF, burst age, morphology) are found and the role of each observational constraint in deriving satisfactory models is extensively discussed. The acceptable contamination of the K band light by the

  7. The Gaia-ESO Survey: Tracing interstellar extinction

    NASA Astrophysics Data System (ADS)

    Schultheis, M.; Kordopatis, G.; Recio-Blanco, A.; de Laverny, P.; Hill, V.; Gilmore, G.; Alfaro, E. J.; Costado, M. T.; Bensby, T.; Damiani, F.; Feltzing, S.; Flaccomio, E.; Lardo, C.; Jofre, P.; Prisinzano, L.; Zaggia, S.; Jimenez-Esteban, F.; Morbidelli, L.; Lanzafame, A. C.; Hourihane, A.; Worley, C.; Francois, P.

    2015-05-01

    Context. Large spectroscopic surveys have in recent years enabled computing three-dimensional interstellar extinction maps thanks to the accurate stellar atmospheric parameters and line-of-sight distances these surveys provide. Interstellar extinction maps are complementary to 3D maps extracted from photometry and allow a more thorough studying of the dust properties. Aims: Our goal is to use the high-resolution spectroscopic survey Gaia-ESO to obtain with a good distance resolution the interstellar extinction and its dependency as a function of the environment and the Galactocentric position. Methods: We used the stellar atmospheric parameters of more than 5000 stars, obtained from the Gaia-ESO survey second internal data release, and combined them with optical (SDSS) and near-infrared (VISTA) photometry as well as different sets of theoretical stellar isochrones to calculate line-of-sight extinction and distances. The extinction coefficients were then compared with the literature to discuss their dependency on the stellar parameters and position in the Galaxy. Results: Within the errors of our method, our work does not show any dependence of the interstellar extinction coefficient on the stellar atmospheric parameters. We find no evidence of a variation of E(J - H) /E(J - K) with the angle from the Galactic centre or with Galactocentric distance. This suggests that we are dealing with a uniform extinction law in the SDSS ugriz bands and the near-IR JHKs bands. Therefore, extinction maps built from mean colour-excesses that assume a constant extinction coefficient can be used without introducing any systematic errors. Based on observations collected with the FLAMES spectrograph at the VLT/UT2 telescope (Paranal Observatory, ESO, Chile), for the Gaia-ESO Large Public Survey, programme 188.B-300.Appendix A is available in electronic form at http://www.aanda.org

  8. Near-IR Spectroscopy of Amalthea (JV) and Thebe (JXIV)

    NASA Astrophysics Data System (ADS)

    Bustani, D.; Bell, J. F., III; Veverka, J.; Brown, R. H.; Cruikshank, D. P.

    1997-07-01

    We used the NASA IRTF, the NSFCAM 256x256 InSb array camera, and the JPL Cooled Coronograph (CoCo) to obtain H and K spectra of the faint inner Jovian satellites Amalthea (JV, Mv=14.1) and Thebe (JXIV, Mv=15.7). The observations were obtained on 25 and 26 July 1996 UT, near Jupiter opposition, when the satellites had a maximum limb elongation of 36" (JV) and 49" (JXIV). CoCo was designed for imaging of faint sources in the vicinity of much brighter sources (e.g., stellar companions), but in order to further supress scattered light from Jupiter (an extended source ~ 10(4) times brighter than these faint satellites), we inserted a special hard mask aperture ahead of the NSFCAM/CoCo optical path. In order to obtain spectra with this setup we attached a crude ~ 2" wide razor-edge slit to the top of the hard mask. The resulting spectral resolution is moderate (R ~ 440 in H and R ~ 870 in K) and is adequate for initial near-IR survey spectra of these objects. We obtained 4 spectra each of JV and JXIV in H (1.44 to 1.98 mu m) and 4 spectra each of JV and JXIV in K (2.0 to 2.35 mu m), as well as comparison spectra of Titan, Mimas, two solar-type stars, and Ne and Kr wavelength calibration lamps. Our calibrated Titan and Mimas CoCo spectra are consistent with previous H and K measurements of these objects. Our preliminary spectra of Amalthea reveal a relatively featureless spectrum in the 1.44 to 1.98 mu m and 2.06 to 2.17 mu m regions, but show evidence for an as-yet unidentified absorption from 2.20 to 2.30 mu m, apparently centered near 2.27 mu m. Our preliminary spectra of Thebe reveal a relatively featureless spectrum from 1.44 to 1.65 mu m and from 2.00 to 2.27 mu m, but show evidence for an as-yet unidentified weak absorption from ~ 1.70 to ~ 1.80 mu m, centered near 1.75 mu m. Continued refinement of the reflectance and wavelength calibrations is proceeding, and possible origins and band assignments for these near-IR absorption features are being investigated.

  9. Active multispectral near-IR detection of small surface targets

    NASA Astrophysics Data System (ADS)

    de Jong, Arie N.; Winkel, Hans; Roos, Marco J. J.

    2001-10-01

    The detection and identification of small surface targets with Electro-Optical sensors is seriously hampered by ground clutter, leading to false alarms and reduced detection probabilities. Active ground illumination can improve the detection performance of EO sensors compared to passive skylight illumination because of the knowledge of the illumination level and of its temporal stability. Sun and sky cannot provide this due to the weather variability. In addition multispectral sensors with carefully chosen spectral bands ranging from the visual into the near IR from 400-2500 nm wavelength can take benefit of a variety of cheap active light sources, ranging from lasers to Xenon or halogen lamps. Results are presented, obtained with a two- color laser scanner with one wavelength in the chlorophyll absorption dip. Another active scanner is described operating at 4 wavebands between 1400 and 2300 nm, using tungsten halogen lamps. Finally a simple TV camera was used with either a ste of narrow band spectral filters or polarization filters in front of the lamps. The targets consisted of an array of mixed objects, most of them real mines. The results how great promise in enhancing the detection and identification probabilities of EO sensors against small surface targets.

  10. Near-IR imaging of moderate redshift galaxy clusters

    NASA Technical Reports Server (NTRS)

    Stanford, S. A.; Dickinson, M. E.; Eisenhardt, P. R. M.

    1993-01-01

    We have obtained near-IR imaging of 3 moderate-z clusters on the 1.3 m at KPNO with SQIID, a new camera offering wide-field (5.5 arcmin) simultaneous JHK band imaging. Our photometry on a sample of approximately 100 likely member galaxies in one of the clusters, Abell 370 at z = 0.37, shows that we can obtain magnitudes good to 20 percent down to K = 18, considerably below the estimated K* = 16.5 at this redshift. These data indicate that there are no systematic problems in obtaining photometry at faint levels with SQIID. With the development of larger arrays, the field is open to progress. The resulting J, H, and K data for three clusters are combined with previously obtained multiband optical photometry. We present an investigation of the spectral properties and evolution of the dominant cold stellar populations by comparing optical-to-IR colors and color-magnitude diagrams to predictions from population synthesis models and galaxy spectral evolution codes.

  11. ESO Vacancy - Editor (EDG 604)

    NASA Astrophysics Data System (ADS)

    2002-09-01

    Assignment: Within the ESO Education and Public Relations Department team, your main tasks and responsibilities will comprise: • Development, update and maintenance of the comprehensive ESO Outreach website in its new look, including preparation of related material (texts, images, etc.) to be displayed; • Design, layout and production of the ESO quarterly journal “The Messenger” (e.g. image selection and processing, technical editing, etc.), in close collaboration with the Messenger editor; • Conception and production of promotional brochures, posters and other EPR products, in close collaboration with the Head of the Education and Public Relations Dept. of ESO Press Releases and various high-level publications, including the ESO Annual Report.

  12. Texaphyrin sensitized near-IR-to-visible photon upconversion.

    PubMed

    Deng, Fan; Sun, Wenfang; Castellano, Felix N

    2014-05-01

    Near-IR (NIR) absorption from a Cd(ii) texaphyrin (TXP) has been successfully coupled with rubrene triplet acceptors/annihilators in vacuum degassed dichloromethane to upconvert NIR (670-800 nm) incident photons into yellow fluorescence through sensitized triplet-triplet annihilation. Stern-Volmer analysis of dynamic energy transfer quenching of TXP by rubrene using transient absorption spectroscopy revealed Stern-Volmer and bimolecular quenching constants of 21,000 M(-1) and 5.7 × 10(8) M(-1) s(-1) respectively, for the triplet-triplet energy transfer process. The upconverted emission intensity with respect to the incident excitation power density at 750 nm was shown to vary between quadratic and linear, illustrating the expected kinetic limits for the light producing photochemistry under continuous wave illumination. Furthermore, with increasing TXP sensitizer concentration, the characteristic quadratic-to-linear crossover point shifted to lower incident photon power density. This is consistent with the notion that stronger photon capture in the sensitizer leads to experimental conditions promoting upconversion under milder excitation conditions. The maximum quantum yield of the TXP-sensitized rubrene upconverted fluorescence was 1.54 ± 0.04% under dilute conditions determined relative to [Os(phen)3](PF6)2 under continuous wave excitation conditions. This saturating quantum efficiency was realized when the incident light power dependence reached the quadratic-to-linear crossover point and was constant over the region where the composition displayed linear response to incident light power density. In pulsed laser experiments at higher sensitizer concentrations, the triplet-triplet annihilation quantum yield was determined to saturate at approximately 13%, corresponding to an upconversion yield of ∼10%, suggesting that the dichloromethane solvent either lowers the T2 state of the rubrene acceptor or is somehow attenuating the annihilation reaction between

  13. Photodissociation of Peroxynitric Acid in the Near-IR

    NASA Technical Reports Server (NTRS)

    Roehl, Coleen M.; Nizkorodov, Sergey A.; Zhang, Hui; Blake, Geoffrey A.; Wennberg, Paul O.

    2002-01-01

    Temperature-dependent near-IR photodissociation spectra were obtained for several vibrational overtone transitions of peroxynitric acid (HNO4) with a tunable OPO photolysis/OH laser-induced-fluorescence system. Band-integrated photodissociation cross-sections (definity integral of sigma(sub diss)), determined relative to that for the 3nu(sub 1), OH stretching overtone, were measured for three dissociative bands. Assuming unit quantum efficiency for photodissociation of 3nu(sub 1), we find 2nu(sub 1) + nu(sub 3)(8242/cm) = (1.21 x 10(exp -20) (independent of temperature), 2nu(sub 1) (6900/cm) = 4.09 x 10(exp 18) * e(sup (-826,5/T)) (295 K greater than T greater than 224 K), and nu(sub 1) + 2nu(sub 3) (6252/cm) = 1.87 x 10(exp -19) * e(sup (- 1410.7/T)) (278 K greater than T greater than 240 K) sq cm/molecule cm. The photodissociation cross-sections are independent of pressure over the range 2 to 40 Torr. Temperature-dependent quantum yields (phi) for these transitions were obtained using integrated absorption cross-sections (definity integral of sigma(sub abs)) of HNO4 overtone vibrations measured with a FTIR spectrometer. In the atmosphere, photodissociation in the infrared is dominated by excitation of the first overtone of the OH stretching vibration (2nu((sub 1)). Inclusion of all dissociative HNO4 overtone and combination transitions yields a daytime IR photolysis rate of approximately 1 x 10(esp -1)/s. This process significantly shortens the estimated lifetime of HNO4 in the upper troposphere and lower stratosphere.

  14. The Near-Ir Spectrum of CH_3D

    NASA Astrophysics Data System (ADS)

    Yang, Shaoyue; Lehmann, Kevin; Hargreaves, Robert J.; Bernath, Peter F.; Rey, Michael; Nikitin, Andrei V.; Tyuterev, Vladimir

    2016-06-01

    The near-IR spectrum, from 5000-8960 cm-1, of isotopically pure CH_3D was taken at temperatures of 294, 400, 500, 600, 700, 800, and 900K with a high resolution Fourier Transform machine at Old Dominion University. The spectra where analyzed to give the wavenumbers, integrated line intensities, and lower state term values (using lines observed in at least 3 different spectra). For the 294 K spectrum 12080 lines with S between 3.6x10-22 and 1x10-27 cm (not corrected for CH_3D natural abundance) were determined for this spectral interval. A theoretical spectrum of CH_3D has also been calculated at the Univ. of Reins, with >400,000 transitions predicted between 5000-6300 cm-1 with S values between 2.1x10-22 and 1 x 10-27 cm at 294K. Comparison of the predictions with 175 J" = 0 and 1 transitions previously assigned by the ETH group^1 shows that for 130 of these the absolute difference between the observed and predicted line wavenumbers is less than 0.1 cm-1 and for all but one transition the absolute difference is less than 1 cm-1. In this project, we are combining the temperature dependence of the line intensities, combination differences, and comparisons of line positions and strengths with the theoretical spectrum to extend the assignments of CH_3D lines in this spectral region. Selected assignments will be confirmed by IR-IR double resonance measurements at the University of Virginia. Ultimately, we hope to give a global analysis of CH_3D spectrum using a global effective Hamiltonian model. 1. Ulenikov, O.N. et al., Molecular Physics 108, 1209-1240 (2010)

  15. Texaphyrin sensitized near-IR-to-visible photon upconversion.

    PubMed

    Deng, Fan; Sun, Wenfang; Castellano, Felix N

    2014-05-01

    Near-IR (NIR) absorption from a Cd(ii) texaphyrin (TXP) has been successfully coupled with rubrene triplet acceptors/annihilators in vacuum degassed dichloromethane to upconvert NIR (670-800 nm) incident photons into yellow fluorescence through sensitized triplet-triplet annihilation. Stern-Volmer analysis of dynamic energy transfer quenching of TXP by rubrene using transient absorption spectroscopy revealed Stern-Volmer and bimolecular quenching constants of 21,000 M(-1) and 5.7 × 10(8) M(-1) s(-1) respectively, for the triplet-triplet energy transfer process. The upconverted emission intensity with respect to the incident excitation power density at 750 nm was shown to vary between quadratic and linear, illustrating the expected kinetic limits for the light producing photochemistry under continuous wave illumination. Furthermore, with increasing TXP sensitizer concentration, the characteristic quadratic-to-linear crossover point shifted to lower incident photon power density. This is consistent with the notion that stronger photon capture in the sensitizer leads to experimental conditions promoting upconversion under milder excitation conditions. The maximum quantum yield of the TXP-sensitized rubrene upconverted fluorescence was 1.54 ± 0.04% under dilute conditions determined relative to [Os(phen)3](PF6)2 under continuous wave excitation conditions. This saturating quantum efficiency was realized when the incident light power dependence reached the quadratic-to-linear crossover point and was constant over the region where the composition displayed linear response to incident light power density. In pulsed laser experiments at higher sensitizer concentrations, the triplet-triplet annihilation quantum yield was determined to saturate at approximately 13%, corresponding to an upconversion yield of ∼10%, suggesting that the dichloromethane solvent either lowers the T2 state of the rubrene acceptor or is somehow attenuating the annihilation reaction between

  16. On the nature of near-IR emitting Bi centres in glass

    SciTech Connect

    Dianov, Evgenii M

    2010-06-23

    Based on analysis of the structure and optical properties of Tl, Pb and Bi centres in crystals and comparison of their spectra with the near-IR luminescence spectra of bismuth-doped glasses, a model is proposed for the near-IR emitting bismuth centres in glass. Experimental evidence is presented in support of the model. (letters)

  17. PESSTO: survey description and products from the first data release by the Public ESO Spectroscopic Survey of Transient Objects

    NASA Astrophysics Data System (ADS)

    Smartt, S. J.; Valenti, S.; Fraser, M.; Inserra, C.; Young, D. R.; Sullivan, M.; Pastorello, A.; Benetti, S.; Gal-Yam, A.; Knapic, C.; Molinaro, M.; Smareglia, R.; Smith, K. W.; Taubenberger, S.; Yaron, O.; Anderson, J. P.; Ashall, C.; Balland, C.; Baltay, C.; Barbarino, C.; Bauer, F. E.; Baumont, S.; Bersier, D.; Blagorodnova, N.; Bongard, S.; Botticella, M. T.; Bufano, F.; Bulla, M.; Cappellaro, E.; Campbell, H.; Cellier-Holzem, F.; Chen, T.-W.; Childress, M. J.; Clocchiatti, A.; Contreras, C.; Dall'Ora, M.; Danziger, J.; de Jaeger, T.; De Cia, A.; Della Valle, M.; Dennefeld, M.; Elias-Rosa, N.; Elman, N.; Feindt, U.; Fleury, M.; Gall, E.; Gonzalez-Gaitan, S.; Galbany, L.; Morales Garoffolo, A.; Greggio, L.; Guillou, L. L.; Hachinger, S.; Hadjiyska, E.; Hage, P. E.; Hillebrandt, W.; Hodgkin, S.; Hsiao, E. Y.; James, P. A.; Jerkstrand, A.; Kangas, T.; Kankare, E.; Kotak, R.; Kromer, M.; Kuncarayakti, H.; Leloudas, G.; Lundqvist, P.; Lyman, J. D.; Hook, I. M.; Maguire, K.; Manulis, I.; Margheim, S. J.; Mattila, S.; Maund, J. R.; Mazzali, P. A.; McCrum, M.; McKinnon, R.; Moreno-Raya, M. E.; Nicholl, M.; Nugent, P.; Pain, R.; Pignata, G.; Phillips, M. M.; Polshaw, J.; Pumo, M. L.; Rabinowitz, D.; Reilly, E.; Romero-Cañizales, C.; Scalzo, R.; Schmidt, B.; Schulze, S.; Sim, S.; Sollerman, J.; Taddia, F.; Tartaglia, L.; Terreran, G.; Tomasella, L.; Turatto, M.; Walker, E.; Walton, N. A.; Wyrzykowski, L.; Yuan, F.; Zampieri, L.

    2015-07-01

    Context. The Public European Southern Observatory Spectroscopic Survey of Transient Objects (PESSTO) began as a public spectroscopic survey in April 2012. PESSTO classifies transients from publicly available sources and wide-field surveys, and selects science targets for detailed spectroscopic and photometric follow-up. PESSTO runs for nine months of the year, January - April and August - December inclusive, and typically has allocations of 10 nights per month. Aims: We describe the data reduction strategy and data products that are publicly available through the ESO archive as the Spectroscopic Survey data release 1 (SSDR1). Methods: PESSTO uses the New Technology Telescope with the instruments EFOSC2 and SOFI to provide optical and NIR spectroscopy and imaging. We target supernovae and optical transients brighter than 20.5m for classification. Science targets are selected for follow-up based on the PESSTO science goal of extending knowledge of the extremes of the supernova population. We use standard EFOSC2 set-ups providing spectra with resolutions of 13-18 Å between 3345-9995 Å. A subset of the brighter science targets are selected for SOFI spectroscopy with the blue and red grisms (0.935-2.53 μm and resolutions 23-33 Å) and imaging with broadband JHKs filters. Results: This first data release (SSDR1) contains flux calibrated spectra from the first year (April 2012-2013). A total of 221 confirmed supernovae were classified, and we released calibrated optical spectra and classifications publicly within 24 h of the data being taken (via WISeREP). The data in SSDR1 replace those released spectra. They have more reliable and quantifiable flux calibrations, correction for telluric absorption, and are made available in standard ESO Phase 3 formats. We estimate the absolute accuracy of the flux calibrations for EFOSC2 across the whole survey in SSDR1 to be typically ~15%, although a number of spectra will have less reliable absolute flux calibration because of

  18. Eso's Situation in Chile

    NASA Astrophysics Data System (ADS)

    1995-02-01

    Congress (Parliament) in 1964. According to this, the Chilean Government "grants to ESO the same immunities, prerogatives, privileges and facilities as the Government applies to the United Nations Economic Commission for Latin America (CEPAL), as granted in the Convention signed in Santiago on 16 February 1953" (Article 4 of the Chile-ESO Convention). Through this, the Chilean Government has in particular recognized that "the possessions and properties of (ESO) wherever they may be, and whoever may have them in his possession, shall be exempt of registration, requisition, confiscation, expropriation and of whatever interference, may it be through executive, administrative, judicial or legislative action" (Art. 4, Sec. 8, CEPAL Convention). Such privileges and immunities are not peculiar to the relations between Chile and ESO. They apply, as already mentioned, to CEPAL as well as to all other United Nations' Agencies and they are today typically recognized by the host states of International Organisations throughout the world. The Chilean Government and ESO agreed in 1983-84 by an exchange of diplomatic notes that these privileges and immunities apply not only to the La Silla observatory, but equally to any other observatory site that the Organisation may establish in the future in the Republic of Chile. It is obvious that, in order to exclude a possible breach of international law, the reported preliminary decision requires to be considered and interpreted in the light of these privileges and immunities. ESO trusts that the competent Chilean authorities will take the appropriate action and decisions which are required for ensuring the Organisation's international status and its protection from any public interference into its possessions and properties. In a Press Conference at the ESO Headquarters in Santiago de Chile on February 13, 1995, Mr. Daniel Hofstadt, ESO's highest-ranking representative in Chile, stated on behalf of the Organisation that "ESO is in Chile with

  19. Imaging of occlusal dental caries (decay) with near-IR light at 1310-nm.

    PubMed

    Bühler, Christopher; Ngaotheppitak, Patara; Fried, Daniel

    2005-01-24

    Dental enamel manifests high transparency in the near-IR. Previous work demonstrated that near-IR light at 1310-nm is ideally suited for the transillumination of interproximal dental caries (dental decay in between teeth) [1]. However, most new dental decay occurs in the pits and fissures of the occlusal (biting) surfaces of posterior teeth. These caries lesions cannot be detected by x-rays during the early stages of decay due to the overlapping topography of the crown of the tooth. In this study, a near- IR imaging system operating at 1310-nm was used to acquire occlusal images by launching the near-IR light into the buccal surface of the tooth just above the gingival margin (gum-line). The near-IR light diffuses through the highly scattering dentin providing uniform back illumination of the enamel of the crowns allowing imaging of the occlusal surfaces. The near-IR images show high contrast between sound and demineralized areas. Demineralization (decay) can be easily differentiated from stains, pigmentation, and hypomineralization (fluorosis). Moreover, the high transparency of the enamel enables imaging at greater depth for the detection of subsurface decay hidden under the enamel. These early images suggest that the near-IR offers significant advantages over conventional visual, tactile and radiographic caries detection methods.

  20. Imaging of occlusal dental caries (decay) with near-IR light at 1310-nm

    NASA Astrophysics Data System (ADS)

    Bühler, Christopher M.; Ngaotheppitak, Patara; Fried, Daniel

    2005-01-01

    Dental enamel manifests high transparency in the near-IR. Previous work demonstrated that near-IR light at 1310-nm is ideally suited for the transillumination of interproximal dental caries (dental decay in between teeth) [1]. However, most new dental decay occurs in the pits and fissures of the occlusal (biting) surfaces of posterior teeth. These caries lesions cannot be detected by x-rays during the early stages of decay due to the overlapping topography of the crown of the tooth. In this study, a near- IR imaging system operating at 1310-nm was used to acquire occlusal images by launching the near-IR light into the buccal surface of the tooth just above the gingival margin (gum-line). The near-IR light diffuses through the highly scattering dentin providing uniform back illumination of the enamel of the crowns allowing imaging of the occlusal surfaces. The near-IR images show high contrast between sound and demineralized areas. Demineralization (decay) can be easily differentiated from stains, pigmentation, and hypomineralization (fluorosis). Moreover, the high transparency of the enamel enables imaging at greater depth for the detection of subsurface decay hidden under the enamel. These early images suggest that the near-IR offers significant advantages over conventional visual, tactile and radiographic caries detection methods.

  1. ESO's Astronomy Education Programme

    NASA Astrophysics Data System (ADS)

    Pierce-Price, D. P. I.; Boffin, H.; Madsen, C.

    2006-08-01

    ESO, the European Organisation for Astronomical Research in the Southern Hemisphere, has operated a programme of astronomy education for some years, with a dedicated Educational Office established in 2001. We organise a range of activities, which we will highlight and discuss in this presentation. Many are run in collaboration with the European Association for Astronomy Education (EAAE), such as the "Catch a Star!" competition for schools, now in its fourth year. A new endeavour is the ALMA Interdisciplinary Teaching Project (ITP). In conjunction with the EAAE, we are creating a set of interdisciplinary teaching materials based around the Atacama Large Millimeter Array project. The unprecedented astronomical observations planned with ALMA, as well as the uniqueness of its site high in the Atacama Desert, offer excellent opportunities for interdisciplinary teaching that also encompass physics, engineering, earth sciences, life sciences, and culture. Another ongoing project in which ESO takes part is the "Science on Stage" European science education festival, organised by the EIROforum - the group of seven major European Intergovernmental Research Organisations, of which ESO is a member. This is part of the European Science Teaching Initiative, along with Science in School, a newly-launched European journal for science educators. Overviews of these projects will be given, including results and lessons learnt. We will also discuss possibilities for a future European Astronomy Day project, as a new initiative for European-wide public education.

  2. ESO's Two Observatories Merge

    NASA Astrophysics Data System (ADS)

    2005-02-01

    astronomical technology and is one of the premier facilities in the world for optical and near-infrared observations. In addition to the state-of-the-art Very Large Telescope and the four Auxiliary Telescopes of 1.8-m diameter which can move to relocate in up to 30 different locations feeding the interferometer, Paranal will also be home to the 2.6-m VLT Survey telescope (VST) and the 4.2-m VISTA IR survey telescope. Both Paranal and La Silla have a proven record of their unique ability to address most current issues in observational astronomy. In 2004 alone, each observatory provided data for the publication of about 350 peer-reviewed journal articles, more than any other ground-based observatory. With the present merging of these top-ranking astronomical observatories, fostering synergies and harmonizing the many diverse activities, ESO and the entire community of European astronomers will profit even more from these highly efficient research facilities. Images of ESO's observatories and telescopes are available in the ESO gallery.

  3. Attenuation of near-IR light through dentin at wavelengths from 1300-1650-nm.

    PubMed

    Chan, Andrew C; Darling, Cynthia L; Chan, Kenneth H; Fried, Daniel

    2014-02-18

    Light scattering in dental enamel decreases markedly from the UV to the near-IR and recent studies employing near-IR transillumination and reflectance imaging including optical coherence tomography indicate that this wavelength region is ideally suited for imaging dental caries due to the high transparency of enamel. The opacity of dentin is an important factor in optimizing the contrast of demineralization in reflectance measurements. It also influences the contrast of occlusal lesions in transillumination. Light scattering in dentin is an order of magnitude larger than in enamel, it is highly anisotropic and has a different spectral light scattering dependence than enamel. The objective of this study was to measure the optical attenuation of near-IR light through dentin at near-IR wavelengths from 1300-1650-nm. In this study the collimated transmission of near-IR light through polished thin sections of dentin of 0.05 to 0.6 mm thickness was measured. Beer-Lambert plots show that the attenuation coefficients range in magnitude from 20 to 40 cm(-1). Attenuation increased significantly with increasing wavelength and the increases were not entirely consistent with increased water absorption. PMID:24839373

  4. LENS MODELS OF HERSCHEL-SELECTED GALAXIES FROM HIGH-RESOLUTION NEAR-IR OBSERVATIONS

    SciTech Connect

    Calanog, J. A.; Cooray, A.; Ma, B.; Casey, C. M.; Fu, Hai; Wardlow, J.; Amber, S.; Baker, A. J.; Baes, M.; Bock, J.; Bourne, N.; Dye, S.; Bussmann, R. S.; Chapman, S. C.; Clements, D. L.; Conley, A.; Dannerbauer, H.; Dunne, L.; Eales, S.; and others

    2014-12-20

    We present Keck-Adaptive Optics and Hubble Space Telescope high resolution near-infrared (IR) imaging for 500 μm bright candidate lensing systems identified by the Herschel Multi-tiered Extragalactic Survey and Herschel Astrophysical Terahertz Large Area Survey. Out of 87 candidates with near-IR imaging, 15 (∼17%) display clear near-IR lensing morphologies. We present near-IR lens models to reconstruct and recover basic rest-frame optical morphological properties of the background galaxies from 12 new systems. Sources with the largest near-IR magnification factors also tend to be the most compact, consistent with the size bias predicted from simulations and previous lensing models for submillimeter galaxies (SMGs). For four new sources that also have high-resolution submillimeter maps, we test for differential lensing between the stellar and dust components and find that the 880 μm magnification factor (μ{sub 880}) is ∼1.5 times higher than the near-IR magnification factor (μ{sub NIR}), on average. We also find that the stellar emission is ∼2 times more extended in size than dust. The rest-frame optical properties of our sample of Herschel-selected lensed SMGs are consistent with those of unlensed SMGs, which suggests that the two populations are similar.

  5. Attenuation of near-IR light through dentin at wavelengths from 1300-1650-nm

    NASA Astrophysics Data System (ADS)

    Chan, Andrew C.; Darling, Cynthia L.; Chan, Kenneth H.; Fried, Daniel

    2014-02-01

    Light scattering in dental enamel decreases markedly from the UV to the near-IR and recent studies employing near-IR transillumination and reflectance imaging including optical coherence tomography indicate that this wavelength region is ideally suited for imaging dental caries due to the high transparency of enamel. The opacity of dentin is an important factor in optimizing the contrast of demineralization in reflectance measurements. It also influences the contrast of occlusal lesions in transillumination. Light scattering in dentin is an order of magnitude larger than in enamel, it is highly anisotropic and has a different spectral light scattering dependence than enamel. The objective of this study was to measure the optical attenuation of near-IR light through dentin at near-IR wavelengths from 1300-1650-nm. In this study the collimated transmission of near-IR light through polished thin sections of dentin of 0.05 to 0.6 mm thickness was measured. Beer-Lambert plots show that the attenuation coefficients range in magnitude from 20 to 40 cm-1. Attenuation increased significantly with increasing wavelength and the increases were not entirely consistent with increased water absorption.

  6. Assessment of the remineralization in simulated enamel lesions via dehydration with near-IR reflectance imaging

    NASA Astrophysics Data System (ADS)

    Lee, Robert C.; Darling, Cynthia L.; Fried, Daniel

    2015-02-01

    Previous studies have demonstrated that near-IR imaging can be used to nondestructively monitor the severity of enamel lesions. Arrested lesions typically have a highly mineralized surface layer that reduces permeability and limits diffusion into the lesion. The purpose of this study was to investigate whether the rate of water loss correlates with the degree of remineralization using near-IR reflectance imaging. Artificial bovine (n=15) enamel lesions were prepared by immersion in a demineralization solution for 24 hours and they were subsequently placed in an acidic remineralization solution for different periods. The samples were dehydrated using an air spray for 30 seconds and surfaces were imaged using an InGaAs camera at 1300-1700 nm wavelengths. Near-IR reflectance intensity differences before and after dehydration decreased with longer periods of remineralization. This study demonstrated that near-IR reflectance imaging was suitable for the detection of remineralization in simulated caries lesions and near-IR wavelengths longer than 1400 nm are well suited for the assessment of remineralization.

  7. Transition Metal Dithiolene Near-IR Dyes and Thier Applications in Liquid Crystal Devices

    SciTech Connect

    Marshall, K.L.; Painter, G.; Lotito, K.; Noto, A.G.; Chang, P.

    2006-08-18

    Numerous commercial and military applications exist for guest–host liquid crystal (LC) devices operating in the near- to mid-IR region. Progress in this area has been hindered by the severe lack of near-IR dyes with good solubility in the LC host, low impact on the inherent order of the LC phase, good thermal and chemical stability, and a large absorbance maximum tunable by structural modification over a broad range of the near-IR region. Transition metal complexes based on nickel, palladium, or platinum dithiolene cores show substantial promise in meeting these requirements. In this paper, we overview our past and present activities in the design and synthesis of transition metal dithiolene dyes, show some specific applications examples for these materials as near-IR dyes in LC electro-optical devices, and present our most recent results in the computational modeling of physical and optical properties of this interesting class of organometallic optical materials.

  8. Near-IR Fourier transform Raman spectroscopy in surgery and medicine: ophthalmic applications

    NASA Astrophysics Data System (ADS)

    Nie, Shuming; Yu, Nai-Teng; Ren, Qiushi

    1992-08-01

    This report describes the application of a recently developed spectroscopic technique, near- infrared-excited Fourier transform Raman scattering (abbreviated as near-IR FT-Raman) in the molecular-level characterization of normal and pathological human ocular tissues. The near-IR FT-Raman technique was shown to be particularly well-suited for the noninvasive analysis of intact ophthalmic samples because it exhibits such attractive features as complete fluorescence elimination, great sampling flexibility, high data acquisition speed, and measurement accuracy. For both intact human lenses and corneas, systematic FT-Raman studies were carried out in order to probe detailed molecular changes involved in cataract formation and cornea diseases. FT-Raman measurement was also made for synthetic biomaterials that can be attached to the corneal surface for laser refractive surgery. The technique of near-IR FT- Raman spectroscopy is potentially a nondestructive, non-invasive fingerprinting modality for monitoring lens aging, cataract formation, and corneal disease development.

  9. Near-IR fluorescence and reflectance confocal microscopy for imaging of quantum dots in mammalian skin

    PubMed Central

    Mortensen, Luke J.; Glazowski, Christopher E.; Zavislan, James M.; DeLouise, Lisa A.

    2011-01-01

    Understanding the skin penetration of nanoparticles (NPs) is an important concern due to the increasing presence of NPs in consumer products, including cosmetics. Technical challenges have slowed progress in evaluating skin barrier and NP factors that contribute to skin penetration risk. To limit sampling error and other problems associated with histological processing, many researchers are implementing whole tissue confocal or multiphoton microscopies. This work introduces a fluorescence and reflectance confocal microscopy system that utilizes near-IR excitation and emission to detect near-IR lead sulfide quantum dots (QDs) through ex vivo human epidermis. We provide a detailed prediction and experimental analysis of QD detection sensitivity and demonstrate detection of QD skin penetration in a barrier disrupted model. The unique properties of near-IR lead-based QDs will enable future studies that examine the impact of further barrier-disrupting agents on skin penetration of QDs and elucidate mechanistic insight into QD tissue interactions at the cellular level. PMID:21698023

  10. High Contrast Reflectance Imaging of Simulated Lesions on Tooth Occlusal Surfaces at Near-IR Wavelengths

    PubMed Central

    Fried, William A.; Fried, Daniel; Chan, Kenneth H.; Darling, Cynthia L.

    2015-01-01

    Introduction In vivo and in vitro studies have shown that high contrast images of tooth demineralization can be acquired in the near-infrared (near-IR) without the interference of stain. The purpose of this study is to compare the lesion contrast in reflectance at near-IR wavelengths coincident with high water absorption with those in the visible, the near-IR at 1,300 nm and with fluorescence measurements for early lesions in occlusal surfaces. Methods Twenty-four human molars were used in this in vitro study. Teeth were painted with an acid-resistant varnish, leaving a 4 × 4 mm window in the occlusal surface of each tooth exposed for demineralization. Artificial lesions were produced in the exposed windows after 1- and 2-day exposure to a demineralizing solution at pH 4.5. Lesions were imaged using near-IR reflectance at three wavelengths, 1,300, 1,460, and 1,600 nm using a high definition InGaAs camera. Visible light reflectance, and fluorescence with 405 nm excitation and detection at wavelengths greater than 500 nm were also used to acquire images for comparison. Crossed polarizers were used for reflectance measurements to reduce interference from specular reflectance. Results The contrast of both the 1- and 2-day lesions were significantly higher (P < 0.05) for near-IR reflectance imaging at 1,460 and 1,600 nm than it was for near-IR reflectance imaging at 1,300 nm, visible reflectance imaging, and fluorescence. Conclusion The markedly higher contrast at 1,460 and 1,600 nm wavelengths, coincident with higher water absorption, suggest that these wavelengths are better suited than 1,300 nm for imaging early/shallow demineralization on tooth surfaces. PMID:23857066

  11. Assessment of remineralization via measurement of dehydration rates with thermal and near-IR reflectance imaging

    PubMed Central

    Lee, Robert C.; Darling, Cynthia L.; Fried, Daniel

    2015-01-01

    Objectives Previous studies have demonstrated that the optical changes due to the loss of water from porous lesions can be exploited to assess lesion severity with QLF, thermal and near-IR imaging. Since arrested lesions are less permeable to water due to the highly mineralized surface layer, changes in the rate of water loss can be related to changes in lesion structure. The purpose of this study was to investigate whether the rate of water loss correlates with the degree of remineralization and whether that rate can be measured using thermal and near-IR reflectance imaging. Methods Artificial bovine enamel lesions (n=30) were prepared by immersion in a demineralization solution for either 8 and 24 hours and they were subsequently placed in an acidic remineralization solution for different periods. The samples were dehydrated using an air spray for 30 seconds and surfaces were imaged using a thermal camera and an InGaAs camera at 1300–1700 nm wavelengths. Results The area enclosed by the time-temperature curve, Δ Q, from thermal imaging showed significant differences (P<0.05) between the lesion window and other windows. Near-IR reflectance intensity differences, Δ I, before and after dehydration decreased with longer periods of remineralization. Only near-IR reflectance imaging was capable of detecting significant differences (P<0.05) between the different periods of remineralization. Conclusions This study demonstrated that both thermal and near-IR reflectance imaging were suitable for the detection of remineralization in simulated caries lesions and near-IR wavelengths longer than 1400 nm are well suited for the assessment of remineralization. PMID:25862275

  12. Near-IR spectroscopy of the eruptive variable source V2493 Cyg (HBC 722)

    NASA Astrophysics Data System (ADS)

    Lorenzetti, D.; Efimova, N.; Larionov, V.; Arkharov, A.; Gorshanov, D.; Giannini, T.; Antoniucci, S.; Di Paola, A.

    2012-05-01

    As part of our near-IR spectroscopic monitoring program of EXor pre-Main sequence variables (Lorenzetti et al. 2009 ApJ 693, 1056) on-going at the AZT24 1m IR telescope (Campo Imperatore, Italy), we have recently (2012 May 11) obtained a low resolution (R~250) near-IR spectrum (0.8 - 2.5 μm) of the outbursting source V2493 Cyg (otherwise called HBC 722). Since its outburst in August 2009 (Miller et al.

  13. Finland Becomes Eleventh ESO Member State

    NASA Astrophysics Data System (ADS)

    2004-07-01

    Finland has become the eleventh member state of the European Southern Observatory (ESO) [1]. The formal accession procedure was carried through as planned and has now been completed. Following the signing of the corresponding Agreement earlier this year (ESO PR 02/04), acceptance by the Finnish Parliament and ratification by the Finnish President of the Agreement as well as the ESO Convention and the associated protocols in June [2] and the deposit of the instruments of accession today, Finland has now officially joined ESO. ESO warmly welcomes the new member country and its scientific community that is renowned for their expertise in many frontline areas. The related opportunities will contribute to strenghtening of pioneering research with the powerful facilities at ESO's observatories, to the benefit of Astronomy and Astrophysics as well as European science in general. ESO also looks forward to collaboration with the Finnish high-tech industry. For Finland, the membership in ESO is motivated by scientific and technological objectives as well as by the objective of improving the public understanding of science. The Finnish Government is committed to increasing the public research funding in order to improve the quality, impact and internationalisation of research. Membership in ESO offers unique facilities for astronomical research which would not otherwise be available for Finnish astronomers. Finland is also very interested in taking part in technological development projects in fields like ICT, optics and instrumentation. For young scientists and engineers, ESO is a challenging, international working and learning environment. Finland has already taken part in the educational programmes of ESO, and as a member this activity will be broadened and intensified. In Finland there are also several science journalists and a large community of amateur astronomers who will be very happy to take part in ESO's outreach activities.

  14. The jet of the BL Lacertae object PKS 2201+044: MAD near-IR adaptive optics observations and comparison with optical, radio and X-ray data

    NASA Astrophysics Data System (ADS)

    Liuzzo, E.; Falomo, R.; Treves, A.; Donato, D.; Sambruna, M.; Arcidiacono, C.; Giovannini, G.; Farinato, J.; Moretti, A.; Ragazzoni, R.; Diolaiti, E.; Lombini, M.; Brast, R.; Donaldson, R.; Kolb, J.; Marchetti, E.; Tordo, S.

    2011-04-01

    Context. Relativistic jets are a common feature of radio loud active galactic nuclei. Multifrequency observations are a unique tool to constrain their physics. Aims: We report on a detailed study of the properties of the jet of the nearby BL Lac object PKS 2201+044, one of the rare cases where the jet is detected from radio to X-rays. Methods: We use new adaptive optics near-IR observations of the source, obtained with the ESO multi-conjugated adaptive optics demonstrator (MAD) at the Very Large Telescope. These observations acquired in Ground-Layer Adaptive Optics mode are combined with images previously achieved by HST, VLA and Chandra to perform a morphological and photometric study of the jet. Results: We find a noticeable similarity in the morphology of the jet at radio, near-IR and optical wavelengths. We construct the spectral shape of the main knot of jet that appears dominated by synchrotron radiation. Conclusions: On the basis of the jet morphology and the weak lines spectrum we suggest that PKS 2201+044 belongs to the class of radio sources intermediate between FRIs and FRIIs.

  15. Radio detection of the near-IR discovered supernova 2010P

    NASA Astrophysics Data System (ADS)

    Herrero-Illana, R.; Romero-Canizales, C.; Perez-Torres, M. A.; Alberdi, A.; Kankare, E.; Mattila, S.; Ryder, S. D.

    2012-09-01

    We report the radio detection of supernova 2010P (cf. CBETs 2145, 2149) in Arp 299 in EVLA (8459 MHz) observations from 15th Jun 2011. SN2010P was discovered in near-IR images on 18th Jan 2010, and classified as a Type Ib/IIb SN based on its optical spectrum obtained on 11th Feb 2010 (cf. CBET 2189).

  16. Electronic spectra of Fe3+ oxides and oxide hydroxides in the near IR to near UV.

    USGS Publications Warehouse

    Sherman, David M.; Waite, T.D.

    1985-01-01

    Optical absorption and diffuse reflectance spectra of several Fe2O3 and FeOOH polymorphs (hematite, maghemite, goethite, lepidocrocite) in the near-IR to near-UV spectral regions (2000-200 nm) are presented. The spectra consist primarily of Fe3+ ligand field and ligand-to-metal charge-transfer transitions.-J.A.Z.

  17. Mossbauer and spectral (visible and near-IR) data for Fe(3+)-substituted rutile

    NASA Technical Reports Server (NTRS)

    Lauer, H. V., Jr.; Morris, R. V.; Vempati, R. K.

    1994-01-01

    Titanohematite and rutile containing some Fe(3+) are possible highly oxidized weathering products of ilmenite and titanomagnetities. We report here Moessbauer and reflectivity data (visible and near-IR) for Fe(3+)-substituted rutile as a part of our continuing studies of ferric-substituted minerals that might have bearing on the interpretation of Martian spectral data.

  18. Near-IR polarization imaging of sound and carious dental enamel

    NASA Astrophysics Data System (ADS)

    Darling, Cynthia L.; Jiao, Jane J.; Lee, Chulsung; Kang, Hobin; Fried, Daniel

    2010-02-01

    A thorough understanding of how polarized near-IR light propagates through sound and carious dental hard tissues is important for the development of dental optical imaging systems. New optical imaging tools for the detection and assessment of dental caries (dental decay) such as near-IR imaging and optical coherence tomography can exploit the enhanced contrast provided by polarization sensitivity. In this investigation, an automated system was developed to collect images for the full 16-element Mueller Matrix. The polarized light was controlled by linear polarizers and liquid crystal retarders and the 36 images were acquired as the polarized near-IR light propagates through the enamel of extracted human thin tooth sections. In previous work, we reported that polarized light is rapidly depolarized by demineralized enamel, and sound and demineralized dentin.1 The rapid depolarization of polarized light by dental caries in the near-IR provides high contrast for caries imaging and detection. In this initial study, major differences in the Mueller matrix elements were observed in both sound and demineralized enamel which supports this approach and warrants further investigation.

  19. Near-IR Polarization Imaging of Sound and Carious Dental Enamel.

    PubMed

    Darling, Cynthia L; Jiao, Jane J; Lee, Chulsung; Kang, Hobin; Fried, Daniel

    2010-01-01

    A thorough understanding of how polarized near-IR light propagates through sound and carious dental hard tissues is important for the development of dental optical imaging systems. New optical imaging tools for the detection and assessment of dental caries (dental decay) such as near-IR imaging and optical coherence tomography can exploit the enhanced contrast provided by polarization sensitivity. In this investigation, an automated system was developed to collect images for the full 16-element Mueller Matrix. The polarized light was controlled by linear polarizers and liquid crystal retarders and the 36 images were acquired as the polarized near-IR light propagates through the enamel of extracted human thin tooth sections. In previous work, we reported that polarized light is rapidly depolarized by demineralized enamel, and sound and demineralized dentin.(1) The rapid depolarization of polarized light by dental caries in the near-IR provides high contrast for caries imaging and detection. In this initial study, major differences in the Mueller matrix elements were observed in both sound and demineralized enamel which supports this approach and warrants further investigation.

  20. Improved and Expanded Near-IR Oscillator Strengths for Ti I

    NASA Astrophysics Data System (ADS)

    Wood, Michael P.; Sneden, Chris; Nave, Gillian

    2016-01-01

    We report on recent work to produce an improved and expanded set of near-IR oscillator strengths for Ti I. Emission branching fractions are measured from several spectra recorded with the NIST 2-m FTS covering the region from 4000 Å to 5.5 μm. Traditionally, branching fractions are combined with level lifetimes measured using laser-induced fluorescence; however, this technique becomes problematic for near-IR oscillator strength studies. Instead, we employ thorough and robust reverse stellar analyses of the Sun and Arcturus to obtain lifetimes for new levels of interest. This work makes use of an extensive set of previously reported laboratory Ti I oscillator strengths in the visible to better understand uncertainties and check for systematic effects in the reverse stellar analyses. This method will soon be applied to other species to help address the scarcity of near-IR Fe-group atomic data and support the growing interests of the near-IR astronomical community.

  1. The Spectacular Radio-Near-IR-X-Ray Jet of 3C 111

    NASA Astrophysics Data System (ADS)

    Clautice, Devon; Perlman, Eric S.; Georganopoulos, Markos; Lister, Matthew L.; Tombesi, Francesco; Cara, Mihai; Marshall, Herman L.; Hogan, Brandon Scott; Kazanas, Demos

    2016-01-01

    Relativistic jets from active galactic nuclei (AGN) are powerful phenomena that transport prodigious amounts of energy and mass from the core of a galaxy out to kiloparsec or even megaparsec distances. While most spatially-resolved jets are seen in the radio, an increasing number have been discovered to emit in the optical/near-IR and/or X-ray bands. Here we discuss a spectacular example of this class, the 3C 111 jet, housed in one of the nearest, double-lobed FR II radio galaxies known. The jet itself extends over 100 kpc on each side, making it one of the longest to be seen in the radio, near-IR/optical and X-ray bands; its length and straight nature makes it ideal for studying jet physics over many kiloparsecs. We discuss new, deep Chandra and HST observations that reveal both near-IR and X-ray emission from several components of the 3C 111 jet, as well as both the approaching and receding hotspots. We also discuss new VLA observations of the jet. The near-IR and X-ray emission in the jet is restricted to several knots, and there are important differences between the morphologies seen in the radio, near-IR bands, and X-ray bands. We analyze the broad-band spectral energy distributions of the jet components. We compare competing models of emission as they relate to frequency-dependent relativistic beaming. Synchrotron emission seems to fit adequately the observed emissions of all knots and hotspots.

  2. Targeted near-IR QDs-loaded micelles for cancer therapy and imaging.

    PubMed

    Nurunnabi, Md; Cho, Kwang Jae; Choi, Joon Sig; Huh, Kang Moo; Lee, Yong-kyu

    2010-07-01

    The use of water-soluble, functionalized quantum dots (QDs) that are highly stable against oxidation for biological and biomedical applications is currently one of the fastest growing fields of nanotechnology. Polymer-based nanoparticles are now widely used for drug delivery and targeted therapy. We modified the surface of near Infrared QDs by the solid dispersion method using PEG-PCDA and PCDA-Herceptin conjugates to demonstrate water-solubility and target-specific properties. Upon UV irradiation, QD cores located within nanoprobes were further stabilized by intramicellar cross-linking between neighboring PCDA-Herceptin moieties. These cross-linked nanoprobes showed higher stability and less toxicity. Near-IR QDs-loaded micelles were spherical with diameters of around 130-150 nm. The anti-tumor effect of near-IR QDs-loaded micelles against MDA-MB-231 tumors was remarkably better than that of control. Mice treated with the near-IR QDs-loaded micelles had a tumor volume of about 285 mm(3), indicating shrinkage in initial tumor volume and inhibition of tumor growth by 77.3% compared to that of control group (saline injection). In addition, near-IR QDs-loaded micelles were injected intravenously into tumor-bearing nude mice for simultaneous tumor therapy and imaging. We observed that the targeted near-IR QDs-loaded micelles distributed rapidly throughout the animal body including the tumor in real time. These multi-functional nanoprobes could therefore be used for both active and passive targeting, imaging and treatment of cancers in the early stage. PMID:20409581

  3. The mid-IR and near-IR interferometry of AGNs: key results and their implications

    NASA Astrophysics Data System (ADS)

    Kishimoto, M.

    2015-09-01

    Infrared interferometry has been very productive in directly probing the structure of AGNs at sub-pc scales. With tens of objects already probed in the mid-IR and near-IR, I will summarize the key results and im- plications from this direct exploration. The Keck interferometry in the near-IR and VLTI in the mid-IR shaped the luminosity dependence of the torus size and structure, while the latter also revealed an equatorial structure at several Rsub (dust sublimation radius), and a polar-elongated region at a few tens of Rsub. Notably, this polar component seems to dominate the compact mid-IR flux. This component can persuasively be attributed to a polar outflow. However, interferometry, through emissivity estimations, also indicates that it is not a UV-optically-thin cloud but participating in the obscuration of the nucleus. I will discuss how to accommodate all these facts to build a consistent picture.

  4. Remote Sensing of Water Vapor and Thin Cirrus Clouds using MODIS Near-IR Channels

    NASA Technical Reports Server (NTRS)

    Gao, Bo-Cai; Kaufman, Yoram J.

    2001-01-01

    The Moderate Resolution Imaging Spectroradiometer (MODIS), a major facility instrument on board the Terra Spacecraft, was successfully launched into space in December of 1999. MODIS has several near-IR channels within and around the 0.94 micrometer water vapor bands for remote sensing of integrated atmospheric water vapor over land and above clouds. MODIS also has a special near-IR channel centered at 1.375-micron with a width of 30 nm for remote sensing of cirrus clouds. In this paper, we describe briefly the physical principles on remote sensing of water vapor and cirrus clouds using these channels. We also present sample water vapor images and cirrus cloud images obtained from MODIS data.

  5. Peripheral Substitution of a Near-IR-Absorbing Soluble Phthalocyanine Using "Click" Chemistry

    SciTech Connect

    Mayukh, Mayank; Lu, Chin-Wei; Hernandez, Edgardo; McGrath, Dominic V.

    2011-06-10

    A series of near-IR-absorbing soluble phthalocyanines (Pcs) with eight alkyne moieties as side chains of the chromophore have been synthesized. One of these Pcs has been used as a scaffold for functional group modification using alkyne–azide click chemistry with various azides. This led to a small library of Pcs with photo and thermal crosslinkable, dendritic, and hydrophilic moieties starting from a single Pc molecule. A patterned thin film was fabricated by photocrosslinking one of these Pc derivatives.

  6. Near-IR Image-Guided Laser Ablation of Demineralization on Tooth Occlusal Surfaces

    PubMed Central

    Tom, Henry; Chan, Kenneth H.; Darling, Cynthia L.; Fried, Daniel

    2016-01-01

    Introduction Studies have shown that reflectance images at near-IR wavelengths coincident with higher water absorption are well-suited for image-guided laser ablation of carious lesions since the contrast between sound and demineralized enamel is extremely high and interference from stains is minimized. The objective of this study was to demonstrate that near-IR reflectance images taken at a wavelength range of 1,500–1,700 nm can be used to guide a 9.3 μm CO2 laser for the selective ablation of early demineralization on tooth occlusal surfaces. Methods The occlusal surfaces of ten sound human molars were used in this in vitro study. Shallow simulated caries lesions with random patterns and varying depth and position were produced on tooth occlusal surfaces. Sequential near-IR reflectance images at 1,500–1,700 nm were used to guide the laser for the selective removal of the demineralized enamel. Digital microscopy and polarization sensitive optical coherence tomography (PS-OCT) were used to assess selectivity. Results Images taken before and after lesion removal suggest that the demineralized areas were removed with high selectivity. Although the estimated volume of tissue ablated was typically higher than the initial lesion volume measured with PS-OCT, the volume of enamel removed by the laser correlated well with the initial lesion volume. Conclusion Sequential near-IR reflectance images at 1,500–1,700 nm can be used to guide a 9.3 μm CO2 laser for the selective ablation of early demineralization on tooth occlusal surfaces. PMID:26763111

  7. Wavelength-agile near-IR optical parametric oscillator using a deposited silicon waveguide.

    PubMed

    Wang, Ke-Yao; Foster, Mark A; Foster, Amy C

    2015-06-15

    Using a deposited hydrogenated amorphous silicon (a-Si:H) waveguide, we demonstrate ultra-broad bandwidth (60 THz) parametric amplification via four-wave mixing (FWM), and subsequently achieve the first silicon optical parametric oscillator (OPO) at near-IR wavelengths. Utilization of the time-dispersion-tuned technique provides an optical source with active wavelength tuning over 42 THz with a fixed pump wave.

  8. Dramatic increase of the near-IR flux of the young source V2492 Cyg

    NASA Astrophysics Data System (ADS)

    Arkharov, A. A.; Lorenzetti, D.; Giannini, T.; Antoniucci, S.; Di Paola, A.; Vitali, F.; Larionov, V. M.

    2015-04-01

    In the framework of our EXor monitoring program dubbed EXORCISM (EXOR OptiCal and Infrared Systematic Monitoring - Antoniucci et al. 2013 PPVI, Lorenzetti et al. 2007 ApJ 665, 1182; Lorenzetti et al. 2009 ApJ 693, 1056), we are now observing a new increase of the near-IR brightness of the protostar V2492 Cyg, based on data taken at the AZT24 1m IR telescope (Campo Imperatore, Italy).

  9. The Near-IR Band Strengths of Molecules in N2 and H2O Ices

    NASA Astrophysics Data System (ADS)

    Richey, Christina; Gerakines, P. A.

    2008-09-01

    In order to determine the column density of an ice component, the band strength of an absorption feature must be known. The sizes of near-IR features can be correlated with a previously studied mid-IR feature whose band strength is already known. Molecules in mixtures may affect position, FWHM, shapes and intensities of absorption peaks, as well as band strength. Many satellites within the solar system have surfaces are dominated by either N2 or H2O (Review by Roush 2001). It has already been shown that for CH4 and CO isolated in N2 the peak positions will be shifted, and width and peak intensities will be altered in comparison to pure ice spectra (Quirico et al. 1999). The experiments here focus on changes in band strength, intensity, FWHM, and positioning for N2 mixed with CO, CO2, CH4, NH3, and H2O in 5:1 ratios and H2O mixed with CO, CO2, CH4, NH3, and N2 in 5:1 ratios and is a continuation of previous results published by the Astro- and Solar-System Program at UAB (Gerakines et. al. 2005). These data may be used to determine ice abundances from observed near-IR spectra or to predict the sizes of near-IR features in astrophysical environments.

  10. Multiplexed analysis using time-resolved near-IR fluorescence for the detection of genomic material

    NASA Astrophysics Data System (ADS)

    Stryjewski, Wieslaw J.; Soper, Steven A.; Lassiter, Suzzane; Davis, Lloyd M.

    2002-06-01

    While fluorescence continues to be an important tool in genomics, new challenges are being encountered due to increased efforts toward miniaturization reducing detection volumes and the need for screening multiple targets simultaneously. We have initiated work on developing time- resolved near-IR fluorescence as an additional tool for the multiplexed analyses of DNA, either for sequencing or mutation detection. We have fabricated simple and compact time-resolved fluorescence microscopes for reading fluorescence from electrophoresis or DNA microarrays. These microscopes consist of solid-state diode lasers and diode detectors and due to their compact size, the optical components and laser head can be mounted on high-speed micro-translational stages to read fluorescence from either multi-channel capillary electrophoresis instruments or micro fabricated DNA sorting devices. The detector is configured in a time-correlated single photon counting format to allow acquisition of fluorescence lifetimes on-the-fly during data acquisition in the limit of low counting statistics. In multiplexed analyses, lifetime discrimination serves as a method for dye-reporter identification using only a single readout channel. Also, coupled to multi-color systems, lifetime identification can significantly increase the number of probes monitored in a single instrument. In this work, near-IR fluorescence, including dye-labels and hardware, will be discussed as well as the implementation of near-IR fluorescence in DNA sequencing using slab gel electrophoresis and DNA microarrays.

  11. Spain to Join ESO

    NASA Astrophysics Data System (ADS)

    2006-03-01

    On 13 February, at a ceremony in Madrid, an agreement was signed by the Spanish Minister of Education and Science, Mrs. María Jesús San Segundo, and the ESO Director General, Dr. Catherine Cesarsky, affirming their commitment to securing Spanish membership of ESO.

  12. Near-IR and PS-OCT imaging of developmental defects in dental enamel

    NASA Astrophysics Data System (ADS)

    Hirasuna, Krista; Fried, Daniel; Darling, Cynthia L.

    2007-02-01

    Polarization sensitive optical coherence tomography (PS-OCT) and near-IR (NIR) imaging are promising new technologies under development for monitoring early carious lesions. Fluorosis is a growing problem in the U.S., and the more prevalent mild fluorosis can be visually mistaken for early enamel demineralization. Some initial NIR images suggest that enamel defects and dental caries manifest different optical behavior in the NIR. Unfortunately, there is little quantitative information available regarding the differences in optical properties of sound enamel, enamel developmental defects, and demineralized enamel due to caries. This study tested the hypothesis that hypomineralized enamel due to fluorosis can be differentiated from demineralized enamel due to caries using NIR and PS-OCT imaging because of different optical behavior in the NIR. Thirty extracted human teeth with various degrees of suspected fluorosis and/or caries were imaged using PS-OCT and NIR transillumination. An InGaAs camera and a near-IR diode laser were used to measure the optical attenuation through transverse tooth sections (~200 μm). Developmental defects were clearly visible in the polarization-resolved OCT images, demonstrating that PS-OCT can be used to nondestructively measure the depth and possible severity of the defects. Enamel defects on whole teeth that could be imaged with high contrast with visible light were transparent in the near-IR while demineralized areas due to caries were opaque. In contrast, dental caries could be clearly distinguished from sound enamel. This study suggests that PS-OCT and NIR methods may potentially be used as tools to assess the severity and extent of enamel defects and for the differentiation of mild fluorosis defects from early carious lesions.

  13. Theoretical Near-IR Spectra for Surface Abundance Studies of Massive Stars

    NASA Technical Reports Server (NTRS)

    Sonneborn, George; Bouret, J.

    2011-01-01

    We present initial results of a study of abundance and mass loss properties of O-type stars based on theoretical near-IR spectra computed with state-of-the-art stellar atmosphere models. The James Webb Space Telescope (JWST) will be a powerful tool to obtain high signal-to-noise ratio near-IR (1-5 micron) spectra of massive stars in different environments of local galaxies. Our goal is to analyze model near-IR spectra corresponding to those expected from NIRspec on JWST in order to map the wind properties and surface composition across the parameter range of 0 stars and to determine projected rotational velocities. As a massive star evolves, internal coupling, related mixing, and mass loss impact its intrinsic rotation rate. These three parameters form an intricate loop, where enhanced rotation leads to more mixing which in turn changes the mass loss rate, the latter thus affecting the rotation rate. Since the effects of rotation are expected to be much more pronounced at low metallicity, we pay special attention to models for massive stars in the the Small Magellanic Cloud. This galaxy provides a unique opportunity to probe stellar evolution, and the feedback of massive stars on galactic evol.ution in conditions similar to the epoch of maximal star formation. Plain-Language Abstract: We present initial results of a study of abundance and mass loss properties of massive stars based on theoretical near-infrared (1-5 micron) spectra computed with state-of-the-art stellar atmosphere models. This study is to prepare for observations by the James Webb Space Telescope.

  14. Finland to Join ESO

    NASA Astrophysics Data System (ADS)

    2004-02-01

    Finland will become the eleventh member state of the European Southern Observatory (ESO) [1]. Today, during a ceremony at the ESO Headquarters in Garching (Germany), a corresponding Agreement was signed by the Finnish Minister of Education and Science, Ms. Tuula Haatainen and the ESO Director General, Dr. Catherine Cesarsky, in the presence of other high officials from Finland and the ESO member states (see Video Clip 02/04 below). Following subsequent ratification by the Finnish Parliament of the ESO Convention and the associated protocols [2], it is foreseen that Finland will formally join ESO on July 1, 2004. Uniting European Astronomy ESO PR Photo 03/04 ESO PR Photo 03/04 Caption : Signing of the Finland-ESO Agreement on February 9, 2004, at the ESO Headquarters in Garching (Germany). At the table, the ESO Director General, Dr. Catherine Cesarsky, and the Finnish Minister of Education and Science, Ms. Tuula Haatainen . [Preview - JPEG: 400 x 499 pix - 52k] [Normal - JPEG: 800 x 997 pix - 720k] [Full Res - JPEG: 2126 x 2649 pix - 2.9M] The Finnish Minister of Education and Science, Ms. Tuula Haatainen, began her speech with these words: "On behalf of Finland, I am happy and proud that we are now joining the European Southern Observatory, one of the most successful megaprojects of European science. ESO is an excellent example of the potential of European cooperation in science, and along with the ALMA project, more and more of global cooperation as well." She also mentioned that besides science ESO offers many technological challenges and opportunities. And she added: "In Finland we will try to promote also technological and industrial cooperation with ESO, and we hope that the ESO side will help us to create good working relations. I am confident that Finland's membership in ESO will be beneficial to both sides." Dr. Catherine Cesarsky, ESO Director General, warmly welcomed the Finnish intention to join ESO. "With the accession of their country to ESO, Finnish

  15. Acousto-Optic Tunable Filter Spectroscopic Instrumentation for Quantitative Near-Ir Analysis of Organic Materials.

    NASA Astrophysics Data System (ADS)

    Eilert, Arnold James

    1995-01-01

    The utility of near-IR spectroscopy for routine quantitative analyses of a wide variety of compositional, chemical, or physical parameters of organic materials is well understood. It can be used for relatively fast and inexpensive non-destructive bulk material analysis before, during, and after processing. It has been demonstrated as being a particularly useful technique for numerous analytical applications in cereal (food and feed) science and industry. Further fulfillment of the potential of near-IR spectroscopic analysis, both in the process and laboratory environment, is reliant upon the development of instrumentation that is capable of meeting the challenges of increasingly difficult applications. One approach to the development of near-IR spectroscopic instrumentation that holds a great deal of promise is acousto-optic tunable filter (AOTF) technology. A combination of attributes offered by AOTF spectrometry, including speed, optical throughput, wavelength reproducibility, ruggedness (no -moving-parts operation) and flexibility, make it particularly desirable for numerous applications. A series of prototype (research model) acousto -optic tunable filter instruments were developed and tested in order to investigate the feasibility of the technology for quantitative near-IR spectrometry. Development included design, component procurement, assembly and/or configuration of the optical and electronic subsystems of which each functional spectrometer arrangement was comprised, as well as computer interfacing and acquisition/control software development. Investigation of this technology involved an evolution of several operational spectrometer systems, each of which offered improvements over its predecessor. Appropriate testing was conducted at various stages of development. Demonstrations of the potential applicability of our AOTF spectrometer to quantitative process monitoring or laboratory analysis of numerous organic substances, including food materials, were

  16. Bismuth-doped optical fibres: A new breakthrough in near-IR lasing media

    SciTech Connect

    Dianov, Evgenii M

    2012-09-30

    Recent results demonstrate that bismuth-doped optical fibres have considerable potential as near-IR active lasing media. This paper examines bismuth-doped fibres intended for the fabrication of fibre lasers and optical amplifiers and reviews recent results on the luminescence properties of various types of bismuth-doped fibres and the performance of bismuth-doped fibre lasers and optical amplifiers for the spectral range 1150 - 1550 nm. Problems are discussed that have yet to be solved in order to improve the efficiency of the bismuth lasers and optical amplifiers. (optical fibres, lasers and amplifiers. properties and applications)

  17. Reductant-free colloidal synthesis of near-IR emitting germanium nanocrystals: role of primary amine.

    PubMed

    Ghosh, Batu; Ogawara, Makoto; Sakka, Yoshio; Shirahata, Naoto

    2014-03-01

    High temperature colloidal synthesis without using hazardous reducing agent is demonstrated here to develop a straight forward pathway for synthesizing near-IR (NIR) light emitting germanium nanocrystals (Ge NCs). The NCs were prepared by heating a mixture of germanium (II) iodide and organoamine. This article presents an important role of the primary amine which serves as a reducing agent as well as an inhibitor against oxidation by comparing with the tertiary amine. Interestingly, the difference in chemical reactivity between each amine causes the difference in major structural phase of the products. An efficient route to produce NIR light emitting Ge NCs is demonstrated.

  18. Spain to Join ESO

    NASA Astrophysics Data System (ADS)

    2006-02-01

    Today, during a ceremony in Madrid, an agreement was signed by the Spanish Minister of Education and Science, Mrs. María Jesús San Segundo, and the ESO Director General, Dr. Catherine Cesarsky, affirming their commitment to securing Spanish membership of ESO. ESO PR Photo 05a/06 ESO PR Photo 05a/06 Signature Event in Madrid Following approval by the Spanish Council of Ministers and the ratification by the Spanish Parliament of the ESO Convention and the associated protocols, Spain intends to become ESO's 12th member state on 1 July 2006. "Since long Spain was aware that entering ESO was a logical decision and it was even necessary for a country like Spain because Spain is ranked 8th in astrophysical research", said Mrs. María Jesús San Segundo. "The large scientific installations are not only necessary for research in different fields but are also partners and customers for hi-tech companies, helping to increase the funding of R&D." "Spanish Astronomy has made tremendous strides forward and we are delighted to welcome Spain as a new member of ESO. We very much look forward to working together with our excellent Spanish colleagues," said Dr. Cesarsky. "For ESO, the Spanish accession means that we can draw on the scientific and technological competences, some of them unique in Europe, that have been developed in Spain and, of course, for Europe the Spanish membership of ESO is an important milestone in the construction of the European Research Area." ESO PR Photo 05b/06 ESO PR Photo 05b/06 Signature Event in Madrid Indeed, Spain is an important member of the European astronomical community and has developed impressively over the last three decades, reaching maturity with major contributions in virtually all subjects of astronomy. In addition, Spain hosts, operates or owns a number of competitive facilities dedicated to foster astronomical research, among which the Observatorio del Roque de los Muchachos at La Palma, certainly the premier optical

  19. Tunable diode and fibre laser spectroscopy in the near-IR for measurement of gas parameters

    NASA Astrophysics Data System (ADS)

    Stewart, George; Johnstone, Walter; Arsad, Norhana; Duffin, Kevin

    2008-04-01

    There has been much research performed in recent years on tunable diode laser spectroscopy for detection of gases such as methane, carbon dioxide, acetylene, etc., which possess near-IR absorption lines. To attain adequate sensitivity with weak near-IR lines, wavelength modulation spectroscopy with phase-sensitive detection is normally employed. However injection current modulation of diode lasers produces both wavelength and amplitude modulation, with a phase shift dependent on the modulation frequency. This results in residual amplitude modulation on the output and in distortion of the harmonic signals derived from the absorption line. These are important issues for calibration and where it is desired to accurately recover the line-shape function in order to make simultaneous measurements of gas concentration, pressure or temperature in industrial applications. Here we discuss how calibration-free measurements may be obtained with diode lasers and explore the implications for fibre laser based systems for spectroscopy which conventionally employ thermal or piezoelectric tuning of the wavelength. In particular, we consider modulation techniques which may be applied to ring fibre lasers which use un-pumped erbium fibre as a saturable absorber to prevent mode-hopping or to DFB fibre lasers which use a short cavity with a Bragg grating to ensure single mode operation.

  20. Near-Ir Band Strengths of Molecules Diluted in N_2 and H_2O Ices

    NASA Astrophysics Data System (ADS)

    Richey, C. R.; Gerakines, P. A.

    2010-06-01

    In order to determine the column density of a component of an ice from its infrared absorption features, the strengths of these features must be known. The peak positions, widths, profiles, and strengths of a certain ice component's infrared absorption features are affected be the overall composition of the ice (Quirico et al. 1999). Many satellites within the solar system have surfaces that are dominated by either N_2 or H_2O (Roush 2001). The experiments presented here focus on the near -infrared absorption features of CO, CO_2, CH_4, and NH_3 (μ=10,000-4,000 cm1, λ=1-2.5 μm) and the effects of diluting these molecules in N_2 and H_2O ice (dilution of 5:1). This is a continuation of previous results published by the Astro- and Solar-System Program at UAB by Gerakines et al. (2005). These data may be used to determine ice abundances from observed near-IR spectra or to predict the sizes of near-IR features in astrophysical environments.

  1. Near-IR Band Strengths of Molecules Diluted in Nitrogen and Water Ices

    NASA Astrophysics Data System (ADS)

    Richey, Christina; Gerakines, P. A.

    2010-10-01

    In order to determine the column density of a component of an ice from its infrared absorption features, the strengths of these features must be known. The peak positions, widths, profiles, and strengths of a certain ice component's infrared absorption features are affected be the overall composition of the ice (Quirico et al. 1999). Many satellites within the solar system have surfaces that are dominated by either N2 or H2O (Roush 2001). The experiments presented here focus on the near -infrared absorption features of CO, CO2, CH4, and NH3 (λ =10,000-4,000 cm-1, ν =1-2.5 μm) and the effects of diluting these molecules in N2 and H2O ice (dilution of 5:1). This is a continuation of previous results published by the Astro- and Solar-System Program at UAB by Gerakines et al. (2005). These data may be used to determine ice abundances from observed near-IR spectra or to predict the sizes of near-IR features in astrophysical environments.

  2. Near-IR spectroscopic imaging for skin hydration: the long and the short of it.

    PubMed

    Attas, E Michael; Sowa, Michael G; Posthumus, Trevor B; Schattka, Bernhard J; Mantsch, Henry H; Zhang, Shuliang L

    2002-01-01

    Near-IR spectroscopic methods have been developed to determine the degree of hydration of human skin in vivo. Noncontact reflectance spectroscopic imaging was used to investigate the distribution of skin moisture as a function of location. A human study in a clinical setting has generated quantitative data showing the effects of a drying agent and a moisturizer on delineated regions of the forearms of eight volunteers. Two digital imaging systems equipped with liquid-crystal tunable filters were used to collect stacks of monochromatic images at 10-nm intervals over the 650-1050 and 960-1700 nm wavelength bands. Synthetic images generated from measurements of water absorption band areas at three different near-IR wavelengths (970, 1200, and 1450 nm) showed obvious differences in the apparent distribution of water in the skin. Changes resulting from the skin treatments were much more evident in the long-wavelength images than in the short-wavelength ones. The variable sensitivity of the method at different wavelengths has been interpreted as being the result of different penetration depths of the IR light used in the reflectance studies.

  3. Improved and Expanded Near-IR Oscillator Strengths for Fe-group Elements

    NASA Astrophysics Data System (ADS)

    Wood, Michael P.; Nave, Gillian

    2015-01-01

    The use of modern experimental techniques, including LIF lifetime and FTS branching fraction measurements, has significantly increased the scope and reliability of laboratory atomic transition probabilities in the UV and visible. However, the combination of these techniques is problematic in the IR, a region of increasing importance due to improved detector, spectrometer, and telescope technologies. The result is a significant gap between the capabilities to record new IR astronomical spectra and the data needed to sufficiently understand and analyze them. To aid in closing this gap, we are developing new laboratory techniques to measure improved and expanded sets of oscillator strengths in the near-IR (λ ≈ 1-5 μm), with a primary focus on the Fe-group elements. A description of the methods proposed and their applicability will be presented. Input from the astronomical community is essential in order to focus the research on those lines and atomic species representing the greatest near-IR atomic data needs.

  4. Near-IR Spectral Variability Of Young Stars: A Multi-year Survey

    NASA Astrophysics Data System (ADS)

    Hawkins, Clint; Eisner, J.; Rudolph, A. L.

    2012-01-01

    T-Tauri type stars exhibit variability across the electromagnetic spectrum, including in the visible and the infrared regions. While spectroscopic variability in the optical range has been previously investigated, variability in the near-IR has not been explored as thoroughly. We have been tracking the spectral variability of about 40 young stars in the near-IR during the past year. Using the 90-inch Bok telescope on Kitt Peak, we observed our sample with FSPEC during four five-night runs, two in 2010 separated by one month and two in 2011, also separated by one month. Here we present spectra for each of these epochs that show emission from the Brackett Gamma (BrG) transition of hydrogen. Changes in the BrG line profile from epoch to epoch are used to constrain the properties of accretion onto our young star targets as a function of time. We acknowledge the NSF for funding under Award No. AST-0847170, a PAARE Grant for the Calfornia-Arizona Minority Partnership for Astronomy Research and Education (CAMPARE).

  5. ESO Presentation in Copenhagen

    NASA Astrophysics Data System (ADS)

    Madsen, C.; D'Odorico, S.

    2004-12-01

    On November 8, ESO continued its series of presentations in memberstates with an event in Copenhagen. So far events have been organised in Belgium, Finland, Portugal, Sweden, Switzerland and the United Kingdom. The purpose of these presentations is to raise the awareness of ESO amongst decision-makers, academia and the media. Over time, the scope and specific focus of the national events have varied, considering the particular circumstances and the wishes of the national hosts, and accordingly, the presentation in Denmark was primarily oriented towards industry. The meeting was initiated by the Royal Danish Consulate General in Munich in conjunction with the Confederation of Danish Industries and the Ministry for Science, Technology and Innovation. Leading up to the meeting, several articles about ESO had appeared in the Danish press and the 2nd TV Channel featured a report on the ESO projects also in connection with the event.

  6. The ESO Telescope bibliography at your fingertips

    NASA Astrophysics Data System (ADS)

    Grothkopf, Uta; Meakins, Silvia

    2012-09-01

    Bibliometric studies have become increasingly important in evaluating individual scientists, specific facilities, and entire observatories. The ESO Library has developed and maintains the Telescope Bibliography (telbib), a database of refereed papers that use observational data generated by ESO's facilities. Recently, a new public interface has been released. In addition to classical queries for bibliographic and facility-related information, it provides advanced features like faceted searches and filtering, autosuggest support for author, bibcode and program ID searches, hit highlighting as well as recommendations for other papers of possible interest. An additional tool offers the possibility to create graphical statistics on the fly based on user-defined criteria. The ESO Telescope Bibliography is available at http://telbib.eso.org/.

  7. Current Discussions Between ESO and Chile

    NASA Astrophysics Data System (ADS)

    1995-04-01

    the litigation in Chilean courts about the ownership of the Paranal lands, has repeatedly expressed that the European Organisation is not party of the juridical proceedings. At the same time, the Chilean Government has assured ESO that it will attempt to arrive in the shortest possible time at a solution which definitively resolves the question of ownership and enables ESO to continue its activities at Paranal and all its properties in Chile, without external interference of any type. Concerning ESO's juridical immunity on all of the territory of Chile, the Government of Chile has indicated to ESO that these immunities are clearly stipulated in the 1963 Convention and that it is applicable to all properties and possessions of the Organisation, wherever they are located in Chile. Those properties, according to the Convention, should only be used by the Organisation in Chile for scientific and official purposes. In this spirit of good will and cooperation with the Government and the people of Chile, ESO has expressed its inclination to begin a dialogue with the appropriate Chilean authorities about the use of a major part of its property around Cerro Paranal for activities of scientific character or any others that do not adversely influence the astronomical quality of this site. The Government of Chile and ESO wish to express publicly their desire to continue to work towards the resolution of common problems in a spirit of mutual respect and full collaboration. The signing of this Supplementary, Interpretative and Amending Agreement initiates a new era of relations between Chile and ESO in the conviction that the Chilean and European scientific communities will henceforth share the important scientific discoveries which will be done with the VLT facility at Cerro Paranal. How to obtain ESO Press Information ESO Press Information is made available on the World-Wide Web (URL: http://www.eso.org../). ESO Press Photos may be reproduced, if credit is given to the European

  8. Video rate imaging at 1.5 THz via frequency upconversion to the near-IR

    NASA Astrophysics Data System (ADS)

    Tekavec, Patrick F.; Kozlov, Vladimir G.; McNee, Ian; Lee, Yun-Shik; Vodopyanov, Konstantin

    2015-05-01

    We demonstrate video rate THz imaging in both reflection and transmission by frequency upconverting the THz image to the near-IR. In reflection, the ability to resolve images generated at different depths is shown. By mixing the THz pulses with a portion of the fiber laser pump (1064 nm) in a quasi-phase matched gallium arsenide crystal, distinct sidebands are observed at 1058 nm and 1070 nm, corresponding to sum and difference frequency generation of the pump pulse with the THz pulse. By using a polarizer and long pass filter, the strong pump light can be removed, leaving a nearly background free signal at 1070 nm. We have obtained video rate images with spatial resolution of 1mm and field of view ca. 20 mm in diameter without any post processing of the data.

  9. Near-IR Two-Photon Fluorescent Sensor for K(+) Imaging in Live Cells.

    PubMed

    Sui, Binglin; Yue, Xiling; Kim, Bosung; Belfield, Kevin D

    2015-08-19

    A new two-photon excited fluorescent K(+) sensor is reported. The sensor comprises three moieties, a highly selective K(+) chelator as the K(+) recognition unit, a boron-dipyrromethene (BODIPY) derivative modified with phenylethynyl groups as the fluorophore, and two polyethylene glycol chains to afford water solubility. The sensor displays very high selectivity (>52-fold) in detecting K(+) over other physiological metal cations. Upon binding K(+), the sensor switches from nonfluorescent to highly fluorescent, emitting red to near-IR (NIR) fluorescence. The sensor exhibited a good two-photon absorption cross section, 500 GM at 940 nm. Moreover, it is not sensitive to pH in the physiological pH range. Time-dependent cell imaging studies via both one- and two-photon fluorescence microscopy demonstrate that the sensor is suitable for dynamic K(+) sensing in living cells. PMID:26258885

  10. Nd:AlN polycrystalline ceramics: A candidate media for tunable, high energy, near IR lasers

    NASA Astrophysics Data System (ADS)

    Wieg, A. T.; Grossnickle, M. J.; Kodera, Y.; Gabor, N. M.; Garay, J. E.

    2016-09-01

    We present processing and characterization of Nd-doped aluminum nitride (Nd:AlN) polycrystalline ceramics. We compare ceramics with significant segregation of Nd to those exhibiting minimal segregation. Spatially resolved photoluminescence maps reveal a strong correlation between homogeneous Nd doping and spatially homogeneous light emission. The spectroscopically resolved light emission lines show excellent agreement with the expected Nd electronic transitions. Notably, the lines are significantly broadened, producing near IR emission (˜1077 nm) with a remarkable ˜100 nm bandwidth at room temperature. We attribute the broadened lines to a combination of effects: multiple Nd-sites, anisotropy of AlN and phonon broadening. These broadened, overlapping lines in a media with excellent thermal conductivity have potential for Nd-based, tunable lasers with high average power.

  11. Transillumination and reflectance probes for in vivo near-IR imaging of dental caries

    NASA Astrophysics Data System (ADS)

    Simon, Jacob C.; Lucas, Seth A.; Staninec, Michal; Tom, Henry; Chan, Kenneth H.; Darling, Cynthia L.; Fried, Daniel

    2014-02-01

    Previous studies have demonstrated the utility of near infrared (NIR) imaging for caries detection employing transillumination and reflectance imaging geometries. Three intra-oral NIR imaging probes were fabricated for the acquisition of in vivo, real time videos using a high definition InGaAs SWIR camera and near-IR broadband light sources. Two transillumination probes provide occlusal and interproximal images using 1300-nm light where water absorption is low and enamel manifests the highest transparency. A third reflectance probe utilizes cross polarization and operates at >1500-nm, where water absorption is higher which reduces the reflectivity of sound tissues, significantly increasing lesion contrast. These probes are being used in an ongoing clinical study to assess the diagnostic performance of NIR imaging for the detection of caries lesions in teeth scheduled for extraction for orthodontic reasons.

  12. Near-IR brightening of the blazar CTA 102 (2230+114) observed by the GASP

    NASA Astrophysics Data System (ADS)

    Carnerero, M. I.; Acosta-Pulido, J. A.; Arevalo, M. J.; Bueno, A.; Gonzalez, A. I.; Puerto-Gimenez, I.; Raiteri, C. M.; Villata, M.; GASP Collaboration

    2012-06-01

    The GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT) reports on the recent observation of a strong near-IR brightening of the gamma-loud quasar CTA 102. This is one of the 28 blazars for which the GASP performs a long-term, multiwavelength monitoring. Observations performed at the Teide Observatory on 2012 June 5.2 UT revealed J = 14.02 +/- 0.02, H = 13.19 +/- 0.02, and Ks = 12.36 +/- 0.02, compared to J = 15.42 +/- 0.04, H = 14.99 +/- 0.04, and Ks = 14.30 +/- 0.06 measured on 2011 December 5.9 UT.

  13. EAGLE ISS: a modular twin-channel integral-field near-IR spectrograph

    NASA Astrophysics Data System (ADS)

    Hastings, Peter; Stobie, Brian; Vivès, Sébastien; Vola, Pascal; Wells, Martyn; Evans, Christopher

    2010-07-01

    The ISS (Integral-field Spectrograph System) has been designed as part of the EAGLE Phase A Instrument Study for the E-ELT. It consists of two input channels of 1.65x1.65 arcsec field-of-view, each reconfigured spatially by an imageslicing integral-field unit to feed a single near-IR spectrograph using cryogenic volume-phase-holographic gratings to disperse the image spectrally. A 4k x 4k array detector array records the dispersed images. The optical design employs anamorphic magnification, image slicing, VPH gratings scanned with a novel cryo-mechanism and a three-lens camera. The mechanical implementation features IFU optics in Zerodur, a modular bench structure and a number of highprecision cryo-mechanisms.

  14. Measurement and compensation of laser-induced wavefront deformations and focal shifts in near IR optics.

    PubMed

    Stubenvoll, Martin; Schäfer, Bernd; Mann, Klaus

    2014-10-20

    We demonstrate the feasibility of passive compensation of the thermal lens effect in fused silica optics, placing suitable optical materials with negative dn/dT in the beam path of a high power near IR fiber laser. Following a brief overview of the involved mechanisms, photo-thermal absorption measurements with a Hartmann-Shack sensor are described, from which coefficients for surface/coating and bulk absorption in various materials are determined. Based on comprehensive knowledge of the 2D wavefront deformations resulting from absorption, passive compensation of thermally induced aberrations in complex optical systems is possible, as illustrated for an F-Theta objective. By means of caustic measurements during high-power operation we are able to demonstrate a 60% reduction of the focal shift in F-Theta lenses through passive compensation.

  15. Near-IR Two-Photon Fluorescent Sensor for K(+) Imaging in Live Cells.

    PubMed

    Sui, Binglin; Yue, Xiling; Kim, Bosung; Belfield, Kevin D

    2015-08-19

    A new two-photon excited fluorescent K(+) sensor is reported. The sensor comprises three moieties, a highly selective K(+) chelator as the K(+) recognition unit, a boron-dipyrromethene (BODIPY) derivative modified with phenylethynyl groups as the fluorophore, and two polyethylene glycol chains to afford water solubility. The sensor displays very high selectivity (>52-fold) in detecting K(+) over other physiological metal cations. Upon binding K(+), the sensor switches from nonfluorescent to highly fluorescent, emitting red to near-IR (NIR) fluorescence. The sensor exhibited a good two-photon absorption cross section, 500 GM at 940 nm. Moreover, it is not sensitive to pH in the physiological pH range. Time-dependent cell imaging studies via both one- and two-photon fluorescence microscopy demonstrate that the sensor is suitable for dynamic K(+) sensing in living cells.

  16. AOTF near-IR spectrometers for study of Lunar and Martian surface composition

    NASA Astrophysics Data System (ADS)

    Korablev, O.; Kiselev, A.; Vyazovetskiy, N.; Fedorova, A.; Evdokimova, N.; Stepanov, A.; Titov, A.; Kalinnikov, Y.; Kuzmin, R. O.; Bazilevsky, A. T.; Bondarenko, A.; Moiseev, P.

    2013-09-01

    The series of the AOTF near-IR spectrometers is developed in Moscow Space Research Institute for study of Lunar and Martian surface composition in the vicinity of a lander or a rover. Lunar Infrared Spectrometer (LIS) is an experiment onboard Luna-Glob (launch in 2015) and Luna-Resurs (launch in 2017) Russian surface missions. The LIS is mounted on the mechanic arm of landing module in the field of view (45°) of stereo TV camera. Infrared Spectrometer for ExoMars (ISEM) is an experiment onboard ExoMars (launch in 2018) ESARoscosmos rover. The ISEM instrument is mounted on the rover's mast together with High Resolution camera (HRC). Spectrometers will provide measurements of selected surface area in the spectral range of 1.15-3.3 μm. The electrically commanded acousto-optic filter scans sequentially at a desired sampling, with random access, over the entire spectral range.

  17. Near-IR Electrochromism in Electrodeposited Thin Films of Cyclometalated Complexes.

    PubMed

    Ionescu, Andreea; Aiello, Iolinda; La Deda, Massimo; Crispini, Alessandra; Ghedini, Mauro; De Santo, Maria Penelope; Godbert, Nicolas

    2016-05-18

    Homogeneous thin films of controlled thickness obtained from cyclometalated complexes of general formula [(C(∧)N)M(O(∧)N)], where M = Pd(II) or Pt(II), H(C(∧)N) = 2-phenylpyridine and, respectively, 2-thienylpyridine and H(O(∧)N) = a triphenylamine functionalized Schiff base, have been deposited by oxidative electropolymerization. The films have been electrochemically and morphologically characterized. The metallopolymeric thin films present stable reversible redox behavior and typical cauliflower-like textures in agreement with a nucleation-growth electropolymerization mechanism. However, the film growth is greatly influenced by the nature of the metal center, with a higher tendency of the Pt complexes to promote the 3D growth. Furthermore, a complete spectroelectrochemical study has been performed on electrodeposited films showing near-IR absorption in the oxidized state, high contrast ratios (up to 65%) and low response times.

  18. Near-IR Electrochromism in Electrodeposited Thin Films of Cyclometalated Complexes.

    PubMed

    Ionescu, Andreea; Aiello, Iolinda; La Deda, Massimo; Crispini, Alessandra; Ghedini, Mauro; De Santo, Maria Penelope; Godbert, Nicolas

    2016-05-18

    Homogeneous thin films of controlled thickness obtained from cyclometalated complexes of general formula [(C(∧)N)M(O(∧)N)], where M = Pd(II) or Pt(II), H(C(∧)N) = 2-phenylpyridine and, respectively, 2-thienylpyridine and H(O(∧)N) = a triphenylamine functionalized Schiff base, have been deposited by oxidative electropolymerization. The films have been electrochemically and morphologically characterized. The metallopolymeric thin films present stable reversible redox behavior and typical cauliflower-like textures in agreement with a nucleation-growth electropolymerization mechanism. However, the film growth is greatly influenced by the nature of the metal center, with a higher tendency of the Pt complexes to promote the 3D growth. Furthermore, a complete spectroelectrochemical study has been performed on electrodeposited films showing near-IR absorption in the oxidized state, high contrast ratios (up to 65%) and low response times. PMID:27115248

  19. ATLAST Detector Needs for Direct Spectroscopic Biosignature Characterization in the Visible and Near-IR

    NASA Technical Reports Server (NTRS)

    Rauscher, Bernard J.; Bolcar, Matthew R.; Clampin, Mark; Domagal-Goldman, Shawn D.; McElwain, Michael W.; Moseley, S. H.; Stahle, Carl; Stark, Christopher C.; Thronson, Harley A.

    2015-01-01

    Are we alone? Answering this ageless question will be a major focus for astrophysics in coming decades. Our tools will include unprecedentedly large UV-Optical-IR space telescopes working with advanced coronagraphs and starshades. Yet, these facilities will not live up to their full potential without better detectors than we have today. To inform detector development, this paper provides an overview of visible and near-IR (VISIR; lambda = 0.4 - 1.8 micrometers) detector needs for the Advanced Technology Large Aperture Space Telescope (ATLAST), specifically for spectroscopic characterization of atmospheric biosignature gasses. We also provide a brief status update on some promising detector technologies for meeting these needs in the context of a passively cooled ATLAST.

  20. Measurement and compensation of laser-induced wavefront deformations and focal shifts in near IR optics.

    PubMed

    Stubenvoll, Martin; Schäfer, Bernd; Mann, Klaus

    2014-10-20

    We demonstrate the feasibility of passive compensation of the thermal lens effect in fused silica optics, placing suitable optical materials with negative dn/dT in the beam path of a high power near IR fiber laser. Following a brief overview of the involved mechanisms, photo-thermal absorption measurements with a Hartmann-Shack sensor are described, from which coefficients for surface/coating and bulk absorption in various materials are determined. Based on comprehensive knowledge of the 2D wavefront deformations resulting from absorption, passive compensation of thermally induced aberrations in complex optical systems is possible, as illustrated for an F-Theta objective. By means of caustic measurements during high-power operation we are able to demonstrate a 60% reduction of the focal shift in F-Theta lenses through passive compensation. PMID:25401572

  1. Vegetation assessment using a combination of visible, near-IR and thermal-IR AVHRR data

    NASA Technical Reports Server (NTRS)

    Whitehead, V. S.; Johnson, W.; Boatright, J.

    1985-01-01

    Twelve hour temperature difference (thermal inertia) maps generated by rectifying and registering ascending (day) passes and descending (night) passes of the NOAA-7 Advanced Very High Resolution Radiometer (AVHRR) are compared to vegetation index maps generated from the visible and near IR data from the day pass of that satellite. There appears to be significant and unique information concerning surface characteristics in the temperature difference data on the 1 km scale of the AVHRR. A scatter diagram is provided which shows the pattern of day-night temperature difference compared to vegetation index for irrigated agriculture, dry rangeland, lakes, wet areas and burned rangeland. A detailed description of the techniques employed to provide the day-night temperature maps is provided.

  2. Vegetation assessment using a combination of visible, near-IR, and thermal-IR AVHRR data

    NASA Technical Reports Server (NTRS)

    Whitehead, V. S.; Johnson, W. R.; Boatright, J. A.

    1986-01-01

    Twelve-hour temperature difference (thermal inertia) maps generated by rectifying and registering ascending (day) passes and descending (night) passes of the NOAA-7 Advanced Very High Resolution Radiometer (AVHRR) are compared to vegetation index maps generated from the visible and near IR data from the day pass of that satellite. There appears to be significant and unique information concerning surface characteristics in the temperature difference data on the 1-km scale of the AVHRR. A scatter diagram is provided which shows the pattern of day-night temperature difference compared to vegetation index for irrigated agriculture, dry rangeland, lakes, wet areas and burned rangeland. A detailed description of the techniques employed to provide the day-night temperature maps is provided.

  3. Near-IR Extragalactic Background Results from the Cosmic Infrared Background Experiment (CIBER)

    NASA Astrophysics Data System (ADS)

    Zemcov, Michael B.; CIBER

    2016-01-01

    The near IR extragalactic background light (EBL) encodes the integrated light production over cosmic history, so represents the total emission from all galaxies along the line of sight up to ancient first-light objects present during the epoch of reionization (EOR). This EOR emission necessarily comprises part of the background, and indeed a minimum level is required to supply enough photons to ionize the intergalactic medium, corresponding to an EBL brightness less than 1 nW m^-2 sr^-1, about one tenth of the integrated galactic light (IGL). In addition to emission from these IGL and EOR populations, low surface brightness tidal streams of stars stripped by gravitational interactions during galaxy formation at low redshifts, called intrahalo light (IHL), may also contribute a significant fraction of the EBL. Models for these components can be constrained both through direct photometric measurements, as well as the new technique of EBL anisotropy intensity mapping that takes advantage of the fact that the Zodiacal Light is spatially smooth while distant populations produce anisotropies with distinct spatial and spectral characteristics. This talk will present recent results from the Cosmic Infrared Background Experiment (CIBER), a sounding rocket borne payload designed to measure both the fluctuations and direct photometric emission of the extra-galactic background light. The anisotropy of the near-IR EBL suggests the presence of a bright component approximately as bright as the IGL component near 1 micron which we interpret as the aggregate emission from low-redshift IHL. New direct photometric measurements from CIBER's low resolution spectrometer will also be discussed.

  4. Near-IR-induced, UV-induced, and spontaneous isomerizations in 5-methylcytosine and 5-fluorocytosine.

    PubMed

    Lapinski, Leszek; Reva, Igor; Rostkowska, Hanna; Fausto, Rui; Nowak, Maciej J

    2014-03-20

    Monomeric 5-methylcytosine (5mCyt) and 5-fluorocytosine (5FCyt) were studied using the matrix-isolation method. In 5mCyt and 5FCyt, the most stable form, dominating in low-temperature matrixes, is the amino-hydroxy (AH) tautomer. For both compounds, irradiation of the matrixes with near-IR laser light or with broadband near-IR or mid-IR light induces interconversions between the two rotamers of tautomer AH. In addition, for matrixes kept in darkness, a spontaneous tunneling conversion of the higher-energy hydroxy conformer (with the OH group directed toward the N3 atom) into the lower-energy form (OH directed toward N1) was occurring, with half-life time of 70 min for 5mCyt and 127 min for 5FCyt. These tunneling processes are much faster than that found for unsubstituted cytosine, where the half-life time is more than 30 h. UV irradiation of 5mCyt (at 316 nm) led to phototautomeric conversion of the amino-oxo form into the amino-hydroxy tautomer. Another phototransformation induced by irradiation of 5mCyt at 316 nm was the cleavage of the C-N bond in the amino-oxo form, resulting in generation of the open-ring conjugated isocyanate product. Irradiation of 5mCyt at shorter waves (λ ≤ 310 nm) induced the syn-anti photoisomerization within the imino-oxo forms of the compound. For matrix-isolated 5FCyt, the amount of the amino-oxo form was very small (with respect to the amino-hydroxy tautomer), while the imino-oxo isomers were not detected at all.

  5. Transition metal dithiolene complexes as near-IR dyes for liquid crystal device applications

    NASA Astrophysics Data System (ADS)

    Marshall, Kenneth L.; Schudel, Benjamin; Lippa, Irene A.

    2003-12-01

    Both commercial and military applications (e.g. free-space IR communications and sensor protection) exist for guest-host LC devices operating in the near-to mid IR region. Progress in this area has been hindered by the severe lack of near IR dyes with good solubility in the LC host, low impact on the inherent order of the LC phase, good thermal and chemical stability, and a large absorbance maximum tunable by structural modification over a broad range of the near IR region. Transition metal complexes based on nickel, palladium, or platinum dithiolene cores show substantial promise in meeting these requirements. These new dye complexes are extraordinarily stable, possess liquid crystalline phases in their own right with the proper terminal functional groups, and can have melting points below room temperature. The latter property is especially significant for producing liquid crystal/dye mixtures with both high dye concentration and good resistance to phase separation. Because they are zerovalent, they can exhibit high solubility in LC hosts (up to 10% wt%). The absorbance maximum in these materials can range from 600 nm to 1500 nm, depending on structure. With enantiomerically-enriched terminal substituents, nickel dithiolenes can induce a chiral mesophase in a non-chiral nematic host. This finding opens the possibility of generating novel LC mixtures with two degrees of tunability- an electronic absorbance band tunable by synthesis, and a selective reflection band tunable by temperature or applied electric field. Such a materials system would be particularly advantageous in sensor protection for dealing with frequency-agile laser threats.

  6. Transition metal dithiolene complexes as near-IR dyes for liquid crystal device applications

    NASA Astrophysics Data System (ADS)

    Marshall, Kenneth L.; Schudel, Benjamin; Lippa, Irene A.

    2004-01-01

    Both commercial and military applications (e.g., free-space IR communications and sensor protection) exist for guest-host liquid crystal (LC) devices operating in the near- to mid-IR region. Progress in this area has been hindered by the severe lack of near-IR dyes with good solubility in the LC host, low impact on the inherent order of the LC phase, good thermal and chemical stability, and a large absorbance maximum tunable by structural modification over a broad range of the near-IR region. Transition metal complexes based on nickel, palladium, or platinum dithiolene cores show substantial promise in meeting these requirements. These new dye complexes are extraordinarily stable, possess liquid crystalline phases in their own right with the proper terminal functional groups, and can have melting points below room temperature. The latter property is especially significant for producing liquid crystal/dye mixtures with both high dye concentration and good resistance to phase separation. Because they are zerovalent, they can exhibit high solubility in LC hosts (up to 10 wt%). The λmax in these materials can range from 600 nm to 1600 nm, depending on structure. With enantiomerically enriched terminal substituents, nickel dithiolenes can induce a chiral mesophase in a nonchiral nematic host. This finding opens the possibility of generating novel LC mixtures with two degrees of tunability: an electronic absorbance band tunable by synthesis, and a selective reflection band tunable by temperature or applied electric field. Such a materials system would be particularly advantageous in sensor protection for dealing with frequency-agile laser threats.

  7. Real-time near-IR imaging of laser-ablation crater evolution in dental enamel

    NASA Astrophysics Data System (ADS)

    Darling, Cynthia L.; Fried, Daniel

    2007-02-01

    We have shown that the enamel of the tooth is almost completely transparent near 1310-nm in the near-infrared and that near-IR (NIR) imaging has considerable potential for the optical discrimination of sound and demineralized tissue and for observing defects in the interior of the tooth. Lasers are now routinely used for many applications in dentistry including the ablation of dental caries. The objective of this study was to test the hypothesis that real-time NIR imaging can be used to monitor laser-ablation under varying conditions to assess peripheral thermal and transient-stress induced damage and to measure the rate and efficiency of ablation. Moreover, NIR imaging may have considerable potential for monitoring the removal of demineralized areas of the tooth during cavity preparations. Sound human tooth sections of approximately 3-mm thickness were irradiated by a CO II laser under varying conditions with and without a water spray. The incision area in the interior of each sample was imaged using a tungsten-halogen lamp with band-pass filter centered at 131--nm combined with an InGaAs focal plane array with a NIR zoom microscope in transillumination. Due to the high transparency of enamel at 1310-nm, laser-incisions were clearly visible to the dentin-enamel junction and crack formation, dehydration and irreversible thermal changes were observed during ablation. This study showed that there is great potential for near-IR imaging to monitor laser-ablation events in real-time to: assess safe laser operating parameters by imaging thermal and stress-induced damage, elaborate the mechanisms involved in ablation such as dehydration, and monitor the removal of demineralized enamel.

  8. Near-IR spectroscopy of the highly inflated, hottest known Jupiter KOI-13.01

    NASA Astrophysics Data System (ADS)

    Zhao, Ming

    2013-10-01

    We propose to use the WFC3 IR-G141 grism to measure the near-IR dayside emission spectrum of the highly inflated, hottest known Jupiter KOI-13.01 via secondary eclipses. The A-type host star of KOI-13.01 has the highest temperature among all known hot Jupiter hosts, producing extreme irradiation and making the planet's atmosphere probably quite different from others'. It is therefore an extreme and unique target to test exoplanetary atmosphere models and observed correlation between thermal inversion and irradiation. The host star of KOI-13.01 has a companion of same brightness and spectral type at 1.2 arcsec. Because the two stars will be well-resolved by WFC3, the stellar companion provides a unique advantage to calibrate the common-mode systematics of the eclipse light curves, enabling high precision and high fidelity spectroscopy of the planet's dayside emission. The WFC3 observations will definitively determine the presence or absence of a thermal inversion in the planet's upper atmosphere by probing the water bands between 1.1 - 1.7 microns. When combined with the Kepler nightside thermal emission measurement in visible light, the near-IR spectroscopy from WFC3 will also help tightly constrain its albedo and heat transport efficiency. Furthermore, resolving the binary and measuring the secondary eclipses will allow us to definitively verify whether the brigher star is indeed the host of the planet. This study can only be done with HST because of the ultra-high precision requisite and the coverage of water bands unavailable from ground.

  9. Stimulus responsive nanogel with innate near IR fluorescent capability for drug delivery and bioimaging.

    PubMed

    Vijayan, Vineeth M; Shenoy, Sachin J; Victor, Sunita P; Muthu, Jayabalan

    2016-10-01

    A brighter, non toxic and biocompatible optical imaging agent is one of the major quests of biomedical research. Here in, we report a photoluminescent comacromer [PEG-poly(propylene fumarate)-citric acid-glycine] and novel stimulus (pH) responsive nanogel endowed with excitation wavelength dependent fluorescence (EDF) for combined drug delivery and bioimaging applications. The comacromer when excited at different wavelengths in visible region from 400nm to 640nm exhibits fluorescent emissions from 510nm to 718nm in aqueous condition. It has high Stokes shift (120nm), fluorescent lifetime (7 nanoseconds) and quantum yield (50%). The nanogel, C-PLM-NG, prepared with this photoluminescent comacromer and N,N-dimethyl amino ethylmethacrylate (DMEMA) has spherical morphology with particle size around 100nm and 180nm at pH 7.4 (physiological) and 5.5 (intracellular acidic condition of cancer cells) respectively. The studies on fluorescence characteristics of C-PLM NG in aqueous condition reveal large red-shift with emissions from 523nm to 700nm for excitations from 460nm to 600nm ascertaining the EDF characteristics. Imaging the near IR emission with excitation at 535nm was accomplished using cut-off filters. The nanogel undergoes pH responsive swelling and releases around 50% doxorubicin (DOX) at pH 5.5 in comparison with 15% observed at pH 7.4. The studies on in vitro cytotoxicity with MTT assay and hemolysis revealed that the present nanogel is non-toxic. The DOX-loaded C-PLM-NG encapsulated in Hela cells induces lysis of cancer cells. The inherent EDF characteristics associated with C-PLM NG enable cellular imaging of Hela cells. The studies on biodistribution and clearance mechanism of C-PLM-NG from the body of mice reveal bioimaging capability and safety of the present nanogel. This is the first report on a polymeric nanogel with innate near IR emissions for bioimaging applications.

  10. Serial removal of caries lesions from tooth occlusal surfaces using near-IR image-guided IR laser ablation

    PubMed Central

    Chan, Kenneth H.; Tom, Henry; Darling, Cynthia L.; Fried, Daniel

    2015-01-01

    Previous studies have established that caries lesions can be imaged with high contrast without the interference of stains at near-IR wavelengths greater than 1300-nm. It has been demonstrated that computer controlled laser scanning systems utilizing IR lasers operating at high pulse repetition rates can be used for serial imaging and selective removal of caries lesions. In this study, we report our progress towards the development of algorithms for generating rasterized ablation maps from near-IR reflectance images for the removal of natural lesions from tooth occlusal surfaces. An InGaAs camera and a filtered tungsten-halogen lamp producing near-IR light in the range of 1500–1700-nm were used to collect crosspolarization reflectance images of tooth occlusal surfaces. A CO2 laser operating at a wavelength of 9.3- μm with a pulse duration of 10–15-μs was used for image-guided ablation. PMID:25914499

  11. Serial removal of caries lesions from tooth occlusal surfaces using near-IR image-guided IR laser ablation

    NASA Astrophysics Data System (ADS)

    Chan, Kenneth H.; Tom, Henry; Darling, Cynthia L.; Fried, Daniel

    2015-02-01

    Previous studies have established that caries lesions can be imaged with high contrast without the interference of stains at near-IR wavelengths greater than 1300-nm. It has been demonstrated that computer controlled laser scanning systems utilizing IR lasers operating at high pulse repetition rates can be used for serial imaging and selective removal of caries lesions. In this study, we report our progress towards the development of algorithms for generating rasterized ablation maps from near-IR reflectance images for the removal of natural lesions from tooth occlusal surfaces. An InGaAs camera and a filtered tungsten-halogen lamp producing near-IR light in the range of 1500-1700-nm were used to collect crosspolarization reflectance images of tooth occlusal surfaces. A CO2 laser operating at a wavelength of 9.3- μm with a pulse duration of 10-15-μs was used for image-guided ablation.

  12. Photo-redox activated drug delivery systems operating under two photon excitation in the near-IR

    NASA Astrophysics Data System (ADS)

    Guardado-Alvarez, Tania M.; Devi, Lekshmi Sudha; Vabre, Jean-Marie; Pecorelli, Travis A.; Schwartz, Benjamin J.; Durand, Jean-Olivier; Mongin, Olivier; Blanchard-Desce, Mireille; Zink, Jeffrey I.

    2014-04-01

    We report the design and synthesis of a nano-container consisting of mesoporous silica nanoparticles with the pore openings covered by ``snap-top'' caps that are opened by near-IR light. A photo transducer molecule that is a reducing agent in an excited electronic state is covalently attached to the system. Near IR two-photon excitation causes inter-molecular electron transfer that reduces a disulfide bond holding the cap in place, thus allowing the cargo molecules to escape. We describe the operation of the ``snap-top'' release mechanism by both one- and two-photon activation. This system presents a proof of concept of a near-IR photoredox-induced nanoparticle delivery system that may lead to a new type of photodynamic drug release therapy.We report the design and synthesis of a nano-container consisting of mesoporous silica nanoparticles with the pore openings covered by ``snap-top'' caps that are opened by near-IR light. A photo transducer molecule that is a reducing agent in an excited electronic state is covalently attached to the system. Near IR two-photon excitation causes inter-molecular electron transfer that reduces a disulfide bond holding the cap in place, thus allowing the cargo molecules to escape. We describe the operation of the ``snap-top'' release mechanism by both one- and two-photon activation. This system presents a proof of concept of a near-IR photoredox-induced nanoparticle delivery system that may lead to a new type of photodynamic drug release therapy. Electronic supplementary information (ESI) available: ssNMR, UV-vis spectra of 2PNT, pXRD, synthesis of 2PNT. See DOI: 10.1039/c3nr06155h

  13. Stimulus responsive nanogel with innate near IR fluorescent capability for drug delivery and bioimaging.

    PubMed

    Vijayan, Vineeth M; Shenoy, Sachin J; Victor, Sunita P; Muthu, Jayabalan

    2016-10-01

    A brighter, non toxic and biocompatible optical imaging agent is one of the major quests of biomedical research. Here in, we report a photoluminescent comacromer [PEG-poly(propylene fumarate)-citric acid-glycine] and novel stimulus (pH) responsive nanogel endowed with excitation wavelength dependent fluorescence (EDF) for combined drug delivery and bioimaging applications. The comacromer when excited at different wavelengths in visible region from 400nm to 640nm exhibits fluorescent emissions from 510nm to 718nm in aqueous condition. It has high Stokes shift (120nm), fluorescent lifetime (7 nanoseconds) and quantum yield (50%). The nanogel, C-PLM-NG, prepared with this photoluminescent comacromer and N,N-dimethyl amino ethylmethacrylate (DMEMA) has spherical morphology with particle size around 100nm and 180nm at pH 7.4 (physiological) and 5.5 (intracellular acidic condition of cancer cells) respectively. The studies on fluorescence characteristics of C-PLM NG in aqueous condition reveal large red-shift with emissions from 523nm to 700nm for excitations from 460nm to 600nm ascertaining the EDF characteristics. Imaging the near IR emission with excitation at 535nm was accomplished using cut-off filters. The nanogel undergoes pH responsive swelling and releases around 50% doxorubicin (DOX) at pH 5.5 in comparison with 15% observed at pH 7.4. The studies on in vitro cytotoxicity with MTT assay and hemolysis revealed that the present nanogel is non-toxic. The DOX-loaded C-PLM-NG encapsulated in Hela cells induces lysis of cancer cells. The inherent EDF characteristics associated with C-PLM NG enable cellular imaging of Hela cells. The studies on biodistribution and clearance mechanism of C-PLM-NG from the body of mice reveal bioimaging capability and safety of the present nanogel. This is the first report on a polymeric nanogel with innate near IR emissions for bioimaging applications. PMID:27262258

  14. Near IR Spectral Mapping of Mars: Temperatures, Aerosols and CO2 Ice

    NASA Astrophysics Data System (ADS)

    Glenar, D. A.; Bjoraker, G.; Smith, M.; Pearl, J.; Blaney, D.; Hansen, G.; Klassen, D.

    2003-05-01

    We summarize recent progress derived from the analysis of near infrared long-slit, drift scan spectra of Mars acquired during the 2001 opposition, using the SpeX grating spectrometer at the NASA IRTF. Under stable observing conditions the drift-scan technique produces high spectral resolution, spectral image cubes (x-y-wavelength) with full hemispherical image content. This approach has previously been used in a study of the diurnal properties of aphelion season clouds (Glenar et al., Icarus, v161, 2003). Temperatures: At SpeX resolving power (R= 1200-1800), the spectral shape of the 2 micron gaseous CO2 absorption band is a sensitive function of temperature. This band thus serves as a low altitude atmospheric thermometer, since the reflectance (R) contribution function dR/dTj (j=layer) within this band mimics the pressure-height profile P(j). Least-squares fits to SpeX measurements using a set of reference opacity spectra allow measurements of temperature versus position in regions of low dust opacity. Dust Optical Depth: Near-IR dust optical depth can be measured by the extent to which it suppresses the 2 micron CO2 band shape. We have been evolving an IDL-based dust optical depth mapping algorithm which incorporates multi-stream scattering model computations (DISORT), and newly available dust radiative transfer parameters at these wavelengths. However, we presently observe large (20-30 discrepancies between CO2 surface pressures predicted by forcing this model to agree with measurements, and those predicted from Viking lander data with position corrections from the MOLA data set. This latter approach is routinely used as a boundary value for temperature retrievals by the TES team. CO2 Ice Parameters: Near-IR bidirectional reflectance spectra of the south polar CO2 ice cap has been modeled as a function of grain size and contamination by dust and water ice. These parameters are of direct importance to the cap thermal balance since they affect albedo and

  15. Axion Decay and Anisotropy of Near-IR Extragalactic Background Light

    NASA Astrophysics Data System (ADS)

    Gong, Yan; Cooray, Asantha; Mitchell-Wynne, Ketron; Chen, Xuelei; Zemcov, Michael; Smidt, Joseph

    2016-07-01

    The extragalactic background light (EBL) is composed of the cumulative radiation from all galaxies and active galactic nuclei over cosmic history. In addition to point sources, the EBL also contains information from diffuse sources of radiation. The angular power spectra of the near-infrared intensities could contain additional signals, and a complete understanding of the nature of the infrared (IR) background is still lacking in the literature. Here we explore the constraints that can be placed on particle decays, especially candidate dark matter (DM) models involving axions that trace DM halos of galaxies. Axions with a mass around a few electronvolts will decay via two photons with wavelengths in the near-IR band and will leave a signature in the IR background intensity power spectrum. Using recent power spectra measurements from the Hubble Space Telescope and the Cosmic Infrared Background Experiment, we find that the 0.6-1.6 μm power spectra can be explained by axions with masses around 4 eV. The total axion abundance Ω a ≃ 0.05, and it is comparable to the baryon density of the universe. The suggested mean axion mass and abundance are not ruled out by existing cosmological observations. Interestingly, the axion model with a mass distribution is preferred by the data, which cannot be explained by the standard quantum chromodynamics theory and needs further discussion.

  16. GFIT2: an experimental algorithm for vertical profile retrieval from near-IR spectra

    NASA Astrophysics Data System (ADS)

    Connor, Brian J.; Sherlock, Vanessa; Toon, Geoff; Wunch, Debra; Wennberg, Paul O.

    2016-08-01

    An algorithm for retrieval of vertical profiles from ground-based spectra in the near IR is described and tested. Known as GFIT2, the algorithm is primarily intended for CO2, and is used exclusively for CO2 in this paper. Retrieval of CO2 vertical profiles from ground-based spectra is theoretically possible, would be very beneficial for carbon cycle studies and the validation of satellite measurements, and has been the focus of much research in recent years. GFIT2 is tested by application both to synthetic spectra and to measurements at two Total Carbon Column Observing Network (TCCON) sites. We demonstrate that there are approximately 3° of freedom for the CO2 profile, and the algorithm performs as expected on synthetic spectra. We show that the accuracy of retrievals of CO2 from measurements in the 1.61μ (6220 cm-1) spectral band is limited by small uncertainties in calculation of the atmospheric spectrum. We investigate several techniques to minimize the effect of these uncertainties in calculation of the spectrum. These techniques are somewhat effective but to date have not been demonstrated to produce CO2 profile retrievals with sufficient precision for applications to carbon dynamics. We finish by discussing ongoing research which may allow CO2 profile retrievals with sufficient accuracy to significantly improve the scientific value of the measurements from that achieved with column retrievals.

  17. Axion Decay and Anisotropy of Near-IR Extragalactic Background Light

    NASA Astrophysics Data System (ADS)

    Gong, Yan; Cooray, Asantha; Mitchell-Wynne, Ketron; Chen, Xuelei; Zemcov, Michael; Smidt, Joseph

    2016-07-01

    The extragalactic background light (EBL) is composed of the cumulative radiation from all galaxies and active galactic nuclei over cosmic history. In addition to point sources, the EBL also contains information from diffuse sources of radiation. The angular power spectra of the near-infrared intensities could contain additional signals, and a complete understanding of the nature of the infrared (IR) background is still lacking in the literature. Here we explore the constraints that can be placed on particle decays, especially candidate dark matter (DM) models involving axions that trace DM halos of galaxies. Axions with a mass around a few electronvolts will decay via two photons with wavelengths in the near-IR band and will leave a signature in the IR background intensity power spectrum. Using recent power spectra measurements from the Hubble Space Telescope and the Cosmic Infrared Background Experiment, we find that the 0.6–1.6 μm power spectra can be explained by axions with masses around 4 eV. The total axion abundance Ω a ≃ 0.05, and it is comparable to the baryon density of the universe. The suggested mean axion mass and abundance are not ruled out by existing cosmological observations. Interestingly, the axion model with a mass distribution is preferred by the data, which cannot be explained by the standard quantum chromodynamics theory and needs further discussion.

  18. VizieR Online Data Catalog: Near-IR BN/KL outflow images (Bally+, 2015)

    NASA Astrophysics Data System (ADS)

    Bally, J.; Ginsburg, A.; Silvia, D.; Youngblood, A.

    2015-02-01

    The Gemini Multi-conjugate adaptive optics System (GeMS) at the Gemini South telescope on Cerro Pachon is the first and only sodium-based multi-laser guide star (LGS) adaptive optics system. GeMS works with a LGS constellation of 5-spots: 4 of the LGS spots are at the corners of a 60" square, with the 5-th positioned in the center. The Adaptive Optics (AO) bench called Canopus is mounted on one of the f/16 Cassegrain ports. Gemini South Adaptive Optics Imager (GSAOI) is a wide-field 4096 by 4096 pixel (85" by 85" field of view) camera designed to work at the diffraction limit of the 8- meter telescope in the near-infrared. Three 85" diameter fields were observed in OMC1 between 30 December 2012 and 28 February 2013 using GSAOI. Observations of each field were obtained through 1% bandpass narrow-band filters centered on the 1.644um [FeII] and 2.122um H2 emission lines and the broad-band Ks filter. The corrected images have FWHM diameters of 0.080" to 0.10", providing the highest angular resolution images of the BN/KL outflow ever obtained in the near-IR. (2 data files).

  19. Nondestructive Clinical Assessment of Occlusal Caries Lesions using Near-IR Imaging Methods

    PubMed Central

    Staninec, Michal; Douglas, Shane M.; Darling, Cynthia L.; Chan, Kenneth; Kang, Hobin; Lee, Robert C.; Fried, Daniel

    2011-01-01

    Objective Enamel is highly transparent in the near-IR (NIR) at wavelengths near 1300-nm, and stains are not visible. The purpose of this study was to use NIR transillumination and optical coherence tomography (OCT) to estimate the severity of caries lesions on occlusal surfaces both in vivo and on extracted teeth. Methods Extracted molars with suspected occlusal lesions were examined with OCT and polarization sensitive OCT (PS-OCT), and subsequently sectioned and examined with polarized light microscopy (PLM) and transverse microradiography (TMR). Teeth in test subjects with occlusal caries lesions that were not cavitated or visible on radiographs were examined using NIR transillumination at 1310 nm using a custom built probe attached to an indium gallium arsenide (InGaAs) camera and a linear OCT scanner. After imaging, cavities were prepared using dye staining to guide caries removal and physical impressions of the cavities were taken. Results The lesion severity determined from OCT and PS-OCT scans in vitro correlated with the depth determined using polarized light microscopy (PLM) and transverse microradiography (TMR). Occlusal caries lesions appeared in NIR images with high contrast in vivo. OCT scans showed that most of the lesions penetrated to dentin and spread laterally below the sound enamel. Conclusion This study demonstrates that both NIR transillumination and OCT are promising new methods for the clinical diagnosis of occlusal caries. PMID:22109697

  20. Design of a near-IR Doppler instrument for planet searches

    NASA Astrophysics Data System (ADS)

    Zhao, Bo; Ge, Jian; Nguyen, Duy Cuong; Wang, Ji; Groot, John

    2010-07-01

    Doppler searches are extending to the near infrared to detect and characterize habitable planets around low mass stars. We present an optical design and performance of a near-IR Doppler instrument. This instrument has two operating modes covering 0.8-1.8 microns. One mode is called IRET, which consists of a fix-delay interferometer and a crossdispersed echelle spectrograph to simultaneously cover 0.8-1.35 microns with a spectral resolution of R=22000 on a 2k x 2k H2RG IR array. The other mode is called FIRST, which uses a silicon immersion grating as the main disperser to simultaneously cover 1.4-1.8 microns with a spectral resolution of R=55000 on the same detector as IRET. The triplepass parabola white pupil design is used to restrain background scatter radiation with stable configuration for precision radial velocity measurements. We used high index standard glasses for camera optics and VPH gratings as crossdispersers in both modes. The FIRST mode can be switched in and out conveniently while the IRET mode is kept without moving parts to increase its stability. This instrument is designed to deliver up to 1 m/s Doppler precision RV measurements of nearby bright M dwarfs at the Apache Point Observatory 3.5 meter telescope. The instrument is expected to be operational in the spring 2011.

  1. Near-IR luminescent lanthanide complexes with 1,8-diaminoanthraquinone-based chromophoric ligands.

    PubMed

    Stacey, Oliver J; Ward, Benjamin D; Amoroso, Angelo J; Pope, Simon J A

    2016-04-21

    Three new chromophoric anthraquinone-based multidentate ligands have been synthesised in a step-wise manner from 1,8-dichloroanthraquinone. The ligands each comprise two dipicolyl amine units and react with trivalent lanthanide ions to form monometallic complexes of the form [Ln(L)](OTf)3 as indicated by MS studies and elemental analyses. Supporting DFT studies show that the monometallic species are highly favoured (>1000 kJ mol(-1)) over the formation of a 2 : 2 dimetallic congener. Both ligands and complexes absorb light efficiently (ε ∼ 10(4) M(-1) cm(-1)) in the visible part of the spectrum, with λabsca. 535-550 nm through an intramolecular charge transfer (ICT) transition localised on the substituted anthraquinone unit. In all cases the complexes show a fluorescence band at ca. 675 nm due to the ICT emitting state. The corresponding Nd(iii), Yb(iii) and Er(iii) complexes also reveal sensitised near-IR emission characteristic of each ion following excitation of the ICT visible absorption band at 535 nm. PMID:26974664

  2. ARCHONS: a highly multiplexed superconducting optical to near-IR camera

    NASA Astrophysics Data System (ADS)

    Mazin, Benjamin A.; O'Brien, Kieran; McHugh, Sean; Bumble, Bruce; Moore, David; Golwala, Sunil; Zmuidzinas, Jonas

    2010-07-01

    We report on the development of ARCONS, the ARray Camera for Optical to Near-IR Spectrophotometry. This photon counting integral field unit (IFU), being built at UCSB and Caltech with detectors fabricated at JPL, will use a unique, highly multiplexed low temperature detector technology known as Microwave Kinetic Inductance Detectors (MKIDs). These detectors, which operate at 100 mK, should provide photon counting with energy resolution of R = E/δE > 20 and time resolution of a microsecond, with a quantum efficiency of around 50%. We expect to field the instrument at the Palomar 200" telescope in the first quarter of 2011 with an array containing 1024 pixels in a 32×32 pixel form factor to yield a field of view of approximately 10×10 arcseconds. The bandwidth of the camera is limited by the rising sky count rate at longer wavelengths, but we anticipate a bandwidth of 0.35 to 1.35 μm will be achievable. A simple optical path and compact dewar utilizing a cryogen-free adiabatic demagnetization refridgerator (ADR) allows the camera to be deployed quickly at Naysmith or Coudé foci at a variety of telescopes. A highly expandable software defined radio (SDR) readout that can scale up to much larger arrays has been developed.

  3. Phthalocyanine dimerization-based molecular beacons using near-IR fluorescence.

    PubMed

    Nesterova, Irina V; Erdem, S Sibel; Pakhomov, Serhii; Hammer, Robert P; Soper, Steven A

    2009-02-25

    Herein we demonstrate the use of a novel dimerization-based molecular beacon (MB) probe consisting of two metallo-phthalocyanine (Pc) fluorophores that use near-IR fluorescence, appropriate for highly specific and sensitive in vivo and/or in vitro DNA/RNA detection. Pc's possess a propensity to form nonfluorescent H-dimers that is utilized as the molecular "off" switch in the closed MB conformation. The "on" switch, which is generated when the solution target binds to the loop of the MB forming the open form, also provides two fluorophores for transduction resulting in a doubling of the extinction coefficient and improving the resulting fluorescence yield compared to a classical single-fluorophore/quencher MB system. In addition, the Pc-based MBs possess high thermal, photo, and chemical stabilities that are essential for many highly sensitive applications, such as molecular imaging. The dimer-based MBs were obtained using a simple single-step synthesis procedure and demonstrated excellent quenching efficiencies (98%) as well as a high signal-to-background ratio (approximately 60) exceeding the performance characteristics of many conventionally available MB probes.

  4. AOTF near-IR spectrometers for study of Lunar and Martian surface composition

    NASA Astrophysics Data System (ADS)

    Ivanov, A.; Korablev, O.; Mantsevich, S.; Vyazovetskiy, N.; Fedorova, A.; Evdokimova, N.; Stepanov, A.; Titov, A.; Kalinnikov, Y.; Kuzmin, R.; Kiselev, A.; Bazilevsky, A.; Bondarenko, A.; Dokuchaev, I.; Moiseev, P.; Victorov, A.; Berezhnoy, A.; Skorov, Y.; Bisikalo, D.; Velikodsky, Y.

    2014-04-01

    The series of the AOTF near-IR spectrometers is developed in Moscow Space Research Institute for study of Lunar and Martian surface composition in the vicinity of a lander or a rover. Lunar Infrared Spectrometer (LIS) is an experiment onboard Luna-Glob (launch in 2017) and Luna- Resurs (launch in 2019) Russian surface missions. It's a pencil-beam spectrometer to be pointed by a robotic arm of the landing module. The instrument's field of view (FOV) of 1° is co-aligned with the FOV(45°) of a stereo TV camera. Infrared Spectrometer for ExoMars (ISEM) is an experiment onboard ExoMars (launch in 2018) ESARoscosmos rover. It's spectrometer based on LIS with required redesign for ExoMars mission. The ISEM instrument is mounted on the rover's mast coaligned with the FOV (5°) of High Resolution camera (HRC). Spectrometers and are intended for study of the surface composition in the vicinity of the lander and rover. The spectrometers will provide measurements of selected surface areas in the spectral range of 1.15-3.3 μm. The spectral selection is provided by acoustooptic tunable filter (AOTF), which scans the spectral range sequentially. Electrical command of the AOTF allows selecting the spectral sampling, and permits a random access if needed.

  5. Optical/near-IR surface photometry of blue low surface brightness galaxies

    NASA Astrophysics Data System (ADS)

    Bergvall, Nils; Rönnback, Jari; Masegosa, Josefa; Östlin, Göran

    1999-01-01

    We present luminosity profiles, colour profiles and disk parameters based on near-infrared JHK surface photometry of a sample of blue low surface brightness galaxies (BLSBGs). The results are discussed along with previously obtained optical data. We find that the morphological properties in optical and near-IR are quite similar. The luminosity profiles have exponential shapes modified by a small central bulge or, below $calM u_{B,0}\\sim23 magnitudes arcsec^{-2}$, a trough. The blue LSBGs have scalelengths intermediate between normal LSB disks and gas rich dwarf galaxies. A correlation between scalelength and B-V colour is found for LSBGs in general. In comparison with normal late type disk galaxies our galaxies are bluer and smaller. At the same B scalelength, the two types differ in luminosity with 2 magnitudes, corresponding to a difference in mean star formation rate of a factor 5-10. Several photometric properties indicate that they contain very little dust and that, at the lowest surface brightnesses, the stellar population is homogeneous.

  6. The Orion Fingers: Near-IR Spectral Imaging of an Explosive Outflow

    NASA Astrophysics Data System (ADS)

    Youngblood, Allison; Ginsburg, Adam; Bally, John

    2016-06-01

    We present near-IR (1.1-2.4 μm) position-position-velocity cubes of the 500 year old Orion BN/KL explosive outflow with spatial resolution 1″ and spectral resolution 86 km s-1. We construct integrated intensity maps free of continuum sources of 15 H2 and [Fe ii] lines while preserving kinematic information of individual outflow features. Included in the detected H2 lines are the 1-0 S(1) and 1-0 Q(3) transitions, allowing extinction measurements across the outflow. Additionally, we present dereddened flux ratios for over two dozen outflow features to allow for the characterization of the true excitation conditions of the BN/KL outflow. All of the ratios show the dominance of the shock excitation of the H2 emission, although some features exhibit signs of fluorescent excitation from stellar radiation or J-type shocks. We also detect tracers of the PDR/ionization front north of the Trapezium stars in [O i] and [Fe ii] and analyze other observed outflows not associated with the BN/KL outflow.

  7. Spectroscopic observations of the Uranus' satellite Miranda in Near-IR

    NASA Astrophysics Data System (ADS)

    Gourgeot, F.; Dumas, C.; Merlin, F.; Vernazza, P.; Alvarez-Candal, A.

    2013-09-01

    We present new Near-IR spectra of the Uranus' icy satellite Miranda. This body is probably the most remarkable of all satellites of Uranus, displaying series of surface features such as faults, craters and largescale upwelling, remnant of a geologically very active past. The observations were performed first at the Palomar Observatory with the PHARO instrument (Palomar High Angular Resolution Observer) and then at the Mauna Kea Observatory with SpeX instrument based on the IRTF (Infra-Red Telescope Facility). Water ice is clearly visible in K-band (large 2.0 μm absorption band) and crystalline water ice (at 1.65 μm) seems to cover the most part of the satellite's surface. We focused the study in H band on the 1.42-1.72 μm range at observations dates corresponding to the leading and trailing hemispheres of Miranda. Contrary to the other outer Uranus' moons (Grundy et al. 2006), we did not found any significative differences between both hemispheres in this spectral range. We also studied the possible presence of volatiles like ammonia hydrate and do not exclude the possible presence of a tiny 2.22 μm band yet observed by Bauer et al. 2002. No significant features of carbon dioxide were identified on any spectra. We performed spectral models, based on bi-hemispherical reflectance theory (Hapke 1993) in order to obtain more details on the chemical compounds possibly present on the surface of this Uranian satellite.

  8. Near-IR multi-modal imaging of natural occlusal lesions

    NASA Astrophysics Data System (ADS)

    Lee, Dustin; Fried, Daniel; Darling, Cynthia L.

    2009-02-01

    Reflectance and transillumination imaging show demineralization with high contrast in the near-IR. The objective of this study is to use lesion size and contrast acquired in reflectance and transillumination near-infrared imaging modes to estimate the severity of natural occlusal caries lesions. Previous studies have shown that near-infrared (NIR) light can be used to effectively image artificial carious lesions. However, its efficacy on natural lesions requires further exploration. Fifty extracted teeth with varying amounts of occlusal decay were examined using a NIR imaging system operating at 1310-nm. Image analysis software was used to calculate contrast values between sound and carious tooth structure. After imaging, teeth were histologically sampled at 1-mm intervals in order to determine lesion depth. Lesion contrast in transillumination mode significantly increased with lesion depth (p<0.001), while lesion contrast in reflectance mode did not increase. The lesion area demonstrated a significant increase with lesion severity in both imaging modes. These results suggest that lesion contrast and area can be used to estimate lesion severity in NIR images.

  9. ESO PR Highlights in 2007

    NASA Astrophysics Data System (ADS)

    2008-01-01

    Another great year went by for ESO, the European Organisation for Astronomical Research in the Southern Hemisphere. From 1 January 2007, with the official joining of the Czech Republic, ESO has 13 member states, and since September, ESO has a new Director General, Tim de Zeeuw (ESO 03/07 and 38/07). Many scientific discoveries were made possible with ESO's telescopes. Arguably, the most important is the discovery of the first Earth-like planet in the habitable zone of a low-mass red dwarf (ESO 22/07). If there is water on this planet, then it should be liquid! ESO PR Highlights 2007 This is a clickable map. These are only some of the press releases issued by ESO in 2007. For a full listing, please go to ESO 2007 page. In our own Solar System also, astronomers made stunning breakthroughs with ESO's telescopes, observing the effect of the light from the Sun on an asteroid's rotation (ESO 11/07), describing in unprecedented detail the double asteroid Antiope (ESO 18/07), peering at the rings of Uranus (ESO 37/07), discovering a warm south pole on Neptune (ESO 41/07), showing a widespread and persistent morning drizzle of methane over the western foothills of Titan's major continent (ESO 47/07), and studying in the greatest details the wonderful Comet McNaught (ESO 05/07 and 07/07). In the study of objects slightly more massive than planets, the VLT found that brown dwarfs form in a similar manner to normal stars (ESO 24/07). The VLT made it also possible to measure the age of a fossil star that was clearly born at the dawn of time (ESO 23/07). Other discoveries included reconstructing the site of a flare on a solar-like star (ESO 53/07), catching a star smoking (ESO 34/07), revealing a reservoir of dust around an elderly star (ESO 43/07), uncovering a flat, nearly edge-on disc of silicates in the heart of the magnificent Ant Nebula (ESO 42/07), finding material around a star before it exploded (ESO 31/07), fingerprinting the Milky Way (ESO 15/07), revealing a rich

  10. Highly selective and responsive visible to near-IR ytterbium emissive probe for monitoring mercury(II).

    PubMed

    Zhang, Tao; Chan, Chi-Fai; Lan, Rongfeng; Wong, Wai-Kwok; Wong, Ka-Leung

    2014-01-20

    A new lanthanide probe based on the fluorescence resonance energy transfer (FRET) process with the combination of ytterbium porphyrinate complex and a rhodamine B derivative unit was synthesized to detect the Hg(2+) ion with responsive emission in the visible and near-IR region with a detection limit of 10 μM.

  11. THE GEMINI SPECTRAL LIBRARY OF NEAR-IR LATE-TYPE STELLAR TEMPLATES AND ITS APPLICATION FOR VELOCITY DISPERSION MEASUREMENTS

    SciTech Connect

    Winge, Claudia

    2009-11-01

    We present a spectroscopic library of late spectral type stellar templates in the near-IR range 2.15-2.42 {mu}m, at R = 5300-5900 resolution, oriented to support stellar kinematics studies in external galaxies, such as the direct determination of the masses of supermassive black holes in nearby active (or non-active) galaxies. The combination of high spectral resolution and state-of-the-art instrumentation available in 8 m class telescopes has made the analysis of circumnuclear stellar kinematics using the near-IR CO band heads one of the most used techniques for such studies, and this library aims to provide the supporting data sets required by the higher spectral resolution and larger spectral coverage currently achieved with modern near-IR spectrographs. Examples of the application for kinematical analysis are given for data obtained with two Gemini instruments, but the templates can be easily adjusted for use with other near-IR spectrographs at similar or lower resolution. The example data sets are also used to revisit the 'template mismatch' effect and the dependence of the velocity dispersion values obtained from the fitting process with the characteristics of the stellar templates. The library is available in electronic form from the Gemini Web pages.

  12. ESO's Hidden Treasures Brought to Light

    NASA Astrophysics Data System (ADS)

    2011-01-01

    ESO's Hidden Treasures 2010 astrophotography competition attracted nearly 100 entries, and ESO is delighted to announce the winners. Hidden Treasures gave amateur astronomers the opportunity to search ESO's vast archives of astronomical data for a well-hidden cosmic gem. Astronomy enthusiast Igor Chekalin from Russia won the first prize in this difficult but rewarding challenge - the trip of a lifetime to ESO's Very Large Telescope at Paranal, Chile. The pictures of the Universe that can be seen in ESO's releases are impressive. However, many hours of skilful work are required to assemble the raw greyscale data captured by the telescopes into these colourful images, correcting them for distortions and unwanted signatures of the instrument, and enhancing them so as to bring out the details contained in the astronomical data. ESO has a team of professional image processors, but for the ESO's Hidden Treasures 2010 competition, the experts decided to give astronomy and photography enthusiasts the opportunity to show the world what they could do with the mammoth amount of data contained in ESO's archives. The enthusiasts who responded to the call submitted nearly 100 entries in total - far exceeding initial expectations, given the difficult nature of the challenge. "We were completely taken aback both by the quantity and the quality of the images that were submitted. This was not a challenge for the faint-hearted, requiring both an advanced knowledge of data processing and an artistic eye. We are thrilled to have discovered so many talented people," said Lars Lindberg Christensen, Head of ESO's education and Public Outreach Department. Digging through many terabytes of professional astronomical data, the entrants had to identify a series of greyscale images of a celestial object that would reveal the hidden beauty of our Universe. The chance of a great reward for the lucky winner was enough to spur on the competitors; the first prize being a trip to ESO's Very Large

  13. ESO's First Observatory Celebrates 40th Anniversary

    NASA Astrophysics Data System (ADS)

    2009-03-01

    ESO's La Silla Observatory, which is celebrating its 40th anniversary, became the largest astronomical observatory of its time. It led Europe to the frontline of astronomical research, and is still one of the most scientifically productive in ground-based astronomy. ESO PR Photo 12a/09 La Silla Aerial View ESO PR Photo 12b/09 The ESO New Technology Telescope ESO PR Photo 12c/09 SEST on La Silla ESO PR Photo 12d/09 Looking for the best site ESO PR Video 12a/09 ESOcast 5 With about 300 refereed publications attributable to the work of the observatory per year, La Silla remains at the forefront of astronomy. It has led to an enormous number of scientific discoveries, including several "firsts". The HARPS spectrograph is the world's foremost exoplanet hunter. It detected the system around Gliese 581, which contains what may be the first known rocky planet in a habitable zone, outside the Solar System (ESO 22/07). Several telescopes at La Silla played a crucial role in discovering that the expansion of the Universe is accelerating (ESO 21/98) and in linking gamma-ray bursts -- the most energetic explosions in the Universe since the Big Bang - with the explosions of massive stars (ESO 15/98). Since 1987, the ESO La Silla Observatory has also played an important role in the study and follow-up of the nearest supernova, SN 1987A (ESO 08/07). "The La Silla Observatory continues to offer the astronomical community exceptional capabilities," says ESO Director General, Tim de Zeeuw. "It was ESO's first presence in Chile and as such, it triggered a very long and fruitful collaboration with this country and its scientific community." The La Silla Observatory is located at the edge of the Chilean Atacama Desert, one of the driest and loneliest areas of the world. Like other observatories in this geographical area, La Silla is located far from sources of polluting light and, as the Paranal Observatory that houses the Very Large Telescope, it has one of the darkest and clearest

  14. Searching for heavily obscured post-AGB stars and planetary nebulae. II. Near-IR observations of IRAS sources

    NASA Astrophysics Data System (ADS)

    Ramos-Larios, G.; Guerrero, M. A.; Suárez, O.; Miranda, L. F.; Gómez, J. F.

    2012-09-01

    The most massive AGB stars are expected to result in heavily obscured post-AGB stars, proto-PNe and PNe with highly axisymmetric morphologies. To investigate this evolutionary connection, we have selected a sample of 165 presumably obscured IRAS post-AGB star and PN candidates and obtained near-IR JHK images for 164 of them. These images, in conjunction with DSS, 2MASS, Spitzer GLIMPSE, MSX, AKARI, and IRAS archival data, have allowed us to identify the near-IR counterparts of 154 of these sources, providing reliable finding charts and coordinates. Near-IR narrow-band Brγ, H2, and K continuum images were acquired for 6 of these sources that were found to be resolved in near-IR JHK images. Among the extended post-AGB source and PN candidates, three are round and seven have bipolar morphologies. Five of the extended sources are ionized and may have thus entered the PN stage. We note that all extended sources with water maser emission have bipolar morphology. We have investigated the Galactic distribution of sources with the largest flux drop from the 9 μm AKARI band to the near-IR J band and found that the width of the distribution in Galactic latitude is consistent with those of bipolar PNe and DUPLEX (DUst-Prominent Longitudinally EXtended) sources. Based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere, Chile (081.D-0812), observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, and on observations with AKARI, a JAXA project with the participation of ESA.

  15. Near-IR imaging of Erbium Laser Ablation with a Water Spray.

    PubMed

    Darling, Cynthia L; Maffei, Marie E; Fried, William A; Fried, Daniel

    2008-01-20

    Near-IR (NIR) imaging can be used to view the formation of ablation craters during laser ablation since the enamel of the tooth is almost completely transparent near 1310-nm(1). Laser ablation craters can be monitored under varying irradiation conditions to assess peripheral thermal and transient-stress induced damage, measure the rate and efficiency of ablation and provide insight into the ablation mechanism. There are fundamental differences in the mechanism of enamel ablation using erbium lasers versus carbon dioxide laser systems due to the nature of the primary absorber and it is necessary to have water present on the tooth surface for efficient ablation at erbium laser wavelengths. In this study, sound human tooth sections of approximately 2-3-mm thickness were irradiated by free running and Q-switched Er:YAG & Er:YSGG lasers under varying conditions with and without a water spray. The incision area in the interior of each sample was imaged using a tungsten-halogen lamp with a band-pass filter centered at 1310-nm combined with an InGaAs area camera with a NIR zoom microscope. Obvious differences in the crater evolution were observed between CO(2) and erbium lasers. Ablation stalled after a few laser pulses without a water spray as anticipated. Efficient ablation was re-initiated by resuming the water spray. Micro-fractures were continuously produced apparently driven along prism lines during multi-pulse ablation. These fractures or fissures appeared to merge together as the crater evolved to form the leading edge of the ablation crater. These observations support the proposed thermo-mechanical mechanisms of erbium laser involving the strong mechanical forces generated by selective absorption by water. PMID:21892255

  16. A Concept for Seeing-Limited Near-IR Spectroscopy on the Giant Magellan Telescope

    NASA Astrophysics Data System (ADS)

    Simcoe, Robert A.; Furesz, Gabor; Egan, Mark; Malonis, Andrew; Hellickson, Tim

    2016-09-01

    We present a simple seeing-limited IR spectrometer design for the Giant Magellan Telescope, with continuous R = 6000 coverage from 0.87-2.50 microns for a 0:7" slit. The instrument's design is based on an asymmetric white pupil echelle layout, with dichroics splitting the optical train into yJ, H, and K channels after the pupil transfer mirror. A separate low-dispersion mode offers single-object R ~ 850 spectra which also cover the full NIR bandpass in each exposure. Catalog gratings and H2RG detectors are used to minimize cost, and only two cryogenic rotary mechanisms are employed, reducing mechanical complexity. The instrument dewar occupies an envelope of 1:8×1:5×1:2 meters, satisfying mass and volume requirements for GMT with comfortable margin. We estimate the system throughput at ~35% including losses from the atmosphere, telescope, and instrument (i.e. all coatings, gratings, and sensors). This optical efficiency is comparable to the FIRE spectrograph on Magellan, and we have specified and designed fast cameras so the GMT instrument will have an almost identical pixel scale as FIRE. On the 6.5 meter Magellan telescopes, FIRE is read-noise limited in the y and J bands, similar to other existing near-IR spectrometers and also to JWST/NIRSPEC. GMT's twelve-fold increase in collecting area will therefore offer gains in signal-to-noise per exposure that exceed those of moderate resolution optical instruments, which are already sky-noise limited on today's telescopes. Such an instrument would allow GMT to pursue key early science programs on the Epoch of Reionization, galaxy formation, transient astronomy, and obscured star formation environments prior to commissioning of its adaptive optics system. This design study demonstrates the feasibility of developing relatively affordable spectrometers at the ELT scale, in response to the pressures of joint funding for these telescopes and their associated instrument suites.

  17. Optical design of a versatile FIRST high-resolution near-IR spectrograph

    NASA Astrophysics Data System (ADS)

    Zhao, Bo; Ge, Jian

    2012-09-01

    We report the update optical design of a versatile FIRST high resolution near IR spectrograph, which is called Florida IR Silicon immersion grating spectromeTer (FIRST). This spectrograph uses cross-dispersed echelle design with white pupils and also takes advantage of the image slicing to increase the spectra resolution, while maintaining the instrument throughput. It is an extremely high dispersion R1.4 (blazed angle of 54.74°) silicon immersion grating with a 49 mm diameter pupil is used as the main disperser at 1.4μm -1.8μm to produce R=72,000 while an R4 echelle with the same pupil diameter produces R=60,000 at 0.8μm -1.35μm. Two cryogenic Volume Phase Holographic (VPH) gratings are used as cross-dispersers to allow simultaneous wavelength coverage of 0.8μm -1.8μm. The butterfly mirrors and dichroic beamsplitters make a compact folding system to record these two wavelength bands with a 2kx2k H2RG array in a single exposure. By inserting a mirror before the grating disperser (the SIG and the echelle), this spectrograph becomes a very efficient integral field 3-D imaging spectrograph with R=2,000-4,000 at 0.8μm-1.8μm by coupling a 10x10 telescope fiber bundle with the spectrograph. Details about the optical design and performance are reported.

  18. Formation of Random, RIE-Textured Silicon Surfaces with Reduced Reflection and Enhanced Near IR Absorption

    SciTech Connect

    ZAIDI, SALEEM H

    2001-04-01

    The authors have developed novel metal-assisted texturing processes that have led to optically favorable surfaces for solar cells. Large area ({approximately} 200 cm{sup 2}) uniform texturing has been achieved. The physical dimensions of the chamber limited texturing of even larger wafers. Surface contamination and residual RIE-induced damage were removed by incorporation of a complete RCA clean process followed by wet-chemical etching treatments. RIE-textured solar cells with optimized profiles providing performance comparable to the random, wet-chemically etched cells have been demonstrated. A majority of the texture profiles exhibit an enhanced IQE response in the near IR region.using scanning electron microscope measurements, they carried out a detailed analysis of the microstructure of random RIE-textured surfaces. The random microstructure represents a superposition of sub-{micro}m grating structures with a wide distribution of periods, depths, and profiles as determined by the SEM measurements. These structures were modeled using GSOLVER{trademark} software for periodic patterns. The enhanced IR response from random, RIE-textured surfaces is attributed to enhanced coupling of light into the transmitted diffraction orders. These obliquely propagating diffraction orders generate electron-hole pairs closer to the surface, thus, reducing bulk recombination losses relative to a non-scattering, planar surface with identical hemispherical reflection. The optimized texture and damage removal processes have been applied to large area (100--132 cm{sup 2}) multi-crystalline wafers. initial results have demonstrated improved performance relative to planar, control wafers. However, the texture and solar cell fabrication processes require further optimization in the RCA clean, DRE treatments, and emitter formation in order to fully realize the benefits of the low-reflection ({approximately}1-2%) textured surfaces.

  19. LIGO Gravitational Wave Detection, Primordial Black Holes, and the Near-IR Cosmic Infrared Background Anisotropies

    NASA Astrophysics Data System (ADS)

    Kashlinsky, A.

    2016-06-01

    LIGO's discovery of a gravitational wave from two merging black holes (BHs) of similar masses rekindled suggestions that primordial BHs (PBHs) make up the dark matter (DM). If so, PBHs would add a Poissonian isocurvature density fluctuation component to the inflation-produced adiabatic density fluctuations. For LIGO's BH parameters, this extra component would dominate the small-scale power responsible for collapse of early DM halos at z ≳ 10, where first luminous sources formed. We quantify the resultant increase in high-z abundances of collapsed halos that are suitable for producing the first generation of stars and luminous sources. The significantly increased abundance of the early halos would naturally explain the observed source-subtracted near-IR cosmic infrared background (CIB) fluctuations, which cannot be accounted for by known galaxy populations. For LIGO's BH parameters, this increase is such that the observed CIB fluctuation levels at 2-5 μm can be produced if only a tiny fraction of baryons in the collapsed DM halos forms luminous sources. Gas accretion onto these PBHs in collapsed halos, where first stars should also form, would straightforwardly account for the observed high coherence between the CIB and unresolved cosmic X-ray background in soft X-rays. We discuss modifications possibly required in the processes of first star formation if LIGO-type BHs indeed make up the bulk or all of DM. The arguments are valid only if the PBHs make up all, or at least most, of DM, but at the same time the mechanism appears inevitable if DM is made of PBHs.

  20. IGRINS Near-IR High-resolution Spectroscopy of Multiple Jets around LkHα 234

    NASA Astrophysics Data System (ADS)

    Oh, Heeyoung; Pyo, Tae-Soo; Yuk, In-Soo; Park, Byeong-Gon; Park, Chan; Chun, Moo-Young; Pak, Soojong; Kim, Kang-Min; Sok Oh, Jae; Jeong, Ueejeong; Yu, Young Sam; Lee, Jae-Joon; Kim, Hwihyun; Hwang, Narae; Kaplan, Kyle; Pavel, Michael; Mace, Gregory; Lee, Hye-In; Nguyen Le, Huynh Anh; Lee, Sungho; Jaffe, Daniel T.

    2016-02-01

    We present the results of high-resolution near-IR spectroscopy toward the multiple outflows around the Herbig Be star LkHα 234 using the Immersion Grating Infrared Spectrograph. Previous studies indicate that the region around LkHα 234 is complex, with several embedded young stellar objects and the outflows associated with them. In simultaneous H- and K-band spectra from HH 167, we detected 5 [Fe ii] and 14 H2 emission lines. We revealed a new [Fe ii] jet driven by radio continuum source VLA 3B. Position-velocity diagrams of the H2 1-0 S(1) λ2.122 μm line show multiple velocity peaks. The kinematics may be explained by a geometrical bow shock model. We detected a component of H2 emission at the systemic velocity (VLSR = -10.2 km s-1) along the whole slit in all slit positions, which may arise from the ambient photodissociation region. Low-velocity gas dominates the molecular hydrogen emission from knots A and B in HH 167, which is close to the systemic velocity; [Fe ii] emission lines are detected farther from the systemic velocity, at VLSR = -100--130 km s-1. We infer that the H2 emission arises from shocked gas entrained by a high-velocity outflow. Population diagrams of H2 lines imply that the gas is thermalized at a temperature of 2500-3000 K and the emission results from shock excitation. This paper includes data taken at The McDonald Observatory of The University of Texas at Austin.

  1. Low altitude cloud height and methane humidity retrievals on Titan in the near-IR

    NASA Astrophysics Data System (ADS)

    Adamkovics, M.; Hayes, A.; Mitchell, J.; De Pater, I.; Young, E.

    2013-12-01

    The formation of low altitude clouds on Titan, with cloud-top altitudes below ~10km, likely occurs by a fundamentally different mechanism than for the clouds commonly observed to have cloud-tops in the upper troposphere, above ~15km [1]. Near-infrared spectroscopy of clouds has been the method of choice for determining cloud altitudes [2], however, uncertainties in aerosols scattering properties and opacities, together with limitations in laboratory measurements of gas opacities (in particular for methane), lead to uncertainties in how accurately the altitude of low clouds can be retrieved [3]. Here we revisit near-IR spectra obtained with Keck and Cassini using new laboratory methane line data in the HITRAN 2012 database [4] to address the problem of measuring the altitudes of low clouds. We discuss the role of topography in relation to the formation of low clouds and other diagnostics of conditions near the surface, such as the tropospheric methane humidity. We reanalyze measurements the tropospheric humidity variation [5] and describe observational strategies for improved diagnostics of the tropospheric humidity on Titan . Acknowledgements: Funding for this work is provided by the NSF grant AST-1008788 and NASA OPR grant NNX12AM81G. References: [1] Brown, et al. (2009) ApJ, 706, L110-L113. [2] Ádámkovics et al. (2010) Icarus, 208, 868-877. [3] Griffith et al. (2012) Icarus, 218, 975-988. [4] Rothman et al. (2013) AIP Conf. Proc., 1545, 223-231. [5] Penteado & Griffith (2010) Icarus, 206, 345-351.

  2. The Surprising in Vivo Instability of Near-IR-Absorbing Hollow Au–Ag Nanoshells

    PubMed Central

    2015-01-01

    Photothermal ablation based on resonant illumination of near-infrared-absorbing noble metal nanoparticles that have accumulated in tumors is a highly promising cancer therapy, currently in multiple clinical trials. A crucial aspect of this therapy is the nanoparticle size for optimal tumor uptake. A class of nanoparticles known as hollow Au (or Au–Ag) nanoshells (HGNS) is appealing because near-IR resonances are achievable in this system with diameters less than 100 nm. However, in this study, we report a surprising finding that in vivo HGNS are unstable, fragmenting with the Au and the remnants of the sacrificial Ag core accumulating differently in various organs. We synthesized 43, 62, and 82 nm diameter HGNS through a galvanic replacement reaction, with nanoparticles of all sizes showing virtually identical NIR resonances at ∼800 nm. A theoretical model indicated that alloying, residual Ag in the nanoparticle core, nanoparticle porosity, and surface defects all contribute to the presence of the plasmon resonance at the observed wavelength, with the major contributing factor being the residual Ag. While PEG functionalization resulted in stable nanoparticles under laser irradiation in solution, an anomalous, strongly element-specific biodistribution observed in tumor-bearing mice suggests that an avid fragmentation of all three sizes of nanoparticles occurred in vivo. Stability studies across a wide range of pH environments and in serum confirmed HGNS fragmentation. These results show that NIR resonant HGNS contain residual Ag, which does not stay contained within the HGNS in vivo. This demonstrates the importance of tracking both materials of a galvanic replacement nanoparticle in biodistribution studies and of performing thorough nanoparticle stability studies prior to any intended in vivo trial application. PMID:24547810

  3. LIGO Gravitational Wave Detection, Primordial Black Holes, and the Near-IR Cosmic Infrared Background Anisotropies

    NASA Astrophysics Data System (ADS)

    Kashlinsky, A.

    2016-06-01

    LIGO's discovery of a gravitational wave from two merging black holes (BHs) of similar masses rekindled suggestions that primordial BHs (PBHs) make up the dark matter (DM). If so, PBHs would add a Poissonian isocurvature density fluctuation component to the inflation-produced adiabatic density fluctuations. For LIGO's BH parameters, this extra component would dominate the small-scale power responsible for collapse of early DM halos at z ≳ 10, where first luminous sources formed. We quantify the resultant increase in high-z abundances of collapsed halos that are suitable for producing the first generation of stars and luminous sources. The significantly increased abundance of the early halos would naturally explain the observed source-subtracted near-IR cosmic infrared background (CIB) fluctuations, which cannot be accounted for by known galaxy populations. For LIGO's BH parameters, this increase is such that the observed CIB fluctuation levels at 2–5 μm can be produced if only a tiny fraction of baryons in the collapsed DM halos forms luminous sources. Gas accretion onto these PBHs in collapsed halos, where first stars should also form, would straightforwardly account for the observed high coherence between the CIB and unresolved cosmic X-ray background in soft X-rays. We discuss modifications possibly required in the processes of first star formation if LIGO-type BHs indeed make up the bulk or all of DM. The arguments are valid only if the PBHs make up all, or at least most, of DM, but at the same time the mechanism appears inevitable if DM is made of PBHs.

  4. Constraining Composition of Potentially-Hazardous Asteroid 2006 WH1 via Near-IR Spectroscopy

    NASA Astrophysics Data System (ADS)

    Reddy, Vishnu; Gaffey, M. J.; Binzel, R. P.; Hardersen, P. S.; Kumar, S.

    2007-10-01

    Near-infrared spectroscopic observations of potentially-hazardous asteroid (PHA) 2006 WH1 were obtained remotely on December 22, 2006 UT, using the SpeX instrument at NASA IRTF on Mauna Kea, Hawai'i. Near-IR spectrum of 2006 WH1 displays a deep band I feature (band depth 25%) and a weaker band II (band depth 10%) suggesting the presence of the mineral pyroxene in the surface assemblage. The estimated band I and II centers are 0.96±0.005 µm and 2.00±0.01 µm respectively, with a BAR of 0.6±0.1. Weak inflection at 1.30-µm could be due to olivine, plagioclase feldspar or high-Fe pyroxene. 2006 WH1 plots above the pyroxene trend line on the band-band plot (Adams, 1974, Cloutis & Gaffey, 1991) indicating the presence of olivine along with pyroxene. Upon applying the band I displacement correction of 0.032 µm for olivine (Gaffey et al., 2002), the object's band I drops on to the pyroxene trend line strengthening the case of the presence of olivine. Using methods developed by Cloutis et al., (1986), the estimated amount of pyroxene in a pyroxene + olivine mixture is 0.30±0.05%. The estimated pyroxene chemistry suggests either a eucrite-like pyroxene or the presence of three pyroxenes (low Fe, Ca orthopyroxene; low Fe augite and Eucrite-like pigeonite). Such chemistry supports the presence of a possible non-chondritic surface assemblage on 2006 WH1, while not excluding the remote plausibility of an LL-chondrite-type assemblage. The authors would like to thank NASA IRTF for providing Target of Opportunity observing time for observing 2006 WH1 flyby. This research was supported by NASA Near-Earth Objects Observations Program grant NNG04GI17G and GSA PGD Eugene M. Shoemaker Impact Cratering Award.

  5. ESO and Chile: 10 Years of Productive Scientific Collaboration

    NASA Astrophysics Data System (ADS)

    2006-06-01

    ESO and the Government of Chile launched today the book "10 Years Exploring the Universe", written by the beneficiaries of the ESO-Chile Joint Committee. This annual fund provides grants for individual Chilean scientists, research infrastructures, scientific congresses, workshops for science teachers and astronomy outreach programmes for the public. In a ceremony held in Santiago on 19 June 2006, the European Organisation for Astronomical Research in the Southern Hemisphere (ESO) and the Chilean Ministry of Foreign Affairs marked the 10th Anniversary of the Supplementary Agreement, which granted to Chilean astronomers up to 10 percent of the total observing time on ESO telescopes. This agreement also established an annual fund for the development of astronomy, managed by the so-called "ESO-Chile Joint Committee". ESO PR Photo 21/06 ESO PR Photo 21/06 Ten Years ESO-Chile Agreement Ceremony The celebration event was hosted by ESO Director General, Dr. Catherine Cesarsky, and the Director of Special Policy for the Chilean Ministry of Foreign Affairs, Ambassador Luis Winter. "ESO's commitment is, and always will be, to promote astronomy and scientific knowledge in the country hosting our observatories", said ESO Director General, Dr. Catherine Cesarsky. "We hope Chile and Europe will continue with great achievements in this fascinating joint adventure, the exploration of the universe." On behalf of the Government of Chile, Ambassador Luis Winter outlined the historical importance of the Supplementary Agreement, ratified by the Chilean Congress in 1996. "Such is the magnitude of ESO-Chile Joint Committee that, only in 2005, this annual fund represented 8 percent of all financing sources for Chilean astronomy, including those from Government and universities", Ambassador Winter said. The ESO Representative and Head of Science in Chile, Dr. Felix Mirabel, and the appointed Chilean astronomer for the ESO-Chile Joint Committee, Dr. Leonardo Bronfman, also took part in the

  6. Near-IR 2D-spectroscopy of the 4''x 4'' region around the Active Galactic Nucleus of NGC 1068 with ISAAC/VLT

    NASA Astrophysics Data System (ADS)

    Galliano, E.; Alloin, D.

    2002-10-01

    New near-IR long slit spectroscopic data obtained with ISAAC on VLT/ANTU (ESO/Paranal) complement and extend our previously published near-IR data (Alloin et al. \\cite{all01}) to produce Brgamma and H2 emission line maps and line profile grids of the central 4'' x 4'' region surrounding the central engine of NGC 1068. The seeing quality together with the use of an 0.3'' wide slit and 0.3'' slit position offsets allow one to perform 2D-spectroscopy at a spatial resolution ~ 0.5''. Slit orientations (PA = 102 degr and PA = 12 degr) were chosen so as to match respectively the equatorial plane and the axis of the suspected molecular/dusty torus in NGC 1068. The selected wavelength range from 2.1 to 2.2μm is suitable to detect and analyze the Brgamma and H2 emission lines at a spectral resolution corresponding to 35km s-1. An asymmetric distribution of H2 emission around the continuum peak is observed. No H2 emission is detected at the location of the strong 2.2μm continuum core (coincident within error-bars with the central engine location), while two conspicuous knots of H2 emission are detected at about 1'' on each side of the central engine along PA = 90 degr, with a projected velocity difference of 140km s-1: this velocity jump has been interpreted in Alloin et al. (\\cite{all01}) as the signature of a rotating disk of molecular material. From this new data set, we find that only very low intensity Brgamma emission is detected at the location of the two main knots of H2 emission. Another knot with both H2 and Brgamma emission is detected to the North of the central engine, close to the radio source C where the small scale radio jet is redirected and close to the brightest [OIII] cloud NLR-B. It has a counterpart to the South, placed almost symmetrically with respect to the central engine, although mainly visible in the Brgamma emission. The northern and southern knots appear to be related to the ionization cone. At the achieved spectral resolution, the H2

  7. ESO's Two Observatories Merge

    NASA Astrophysics Data System (ADS)

    2005-02-01

    On February 1, 2005, the European Southern Observatory (ESO) has merged its two observatories, La Silla and Paranal, into one. This move will help Europe's prime organisation for astronomy to better manage its many and diverse projects by deploying available resources more efficiently where and when they are needed. The merged observatory will be known as the La Silla Paranal Observatory. Catherine Cesarsky, ESO's Director General, comments the new development: "The merging, which was planned during the past year with the deep involvement of all the staff, has created unified maintenance and engineering (including software, mechanics, electronics and optics) departments across the two sites, further increasing the already very high efficiency of our telescopes. It is my great pleasure to commend the excellent work of Jorge Melnick, former director of the La Silla Observatory, and of Roberto Gilmozzi, the director of Paranal." ESO's headquarters are located in Garching, in the vicinity of Munich (Bavaria, Germany), and this intergovernmental organisation has established itself as a world-leader in astronomy. Created in 1962, ESO is now supported by eleven member states (Belgium, Denmark, Finland, France, Germany, Italy, The Netherlands, Portugal, Sweden, Switzerland, and the United Kingdom). It operates major telescopes on two remote sites, all located in Chile: La Silla, about 600 km north of Santiago and at an altitude of 2400m; Paranal, a 2600m high mountain in the Atacama Desert 120 km south of the coastal city of Antofagasta. Most recently, ESO has started the construction of an observatory at Chajnantor, a 5000m high site, also in the Atacama Desert. La Silla, north of the town of La Serena, has been the bastion of the organization's facilities since 1964. It is the site of two of the most productive 4-m class telescopes in the world, the New Technology Telescope (NTT) - the first major telescope equipped with active optics - and the 3.6-m, which hosts HARPS

  8. Predicting future space near-IR grism surveys using the WFC3 infrared spectroscopic parallels survey

    SciTech Connect

    Colbert, James W.; Atek, Hakim; Teplitz, Harry; Rafelski, Marc; Bunker, Andrew; Ross, Nathaniel; Malkan, Matt; Scarlata, Claudia; Bedregal, Alejandro G.; Dominguez, Alberto; Masters, Dan; Siana, Brian; Dressler, Alan; McCarthy, Patrick; Henry, Alaina; Martin, Crystal L.

    2013-12-10

    We present near-infrared emission line counts and luminosity functions from the Hubble Space Telescope Wide Field Camera 3 Infrared Spectroscopic Parallels (WISP) program for 29 fields (0.037 deg{sup 2}) observed using both the G102 and G141 grism. Altogether we identify 1048 emission line galaxies with observed equivalent widths greater than 40 Å, 467 of which have multiple detected emission lines. We use simulations to correct for significant (>20%) incompleteness introduced in part by the non-dithered, non-rotated nature of the grism parallels. The WISP survey is sensitive to fainter flux levels ((3-5) × 10{sup –17} erg s{sup –1} cm{sup –2}) than the future space near-infrared grism missions aimed at baryonic acoustic oscillation cosmology ((1-4) × 10{sup –16} erg s{sup –1} cm{sup –2}), allowing us to probe the fainter emission line galaxies that the shallower future surveys may miss. Cumulative number counts of 0.7 < z < 1.5 galaxies reach 10,000 deg{sup –2} above an Hα flux of 2 × 10{sup –16} erg s{sup –1} cm{sup –2}. Hα-emitting galaxies with comparable [O III] flux are roughly five times less common than galaxies with just Hα emission at those flux levels. Galaxies with low Hα/[O III] ratios are very rare at the brighter fluxes that future near-infrared grism surveys will probe; our survey finds no galaxies with Hα/[O III] < 0.95 that have Hα flux greater than 3 × 10{sup –16} erg s{sup –1} cm{sup –2}. Our Hα luminosity function contains a comparable number density of faint line emitters to that found by the Near IR Camera and Multi-Object Spectrometer near-infrared grism surveys, but significantly fewer (factors of 3-4 less) high-luminosity emitters. We also find that our high-redshift (z = 0.9-1.5) counts are in agreement with the high-redshift (z = 1.47) narrowband Hα survey of HiZELS (Sobral et al.), while our lower redshift luminosity function (z = 0.3-0.9) falls slightly below their z = 0.84 result. The evolution

  9. Predicting Future Space Near-IR Grism Surveys Using the WFC3 Infrared Spectroscopic Parallels Survey

    NASA Astrophysics Data System (ADS)

    Colbert, James W.; Teplitz, Harry; Atek, Hakim; Bunker, Andrew; Rafelski, Marc; Ross, Nathaniel; Scarlata, Claudia; Bedregal, Alejandro G.; Dominguez, Alberto; Dressler, Alan; Henry, Alaina; Malkan, Matt; Martin, Crystal L.; Masters, Dan; McCarthy, Patrick; Siana, Brian

    2013-12-01

    We present near-infrared emission line counts and luminosity functions from the Hubble Space Telescope Wide Field Camera 3 Infrared Spectroscopic Parallels (WISP) program for 29 fields (0.037 deg2) observed using both the G102 and G141 grism. Altogether we identify 1048 emission line galaxies with observed equivalent widths greater than 40 Å, 467 of which have multiple detected emission lines. We use simulations to correct for significant (>20%) incompleteness introduced in part by the non-dithered, non-rotated nature of the grism parallels. The WISP survey is sensitive to fainter flux levels ((3-5) × 10-17 erg s-1 cm-2) than the future space near-infrared grism missions aimed at baryonic acoustic oscillation cosmology ((1-4) × 10-16 erg s-1 cm-2), allowing us to probe the fainter emission line galaxies that the shallower future surveys may miss. Cumulative number counts of 0.7 < z < 1.5 galaxies reach 10,000 deg-2 above an Hα flux of 2 × 10-16 erg s-1 cm-2. Hα-emitting galaxies with comparable [O III] flux are roughly five times less common than galaxies with just Hα emission at those flux levels. Galaxies with low Hα/[O III] ratios are very rare at the brighter fluxes that future near-infrared grism surveys will probe; our survey finds no galaxies with Hα/[O III] < 0.95 that have Hα flux greater than 3 × 10-16 erg s-1 cm-2. Our Hα luminosity function contains a comparable number density of faint line emitters to that found by the Near IR Camera and Multi-Object Spectrometer near-infrared grism surveys, but significantly fewer (factors of 3-4 less) high-luminosity emitters. We also find that our high-redshift (z = 0.9-1.5) counts are in agreement with the high-redshift (z = 1.47) narrowband Hα survey of HiZELS (Sobral et al.), while our lower redshift luminosity function (z = 0.3-0.9) falls slightly below their z = 0.84 result. The evolution in both the Hα luminosity function from z = 0.3-1.5 and the [O III] luminosity function from z = 0.7-2.3 is

  10. Fabrication of 3D polymer photonic crystals for near-IR applications

    NASA Astrophysics Data System (ADS)

    Yao, Peng; Qiu, Liang; Shi, Shouyuan; Schneider, Garrett J.; Prather, Dennis W.; Sharkawy, Ahmed; Kelmelis, Eric

    2008-02-01

    occurred as we reduced the lattice constant for near-IR applications. In this work, we address this problem by employing SU8. The exposure is vertically confined by using a mismatched 220nm DUV source. Intermixing problem is eliminated due to more densely crosslinked resist molecules. Using this method, we have demonstrated 3D "woodpile" structure with 1.55μm lattice constant and a 2mm-by-2mm pattern area.

  11. Near-IR resonance Raman spectroscopy of archaerhodopsin 3: effects of transmembrane potential.

    PubMed

    Saint Clair, Erica C; Ogren, John I; Mamaev, Sergey; Russano, Daniel; Kralj, Joel M; Rothschild, Kenneth J

    2012-12-20

    Archaerhodopsin 3 (AR3) is a light driven proton pump from Halorubrum sodomense that has been used as a genetically targetable neuronal silencer and an effective fluorescent sensor of transmembrane potential. Unlike the more extensively studied bacteriorhodopsin (BR) from Halobacterium salinarum, AR3 readily incorporates into the plasma membrane of both E. coli and mammalian cells. Here, we used near-IR resonance Raman confocal microscopy to study the effects of pH and membrane potential on the AR3 retinal chromophore structure. Measurements were performed both on AR3 reconstituted into E. coli polar lipids and in vivo in E. coli expressing AR3 in the absence and presence of a negative transmembrane potential. The retinal chromophore structure of AR3 is in an all-trans configuration almost identical to BR over the entire pH range from 3 to 11. Small changes are detected in the retinal ethylenic stretching frequency and Schiff Base (SB) hydrogen bonding strength relative to BR which may be related to a different water structure near the SB. In the case of the AR3 mutant D95N, at neutral pH an all-trans retinal O-like species (O(all-trans)) is found. At higher pH a second 13-cis retinal N-like species (N(13-cis)) is detected which is attributed to a slowly decaying intermediate in the red-light photocycle of D95N. However, the amount of N(13-cis) detected is less in E. coli cells but is restored upon addition of carbonyl cyanide m-chlorophenyl hydrazone (CCCP) or sonication, both of which dissipate the normal negative membrane potential. We postulate that these changes are due to the effect of membrane potential on the N(13-cis) to M(13-cis) levels accumulated in the D95N red-light photocycle and on a molecular level by the effects of the electric field on the protonation/deprotonation of the cytoplasmic accessible SB. This mechanism also provides a possible explanation for the observed fluorescence dependence of AR3 and other microbial rhodopsins on transmembrane

  12. Charon's, Hydra's, and Nix's near IR spectra as seen by New Horizons

    NASA Astrophysics Data System (ADS)

    Dalle Ore, Cristina M.; Cook, Jason C.; Cruikshank, Dale P.; Protopapa, Silvia; Grundy, William M.; Olkin, Catherine B.; Ennico, Kimberly; Stern, S. Alan; Weaver, Harold A.; Young, Leslie; New Horizons Surface Composition Theme Team

    2016-10-01

    Charon, Pluto's largest satellite, is a predominantly grey-color icy world covered mostly in H2O ice, with spectral evidence for NH3 and/or its hydrates, as previously reported (Cook et al. 2007, ApJ. 663, 1406; Verbiscer et al. 2007, LPSC 38, 2318; Merlin et al. 2010, Icarus, 210, 930; Cook et al. 2014, AAS/DPS Abstracts, 46, #401.04; Holler et al. 2016, submitted, arXiv:1606.05695). In their 2010 work, Merlin et al. reported the presence of ammonia species along with H2O ice both in crystalline and amorphous phase. They introduced a blue component to model the slope present in their near-IR observations, which could not be otherwise reproduced without the adoption of an ad hoc component. The presence of ammonia and H2O in its crystalline form prompted Cook et al. (2007) to suggest cryovolcanism as a favored mechanism of resurfacing although the geological evidence for volcanism reported from New Horizons imaging observations does not appear to be recent (Moore et al. Science, 351, 1284).We analyze one of New Horizons' observations of Charon taken with the LEISA imaging spectrometer from a distance of ~82,000 km at high spatial resolution (4.9 km/pixel). Images from the New Horizons spacecraft reveal a surface with terrains of seemingly different ages and a moderate degree of localized coloration.Hydra was observed by New Horizons at a distance 240,000 and 370,000 hardly resolving its disk. Nix on the other hand was observed from a much more favorable distance of 60,000 and 162,000 km revealing a nearly uniform surface coloration and structure.Although Hydra could hardly be resolved at the flyby distance we have obtained its spectral signature and we compare it with those of Charon and Nix. A feature at ~2.2 µm, corresponding to the NH3 and/or NH3 hydrates, is visible subtly on Charon and clearly on Hydra and Nix hinting at the possibility that NH3 might be less volatile than previously thought and making the need for recent cryovolcanism less crucial

  13. Optical Testing of Diamond Machined, Aspheric Mirrors for Groundbased, Near-IR Astronomy

    NASA Technical Reports Server (NTRS)

    Chambers, V. John; Mink, Ronald G.; Ohl, Raymond G.; Connelly, Joseph A.; Mentzell, J. Eric; Arnold, Steven M.; Greenhouse, Matthew A.; Winsor, Robert S.; MacKenty, John W.

    2002-01-01

    The Infrared Multi-Object Spectrometer (IRMOS) is a facility-class instrument for the Kitt Peak National Observatory 4 and 2.1 meter telescopes. IRMOS is a near-IR (0.8-2.5 micron) spectrometer and operates at approximately 80 K. The 6061-T651 aluminum bench and mirrors constitute an athermal design. The instrument produces simultaneous spectra at low- to mid-resolving power (R=lambda/delta lambda= 300-3000) of approximately 100 objects in its 2.8 x 2.0 arcmin field. We describe ambient and cryogenic optical testing of the IRMOS mirrors across a broad range in spatial frequency (figure error, mid-frequency error, and microroughness). The mirrors include three rotationally symmetric, off-axis conic sections, one off-axis biconic, and several flat fold mirrors. The symmetric mirrors include convex and concave prolate and oblate ellipsoids. They range in aperture from 94x86 mm to 286x269 mm and in f-number from 0.9 to 2.4. The biconic mirror is concave and has a 94x76 mm aperture, R(sub x)=377 mm, k(sub x)=0.0778, R(sub y)=407 mm, and k(sub y)=0.1265 and is decentered by -2 mm in X and 227 mm in Y. All of the mirrors have an aspect ratio of approximately 6:1. The surface error fabrication tolerances are less than 10 nm RMS microroughness, 'best effort' for mid-frequency error, and less than 63.3 nm RMS figure error. Ambient temperature (approximately 293 K) testing is performed for each of the three surface error regimes, and figure testing is also performed at approximately 80 K. Operation of the ADE Phaseshift MicroXAM white light interferometer (micro-roughness) and the Bauer Model 200 profilometer (mid-frequency error) is described. Both the sag and conic values of the aspheric mirrors make these tests challenging. Figure testing is performed using a Zygo GPI interferometer, custom computer generated holograms (CGH), and optomechanical alignment fiducials. Cryogenic CGH null testing is discussed in detail. We discuss complications such as the change in

  14. Near-IR spectroscopic monitoring of CLASS I protostars: Variability of accretion and wind indicators

    SciTech Connect

    Connelley, Michael S.; Greene, Thomas P.

    2014-06-01

    We present the results of a program that monitored the near-IR spectroscopic variability of a sample of 19 embedded protostars. Spectra were taken on time intervals from 2 days to 3 yr, over a wavelength range from 0.85 μm to 2.45 μm, for 4-9 epochs of observations per target. We found that the spectra of all targets are variable and that every emission feature observed is also variable (although not for all targets). With one exception, there were no drastic changes in the continua of the spectra, nor did any line completely disappear, nor did any line appear that was not previously apparent. This analysis focuses on understanding the connection between accretion (traced by H Br γ and CO) and the wind (traced by He I, [Fe II], and sometimes H{sub 2}). For both accretion and wind tracers, the median variability was constant versus the time interval between observations; however, the maximum variability that we observed increased with the time interval between observations. Extinction is observed to vary within the minimum sampling time of 2 days, suggesting extinguishing material within a few stellar radii at high disk latitudes. The variability of [Fe II] and H{sub 2} were correlated for most (but not all) of the 7 young stellar objects showing both features, and the amplitude of the variability depends on the veiling. Although the occurrence of CO and Br γ emission are connected, their variability is uncorrelated, suggesting that these emissions originate in separate regions near the protostar (e.g., disk and wind). The variability of Br γ and wind tracers were found to be positively correlated, negatively correlated, or uncorrelated, depending on the target. The variability of Br γ, [Fe II], and H{sub 2} always lies on a plane, although the orientation of the plane in three dimensions depends on the target. While we do not understand all interactions behind the variability that we observed, we have shown that spectroscopic variability is a powerful tool

  15. AN ANALYSIS OF THE SHAPES OF INTERSTELLAR EXTINCTION CURVES. VI. THE NEAR-IR EXTINCTION LAW

    SciTech Connect

    Fitzpatrick, E. L.; Massa, D. E-mail: massa@derckmassa.net

    2009-07-10

    We combine new observations from the Hubble Space Telescope's Advanced Camera of Survey with existing data to investigate the wavelength dependence of near-IR (NIR) extinction. Previous studies suggest a power law form for NIR extinction, with a 'universal' value of the exponent, although some recent observations indicate that significant sight line-to-sight line variability may exist. We show that a power-law model for the NIR extinction provides an excellent fit to most extinction curves, but that the value of the power, {beta}, varies significantly from sight line to sight line. Therefore, it seems that a 'universal NIR extinction law' is not possible. Instead, we find that as {beta} decreases, R(V) {identical_to} A(V)/E(B - V) tends to increase, suggesting that NIR extinction curves which have been considered 'peculiar' may, in fact, be typical for different R(V) values. We show that the power-law parameters can depend on the wavelength interval used to derive them, with the {beta} increasing as longer wavelengths are included. This result implies that extrapolating power-law fits to determine R(V) is unreliable. To avoid this problem, we adopt a different functional form for NIR extinction. This new form mimics a power law whose exponent increases with wavelength, has only two free parameters, can fit all of our curves over a longer wavelength baseline and to higher precision, and produces R(V) values which are consistent with independent estimates and commonly used methods for estimating R(V). Furthermore, unlike the power-law model, it gives R(V)s that are independent of the wavelength interval used to derive them. It also suggests that the relation R(V) = -1.36 E(K-V)/(E(B-V)) - 0.79 can estimate R(V) to {+-}0.12. Finally, we use model extinction curves to show that our extinction curves are in accord with theoretical expectations, and demonstrate how large samples of observational quantities can provide useful constraints on the grain properties.

  16. The Orion fingers: Near-IR adaptive optics imaging of an explosive protostellar outflow

    NASA Astrophysics Data System (ADS)

    Bally, John; Ginsburg, Adam; Silvia, Devin; Youngblood, Allison

    2015-07-01

    Aims: Adaptive optics (AO) images are used to test the hypothesis that the explosive BN/KL outflow from the Orion OMC1 cloud core was powered by the dynamical decay of a non-hierarchical system of massive stars. Methods: Narrow-band H2, [Fe ii], and broad-band Ks obtained with the Gemini South multi-conjugate AO system GeMS and near-IR imager GSAOI are presented. The images reach resolutions of 0.08 to 0.10'', close to the 0.07'' diffraction limit of the 8-m telescope at 2.12 μm. Comparison with previous AO-assisted observations of sub-fields and other ground-based observations enable measurements of proper motions and the investigation of morphological changes in H2 and [Fe ii] features with unprecedented precision. The images are compared with numerical simulations of compact, high-density clumps moving ~103 times their own diameter through a lower density medium at Mach 103. Results: Several sub-arcsecond H2 features and many [Fe ii] "fingertips" on the projected outskirts of the flow show proper motions of ~300 km s-1. High-velocity, sub-arcsecond H2 knots ("bullets") are seen as far as 140'' from their suspected ejection site. If these knots propagated through the dense Orion A cloud, their survival sets a lower bound on their densities of order 107 cm-3, consistent with an origin within a few au of a massive star and accelerated by a final multi-body dynamic encounter that ejected the BN object and radio source I from OMC1 about 500 yr ago. Conclusions: Over 120 high-velocity bow-shocks propagating in nearly all directions from the OMC1 cloud core provide evidence for an explosive origin for the BN/KL outflow triggered by the dynamic decay of a non-hierarchical system of massive stars. Such events may be linked to the origin of runaway, massive stars. The final set of FITS files is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/579/A130

  17. Anticancer drug released from near IR-activated prodrug overcomes spatiotemporal limits of singlet oxygen.

    PubMed

    Rajaputra, Pallavi; Bio, Moses; Nkepang, Gregory; Thapa, Pritam; Woo, Sukyung; You, Youngjae

    2016-04-01

    Photodynamic therapy (PDT) is a cancer treatment modality where photosensitizer (PS) is activated by visible and near IR light to produce singlet oxygen ((1)O2). However, (1)O2 has a short lifetime (<40 ns) and cannot diffuse (<20 nm) beyond the cell diameter (e.g., ∼ 1800 nm). Thus, (1)O2 damage is both spatially and temporally limited and does not produce bystander effect. In a heterogeneous tumor, cells escaping (1)O2 damage can regrow after PDT treatment. To overcome these limitations, we developed a prodrug concept (PS-L-D) composed of a photosensitizer (PS), an anti-cancer drug (D), and an (1)O2-cleavable linker (L). Upon illumination of the prodrug, (1)O2 is generated, which damages the tumor and also releases anticancer drug. The locally released drug could cause spatially broader and temporally sustained damage, killing the surviving cancer cells after the PDT damage. In our previous report, we presented the superior activity of our prodrug of CA4 (combretastatin A-4), Pc-(L-CA4)2, compared to its non-cleavable analog, Pc-(NCL-CA4)2, that produced only PDT effects. Here, we provide clear evidence demonstrating that the released anticancer drug, CA4, indeed damages the surviving cancer cells over and beyond the spatial and temporal limits of (1)O2. In the limited light illumination experiment, cells in the entire well were killed due to the effect of released anti-cancer drug, whereas only a partial damage was observed in the pseudo-prodrug treated wells. A time-dependent cell survival study showed more cell death in the prodrug-treated cells due to the sustained damage by the released CA4. Cell cycle analysis and microscopic imaging data demonstrated the typical damage patterns by CA4 in the prodrug treated cells. A time-dependent histological study showed that prodrug-treated tumors lacked mitotic bodies, and the prodrug caused broader and sustained tumor size reduction compared to those seen in the tumors treated with the pseudo-prodrug. This data

  18. Characterization and monitoring of Flamingos-II, a near-IR imager and spectrograph at Gemini South

    NASA Astrophysics Data System (ADS)

    Krogsrud, David; Diaz, Ruben; Ferrero, Gabriel; Mora, Marcelo; Navarete, Felipe; Schirmer, Mischa

    2015-01-01

    We present results of the characterization and continual monitoring of the Flamingos-II instrument. Currently installed at Gemini South Observatory, Flamingos-II is a near-IR imager and longslit/multi-object spectrograph. In addition to the characterization of the detector, methodologies and results of the Science Verification pipeline, Telluric corrections, and Multi-Object Spectrograph (MOS) mask design software are presented.

  19. Behavior of [S/Fe] Obtained from Near-IR S I Lines at 10456-9 Å

    NASA Astrophysics Data System (ADS)

    Takada-Hidai, M.; Takeda, Y.

    2012-08-01

    Behavior of [S/Fe] was examined based on near-IR S I 10456-9 Å lines observed with the Subaru IRCS+AO188. We found that the behavior of their [S/Fe] shows a flat trend in the range of [Fe/H]< -1, which is consistent with that of [S/Fe] obtained from 9212-28-37 Å lines. The full papers of this presentation are published in Takeda & Takada-Hidai (2011, 2012).

  20. ESO from an Italian perspective

    NASA Astrophysics Data System (ADS)

    Tosi, M.

    Italy joined the European Southern Observatory (ESO) 30 years ago. This membership has allowed Italian scientists and engineers to exploit the superior facilities provided by ESO and to successfully participate to their development and construction. Some of the effects on Italian astrophysics of these thirty years of membership and collaboration are briefly summarized. A few examples of high impact results obtained by Italians with the ESO telescopes are given for the fields of resolved stellar populations and galaxy evolution.

  1. Near-IR laser-triggered target cell collection using a carbon nanotube-based cell-cultured substrate.

    PubMed

    Sada, Takao; Fujigaya, Tsuyohiko; Niidome, Yasuro; Nakazawa, Kohji; Nakashima, Naotoshi

    2011-06-28

    Unique near-IR optical properties of single-walled carbon nanotube (SWNTs) are of interest in many biological applications. Here we describe the selective cell detachment and collection from an SWNT-coated cell-culture dish triggered by near-IR pulse laser irradiation. First, HeLa cells were cultured on an SWNT-coated dish prepared by a spraying of an aqueous SWNT dispersion on a glass dish. The SWNT-coated dish was found to show a good cell adhesion behavior as well as a cellular proliferation rate similar to a conventional glass dish. We discovered, by near-IR pulse laser irradiation (at the laser power over 25 mW) to the cell under optical microscopic observation, a quick single-cell detachment from the SWNT-coated surface. Shockwave generation from the irradiated SWNTs is expected to play an important role for the cell detachment. Moreover, we have succeeded in catapulting the target single cell from the cultured medium when the depth of the medium was below 150 μm and the laser power was stronger than 40 mW. The captured cell maintained its original shape. The retention of the genetic information of the cell was confirmed by the polymerase chain reaction (PCR) technique. A target single-cell collection from a culture medium under optical microscopic observation is significant in wide fields of single-cell studies in biological areas.

  2. Broadband near-IR emission from cubic perovskite KZnF(3):Ni(2+) nanocrystals embedded glass-ceramics.

    PubMed

    Lin, Changgui; Liu, Chao; Zhao, Zhiyong; Li, Legang; Bocker, Christian; Rüssel, Christian

    2015-11-15

    Transparent KF-ZnF(2)-SiO(2) glass-ceramics were prepared with the precipitation of KZnF(3)Ni(2+) nanocrystals. During excitation with a wavelength of 405 nm at room temperature, a broadband near-IR emission centered at 1695 nm with the FWHM of more than 350 nm was observed, which is originated from the T(2g)3(F3)→A(2g)3(F3) transition of octahedral Ni(2+) incorporated in the KZnF(3) crystalline phase. In comparison to oxide glass-ceramics, a redshift of the luminescence is observed, which is due to the low crystal field of these octahedral Ni(2+). The shift and extension of near-IR emission in the KZnF(3):Ni(2+) nanocrystals embedded in a glassy matrix do not only complete the broadband emission in the whole near-IR region for the Ni(2+) ions-based photonics, but also open an easy way to approach the broadband optical amplifier and tunable lasers operating in the wavelength region near 1800 nm, which was up to now achieved by codoping of several types of active ions. PMID:26565850

  3. Relations Between Chile and ESO

    NASA Astrophysics Data System (ADS)

    1994-06-01

    As announced in an earlier Press Release (PR 08/94 of 6 May 1994), a high-ranking ESO delegation visited Santiago de Chile during the week of 24 - 28 May 1994 to discuss various important matters of mutual interest with the Chilean Government. It consisted of Dr. Peter Creola (President of ESO Council), Dr. Catherine Cesarsky (Vice-President of ESO Council), Dr. Henrik Grage (Former Vice-President of ESO Council) and Professor Riccardo Giacconi (ESO Director General), the latter accompanied by his advisers. THE SUPPLEMENTARY TREATY BETWEEN CHILE AND ESO Following a meeting with the ambassadors to Chile of the eight ESO member countries, the ESO delegation was received by the Chilean Minister of Foreign Affairs, Mr. Carlos Figueroa, and members of his staff. The ESO delegation was pleased to receive assurances that the present Chilean Government, like its predecessors, will continue to honour all contractual agreements, in particular the privileges and immunities of this Organisation, which were laid down in the Treaty between ESO and Chile that was signed by the parties in 1963 and ratified the following year. The discussions covered some aspects of the proposed Supplementary Treaty which has been under preparation during the past year. This included in particular the desire of the Chilean side to further increase the percentage of guaranteed time for Chilean astronomers at the future ESO Very Large Telescope (VLT) and also the rules governing the installation by ESO member countries of additional telescopes at the ESO observatories in Chile. ESO invited a Chilean delegation to visit the ESO Headquarters in Garching (Germany) later this year for the final adjustment of the text of the Supplementary Treaty, after which it should be possible to proceed rapidly with the signing and ratification by the Chilean Parliament and the ESO Council. THE SITUATION AROUND PARANAL The ESO delegation expressed its deep concern to the Chilean Government about the continuing legal

  4. Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey -- UDS Field

    NASA Astrophysics Data System (ADS)

    Faber, Sandra

    2010-09-01

    The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey {CANDELS}is designed to document the ?rst third of galactic evolution from z =8 to 1.5 via deep imaging of more than 250,000 galaxies with WFC3/IRand ACS. It will also find the first Type Ia SNe beyond z > 1.5 andestablish their accuracy as standard candles for cosmology. Fivepremier multi-wavelength sky regions are selected from the SpitzerExtragalactic Deep Survey {SEDS} to provide complementary IRAC imagingdata down to 26.5 AB mag, a unique resource for stellar masses at allredshifts. The use of ?ve widely separated ?elds mitigates cosmicvariance and yields statistically robust and complete samples ofgalaxies down to 10^9 solar masses out to z 8.The program merges two originally separate MCT proposals. The Faberprogram incorporates a ?Wide? imaging survey in three separate fieldsto 2 orbit depth over 0.2 sq. degrees, plus a ?Deep? imaging surveyto 12 orbit depth in the two GOODS regions over 0.04 sq. degrees.In combination with ultra-deep imaging from the Hubble Ultradeep Fieldprogram {GO 11563}, the result is a three-tiered strategy that ef?cientlysamples both bright/rare and faint/common extragalactic objects. TheFerguson program adds an extensive high-redshift Type Ia SNe search,plus ultraviolet "daytime" UVIS exposures in GOODS-N to exploit theCVZ opportunity in that field.This program, GO 12064, is part of the Wide mosaic survey, which has thefollowing field centers and sizes: Field ID RA{2000} Dec{2000} WFC3 Dim. PA on sky UDS 02 17 38 -05 12 02 4x11 270 COSMOS 10 00 31 +02 24 00 4x11 180 EGS 14 19 31 +52 54 10 3x15 41 Science highlights from the Wide program: * Underlying structural properties of galaxies as revealed by WFC3-IR images sensitive to older stars {beyond the 4000-A break} and less affected by dust than ACS. A key redshift is z 2, where star-formation peaks, QSOs are most abundant, and where restframe B-band is still accessible to WFC3. Sample questions include: - Structure in young

  5. ESO: Present and Future

    NASA Astrophysics Data System (ADS)

    de Zeeuw, P. T.

    2014-01-01

    ESO is an intergovernmental organization for astronomy founded in 1962 by five countries. It currently has 14 Member States in Europe with Brazil poised to join as soon as the Accession Agreement has been ratified. Together these countries represent approximately 30 percent of the world’s astronomers. ESO operates optical/infrared observatories on La Silla and Paranal in Chile, partners in the sub-millimeter radio observatories APEX and ALMA on Chajnantor and is about to start construction of the Extremely Large Telescope on Armazones. La Silla hosts various robotic telescopes and experiments as well as the NTT and the venerable 3.6m telescope. The former had a key role in the discovery of the accelerating expansion of the Universe and the latter hosts the ultra-stable spectrograph HARPS which is responsible for the discovery of nearly two-thirds of all confirmed exoplanets with masses below that of Neptune. On Paranal the four 8.2m units of the Very Large Telescope, the Interferometer and the survey telescopes VISTA and VST together constitute an integrated system which supports 16 powerful facility instruments, including adaptive-optics-assisted imagers and integral-field spectrographs, with half a dozen more on the way and the Extremely Large Telescope with its suite of instruments to be added in about ten years time. Scientific highlights include the characterisation of the supermassive black hole in the Galactic Centre, the first image of an exoplanet, studies of gamma-ray bursts enabled by the Rapid Response Mode and milliarcsec imaging of evolved stars and active galactic nuclei. The single dish APEX antenna, equipped with spectrometers and wide-field cameras, contributes strongly to the study of high-redshift galaxies and of star- and planet-formation. Early Science results obtained with the ALMA interferometer already demonstrate its tremendous potential for observations of the cold Universe. The plenary talk will outline the development of ESO

  6. A Catalog of Near-IR Sources Found to be Unresolved with Milliarcsecond Resolution

    NASA Astrophysics Data System (ADS)

    Richichi, A.; Fors, O.; Cusano, F.; Moerchen, M.

    2012-12-01

    Calibration is one of the long-standing problems in optical interferometric measurements, particularly with long baselines which demand stars with angular sizes on the milliarcsecond scale and no detectable companions. While systems of calibrators have been generally established for the near-infrared in the bright source regime (K <~ 3 mag), modern large interferometers are sensitive to significantly fainter magnitudes. We aim to provide a list of sources found to be unresolved from direct observations with high angular resolution and dynamic range, which can be used to choose interferometric calibrators. To this purpose, we have used a large number of lunar occultations recorded with the ISAAC instrument at the Very Large Telescope to select sources found to be unresolved and without close companions. An algorithm has been used to determine the limiting angular resolution achieved for each source, taking into account a noise model built from occulted and unocculted portions of the light curves. We have obtained upper limits on the angular sizes of 556 sources, with magnitudes ranging from K s ≈ 4 to 10, with a median of 7.2 mag. The upper limits on possible undetected companions (within ≈0.''5) range from K s ≈ 8 to 13, with a median of 11.5 mag. One-third of the sources have angular sizes <=1 mas, and two-thirds have sizes <=2 mas. This list of unresolved sources matches well the capabilities of current large interferometric facilities. We also provide available cross-identifications, magnitudes, spectral types, and other auxiliary information. A fraction of the sources are found to be potentially variable. The list covers parts of the Galactic Bulge and in particular the vicinity of the Galactic Center, where extinction is very significant and traditional lists of calibrators are often insufficient. Based on observations made with ESO telescopes at the Paranal Observatory.

  7. Near-IR Imaging of the Most Distant Spectroscopically-Confirmed Galaxies in the Subaru Deep Field

    NASA Astrophysics Data System (ADS)

    Jiang, Linhua

    2011-10-01

    The last decade saw great progress in our understanding of the distant Universe as a number of objects at z > 6 were discovered. In particular, with the power of the HST WFC3/IR camera, galaxies and galaxy candidates at z > 6 {up to 10} are being routinely found. However, we still know very little about their physical properties due to a lack of a large and bright galaxy sample with secure redshifts. Here we propose to carry out HST/WFC3 near-IR imaging of a large sample of spectroscopically-confirmed galaxies at 5.7 < z < 7 in the Subaru Deep Field {SDF}. SDF is unique: it covers more than 800 sq arcmin; it has the deepest optical images among all ground-based imaging data; it has the largest sample of spectroscopically-confirmed galaxies at z >= 6 so far; it also has deep IRAC { 6 hours} coverage from our Spitzer programs. From the proposed observations and our previous HST programs, we will obtain high-quality near-IR data {rest-frame UV} for about 60 galaxies. The near-IR data is the key to measure the properties of young stellar populations, while the IRAC data constrains mature populations. Using SED modeling with spectroscopic redshifts, we will be able to fully characterize the physical properties of these galaxies and obtain accurate information of age and stellar mass etc. We will also address the physical difference or similarity between Lyman alpha emitters and Lyman break galaxies at z >= 6. All these help us to understand the earliest galaxy formation and evolution and the galaxy contribution to cosmic reionization. Our WFC3 data will enable many other sciences, such as galaxy morphology at z >= 6 and search of bright galaxies at z > 7.

  8. Airborne observed solar elevation and row direction effects on the near-IR/red ratio of cotton

    NASA Technical Reports Server (NTRS)

    Millard, J. P.; Jackson, R. D.; Goettelman, R. C.; Leroy, M. J. (Principal Investigator)

    1981-01-01

    An airborne multispectral scanner was used to obtain data over two adjacent cotton fields having rows perpendicular to one another, at three times of day (different solar elevations), and on two dates (different plant size). The near IR/red ratios were displayed in image form, so that within-field variations and differences between fields could be easily assessed. The ratio varied with changing Sun elevation for north-south oriented rows, but no variation was detected for east-west oriented rows.

  9. VizieR Online Data Catalog: Empirical calibration of the near-IR Ca triplet (Cenarro+ 2001)

    NASA Astrophysics Data System (ADS)

    Cenarro; A. J.; Cardiel; N.; Gorgas; J.; Peletier; R. F.; Vazdekis; A.; Prada; F.

    2001-09-01

    File table contains details of the new near-IR stellar library observed to calibrate the Ca II triplet. It includes the indices CaT*, CaT and PaT measured over the final spectra as well as their corresponding errors. The Henry Draper Catalogue number, other names (mainly HR and BD numbers), coordinates, spectral type, luminosity class, apparent magnitude and atmospheric parameters (as derived in Paper II; Cenarro et al., 2001MNRAS.326..981C) are also given. (1 data file).

  10. Visible and Near-IR Reflectance Spectra of Mars Analogue Materials Under Arid Conditions for Interpretation of Martian Surface Mineralogy

    NASA Technical Reports Server (NTRS)

    Morris, R. V.; Graff, T. G.; Achilles, C. N.; Agresti, D. G.; Ming, D. W.; Golden, D. C.

    2011-01-01

    Visible and near-IR (VNIR) spectra from the hyper-spectral imagers MRO-CRISM and Mars Express OMEGA in martian orbit have signatures from Fe-bearing phases (e.g., olivine, pyroxene, and jarosite), H2O/OH-bearing phases (e.g., smectites and other phyllosilicates, sulfates, and high-SiO2 phases), and carbonate [e.g., 1-5]. Mineralogical assignments of martian spectral features are made on the basis of VNIR spectra acquired in the laboratory under appropriate environmental conditions on samples whose mineralogical composition is known. We report here additional results for our ongoing project [6] to acquire VNIR spectra under arid conditions.

  11. ESO PR Highlights in 2003

    NASA Astrophysics Data System (ADS)

    2004-01-01

    Among the many astronomical highlights of 2003, the Transit of Mercury certainly attracted great attention as shown by the record number of hits the ESO web page received on that day. But this was a mere rehearsal of an even bigger event we will enjoy in 2004: the Venus Transit. ESO, in partnership with several institutions, is organising a major educational event in connection with it. During 2003, the ESO Educational Office was also involved in various other programmes. They included the web-based "Catch a Star!" and the "Physics and Life" projects, organised with EC sponsorship in connection with the 2003 European Science and Technology Week. The ALMA project, an European-North American collaboration to build an array of 64 12-m submillimetre antennas, moved forward with the signature of the agreement between ESO and the NSF and with the Ground-breaking at Chajnantor. Conceptual studies of a 100-m optical/infrared telescope (OWL) also proceeded well. Several new instruments were installed at ESO telescopes, e.g. HARPS . And the VLT Interferometer (VLTI) received a powerful Adaptive Optics System and made the first detection through infrared interferometry of an extragalactic object. A rapidly increasing number of new scientific results were obtained on the basis of data from ESO telescopes, some of which were highlighted in ESO Press Releases. A number of beautiful images were published. Many of these developments are described in ESO's Press Releases, most with Press Photos, cf. the 2003 PR Index. Some of last year's ESO PR highlights may be accessed directly via the clickable image above.

  12. News from the ESO Science Archive Facility

    NASA Astrophysics Data System (ADS)

    Dobrzycki, A.; Arnaboldi, M.; Bierwirth, T.; Boelter, M.; Da Rocha, C.; Delmotte, N.; Forchì, V.; Fourniol, N.; klein Gebbinck, M.; Lange, U.; Mascetti, L.; Micol, A.; Moins, C.; Munte, C.; Pluciennik, C.; Retzlaff, J.; Romaniello, M.; Rosse, N.; Sequeiros, I. V.; Vuong, M.-H.; Zampieri, S.

    2015-09-01

    ESO Science Archive Facility (SAF) - one of the world's biggest astronomical archives - combines two roles: operational (ingest, tallying, safekeeping and distribution to observers of raw data taken with ESO telescopes and processed data generated both internally and externally) and scientific (publication and delivery of all flavours of data to external users). This paper presents the “State of the SAF.” SAF, as a living entity, is constantly implementing new services and upgrading the existing ones. We present recent and future developments related to the Archive's Request Handler and metadata handling as well as performance and usage statistics and trends. We also discuss the current and future datasets on offer at SAF.

  13. ESO: research facilities in Santiago

    NASA Astrophysics Data System (ADS)

    Alloin, D.

    2001-09-01

    With the start of operations on Paranal, a major increase of the ESO staff with duty station in Chile has taken place: as of today, the number of ESO scientists (staff, postdocs, paid associates and PhD students) has doubled with respect to 1998, leading as well to a larger number of visiting scientists and students on short-term training. The research facilities offered by ESO to its staff in Chile had to be adapted to this growth and the scientific life had to be boosted accordingly.

  14. Properties of the fullerene C60-containing PN Lin49 in the SMC; Explanations of strong near-IR excess

    NASA Astrophysics Data System (ADS)

    Otsuka, Masaaki; Kemper, Francisca; Leal-Ferreira, Marcelo L.; Aleman, Isabel; Bernard-Salas, Jeronimo; Cami, Jan; Ochsendorf, Bram; Peeters, Els

    2016-07-01

    We performed a detailed spectroscopic analysis of the fullerene C6o-containing planetary nebula (PN) Lin49 in the Small Magellanic Cloud (SMC). Lin49 is a C-rich and metal- deficient PN (Z∼⃒0.0006) and its nebular abundances are in agreement with the AGB model for the initially 1.25Mʘ stars with the metallicity Z = 0.001 of Fishlock et al. (2014, [1]). By stellar absorption fitting with TLUSTY, we derived stellar abundances, effective temperature, and surface gravity. We constructed the photo-ionization model with CLOUDY in order to investigate physical conditions of Lin49. The model with the 0.005-0.1 μm radius graphite and a constant hydrogen density shell could not fit the ∼⃒1-5 μm SED owing to the strong near-IR excess. We propose that the near-IR excess indicates (1) the presence of extremely small carbon molecules or (2) the presence of high-density structure surrounding the central star.

  15. Measurement of Gas and Aerosol Phase Absorption Spectra across the Visible and Near-IR Using Supercontinuum Photoacoustic Spectroscopy.

    PubMed

    Radney, James G; Zangmeister, Christopher D

    2015-07-21

    We demonstrate a method to measure the absorption spectra of gas and aerosol species across the visible and near-IR (500 to 840 nm) using a photoacoustic (PA) spectrometer and a pulsed supercontinuum laser source. Measurements of gas phase absorption spectra were demonstrated using H2O(g) as a function of relative humidity (RH). The measured absorption intensities and peak shapes were able to be quantified and compared to spectra calculated using the 2012 High Resolution Transmission (HITRAN2012) database. Size and mass selected nigrosin aerosol was used to measure absorption spectra across the visible and near-IR. Spectra were measured as a function of aerosol size/mass and show good agreement to Mie theory calculations. Lastly, we measured the broadband absorption spectrum of flame generated soot aerosol at 5% and 70% RH. For the high RH case, we are able to quantifiably separate the soot and water absorption contributions. For soot, we observe an enhancement in the mass specific absorption cross section ranging from 1.5 at 500 nm (p < 0.01) to 1.2 at 840 nm (p < 0.2) and a concomitant increase in the absorption Ångström exponent from 1.2 ± 0.4 (5% RH) to 1.6 ± 0.3 (70% RH). PMID:26098142

  16. Fluorenyl benzothiadiazole and benzoselenadiazole near-IR fluorescent probes for two-photon fluorescence imaging (Conference Presentation)

    NASA Astrophysics Data System (ADS)

    Belfield, Kevin D.; Yao, Sheng; Kim, Bosung; Yue, Xiling

    2016-03-01

    Imaging biological samples with two-photon fluorescence (2PF) microscopy has the unique advantage of resulting high contrast 3D resolution subcellular image that can reach up to several millimeters depth. 2PF probes that absorb and emit at near IR region need to be developed. Two-photon excitation (2PE) wavelengths are less concerned as 2PE uses wavelengths doubles the absorption wavelength of the probe, which means 2PE wavelengths for probes even with absorption at visible wavelength will fall into NIR region. Therefore, probes that fluoresce at near IR region with high quantum yields are needed. A series of dyes based on 5-thienyl-2, 1, 3-benzothiadiazole and 5-thienyl-2, 1, 3-benzoselenadiazole core were synthesized as near infrared two-photon fluorophores. Fluorescence maxima wavelengths as long as 714 nm and fluorescence quantum yields as high as 0.67 were achieved. The fluorescence quantum yields of the dyes were nearly constant, regardless of solvents polarity. These diazoles exhibited large Stokes shift (<114nm), high two-photon absorption cross sections (up to 2,800 GM), and high two-photon fluorescence figure of merit (FM , 1.04×10-2 GM). Cells incubated on a 3D scaffold with one of the new probes (encapsulated in Pluronic micelles) exhibited bright fluorescence, enabling 3D two-photon fluorescence imaging to a depth of 100 µm.

  17. Development of a Near-Ir Cavity Enhanced Absorption Spectrometer for the Detection of Atmospheric Oxidation Products and Organoamines

    NASA Astrophysics Data System (ADS)

    Eddingsaas, Nathan C.; Jewell, Breanna; Thurnherr, Emily

    2014-06-01

    An estimated 10,000 to 100,000 different compounds have been measured in the atmosphere, each one undergoes many oxidation reactions that may or may not degrade air quality. To date, the fate of even some of the most abundant hydrocarbons in the atmosphere is poorly understood. One difficulty is the detection of atmospheric oxidation products that are very labile and decompose during analysis. To study labile species under atmospheric conditions, a highly sensitive, non-destructive technique is needed. Here we describe a near-IR incoherent broadband cavity enhanced absorption spectroscopy (IBBCEAS) setup that we are developing to meet this end. We have chosen to utilize the near-IR, where vibrational overtone absorptions are observed, due to the clean spectral windows and better spectral separation of absorption features. In one spectral window we can simultaneously and continuously monitor the composition of alcohols, hydroperoxides, and carboxylic acids in an air mass. In addition, we have used our CEAS setup to detect organoamines. The long effective path length of CEAS allows for low detection limits, even of the overtone absorption features, at ppb and ppt levels.

  18. Visible/near-IR-light-driven TNFePc/BiOCl organic-inorganic heterostructures with enhanced photocatalytic activity.

    PubMed

    Li, Lu; Zhang, Mingyi; Zhao, Zhenyu; Sun, Baodong; Zhang, Xitian

    2016-06-21

    Although semiconductor photocatalysis has been reported for more than 40 years, the spectral response is still focused on the region of UV-Visible and it is seldom extended to more than 600 nm. In this work, visible/near-IR-light-driven 2,9,16,23-tetranitrophthalocyanine iron (FeTNPc)/bismuth oxychloride (BiOCl) organic-inorganic heterostructures have been synthesized by a two-step solvothermal method. The obtained products were characterized by X-ray diffraction, Fourier transform infrared spectra, scanning electron and transmission microscopy, energy dispersive X-ray spectrometer, UV-vis diffuse reflectance spectroscopy, nitrogen adsorption-desorption, and electrochemical measurements. The photocatalytic activity for the decomposition of methyl orange and bisphenol A solution can be significantly improved under visible/near-IR-light irradiation. Through detecting the main oxidative species by trapping experiments, the results show holes and ˙O2(-) radicals are majorly and minorly responsible for photodegradation respectively. What's more, the FeTNPc/BiOCl composite photocatalyst still retained the photocatalytic activity after three cycle measurements. PMID:27192122

  19. Simultaneous near-IR spectroscopy and magnetic resonance imaging to assess cerebral oxygenation and brain water during hypoxia-ischemia in two-week-old rats

    NASA Astrophysics Data System (ADS)

    Shaw, R. A.; Tuor, U. I.; Foniok, T.; Bascaramurty, S.; Ringland, K.; McKenzie, E.; Qiao, M.; Tomanek, B.; Mantsch, Henry H.

    2001-10-01

    Cerebral near-infrared spectroscopy can potentially probe several parameters related to the onset of stroke and the ensuing tissue damage. One obvious marker of ischemia is cerebral oxygenation, which can be lowered sharply in stroke-affected tissue. Also commonly assessed, though less straightforward to recover, is the redox state of the cytochrome aa3 copper center. Finally, parameters that are in principle available but seldom recovered from in vivo near-IR spectra are changes in water concentration and scattering properties of the tissue. We have evaluated the potential for near-IR spectroscopy to detect relevant changes in cerebral oxygenation, blood volume, water content, and scattering properties in an infant rat stroke model that is well characterized by magnetic resonance imaging methods. The specific aim was to acquire near-IR spectra simultaneously with MR images and to correlate stroke-associated changes detected via these two modalities prior to, during and after a hypoxia-ischemia episode within this stroke model. Presented here are results from the design and testing of a near-IR illumination/detection system that is compatible with an MR imaging system, and the recovery of trends in the near-IR spectra that complement the hypoxic-ischemic changes observed in the MR images. Unexpectedly large intensity changes observed for the in vivo near-IR water absorptions are ascribed to hypoxia-induced variations in effective optical pathlength, suggesting that the water absorptions may prove generally useful as a means to track such changes.

  20. An Extension for ESO Headquarters

    NASA Astrophysics Data System (ADS)

    Fischer, Robert; Walsh, Jeremy

    2009-03-01

    The ESO Headquarters was completed in 1980, but is now too small to house all the ESO staff and currently only about 50% reside in the original building. A decision was taken to seek an extension to the Headquarters building in close proximity to the current one and a competition was launched for architectural designs. Three designs were shortlisted and the process of selection for the final design is described. Construction will begin in 2010 and is due for completion in 2012.

  1. Shaping ESO2020+ Together: Feedback from the Community Poll

    NASA Astrophysics Data System (ADS)

    Primas, F.; Ivison, R.; Berger, J.-P.; Caselli, P.; De Gregorio-Monsalvo, I.; Alonso Herrero, A.; Knudsen, K. K.; Leibundgut, B.; Moitinho, A.; Saviane, I.; Spyromilio, J.; Testi, L.; Vennes, S.

    2015-09-01

    A thorough evaluation and prioritisation of the ESO science programme into the 2020+ timeframe took place under the auspices of a working group, comprising astronomers drawn from ESO’s advisory structure and from within ESO. This group reported to ESO’s Scientific Technical Committee, and to ESO Council, concluding the exercise with the publication of a report, “Science Priorities at ESO”. A community poll and a dedicated workshop, held in January 2015, formed part of the information gathering process. The community poll was designed to probe the demographics of the user community, its scientific interests, use of observing facilities and plans for use of future telescopes and instruments, its views on types of observing programmes and on the provision of data processing and archiving. A total of 1775 full responses to the poll were received and an analysis of the results is presented here. Foremost is the importance of regular observing programmes on all ESO observing facilities, in addition to Large Programmes and Public Surveys. There was also a strong community requirement for ESO to process and archive data obtained at ESO facilities. Other aspects, especially those related to future facilities, are more challenging to interpret because of biases related to the distribution of science expertise and favoured wavelength regime amongst the targeted audience. The results of the poll formed a fundamental component of the report and pro-vide useful data to guide the evolution of ESO’s science programme.

  2. ESO Catalogue Facility Design and Performance

    NASA Astrophysics Data System (ADS)

    Moins, C.; Retzlaff, J.; Arnaboldi, M.; Zampieri, S.; Delmotte, N.; Forchí, V.; Klein Gebbinck, M.; Lockhart, J.; Micol, A.; Vera Sequeiros, I.; Bierwirth, T.; Peron, M.; Romaniello, M.; Suchar, D.

    2013-10-01

    The ESO Phase 3 Catalogue Facility provides investigators with the possibility to ingest catalogues resulting from ESO public surveys and large programs and to query and download their content according to positional and non-positional criteria. It relies on a chain of tools that covers the complete workflow from submission to validation and ingestion into the ESO archive and catalogue repository and a web application to browse and query catalogues. This repository consists of two components. One is a Sybase ASE relational database where catalogue meta-data are stored. The second one is a Sybase IQ data warehouse where the content of each catalogue is ingested in a specific table that returns all records matching a user's query. Spatial indexing has been implemented in Sybase IQ to speed up positional queries and relies on the Spherical Geometry Toolkit from the Johns Hopkins University which implements the Hierarchical Triangular Mesh (HTM) algorithm. It is based on a recursive decomposition of the celestial sphere in spherical triangles and the assignment of an index to each of them. It has been complemented with the use of optimized indexes on the non-positional columns that are likely to be frequently used as query constraints. First tests performed on catalogues such as 2MASS have confirmed that this approach provides a very good level of performance and a smooth user experience that are likely to facilitate the scientific exploitation of catalogues.

  3. Phoenix: automatic science processing of ESO-VLT data

    NASA Astrophysics Data System (ADS)

    Hanuschik, Reinhard

    2014-08-01

    ESO has implemented a process to automatically create science-grade data products and offer them to the scientific community, ready for scientific analysis. This process, called 'phoenix', is built on two main concepts: 1. a certification procedure for pipelines which includes a code review and, if necessary, upgrade; and 2. a certification procedure for calibrations which are processed into master calibrations, scored and trended. These master calibrations contain all information about the intrinsic instrumental variations and instabilities inevitable for ground-based telescopes. The phoenix process then automatically processes all science data using the certified pipeline and the certified master calibrations. Phoenix currently focuses on spectroscopic data. The first phoenix project has been the processing of all science data from UVES, ESO's high-resolution Echelle spectrograph at the VLT. More than 100,000 Echelle spectra of point sources, from begin of operations (March 2000) until now, have been reduced and are available to the public from the ESO archive, http://archive.eso.org/cms/eso-data/eso-data-products.html. The phoenix process will also feed future UVES data into the archive. The second project has been X-SHOOTER slit spectroscopy which currently has more than 30,000 Echelle spectra from the UV to the infrared (up to 2.5μm). The phoenix process will be extended to other, mostly spectroscopic, instruments with certified pipelines, like FLAMES. Also, all future VLT instruments will be supported by phoenix.

  4. Non-invasive, MRI-compatible fibreoptic device for functional near-IR reflectometry of human brain

    SciTech Connect

    Sorvoja, H.S.S.; Myllylae, T S; Myllylae, Risto A; Kirillin, M Yu; Sergeeva, Ekaterina A; Elseoud, A A; Nikkinen, J; Tervonen, O; Kiviniemi, V

    2011-01-24

    A non-invasive device for measuring blood oxygen variations in human brain is designed, implemented, and tested for MRI compatibility. The device is based on principles of near-IR reflectometry; power LEDs serve as sources of probing radiation delivered to patient skin surface through optical fibres. Numerical Monte Carlo simulations of probing radiation propagation in a multilayer brain model are performed to evaluate signal levels at different source - detector separations at three operation wavelengths and an additional wavelength of 915 nm. It is shown that the device can be applied for brain activity studies using power LEDs operating at 830 and 915 nm, while employment of wavelength of 660 nm requires an increased probing power. Employment of the wavelength of 592 nm in the current configuration is unreasonable. (application of lasers and laser-optical methods in life sciences)

  5. Novel 4'-functionalized 4,4''-dicarboxyterpyridine ligands for ruthenium complexes: near-IR sensitization in dye sensitized solar cells.

    PubMed

    Koyyada, Ganesh; Botla, Vinayak; Thogiti, Suresh; Wu, Guohua; Li, Jingzhe; Fang, Xiaqin; Kong, Fantai; Dai, Songyuan; Surukonti, Niveditha; Kotamarthi, Bhanuprakash; Malapaka, Chandrasekharam

    2014-10-28

    Novel ruthenium complexes (MC113-MC117), obtained by modifying the terpyridine ligand of the black dye (N749), have been evaluated as sensitizers for dye sensitized solar cells (DSSCs). The modification is carried out by attaching selected chromophores, with varying electron donating strength, covalently to the central ring of the ligand. The complexes, compared to the parent dye, show red shifted absorption covering visible and near IR regions and higher molar extinction coefficients. We report in this work synthesis of a series of these ruthenium complexes with chromophores such as tert-butyl phenyl, triphenylamine, bithiophene, phenoxazine and phenothiazine. Detailed experimental characterization using optical, electrochemical and photovoltaic techniques has been carried out and complemented by density functional theory studies. The fill factors (ff) obtained for these dyes are larger than those of the parent black dye. In spite of these superior properties, the dyes show only moderate to good power conversion efficiencies. The possible reasons for this have been investigated and discussed.

  6. Seasonal and Global Variations of Water Vapor and High Clouds Observed with MODIS near-IR Channels

    NASA Technical Reports Server (NTRS)

    Gao, Bo-Cai; Yang, Ping; Kaufman, Yoram J.; Wiscombe, Warren J.; Lau, William K. M. (Technical Monitor)

    2002-01-01

    The NASA Moderate Resolution Imaging Spectrometer (MODIS) on the Terra Spacecraft has been collecting scientific data since February of 2000. MODIS is a major facility instrument for remote sensing of the atmosphere, land surfaces, and ocean color. On the MODIS instruments, there are five channels located within and around the .0.94 micron water vapor band absorption region for remote sensing of atmospheric water vapor. There is also a channel located at 1.375 micron for detecting thin cirrus clouds. We will describe the basic principles for using these near-IR channels for remote sensing of water vapor and high clouds. Based on our analysis of two years# measurements with these channels, we have found that reliable observations of water vapor and high clouds on regional and global scales can be made. We will present results on daily, seasonal and annual variations of water vapor and high clouds.

  7. Impact of Humidity on Quartz-Enhanced Photoacoustic Spectroscopy Based CO Detection Using a Near-IR Telecommunication Diode Laser.

    PubMed

    Yin, Xukun; Dong, Lei; Zheng, Huadan; Liu, Xiaoli; Wu, Hongpeng; Yang, Yanfang; Ma, Weiguang; Zhang, Lei; Yin, Wangbao; Xiao, Liantuan; Jia, Suotang

    2016-01-01

    A near-IR CO trace gas sensor based on quartz-enhanced photoacoustic spectroscopy (QEPAS) is evaluated using humidified nitrogen samples. Relaxation processes in the CO-N2-H2O system are investigated. A simple kinetic model is used to predict the sensor performance at different gas pressures. The results show that CO has a ~3 and ~5 times slower relaxation time constant than CH4 and HCN, respectively, under dry conditions. However, with the presence of water, its relaxation time constant can be improved by three orders of magnitude. The experimentally determined normalized detection sensitivity for CO in humid gas is 1.556 × 10(-8) W ⋅ cm (-1)/Hz(1/2).

  8. Directional reflectance response in AVHRR red and near-IR bands for three cover types and varying atmospheric conditions

    NASA Technical Reports Server (NTRS)

    Holben, B.; Kimes, D.; Fraser, R. S.

    1986-01-01

    Surface directional red and near-infrared reflectances of bare soil, orchard grass, and fescue were extracted from a multitemporal data set to correspond to NOAA-7 Advanced Very High Resolution Radiometer (AVHRR) scanning and illumination geometry at 30 deg latitude. Radiances were simulated at satellite altitude and a ratio vegetation index was calculated. The results show that off-nadir directional reflectance measured at the surface in the red and near-IR portions of the spectrum are approximately maintained with AVHRR viewing and illumination characteristics. The two-channel reflectance response is such that the ratio vegetation index is more constant with scan angle and atmospheric conditions than individual channels. It is shown that inclusion of atmospheric and surface reflectance data can greatly improve interpretation of AVHRR data, when knowledge of the range of atmospheric conditions and approximate directional reflectances of major cover types are known.

  9. Exploring the NRO Opportunity for a Hubble-Sized Wide-Field Near-IR Space Telescope - New WFIRST

    NASA Technical Reports Server (NTRS)

    Dressler, Alan; Spergel, David; Mountain, Matt; Postman, Mark; Elliott, Erin; Bendek, Eduardo; Bennett, David; Dalcanton, Julianne; Gaudi, Scott; Gehrels, Neil; Guyon, Olivier; Hirata, Christopher; Kalirai, Jason; Kasdin, Jeremy; Kruk, Jeff; Macintosh, Bruce; Malhotra, Sangeeta; Penny, Matthew; Shaklan, Stuart; Stern, Daniel

    2013-01-01

    We discuss scientific, technical, and programmatic issues related to the use of an NRO 2.4m telescope for the WFIRST initiative of the 2010 Decadal Survey. We show that this implementation of WFIRST, which we call "NEW WFIRST," would achieve the goals of the NWNH Decadal Survey for the WFIRST core programs of Dark Energy and Microlensing Planet Finding, with the crucial benefit of deeper and/or wider near-IR surveys for GO science and a potentially Hubble-like Guest Observer program. NEW WFIRST could also include a coronagraphic imager for direct detection of dust disks and planets around neighboring stars, a high-priority science and technology precursor for future ambitious programs to image Earth-like planets around neighboring stars.

  10. Impact of Humidity on Quartz-Enhanced Photoacoustic Spectroscopy Based CO Detection Using a Near-IR Telecommunication Diode Laser

    PubMed Central

    Yin, Xukun; Dong, Lei; Zheng, Huadan; Liu, Xiaoli; Wu, Hongpeng; Yang, Yanfang; Ma, Weiguang; Zhang, Lei; Yin, Wangbao; Xiao, Liantuan; Jia, Suotang

    2016-01-01

    A near-IR CO trace gas sensor based on quartz-enhanced photoacoustic spectroscopy (QEPAS) is evaluated using humidified nitrogen samples. Relaxation processes in the CO-N2-H2O system are investigated. A simple kinetic model is used to predict the sensor performance at different gas pressures. The results show that CO has a ~3 and ~5 times slower relaxation time constant than CH4 and HCN, respectively, under dry conditions. However, with the presence of water, its relaxation time constant can be improved by three orders of magnitude. The experimentally determined normalized detection sensitivity for CO in humid gas is 1.556×10−8 W⋅cm−1/Hz1/2. PMID:26828491

  11. Status of the BOOTES-IR Project at OSN for GRB near-IR follow-up

    NASA Astrophysics Data System (ADS)

    Cunniffe, R.; Castro-Tirado, A. J.; Jelínek, M.; Gorosabel, J.; Moliné, B.; García-Segura, F.

    2013-07-01

    Bootes-IR (Castro-Tiradoet al. 2005) is a robotic observatory based around a 60 cm alt-az telescope (dubbed T60) that can slew rapidly while carrying heavy instrumentation at the Nasmyth foci. Initially commissioned with an optical camera, with which the optical afterglow to GRB 060707 (http://gcn.gsfc.nasa.gov/gcn3/5290.gcn3) was discovered, we have concentrated our efforts on the near-IR (0.8-2.5 μm) camera (BIRCAM) for which the telescope was specifically designed. The telescope is installed at the Observatorio de Sierra Nevada near Granada in Spain, at an altitude of 3000 m and in an area of very low humidity. The telescope, dome, camera and liquid nitrogen generation and refilling systems have all been recently brought back into operation, and routine observations are expected to begin within the next few months.

  12. Modification of kaolinite surfaces through mechanochemical treatment—a mid-IR and near-IR spectroscopic study

    NASA Astrophysics Data System (ADS)

    Frost, R. L.; Makó, É.; Kristóf, J.; Kloprogge, J. T.

    2002-11-01

    The modification of kaolinite surfaces through mechanochemical treatment has been studied using a combination of mid-IR and near-IR spectroscopy. Kaolinite hydroxyls were lost after 10 h of grinding as evidenced by the decrease in intensity of the OH stretching vibrations at 3695 and 3619 cm -1 and the deformation modes at 937 and 915 cm -1. Concomitantly an increase in the hydroxyl-stretching vibrations of water is observed. The mechanochemical activation (dry grinding) causes destruction in the crystal structure of kaolinite by the rupture of the OH, AlOH, AlOSi and SiO bonds. Evidence of this destruction may be followed using near-IR spectroscopy. Two intense bands are observed in the spectral region of the first overtone of the hydroxyl-stretching vibration at 7065 and 7163 cm -1. These two bands decrease in intensity with mechanochemical treatment and two new bands are observed at 6842 and 6978 cm -1 assigned to the first overtone of the hydroxyl-stretching band of water. Concomitantly the water combination bands observed at 5238 and 5161 cm -1 increase in intensity with mechanochemical treatment. The destruction of the kaolinite surface may be also followed by the loss of intensity of the two hydroxyl combination bands at 4526 and 4623 cm -1. Infrared spectroscopy shows that the kaolinite surface has been modified by the removal of the kaolinite hydroxyls and their replacement with water adsorbed on the kaolinite surface. NIR spectroscopy enables the determination of the optimum time for grinding of the kaolinite. Further NIR allows the possibility of continual on-line analysis of the mechanochemical treatment of kaolinite.

  13. Liquid crystal near-IR laser beam shapers employing photoaddressable alignment layers for high-peak-power applications

    NASA Astrophysics Data System (ADS)

    Marshall, Kenneth L.; Saulnier, Debra; Xianyu, Haiqing; Serak, Svetlana; Tabiryan, Nelson

    2013-09-01

    Large-scale, high-energy Nd:glass laser systems require beam shapers to control the spatial distribution of the incident intensity. Commercially available liquid crystal (LC) electro-optical spatial light modulators (SLM's) are frequently employed for this purpose, but their intrinsic requirement for conductive metal or metal-oxide coatings limits their 1054-nm laser-damage thresholds to 230 mJ/cm2 (2.4 ns, 5 Hz), relegating them for use only in low-fluence areas of the laser system. Previously, we demonstrated that passive near-IR LC beam shapers employing coumarin alignment layers patterned by contact photolithography are capable of high resolution and contrast and can withstand incident 1054-nm laser-fluence levels of <30 J/cm2 (1-ns pulse). An evolutionary step to expand the scope of this simple and robust device would be to identify and incorporate into the device structure photoalignment layers that trigger LC bulk reorientation by undergoing reversible optical switching between two predetermined alignment patterns using low-energy polarized UV/visible incident light and have a high near-IR laser-damage threshold. Such "optically driven" LC beam shapers offer the in-system write/erase flexibility of the electro-optical LC SLM's while eliminating conductive coatings that compromise the laser-damage threshold and electrical interconnects that increase device fragility and complexity. To this end, we have recently identified and evaluated the 1054-nm laser-damage-resistance and coating properties of several commercial azobenzene-based photoswitchable alignment materials. In 1-on-1 and N-on-1 testing, these new materials displayed 1054-nm laser-damage thresholds that compare very favorably to those of previously tested coumarin photoalignment materials (30 to 60 J/cm2).

  14. Image-guided removal of occlusal caries lesions with a λ= 9.3-µm CO2 laser using near-IR transillumination

    PubMed Central

    Chung, Leon C.; Tom, Henry; Chan, Kenneth H.; Simon, Jacob C.; Fried, Daniel; Darling, Cynthia L.

    2015-01-01

    Previous studies have shown that near-IR transillumination is well suited for imaging deep occlusal lesions. The purpose of this study was to determine if near-IR images can be used to guide a CO2 laser for the selective removal of natural occlusal lesions on extracted teeth. Near-IR occlusal transillumination images of extracted human teeth with natural occlusal caries lesions were acquired using an InGaAs camera and near-IR light at wavelengths from 1290 to 1470-nm from a filtered tungsten halogen source. A CO2 laser operating at 9.3-µm with a pulse duration of 10–15-µs and a pulse repetition rate of 100–300-Hz was used for caries removal. Optical Coherence tomography was used to confirm lesion presence and serial scans were used to assess selective removal. Teeth were also sectioned for histological examination using polarized light microscopy. This study suggests that near-infrared transillumination is a promising method for the image guided laser ablation of occlusal caries lesions but the use of serial near-IR transillumination imaging for monitoring lesion removal was limited. PMID:25914498

  15. Image-guided removal of occlusal caries lesions with a λ= 9.3-μm CO2 laser using near-IR transillumination

    NASA Astrophysics Data System (ADS)

    Chung, Leon C.; Tom, Henry; Chan, Kenneth H.; Simon, Jacob C.; Fried, Daniel; Darling, Cynthia L.

    2015-02-01

    Previous studies have shown that near-IR transillumination is well suited for imaging deep occlusal lesions. The purpose of this study was to determine if near-IR images can be used to guide a CO2 laser for the selective removal of natural occlusal lesions on extracted teeth. Near-IR occlusal transillumination images of extracted human teeth with natural occlusal caries lesions were acquired using an InGaAs camera and near-IR light at wavelengths from 1290 to 1470-nm from a filtered tungsten halogen source. A CO2 laser operating at 9.3-μm with a pulse duration of 10-15-μs and a pulse repetition rate of 100-300-Hz was used for caries removal. Optical Coherence tomography was used to confirm lesion presence and serial scans were used to assess selective removal. Teeth were also sectioned for histological examination using polarized light microscopy. This study suggests that near-infrared transillumination is a promising method for the image guided laser ablation of occlusal caries lesions but the use of serial near-IR transillumination imaging for monitoring lesion removal was limited.

  16. ESO's User Portal: lessons learned

    NASA Astrophysics Data System (ADS)

    Chavan, A. M.; Tacconi-Garman, L. E.; Peron, M.; Sogni, F.; Dorigo, D.; Nass, P.; Fourniol, N.; Sforna, D.; Haggouchi, K.; Dolensky, M.

    2008-07-01

    ESO introduced a User Portal for its scientific services in November 2007. Registered users have a central entry point for the Observatory's offerings, the extent of which depends on the users' roles - see [1]. The project faced and overcame a number of challenging hurdles between inception and deployment, and ESO learned a number of useful lessons along the way. The most significant challenges were not only technical in nature; organization and coordination issues took a significant toll as well. We also indicate the project's roadmap for the future.

  17. Graphitic carbon nitride C{sub 6}N{sub 9}H{sub 3}.HCl: Characterisation by UV and near-IR FT Raman spectroscopy

    SciTech Connect

    McMillan, Paul F.; Lees, Victoria; Quirico, Eric; Sella, Andrea; Reynard, Bruno; Simon, Patrick; Bailey, Edward; Deifallah, Malek; Cora, Furio

    2009-10-15

    The graphitic layered compound C{sub 6}N{sub 9}H{sub 3}.HCl was prepared by reaction between melamine and cyanuric chloride under high pressure-high temperature conditions in a piston cylinder apparatus and characterised using SEM, powder X-ray diffraction, UV Raman and near-IR Fourier transform Raman spectroscopy with near-IR excitation. Theoretical calculations using density functional methods permitted evaluation of the mode of attachment of H atoms to nitrogen sites in the structure and a better understanding of the X-ray diffraction pattern. Broadening in the UV and near-IR FT Raman spectra indicate possible disordering of the void sites within the graphitic layers or it could be due to electron-phonon coupling effects. - Graphical abstract: The graphitic layered compound C{sub 6}N{sub 9}H{sub 3}.HCl was prepared by reaction between melamine and cyanuric chloride under high pressure-high temperature conditions in a piston cylinder apparatus and characterised using SEM, powder X-ray diffraction, UV Raman and near-IR Fourier transform Raman spectroscopy using near-IR excitation. Theoretical calculations using density functional methods permitted evaluation of the mode of attachment of H atoms to nitrogen sites around the C{sub 12}N{sub 12} voids within the layered structure and also led to better understanding of the X-ray diffraction pattern. Sharp peaks in the UV Raman spectra are due to C{sub 3}N{sub 3} triazine ring units in the structure, that may be enhanced by resonance Raman effects. Broadening in the UV and near-IR FT Raman spectra indicate possible disordering within the graphitic layers or electron-phonon coupling effects.

  18. ESO PR Highlights in 2005

    NASA Astrophysics Data System (ADS)

    2006-01-01

    2005 was the year of Physics. It was thus also in part the year of astronomy and this is clearly illustrated by the numerous breakthroughs that were achieved, in particular using ESO's telescopes. One of the highlights was without any doubt the confirmation of the first image of an exoplanet , around the star 2M1207 (see ESO PR 12/05). ESO's telescopes also found a Neptune-mass exoplanet around a small star ( PR 30/05) - a discovery that proves crucial in the census of other planetary systems, and imaged a tiny companion in the close vicinity of the star GQ Lupi, a very young object still surrounded by a disc, with an age between 100,000 and 2 million years ( PR 09/05). Moreover, using a new high-contrast adaptive optics camera on the VLT, the NACO Simultaneous Differential Imager, or NACO SDI, astronomers were able for the first time to image a companion 120 times fainter than its star , very near the star AB Doradus A. This companion appears to be almost twice as heavy as theory predicts it to be ( PR 02/05). ESO's telescopes proved very useful in helping to solve a 30-year old puzzle . Astronomers have for the first time observed the visible light from a short gamma-ray burst (GRB). Using the 1.5m Danish telescope at La Silla (Chile), they showed that these short, intense bursts of gamma-ray emission most likely originate from the violent collision of two merging neutron stars ( PR 26/05). Additional evidence came from witnessing another event with the VLT ( PR 32/05). Also in this field, astronomers found the farthest known gamma-ray burst with ESO's VLT, observing an object with a redshift 6.3, i.e. that is seen when the Universe was less than 900 million years old ( PR 22/05). On July 4, NASA's Deep Impact spacecraft plunged onto Comet 9P/Tempel 1 with the aim to create a crater and expose pristine material from beneath the surface. For two days before and six days after, all major ESO telescopes have been observing the comet, in a coordinated fashion and in

  19. Summertime Coincident Observations of Ice Water Path in the Visible/Near-IR, Radar, and Microwave Frequencies

    NASA Technical Reports Server (NTRS)

    Pittman, Jasna V.; Robertson, Franklin R.; Atkinson, Robert J.

    2008-01-01

    Accurate representation of the physical and radiative properties of clouds in climate models continues to be a challenge. At present, both remote sensing observations and modeling of microphysical properties of clouds rely heavily on parameterizations or assumptions on particle size distribution (PSD) and cloud phase. In this study, we compare Ice Water Path (IWP), an important physical and radiative property that provides the amount of ice present in a cloud column, using measurements obtained via three different retrieval strategies. The datasets we use in this study include Visible/Near-IR IWP from the Moderate Resolution Imaging Spectroradiometer (MODIS) instrument flying aboard the Aqua satellite, Radar-only IWP from the CloudSat instrument operating at 94 GHz, and NOAA/NESDIS operational IWP from the 89 and 157 GHz channels of the Microwave Humidity Sounder (MHS) instrument flying aboard the NOAA-18 satellite. In the Visible/Near-IR, IWP is derived from observations of optical thickness and effective radius. CloudSat IWP is determined from measurements of cloud backscatter and assumed PSD. MHS IWP retrievals depend on scattering measurements at two different, non-water absorbing channels, 89 and 157 GHz. In order to compare IWP obtained from these different techniques and collected at different vertical and horizontal resolutions, we examine summertime cases in the tropics (30S - 30N) when all 3 satellites are within 4 minutes of each other (approximately 1500 km). All measurements are then gridded to a common 15 km x 15 km box determined by MHS. In a grid box comparison, we find CloudSat to report the highest IWP followed by MODIS, followed by MHS. In a statistical comparison, probability density distributions show MHS with the highest frequencies at IWP of 100-1000 g/m(exp 2) and CloudSat with the longest tail reporting IWP of several thousands g/m(exp 2). For IWP greater than 30 g/m(exp 2), MODIS is consistently higher than CloudSat, and it is higher at

  20. The 3D Structure of Eta Carinae's Nebula: A Definitive Picture from High-Dispersion Near-IR Spectra

    NASA Technical Reports Server (NTRS)

    Smith, N.

    2006-01-01

    High resolution long-slit spectra obtained with the Phoenix spectrograph on Gemini South provide our most accurate probe of the 3D structure of the Homunculus Nebula around Eta Carinae. Emission from molecular hydrogen at 2.122 microns traces a very thin outer skin, which contains the vast majority of the more than 10 solar masses of material in the nebula. This emission, in turn, yields our first definitive picture of the exact shape of the nebula, plus the latitude dependence of the mass-loss rate, speed, kinetic energy, shell thickness, and other properties associated with Eta Car's 19th century explosion. This will be critical for testing any models for the outburst mechanism. A preliminary analysis suggests that explosion from a critically rotating star was the dominant mechanism that gave rise to both the bipolar shape of the nebula and the production of its equatorial disk. [Fe II] emission in the near IR traces a geometrically thicker but less massive shell found on the inner surface of the H2 skin --- this is either a reverse shock that decelerates Eta Car's wind or a warm PDR. [Fe Ill emission also clarifies the structure of an inner "Little Homunculus" seen previously in HST/STlS spectra. Comparing these two tracers of cool molecular gas and warm partially-ionized gas resolves some significant confusion about the complex structure noted in previous studies.

  1. VARIABILITY AT THE EDGE: OPTICAL NEAR/IR RAPID-CADENCE MONITORING OF NEWLY OUTBURSTING FU ORIONIS OBJECT HBC 722

    SciTech Connect

    Green, Joel D.; Robertson, Paul; Pak, Soojong; Meschiari, Stefano; Baek, Giseon; Lee, Jeong-Eun; Pooley, David; Im, Myungshin; Jeon, Yiseul; Choi, Changsu

    2013-02-10

    We present the detection of day-timescale periodic variability in the r-band lightcurve of newly outbursting FU Orionis-type object HBC 722, taken from >42 nights of observation with the CQUEAN instrument on the McDonald Observatory 2.1 m telescope. The optical/near-IR lightcurve of HBC 722 shows a complex array of periodic variability, clustering around 5.8-day (0.044 mag amplitude) and 1.28-day (0.016 mag amplitude) periods, after removal of overall baseline variation. We attribute the unusual number of comparable strength signals to a phenomenon related to the temporary increase in accretion rate associated with FUors. We consider semi-random 'flickering', magnetic braking/field compression and rotational asymmetries in the disk instability region as potential sources of variability. Assuming that the 5.8-day period is due to stellar rotation and the 1.28-day period is indicative of Keplerian rotation at the inner radius of the accretion disk (at 2 R {sub *}), we derive a B-field strength of 2.2-2.7 kG, slightly larger than typical T Tauri stars. If instead the 5.8-day signal is from a disk asymmetry, the instability region has an outer radius of 5.4 R {sub *}, consistent with models of FUor disks. Further exploration of the time domain in this complicated source and related objects will be key to understanding accretion processes.

  2. Near-IR High-Resolution Imaging Polarimetry of the SU Aur Disk: Clues for Tidal Tails?

    NASA Technical Reports Server (NTRS)

    De Leon, Jerome; Michihiro, Takami; Karr, Jennifer; Hashimoto, Jun; Kudo, Tomoyuki; Sitko, Michael; Mayama, Satoshi; Kusakabe, Nobuyuki; Grady, Carol A.; McElwain, Michael W.

    2015-01-01

    We present new high-resolution (approximately 0.09) H-band imaging observations of the circumstellar disk around the T Tauri star SU Aur. Our observations with Subaru-HiCIAO have revealed the presence of scattered light as close as 0.15 (approximately 20 AU) to the star. Within our image, we identify bright emission associated with a disk with a minimum radius of approximately 90 AU, an inclination of approximately 35 deg from the plane of the sky, and an approximate PA of 15 deg for the major axis. We find a brightness asymmetry between the northern and southern sides of the disk due to a non-axisymmetric disk structure. We also identify a pair of asymmetric tail structures extending east and west from the disk. The western tail extends at least 2. 5 (350 AU) from the star, and is probably associated with a reflection nebula previously observed at optical and near-IR wavelengths. The eastern tail extends at least 1 (140 AU) at the present signal-to-noise. These tails are likely due to an encounter with an unseen brown dwarf, but our results do not exclude the explanation that these tails are outflow cavities or jets.

  3. ZnSe hollow nanospheres in mechanically stable near-IR antireflection coatings for ZnSe substrates

    NASA Astrophysics Data System (ADS)

    Li, Chao; Luo, Rui-Chun; Mao, Yong-Qiang; Du, Xi-Wen; Yang, Jing

    2016-09-01

    Though possessing low absorption throughout a wide infrared (IR) spectral regime, owing to a high refractive index, zinc selenide substrates are generally covered by antireflection coatings (ARCs) for practical optical uses. However, achieving a high transmission of ZnSe substrates in the near-IR (NIR) region is still challenging. Herein, for the first time, colloidal ZnSe hollow nanospheres (HNSs) smaller than 100 nm were prepared and adopted to assemble ARCs for ZnSe substrates. The voiding kinetics of the HNSs was found to agree well with the nanoscale Kirkendall effect, and the self-diffusion of the Zn ion in the core was faster than its diffusion through the ZnSe shell. With single-index ARCs, the transmission of ZnSe substrates was remarkably enhanced in the NIR region, with up to an 18% increase at 840 nm. Besides, the ZnSe HNS-based ARCs showed superior mechanical stability even under violent ultrasonication in organic solutions. We expect that ZnSe HNSs will make it possible to construct graded-index ARCs to realize omnidirectional and broadband antireflection in IR, through further tuning of HNSs’ void fraction.

  4. Thiocyanate-free asymmetric ruthenium(II) dye sensitizers containing azole chromophores with near-IR light-harvesting capacity

    NASA Astrophysics Data System (ADS)

    Wu, Guohua; Kaneko, Ryuji; Islam, Ashraful; Zhang, Yaohong; Sugawa, Kosuke; Han, Liyuan; Shen, Qing; Bedja, Idriss; Gupta, Ravindra Kumar; Otsuki, Joe

    2016-11-01

    A new series of thiocyanate-free bis-tridentate Ru(II) complexes containing azole ligands as well as an organometallic Ru-C bond are synthesized, characterized, and evaluated in dye-sensitized solar cells (DSSCs). CF3-substituted pyrazolyl, CF3-substituted triazolyl, and tetrazolyl derivatives are employed as ligands in the three neutral complexes PYZ, TRZ, and TEZ dyes, respectively. Despite their different structures, all the three complexes exhibit similar absorption features and panchromatic absorption covering the visible and near-IR regions. By switching from a pyrazolyl via triazolyl to tetrazolyl moiety in the ligand, the photocurrent value, open-circuit voltage, and overall efficiency are increased accordingly under the same conditions. Among them, photon-to-current conversion efficiency (ƞ) of TEZ dye reaches the maximum of 6.44% with a short-circuit photocurrent density (Jsc) of 17.8 mA cm-2, an open-circuit photovoltage (Voc) of 0.54 V and fill factor (FF) of 0.67 under illumination of an AM1.5G solar simulator. TEZ dye shows a good long term light soaking stability and maintains up to more than 90% of the initial power conversion efficiency after 1000 h.

  5. UV-stimulated near-IR emission of Pr3+ in phosphate glass via twofold-coordinated Sn centers

    NASA Astrophysics Data System (ADS)

    Jiménez, José A.; Sendova, Mariana; Rosim Fachini, Esteban

    2014-11-01

    The optical properties of Pr2O3 and SnO co-doped barium-phosphate glass prepared by the melt-quenching technique have been investigated. Optical absorption and X-ray photoelectron spectroscopy (XPS) are employed in the characterization of tin species. The prevalence of divalent tin is indicated by the XPS data in accord with a conspicuous absorption band detected around 287 nm ascribed to twofold-coordinated Sn centers (isoelectronic with Sn2+). Upon ultraviolet (UV) photoexcitation of the tin centers, near-infrared (IR) emission from Pr3+ ions is realized. An excitation spectrum acquired by monitoring Pr3+ emission from the 1D2 state at 1.03 μm revealed a broad band around 290 nm consistent with a Snsbnd Pr donor-acceptor energy transfer channel. The data supports a mechanism starting with the singlet-to-singlet UV excitation of Sn centers, followed by the intersystem crossing populating their triplet states emitting in the visible. From these, energy transfer occurs to 3P0, 3P1, 1I6, and 3P2 resonant states in Pr3+, from which the near-IR emitting states 1D2 and 1G4 are populated.

  6. Evidence for Interlayer Collapse of Nontronite on Mars from Laboratory Visible and Near-IR Reflective Spectra

    NASA Technical Reports Server (NTRS)

    Morris, Richard V.; Ming, D. W.; Golden, D. C.; Graff, T. G.; Achilles, C. N.

    2010-01-01

    Dioctahedral smectites (e.g., nontronite and montmorillionite) are interpreted to occupy the optical surface of Mars at a number of locations on the basis of spectral features derived from interlayer H2O and MOH (M=Fe(3+)2, Fe(3+)Al, Al2, etc.) as observed by orbiting MRO-CRISM and MEx-OMEGA hyperspectral imaging spectrometers. At wavelengths shorter than approximately 2.7 micrometers, the strongest bands from interlayer H2O occur at approximately 1.4 and 1.9 micrometers from 2v1 and v1+v2, respectively, where v1 and v2 are the fundamental stretching and bending vibrations of the H2O molecule. Smectite MOH vibrations occur near 1.4 micrometers (stretching overtone) and in the region between 2.1 and 2.7 micrometers (stretching + bending combination). Because interlayer H2O can exchange with the martian environment, a number of studies have examined the strength of the interlayer H2O spectral features under Mars-like environmental conditions. The relationship between spectral properties and the underlying crystal structure of the smectites was not determined, and the extent of interlayer H2O removal was not established. We report combined visible and near-IR (VNIR), Mossbauer (MB), and powder X-ray diffraction (XRD) data for samples of the Fe-bearing smectite nontronite where the interlayer was collapsed by complete removal of interlayer H2O.

  7. ZnSe hollow nanospheres in mechanically stable near-IR antireflection coatings for ZnSe substrates.

    PubMed

    Li, Chao; Luo, Rui-Chun; Mao, Yong-Qiang; Du, Xi-Wen; Yang, Jing

    2016-09-01

    Though possessing low absorption throughout a wide infrared (IR) spectral regime, owing to a high refractive index, zinc selenide substrates are generally covered by antireflection coatings (ARCs) for practical optical uses. However, achieving a high transmission of ZnSe substrates in the near-IR (NIR) region is still challenging. Herein, for the first time, colloidal ZnSe hollow nanospheres (HNSs) smaller than 100 nm were prepared and adopted to assemble ARCs for ZnSe substrates. The voiding kinetics of the HNSs was found to agree well with the nanoscale Kirkendall effect, and the self-diffusion of the Zn ion in the core was faster than its diffusion through the ZnSe shell. With single-index ARCs, the transmission of ZnSe substrates was remarkably enhanced in the NIR region, with up to an 18% increase at 840 nm. Besides, the ZnSe HNS-based ARCs showed superior mechanical stability even under violent ultrasonication in organic solutions. We expect that ZnSe HNSs will make it possible to construct graded-index ARCs to realize omnidirectional and broadband antireflection in IR, through further tuning of HNSs' void fraction.

  8. Near-IR imaging of interproximal lesions from occlusal surfaces and the influence of stains and plaque

    NASA Astrophysics Data System (ADS)

    Fried, Daniel; Bühler, Christopher M.; Ngaotheppitak, Patara; Darling, Cynthia L.

    2006-02-01

    Dental enamel manifests high transparency in the near-IR (NIR). Our previous work demonstrated that NIR light at 1310-nm is ideally suited for the transillumination of interproximal dental caries (dental decay in between teeth) and that it can also be used to image decay in the pits and fissures of the occlusal (biting) surfaces of posterior teeth where most new dental decay occurs. Early occlusal lesions cannot be detected by x-rays during the early stages of lesion development due to the overlapping topography of the crown of the tooth. Stains and non-calcified plaque are not visible in the NIR enabling better discrimination of demineralized areas. We also demonstrate that interproximal lesions can be imaged from the occlusal surface (from above). Moreover, multiple illumination and detector angles can be exploited for optimal contrast between caries and sound tissue. These measurements suggest that NIR imaging offers significant advantages over the conventional visual, tactile and radiographic caries detection methods and other optical caries detection and imaging techniques.

  9. ZnSe hollow nanospheres in mechanically stable near-IR antireflection coatings for ZnSe substrates.

    PubMed

    Li, Chao; Luo, Rui-Chun; Mao, Yong-Qiang; Du, Xi-Wen; Yang, Jing

    2016-09-01

    Though possessing low absorption throughout a wide infrared (IR) spectral regime, owing to a high refractive index, zinc selenide substrates are generally covered by antireflection coatings (ARCs) for practical optical uses. However, achieving a high transmission of ZnSe substrates in the near-IR (NIR) region is still challenging. Herein, for the first time, colloidal ZnSe hollow nanospheres (HNSs) smaller than 100 nm were prepared and adopted to assemble ARCs for ZnSe substrates. The voiding kinetics of the HNSs was found to agree well with the nanoscale Kirkendall effect, and the self-diffusion of the Zn ion in the core was faster than its diffusion through the ZnSe shell. With single-index ARCs, the transmission of ZnSe substrates was remarkably enhanced in the NIR region, with up to an 18% increase at 840 nm. Besides, the ZnSe HNS-based ARCs showed superior mechanical stability even under violent ultrasonication in organic solutions. We expect that ZnSe HNSs will make it possible to construct graded-index ARCs to realize omnidirectional and broadband antireflection in IR, through further tuning of HNSs' void fraction. PMID:27482737

  10. The Type IIP SN 2005ay: An Extensive Study From UltraViolet To Near-IR

    NASA Astrophysics Data System (ADS)

    Bufano, F. M.; Turatto, M.; Zampieri, L.; Gal-Yam, A.

    2006-08-01

    Several supernova types are thought to explode via the gravitational collapse of the core of massive stars at the end of their lifetimes. The great observational diversity has not been fully understood even if it clearly involves the progenitor masses and configurations at the time of explosion. These Supernovae, called Core Collapse Supernovae (CC SNe), are expected to dominate the counts of SNe observed at high redshifts and to be the only observable probe of the first generation stars (Pop III). Recently indicated as reliable distance indicators (Hamuy 02, Pastorello `03), CC SNe are objects of great interest but significantly less studied in comparison with the Termonuclear ones. With the aim to understand better the reasons of the heterogeneous behaviour , we have started an extensive study of the properties of SN II with different observational features (luminosity, velocity, etc..). Here we present the last results on our first observed target, SN2005ay, a Type IIP supernova observed in an extended way from the Ultraviolet wavelengths, provided by the GALEX , to the Optical and near-IR , obtained with IISP (Italian Intensive Supernova Program).

  11. Effects of Palagonitic Dust Coatings on Visible, Near-IR, and Mossbauer Spectra of Rocks and Minerals: Implication for Mineralogical Remote Sensing of Mars

    NASA Technical Reports Server (NTRS)

    Morris, R.; Graff, T. G.; Shelfer, T. D.; Bell, J. F., III

    2001-01-01

    Visible, near-IR, and Mossbauer measurements on dust coated rocks and minerals show that a 300 5m thick layer is required to obscure the substrate for VNIR measurements and that a greater than 2000-micron-thick layer is required to obscure the substrate for Mossbauer measurements. Additional information is contained in the original extended abstract.

  12. The ESO Educational Office Reaches Out towards Europe's Teachers

    NASA Astrophysics Data System (ADS)

    2001-12-01

    ESA/ESO Astronomy Exercises Provide a Taste of Real Astronomy [1] Summary The European Southern Observatory (ESO) has been involved in many Europe-wide educational projects during the past years, in particular within European Science Weeks sponsored by the European Commission (EC). In order to further enhance the significant educational potential inherent in the numerous scientific endeavours now carried out by Europe's astronomers with ESO front-line telescope facilities, it has been decided to set up an Educational Office within the ESO EPR Department. It will from now on work closely with astronomy-oriented teachers, in particular at the high-school level , providing support, inspiration and new materials. Much of this interaction will happen via the European Association for Astronomy Education (EAAE) In this context, and in collaboration with the European Space Agency (ESA) , the first instalments of the "ESA/ESO Astronomy Exercise Series" have just been published, on the web ( http://www.astroex.org ) and in print (6 booklets totalling 100 pages; provided free-of-charge to teachers on request). They allow 16-19 year old students to gain exciting hands-on experience in astronomy, making realistic calculations with data obtained from observations by some of the world's best telescopes, the NASA/ESA Hubble Space Telescope (HST) and ESO's Very Large Telescope (VLT) . PR Photo 36/01 : The "ESA/ESO Astronomy Exercise Series" . Educational projects at ESO The European Southern Observatory (ESO) , through its Education and Public Relations Department (EPR) , has long been involved in educational activities, in particular by means of Europe-wide projects during successive European Science Weeks , with support from the European Commission (EC) . A most visible outcome has been the creation of the trailblazing European Association for Astronomy Education (EAAE) - this was first discussed at an international meeting at the ESO Headquarters in November 1994 with the

  13. New low bandgap near-IR conjugated D-A copolymers for BHJ polymer solar cell applications.

    PubMed

    Keshtov, M L; Kuklin, S A; Radychev, N A; Nikolaev, A Y; Ostapov, I E; Krayushkin, M M; Konstantinov, I O; Koukaras, E N; Sharma, Abhishek; Sharma, G D

    2016-03-28

    We synthesized two novel ultra low bandgap donor-acceptor (D-A) copolymers (E(g) ≤ 1.2 eV), containing the thiadiazoloquinoxaline unit as the main electron accepting unit (A) and benzodithiophene (BDT) and dithienosilole (DTS) as different donor units (D), denoted as P1 and P2, respectively, using the cross-coupling Stille reaction. The copolymers possess light absorption ranging from UV (350 nm) to near-IR (1300 nm) with optical bandgaps of 1.16 eV and 1.08 eV, respectively. Quantum-chemical calculations and experimental data were compared for proposing a more detailed concept for the optical and electronic properties of these copolymers which can be used as donors for polymer solar cells (PSCs). The PSCs based on optimized P1:PC71BM and P2:PC71BM showed overall power conversion efficiencies (PCEs) of 4.32% and 3.48%, respectively. Although P2 possesses a broad absorption coverage of up to 1300 nm, the lower PCE may be attributed to the low J(sc), due to the poor driving force for exciton dissociation, since the LUMO offset with PC71BM is less than 0.3 eV. The PCE has been significantly increased to 7.27% and 6.68% for solvent vapor annealing (SVA) treated P1:PC71BM and P2:PC71BM active layers, respectively. This improvement arises from the appropriate nanoscale morphology and an increase in hole mobility, induced by the SVA treatment of the active layers.

  14. An optical-near-IR study of a triplet of super star clusters in the starburst core of M82

    SciTech Connect

    Westmoquette, M. S.; Bastian, N.; Smith, L. J.; Seth, A. C.; Gallagher III, J. S.; Ryon, J. E.; O'Connell, R. W.; Silich, S.; Mayya, Y. D.; González, D. Rosa; Muñoz-Tuñón, C.

    2014-07-10

    We present HST/STIS optical and Gemini/NIFS near-IR IFU spectroscopy and archival Hubble Space Telescope (HST) imaging of the triplet of super star clusters (A1, A2, and A3) in the core of the M82 starburst. Using model fits to the Space Telescope Imaging Spectrograph (STIS) spectra and the weakness of red supergiant CO absorption features (appearing at ∼6 Myr) in the NIFS H-band spectra, the ages of A2 and A3 are 4.5 ± 1.0 Myr. A1 has strong CO bands, consistent with our previously determined age of 6.4 ± 0.5 Myr. The photometric masses of the three clusters are 4-7 × 10{sup 5} M{sub ☉}, and their sizes are R{sub eff} = 159, 104, 59 mas (∼2.8, 1.8, 1.0 pc) for A1, A2, and A3. The STIS spectra yielded radial velocities of 320 ± 2, 330 ± 6, and 336 ± 5 km s{sup –1} for A1, A2, and A3, placing them at the eastern end of the x{sub 2} orbits of M82's bar. Clusters A2 and A3 are in high-density (800-1000 cm{sup –3}) environments, and like A1, are surrounded by compact H II regions. We suggest the winds from A2 and A3 have stalled, as in A1, due to the high ISM ambient pressure. We propose that the three clusters were formed in situ on the outer x{sub 2} orbits in regions of dense molecular gas subsequently ionized by the rapidly evolving starburst. The similar radial velocities of the three clusters and their small projected separation of ∼25 pc suggest that they may merge in the near future unless this is prevented by velocity shearing.

  15. Near-IR excitation transfer and electron transfer in a BF2-chelated dipyrromethane-azadipyrromethane dyad and triad.

    PubMed

    El-Khouly, Mohamed E; Amin, Anu N; Zandler, Melvin E; Fukuzumi, Shunichi; D'Souza, Francis

    2012-04-23

    A molecular dyad and triad, comprised of a known photosensitizer, BF(2)-chelated dipyrromethane (BDP), covalently linked to its structural analog and near-IR emitting sensitizer, BF(2)-chelated tetraarylazadipyrromethane (ADP), have been newly synthesized and the photoinduced energy and electron transfer were examined by femtosecond and nanosecond laser flash photolysis. The structural integrity of the newly synthesized compounds has been established by spectroscopic, electrochemical, and computational methods. The DFT calculations revealed a molecular-clip-type structure for the triad, in which the BDP and ADP entities are separated by about 14 Å with a dihedral angle between the fluorophores of around 70°. Differential pulse voltammetry studies have revealed the redox states, allowing estimation of the energies of the charge-separated states. Such calculations revealed a charge separation from the singlet excited BDP ((1)BDP*) to ADP (BDP(.+)-ADP(.-)) to be energetically favorable in nonpolar toluene and in polar benzonitrile. In addition, the excitation transfer from the singlet BDP to ADP is also envisioned due to good spectral overlap of the BDP emission and ADP absorption spectra. Femtosecond laser flash photolysis studies provided concrete evidence for the occurrence of energy transfer from (1)BDP* to ADP (in benzonitrile and toluene) and electron transfer from BDP to (1)ADP* (in benzonitrile, but not in toluene). The kinetic study of energy transfer was measured by monitoring the rise of the ADP emission and revealed fast energy transfer (ca. 10(11) s(-1)) in these molecular systems. The kinetics of electron transfer via (1)ADP*, measured by monitoring the decay of the singlet ADP at λ=820 nm, revealed a relatively fast charge-separation process from BDP to (1)ADP*. These findings suggest the potential of the examined ADP-BDP molecules to be efficient photosynthetic antenna and reaction center models. PMID:22416038

  16. ESO PR Highlights in 2006

    NASA Astrophysics Data System (ADS)

    2007-01-01

    Last year proved to be another exceptional year for the European organisation for ground-based astronomy. ESO should begin the New Year with two new member states: Spain (PR 05/06) and the Czech Republic (PR 52/06). ESO PR Highlights 2006 2006 was a year of renovation and revolution in the world of planets. A new Earth-like exoplanet has been discovered (PR 03/06) using a network of telescopes from all over the world (including the Danish 1.54-m one at ESO La Silla). It is not the only child of this fruitful year: thanks to the combined use of ESO's Very Large Telescope (VLT) and La Silla instruments, a surprising system of twin giant exoplanets was found (PR 29/06), and a trio of Neptune-like planets hosted by a nearby star were identified (PR 18/06). These results open new perspectives on the search for habitable zones and on the understanding of the mechanism of planet formation. The VISIR instrument on the VLT has been providing unique information to answer this last question, by supplying a high resolution view of a planet-forming disc (PR 36/06). There are not only new members in the planets' register: during the General Assembly of the International Astronomical Union held in Prague (Czech Republic), it was decided that Pluto is not a planet anymore but a 'dwarf planet'. Whatever its status, Pluto still has a satellite, Charon, whose radius and density have been measured more accurately by observing a rare occultation from different sites, including Cerro Paranal (PR 02/06). The scientific community dedicated 2006 to the great physicist James Clerk Maxwell (it was the 175th anniversary of the birth): without his electromagnetic theory of light, none of the astonishing discoveries of modern physics could have been achieved. Nowadays we can look at distant galaxies in great detail: the GIRAFFE spectrograph on the VLT revealed that galaxies 6 billion years ago had the same amount of dark matter relative to stars than nowadays (PR 10/06), while SINFONI gave an

  17. ESO Director General to Become President of AUI

    NASA Astrophysics Data System (ADS)

    1998-11-01

    scientific awards for his work. Prof. Giacconi is a member of the U.S. National Academy of Sciences and the American Academy of Arts and Sciences. He is the author of books as well as more than 200 scientific publications. Note: [1] This is a joint Press Release of ESO and AUI (URL: http://www.aui.edu/ ). How to obtain ESO Press Information ESO Press Information is made available on the World-Wide Web (URL: http://www.eso.org ). ESO Press Photos may be reproduced, if credit is given to the European Southern Observatory.

  18. The ESO Observing Programmes Committee

    NASA Astrophysics Data System (ADS)

    Westerlund, B. E.

    1982-06-01

    Since 1978 the ESO Observing Programmes Committee (OPC) has "the function to inspect and rank the proposals made for observing programmes at La Silla, and thereby to advise the Director General on the distribution of observing time". The members (one from each member country) and their alternates are nominated by the respective national committees for five-year terms (not immediately renewable). The terms are staggered so that each year one or two persons are replaced. The Chairman is appointed annually by the Council. He is invited to attend Council meetings and to report to its members.

  19. Faecal near-IR spectroscopy to determine the nutritional value of diets consumed by beef cattle in east Mediterranean rangelands.

    PubMed

    Landau, S Y; Dvash, L; Roudman, M; Muklada, H; Barkai, D; Yehuda, Y; Ungar, E D

    2016-02-01

    Rapid assessment of the nutritional quality of diets ingested by grazing animals is pivotal for successful cow-calf management in east Mediterranean rangelands, which receive unpredictable rainfall and are subject to hot-spells. Clipped vegetation samples are seldom representative of diets consumed, as cows locate and graze selectively. In contrast, faeces are easily sampled and their near-IR spectra contain information about nutrients and their utilization. However, a pre-requisite for successful faecal near-infrared reflectance spectroscopy (FNIRS) is that the calibration database encompass the spectral variability of samples to be analyzed. Using confined beef cows in Northern and Southern Israel, we calibrated prediction equations based on individual pairs of known dietary attributes and the NIR spectra of associated faeces (n=125). Diets were composed of fresh-cut green fodder of monocots (wheat and barley), dicots (safflower and garden pea) and natural pasture collected at various phenological states over 2 consecutive years, and, optionally, supplements of barley grain and dried poultry litter. A total of 48 additional pairs of faeces and diets sourced from cows fed six complete mixed rations covering a wide range of energy and CP concentrations. Precision (linearity of calibration, R2cal, and of cross-validation, R2cv) and accuracy (standard error of cross-validation, SEcv) were criteria for calibration quality. The calibrations for dietary ash, CP, NDF and in vitro dry matter digestibility yielded R2cal values >0.87, R2cv of 0.81 to 0.89 and SEcv values of 16, 13, 39 and 31 g/kg dry matter, respectively. Equations for nutrient intake were of low quality, with the exception of CP. Evaluation of FNIRS predictions was carried out with grazing animals supplemented or not with poultry litter, and implementation of the method in one herd over 2 years is presented. The potential usefulness of equations was also established by calculating the Mahalanobis (H

  20. Specific features of diffuse reflection of human face skin for laser and non-laser sources of visible and near-IR light

    SciTech Connect

    Dolotov, L E; Sinichkin, Yu P; Tuchin, Valerii V; Al'tshuler, G B; Yaroslavskii, I V

    2011-04-30

    The specific features of diffuse reflection from different areas of human face skin for laser and non-laser sources of visible and near-IR light have been investigated to localise the closed-eye (eyelid) region. In the visible spectral range the reflection from the eyelid skin surface can be differentiated by measuring the slope of the spectral dependence of the effective optical density of skin in the wavelength range from 650 to 700nm. In the near-IR spectral range the reflectances of the skin surface at certain wavelengths, normalised to the forehead skin reflectance, can be used as a criterion for differentiating the eyelid skin. In this case, a maximum discrimination is obtained when measuring the skin reflectances at laser wavelengths of 1310 and 1470nm, which correspond to the spectral ranges of maximum and minimum water absorption. (optical technologies in biophysics and medicine)

  1. Specific features of diffuse reflection of human face skin for laser and non-laser sources of visible and near-IR light

    NASA Astrophysics Data System (ADS)

    Dolotov, L. E.; Sinichkin, Yu P.; Tuchin, Valerii V.; Al'tshuler, G. B.; Yaroslavskii, I. V.

    2011-04-01

    The specific features of diffuse reflection from different areas of human face skin for laser and non-laser sources of visible and near-IR light have been investigated to localise the closed-eye (eyelid) region. In the visible spectral range the reflection from the eyelid skin surface can be differentiated by measuring the slope of the spectral dependence of the effective optical density of skin in the wavelength range from 650 to 700nm. In the near-IR spectral range the reflectances of the skin surface at certain wavelengths, normalised to the forehead skin reflectance, can be used as a criterion for differentiating the eyelid skin. In this case, a maximum discrimination is obtained when measuring the skin reflectances at laser wavelengths of 1310 and 1470nm, which correspond to the spectral ranges of maximum and minimum water absorption.

  2. Perspectives for the study of gas in protoplanetary disks and accretion/ejection phenomena in young stars with the near-IR spectrograph SPIROU at the CFHT

    NASA Astrophysics Data System (ADS)

    Carmona, A.; Bouvier, J.; Delfosse, X.

    2013-11-01

    Near-IR atomic and molecular transitions are powerful tools to trace the warm and hot gas in the circumstellar environment of young stars. Ro-vibrational transitions of H_2 and H_2O, and overtone transitions of CO at 2 μm centered at the stellar velocity trace hot (T˜ 1500 K) gas in the inner few AU of protoplanetary disks. H_2 near-IR lines displaying a blueshift of a few km/s probe molecular disk winds. H_2 lines presenting blueshifts of hundreds of km/s reveal hot shocked gas in jets. Atomic lines such as the HeI line at 10830 Å and the Hydrogen Paschen β and Brakett γ lines trace emission from accretion funnel flows and atomic disk winds. Bright forbidden atomic lines in the near-IR of species such as [Fe II], [N I], [S I], [S II], and [C I] trace atomic and ionized material in jets. The new near-IR high resolution spectrograph SPIROU planned for the Canada France Hawaii Telescope will offer the unique capability of combining high-spectral resolution (R˜75000) with a large wavelength coverage (0.98 to 2.35 μm) in one single exposure. This will provide us with the means of probing accretion funnel flows, winds, jets, and hot gas in the inner disk simultaneously. This opens the exiting possibility of investigating their combined behavior in time by the means of monitoring observations and systematic surveys. SPIROU will be a powerful tool to progress our understanding of the connexion between the accretion/ejection process, disk evolution, and planet formation.

  3. The Spectacular Radio-near-IR-X-Ray Jet of 3C 111: The X-Ray Emission Mechanism and Jet Kinematics

    NASA Astrophysics Data System (ADS)

    Clautice, Devon; Perlman, Eric S.; Georganopoulos, Markos; Lister, Matthew L.; Tombesi, Francesco; Cara, Mihai; Marshall, Herman L.; Hogan, Brandon; Kazanas, Demos

    2016-08-01

    Relativistic jets are the most energetic manifestation of the active galactic nucleus (AGN) phenomenon. AGN jets are observed from the radio through gamma-rays and carry copious amounts of matter and energy from the sub-parsec central regions out to the kiloparsec and often megaparsec scale galaxy and cluster environs. While most spatially resolved jets are seen in the radio, an increasing number have been discovered to emit in the optical/near-IR and/or X-ray bands. Here we discuss a spectacular example of this class, the 3C 111 jet, housed in one of the nearest, double-lobed FR II radio galaxies known. We discuss new, deep Chandra and Hubble Space Telescope (HST) observations that reveal both near-IR and X-ray emission from several components of the 3C 111 jet, as well as both the northern and southern hotspots. Important differences are seen between the morphologies in the radio, X-ray, and near-IR bands. The long (over 100 kpc on each side), straight nature of this jet makes it an excellent prototype for future, deep observations, as it is one of the longest such features seen in the radio, near-IR/optical, and X-ray bands. Several independent lines of evidence, including the X-ray and broadband spectral shape as well as the implied velocity of the approaching hotspot, lead us to strongly disfavor the EC/CMB model and instead favor a two-component synchrotron model to explain the observed X-ray emission for several jet components. Future observations with NuSTAR, HST, and Chandra will allow us to further constrain the emission mechanisms.

  4. Validation of Correction Algorithms for Near-IR Analysis of Human Milk in an Independent Sample Set-Effect of Pasteurization.

    PubMed

    Kotrri, Gynter; Fusch, Gerhard; Kwan, Celia; Choi, Dasol; Choi, Arum; Al Kafi, Nisreen; Rochow, Niels; Fusch, Christoph

    2016-03-01

    Commercial infrared (IR) milk analyzers are being increasingly used in research settings for the macronutrient measurement of breast milk (BM) prior to its target fortification. These devices, however, may not provide reliable measurement if not properly calibrated. In the current study, we tested a correction algorithm for a Near-IR milk analyzer (Unity SpectraStar, Brookfield, CT, USA) for fat and protein measurements, and examined the effect of pasteurization on the IR matrix and the stability of fat, protein, and lactose. Measurement values generated through Near-IR analysis were compared against those obtained through chemical reference methods to test the correction algorithm for the Near-IR milk analyzer. Macronutrient levels were compared between unpasteurized and pasteurized milk samples to determine the effect of pasteurization on macronutrient stability. The correction algorithm generated for our device was found to be valid for unpasteurized and pasteurized BM. Pasteurization had no effect on the macronutrient levels and the IR matrix of BM. These results show that fat and protein content can be accurately measured and monitored for unpasteurized and pasteurized BM. Of additional importance is the implication that donated human milk, generally low in protein content, has the potential to be target fortified. PMID:26927169

  5. Validation of Correction Algorithms for Near-IR Analysis of Human Milk in an Independent Sample Set-Effect of Pasteurization.

    PubMed

    Kotrri, Gynter; Fusch, Gerhard; Kwan, Celia; Choi, Dasol; Choi, Arum; Al Kafi, Nisreen; Rochow, Niels; Fusch, Christoph

    2016-03-01

    Commercial infrared (IR) milk analyzers are being increasingly used in research settings for the macronutrient measurement of breast milk (BM) prior to its target fortification. These devices, however, may not provide reliable measurement if not properly calibrated. In the current study, we tested a correction algorithm for a Near-IR milk analyzer (Unity SpectraStar, Brookfield, CT, USA) for fat and protein measurements, and examined the effect of pasteurization on the IR matrix and the stability of fat, protein, and lactose. Measurement values generated through Near-IR analysis were compared against those obtained through chemical reference methods to test the correction algorithm for the Near-IR milk analyzer. Macronutrient levels were compared between unpasteurized and pasteurized milk samples to determine the effect of pasteurization on macronutrient stability. The correction algorithm generated for our device was found to be valid for unpasteurized and pasteurized BM. Pasteurization had no effect on the macronutrient levels and the IR matrix of BM. These results show that fat and protein content can be accurately measured and monitored for unpasteurized and pasteurized BM. Of additional importance is the implication that donated human milk, generally low in protein content, has the potential to be target fortified.

  6. The Dusty View of DI from ESO Chile

    NASA Astrophysics Data System (ADS)

    Boehnhardt, H.; Ageorges, N.; Bagnulo, S.; Barrera, L.; Bonev, T.; Hainaut, O.; Jehin, E.; Käufl, H. U.; Kerber, F.; Locurto, G.; Manfroid, J.; Marco, O.; Pantin, E.; Pompei, E.; Rauer, H.; Saviane, I.; Selman, F.; Sterken, C.; Tozzi, G. P.; Weiler, M.

    Around the time of the impact of NASA's Deep Impact (DI) mission at comet 9P/Tempel 1, in total 6 telescopes with altogether 7 different instruments, located at the La Silla (LSO) and Paranal (VLT) Observatories of the European Southern Observatory (ESO) in Chile, were used to characterize the dust properties before and after the event. The ejecta cloud expanded at an average speed of about 200 ms-1during the first hours after the event. It reached stagnation distance of 25000 km about 3 days after impact. The pre-impact dust jet and fan activity (`porcupine' pattern) remained undisturbed after impact. In our measurements the jet activity can be traced to a few 100 km nucleus distance. In total 9 comastructures are identified which may originate from at least 4 regions of enhanced dust emission on the nucleus - one of this region may in fact be multiple. No obvious signatures of a new active region created by DI are found. The overall dust production during the impact compares to about 5-10 h of normal activity. The global expansion geometry of the DI cloud is compatible with a majority of dust grains in the micron size range. Indications exist for asymmetric brightness and colour distributions of the dust in the ejecta cloud. The dust temperature rose from about 280-290 K before to 330 K one day after the event and fell to pre-impact level the day thereafter. The dust reflected sunlight was found to be linearly polarized at about 7.5% in the visible and near-IR, at constant level within about 4000 km from the nucleus. No circular polarization of the dust is detected.

  7. Visible and Near-IR Reflectance Spectra of Smectite Acquired Under Dry Conditions for Interpretation of Martian Surface Mineralogy

    NASA Technical Reports Server (NTRS)

    Morris, Richard V.; Achilles, Cherie N; Archer, Paul D.; Graff, Trevor G.; Agresti, David G.; Ming, Douglas W; Golden, Dadi C.; Mertzman, Stanley A.

    2011-01-01

    Visible and near-IR (VNIR) spectra from the MEx OMEGA and the MRO CRISM hyper-spectral imaging instruments have spectral features associated with the H2O molecule and M OH functional groups (M = Mg, Fe, Al, and Si). Mineralogical assignments of martian spectral features are made on the basis of laboratory VNIR spectra, which were often acquired under ambient (humid) conditions. Smectites like nontronite, saponite, and montmorillionite have interlayer H2O that is exchangeable with their environment, and we have acquired smectite reflectance spectra under dry environmental conditions for interpretation of martian surface mineralogy. We also obtained chemical, Moessbauer (MB), powder X-ray diffraction (XRD), and thermogravimetric (TG) data to understand variations in spectral properties. VNIR spectra were recorded in humid lab air at 25-35C, in a dynamic dry N2 atmosphere (50-150 ppmv H2O) after exposing the smectite samples (5 nontronites, 3 montmorillionites, and 1 saponite) to that atmosphere for up to approximately l000 hr each at 25-35C, approximately 105C, and approximately 215C, and after re-exposure to humid lab air. Heating at 105C and 215C for approximately 1000 hr is taken as a surrogate for geologic time scales at lower temperatures. Upon exposure to dry N2, the position and intensity of spectral features associated with M-OH were relatively insensitive to the dry environment, and the spectral features associated with H2O (e.g., approximately 1.90 micrometers) decreased in intensity and are sometimes not detectable by the end of the 215C heating step. The position and intensity of H2O spectral features recovered upon re-exposure to lab air. XRD data show interlayer collapse for the nontronites and Namontmorillionites, with the interlayer remaining collapsed for the latter after re-exposure to lab air. The interlayer did not collapse for the saponite and Ca-montmorillionite. TG data show that the concentration of H2O derived from structural OH was invariant

  8. An optical and near-IR spectroscopic study of the extreme P Cygni-type supergiant HDE 316285

    NASA Astrophysics Data System (ADS)

    Hillier, D. J.; Crowther, P. A.; Najarro, F.; Fullerton, A. W.

    1998-12-01

    A detailed study of the Galactic P Cygni-type supergiant HDE 316285, based on high quality optical (AAT, MSO, CTIO) and near-IR (UKIRT, CFHT, CTIO) spectroscopy, is presented. As has been noted previously, its spectrum is dominated by H, He I, and Fe Ii P Cygni profiles. Emission lines due to N I, N Ii, [N Ii], O I, Na I, Mg Ii, Al Ii, Ca Ii, Si Ii, Si Iii, Fe Ii and [Fe Ii] can also be readily identified. Many of the metal lines are produced by continuum fluorescence. The rich N spectrum, the paucity of the O spectrum (only 2 O lines can be identified), and the apparent absence of emission due to C, strongly suggest that the atmosphere of the star is contaminated by CNO processed material. A comparison of the spectrum of HDE 316285 with P Cygni and He 3-519 is presented. From a spectral analysis using the non-LTE atmosphere code of Hillier (1991), and assuming a distance of 1.85 kpc, our preferred model for HDE 316285 has the following parameters: T_* = 15 kK, log L_* / L_sun = 5.44, spose M = 2.4 x 10(-4) Msun yr(-1) , v_∞ = 410 {km s(-1) }, E_B-V=1.81 mag, and H/He ~ 1.5 by number. Due to the low degree of He ionization the derived H/He abundance ratio and mass-loss rate are strongly coupled. Models with H/He=10 to 0.5 are equally capable of explaining the H and He I\\ spectrum provided the mass-loss rate is scaled according to the approximate formula spose M = 9.1 + 26.3 (He/H -0.1) x 10(-5) M_{\\odot}yr. Preliminary work, however, indicates that a solar H/He ratio can be ruled out on the basis of line strengths of other species - particularly N, Mg, Al. The stellar wind from HDE 316285 is more extreme than P Cygni with a performance number (= ratio of wind momentum to radiative momentum) 30 times greater. The low H/He abundance ratio and high N/He abundance ratio confirms that HDE 316285 is evolved. Although we find no evidence in the literature for photometric variability, we find strong evidence for significant spectral variability. Because of the spectral

  9. Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey -- GOODS-South Field, Non-SNe-Searched Visits

    NASA Astrophysics Data System (ADS)

    Faber, Sandra

    2011-10-01

    The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey {CANDELS}is designed to document the ?rst third of galactic evolution from z =8 to 1.5 via deep imaging of more than 250,000 galaxies with WFC3/IRand ACS. It will also find the first Type Ia SNe beyond z > 1.5 andestablish their accuracy as standard candles for cosmology. Fivepremier multi-wavelength sky regions selected from the SpitzerExtragalactic Deep Survey {SEDS} provide complementary IRAC imagingdata down to 26.5 AB mag, a unique resource for stellar masses at allredshifts. The use of ?ve widely separated ?elds mitigates cosmicvariance and yields statistically robust and complete samples ofgalaxies down to 10^9 solar masses out to z 8.The program merges two originally separate MCT proposals. The Faberprogram incorporates a ?Wide? imaging survey in three separate fieldsto 2 orbit depth over 0.2 sq. degrees, plus a ?Deep? imaging surveyto 12 orbit depth in the two GOODS regions over 0.04 sq. degrees.When combined with ultra-deep imaging from the Hubble Ultradeep Fieldprogram {GO 11563}, the result is a three-tiered strategy that ef?cientlysamples both bright/rare and faint/common extragalactic objects. TheFerguson program adds an extensive high-redshift Type Ia SNe search,plus ultraviolet "daytime" UVIS exposures in GOODS-N to exploit theCVZ opportunity in that field.This program, GO 12064, is part of the Wide mosaic survey, which has thefollowing field centers and sizes: Field ID RA{2000} Dec{2000} WFC3 Dim. PA on sky UDS 02 17 38 -05 12 02 4x11 270 COSMOS 10 00 31 +02 24 00 4x11 180 EGS 14 19 31 +52 54 10 3x15 41 Science highlights from the Wide program: * Underlying structural properties of galaxies as revealed by WFC3-IR images sensitive to older stars {beyond the 4000-A break} and less affected by dust than ACS. A key redshift is z 2, where star-formation peaks, QSOs are most abundant, and where restframe B-band is still accessible to WFC3. Sample questions include: - Structure in young vs. old

  10. The ESO Educational Office Reaches Out towards Europe's Teachers

    NASA Astrophysics Data System (ADS)

    2001-12-01

    ESA/ESO Astronomy Exercises Provide a Taste of Real Astronomy [1] Summary The European Southern Observatory (ESO) has been involved in many Europe-wide educational projects during the past years, in particular within European Science Weeks sponsored by the European Commission (EC). In order to further enhance the significant educational potential inherent in the numerous scientific endeavours now carried out by Europe's astronomers with ESO front-line telescope facilities, it has been decided to set up an Educational Office within the ESO EPR Department. It will from now on work closely with astronomy-oriented teachers, in particular at the high-school level , providing support, inspiration and new materials. Much of this interaction will happen via the European Association for Astronomy Education (EAAE) In this context, and in collaboration with the European Space Agency (ESA) , the first instalments of the "ESA/ESO Astronomy Exercise Series" have just been published, on the web ( http://www.astroex.org ) and in print (6 booklets totalling 100 pages; provided free-of-charge to teachers on request). They allow 16-19 year old students to gain exciting hands-on experience in astronomy, making realistic calculations with data obtained from observations by some of the world's best telescopes, the NASA/ESA Hubble Space Telescope (HST) and ESO's Very Large Telescope (VLT) . PR Photo 36/01 : The "ESA/ESO Astronomy Exercise Series" . Educational projects at ESO The European Southern Observatory (ESO) , through its Education and Public Relations Department (EPR) , has long been involved in educational activities, in particular by means of Europe-wide projects during successive European Science Weeks , with support from the European Commission (EC) . A most visible outcome has been the creation of the trailblazing European Association for Astronomy Education (EAAE) - this was first discussed at an international meeting at the ESO Headquarters in November 1994 with the

  11. ESO Fellowship Programme 2003/2004

    NASA Astrophysics Data System (ADS)

    2003-09-01

    THE EUROPEAN SOUTHERN OBSERVATORY AWARDS SEVERAL POSTDOCTORAL FELLOWSHIPS to provide young scientists opportunities and facilities to enhance their research programmes. Its goal is to bring them into close contact with the instruments, activities, and people at one of the world's foremost observatories. For more information about ESO's astronomical research activities please consult http://www.eso.org/science/

  12. The Gaia-ESO Survey: processing FLAMES-UVES spectra

    NASA Astrophysics Data System (ADS)

    Sacco, G. G.; Morbidelli, L.; Franciosini, E.; Maiorca, E.; Randich, S.; Modigliani, A.; Gilmore, G.; Asplund, M.; Binney, J.; Bonifacio, P.; Drew, J.; Feltzing, S.; Ferguson, A.; Jeffries, R.; Micela, G.; Negueruela, I.; Prusti, T.; Rix, H.-W.; Vallenari, A.; Alfaro, E.; Allende Prieto, C.; Babusiaux, C.; Bensby, T.; Blomme, R.; Bragaglia, A.; Flaccomio, E.; Francois, P.; Hambly, N.; Irwin, M.; Koposov, S.; Korn, A.; Lanzafame, A.; Pancino, E.; Recio-Blanco, A.; Smiljanic, R.; Van Eck, S.; Walton, N.; Bergemann, M.; Costado, M. T.; de Laverny, P.; Heiter, U.; Hill, V.; Hourihane, A.; Jackson, R.; Jofre, P.; Lewis, J.; Lind, K.; Lardo, C.; Magrini, L.; Masseron, T.; Prisinzano, L.; Worley, C.

    2014-05-01

    The Gaia-ESO Survey is a large public spectroscopic survey that aims to derive radial velocities and fundamental parameters of about 105 Milky Way stars in the field and in clusters. Observations are carried out with the multi-object optical spectrograph FLAMES, using simultaneously the medium-resolution (R ~ 20 000) GIRAFFE spectrograph and the high-resolution (R ~ 47 000) UVES spectrograph. In this paper we describe the methods and the software used for the data reduction, the derivation of the radial velocities, and the quality control of the FLAMES-UVES spectra. Data reduction has been performed using a workflow specifically developed for this project. This workflow runs the ESO public pipeline optimizing the data reduction for the Gaia-ESO Survey, automatically performs sky subtraction, barycentric correction and normalisation, and calculates radial velocities and a first guess of the rotational velocities. The quality control is performed using the output parameters from the ESO pipeline, by a visual inspection of the spectra and by the analysis of the signal-to-noise ratio of the spectra. Using the observations of the first 18 months, specifically targets observed multiple times at different epochs, stars observed with both GIRAFFE and UVES, and observations of radial velocity standards, we estimated the precision and the accuracy of the radial velocities. The statistical error on the radial velocities is σ ~ 0.4 km s-1 and is mainly due to uncertainties in the zero point of the wavelength calibration. However, we found a systematic bias with respect to the GIRAFFE spectra (~0.9 km s-1) and to the radial velocities of the standard stars (~0.5 km s-1) retrieved from the literature. This bias will be corrected in the future data releases, when a common zero point for all the set-ups and instruments used for the survey is be established. Based on observations made with the ESO/VLT, at Paranal Observatory, under programme 188.B-3002 (The Gaia-ESO Public

  13. The brown dwarf atmosphere monitoring (BAM) project. I. The largest near-IR monitoring survey of L and T dwarfs

    NASA Astrophysics Data System (ADS)

    Wilson, P. A.; Rajan, A.; Patience, J.

    2014-06-01

    Using the SofI instrument on the 3.5 m New Technology Telescope, we have conducted an extensive near-infrared monitoring survey of an unbiased sample of 69 brown dwarfs spanning the L0 to T8 spectral range, with at least one example of each spectral type. Each target was observed for a 2-4 h period in the Js-band, and the median photometric precision of the data is ~0.7%. A total of 14 brown dwarfs were identified as variables with min-to-max amplitudes ranging from 1.7% to 10.8% over the observed duration. All variables satisfy a statistical significance threshold with a p-value ≤5% based on comparison with a median reference star light curve. Approximately half of the variables show pure sinusoidal amplitude variations similar to 2MASSJ2139+0220, and the remainder show multi-component variability in their light curves similar to SIMPJ0136+0933. It has been suggested that the L-T transition should be a region of a higher degree of variability if patchy clouds are present, and this survey was designed to test the patchy cloud model with photometric monitoring of both the L-T transition and non-transition brown dwarfs. The measured frequency of variables is 13+10-4% across the L7-T4 spectral range, indistinguishable from the frequency of variables of the earlier spectral types (30+11-8%), the later spectral types (13+10-4%), or the combination of all non-transition region brown dwarfs (22+7-5%). The variables are not concentrated in the transition, in a specific colour, or in binary systems. Of the brown dwarfs previously monitored for variability, only ~60% maintained the state of variability (variable or constant), with the remaining switching states. The 14 variables include 9 newly identified variables that will provide important systems for follow-up multi-wavelength monitoring to further investigate brown dwarf atmosphere physics. Based on observations made with ESO Telescopes at La Silla Observatory under programme ID 188.C-0493.Tables 1, 2, and 4 are

  14. Assessment of MODIS-Derived Visible and Near-IR Aerosol Optical Properties and their Spatial Variability in the Presence of Mineral Dust

    NASA Technical Reports Server (NTRS)

    Redemann, J.; Zhang, Q.; Schmid, B.; Russell, P. B.; Livingston, J. M.; Jonsson, H.; Remer, L. A.

    2006-01-01

    Mineral dust aerosol is among the most difficult aerosol species to measure quantitatively from space. In this paper, we evaluate MODIS retrievals of spectral aerosol optical depth (AOD) from the visible to the near-IR off the US West Coast using measurements taken by the NASA Ames Airborne Tracking Sunphotometer, AATS-14, during the EVE (Extended-MODIS-lambda Validation Experiment, 2004) campaign in April of 2004. In EVE, a total of 35 and 49 coincident over-ocean suborbital measurements at the nominal level-2 retrieval scale of 10 km x 10 km were collected for Terra and Aqua, respectively. For MODIS-Terra about 80% of the AOD retrievals are within the estimated uncertainty, DELTA tau = plus or minus 0.03 plus or minus 0.05 tau; this is true for both the visible (here defined to include 466-855 nm) and near-IR (here defined to include 1243-2119 nm) retrievals. For MODIS-Aqua about 45% of the AOD retrievals are within DELTA tau = plus or minus 0.03 plus or minus 0.05 tau; the fraction of near-IR retrievals that fall within this uncertainty range is about 27%. We found an rms difference of 0.71 between the sunphotometer snd MODIS-Aqua estimates of the visible (553-855 nm) Angstrom exponent, while the MODIS-Terra visible Angstrom exponents show an rms difference of only 0.29 when compared to AATS. The cause of the differences in performance between MODIS-Terra and MODIS-Aqua could be instrument calibration and needs to be explored further. The spatial variability of AOD between retrieval boxes as derived by MODIS is generally larger than that indicated by the sunphotometer data.

  15. Spectral phase transfer from near IR to deep UV by broadband phase-matched four-wave mixing in an argon-filled hollow core waveguide

    NASA Astrophysics Data System (ADS)

    Siqueira, J. P.; Mendonça, C. R.; Zilio, S. C.; Misoguti, L.

    2016-10-01

    We report on the implementation of a spectral phase transfer scheme from near IR to deep UV, in which the frequency conversion step is based on the broadband phase-matched four-wave mixing in a gas-filled hollow core waveguide. Micro joule level femtosecond pulses at 260 nm were generated by nonlinear mixing of a Ti:sapphire laser and its second-harmonic. The transfer of a π-step phase in a controllable manner was proposed and confirmed by a modulation observed in the generated deep UV femtosecond pulse spectrum due to an interference process. Numerical simulations confirmed our results.

  16. Visible to Near-IR Spectral Properties of Rocks and Soils at Gusev and Meridiani from the Mars Exploration Rover Pancams

    NASA Astrophysics Data System (ADS)

    Bell, J. F.

    2004-12-01

    Mars Exploration Rover Pancam multispectral images of a wide range of rock and soil targets were acquired using as many as 11 narrowband filters with central wavelengths from 432 to 1009 nm. These images were acquired in order to characterize the overall color properties of materials at the Gusev and Meridiani landing sites, to constrain the iron-bearing mineralogy of these materials based on the nature of crystalline and/or nanophase Fe3+ (ferric) absorptions in the visible to near-IR in altered materials and Fe2+ (ferrous) absorptions in the near-IR from less-altered volcanic materials, and to aid in the selection of specific targets for detailed chemical and mineralogic investigations using the rovers' arm instruments. At Gusev during the plains traverse to the Columbia Hills, most bright soil and rock surfaces appear covered or coated by optically thick fine-grained ferric-iron rich dust. Spectra of some darker rock surfaces, including regions that were brushed or drilled by the RAT, show near-IR signatures consistent with ferrous silicates like pyroxene or olivine. Since Spirit's arrival in the Columbia Hills, Pancam images have revealed evidence for some intrinsically less dusty or less altered rock surfaces, as well as isolated occurrences of more crystalline ferric signatures that may be indicative of enhanced weathering or alteration relative to materials in the plains. At Meridiani during the exploration of Eagle crater and during the traverse to Endurance crater, a wide range of visible to near-IR spectral properties was identified among small rock clasts and spherules. For example, spectra of dark sand, some dark rock clasts, and one larger dark rock found on the plains show spectra consistent with the presence of pyroxene or olivine. Spectra of dark spherules are consistent with the presence of crystalline ferric oxides/oxyhydroxides. Bright materials, including windblown dust, bright spherules, and the sulfur-rich laminated outcrop deposits, have

  17. Diode laser-based sensor system for long-path absorption measurements of atmospheric concentration and near-IR molecular spectral parameters

    SciTech Connect

    Goldstein, N.; Lee, J.; Adler-Golden, S.M.; Bien, F.

    1993-12-31

    Line-locked near-IR diode lasers and a simple retroreflector/telescope system were used for remote sensing of atmospheric constituents over long atmospheric paths. The experimental configuration used in preliminary measurements of atmospheric water vapor and oxygen with AlGaAs diode lasers is presented. A prototype field sensor system currently under development shares the same basic configuration but incorporates interchangeable AlGaAs and InGaAsP diode-laser modules for monitoring a variety of atmospheric gases.

  18. CCDs at ESO: A Systematic Testing Program

    NASA Astrophysics Data System (ADS)

    Abbott, T. M. C.; Warmels, R. H.

    ESO currently offers a stable of 12 CCDs for use by visiting astronomers. It is incumbent upon ESO to ensure that these devices perform according to their advertised specifications (Abbott 1994). We describe a systematic, regular testing program for CCDs which is now being applied at La Silla. These tests are designed to expose failures which may not have catastrophic effects but which may compromise observations. The results of these tests are stored in an archive, accessible to visiting astronomers, and will be subject to trend analysis. The test are integrated in the CCD reduction package of the Munich Image Data Analysis System (ESO-MIDAS).

  19. Report of the ESO OPC Working Group

    NASA Astrophysics Data System (ADS)

    Brinks, E.; Leibundgut, B.; Mathys, G.

    2012-12-01

    With over 1000 proposals per semester for ESO telescopes, the community is facing the problem of fair and robust selection of observing programmes. We report here on a working group to investigate the current selection process and procedures and identify possible improvements. The working group report summarises the current process, based on peer review, that has been in use for many years at ESO and other comparable ground- and space-based observatories, and presents an inventory of the changes and approaches that may be considered to make the process more manageable and less time-consuming, while at the same time preserving its integrity. The working group presented several recommendations, which have been discussed with ESO committees and analysed by the operational groups at ESO.

  20. Using ESO Reflex with Web Services

    NASA Astrophysics Data System (ADS)

    Järveläinen, P.; Savolainen, V.; Oittinen, T.; Maisala, S.; Ullgrén, M. Hook, R.

    2008-08-01

    ESO Reflex is a prototype graphical workflow system, based on Taverna, and primarily intended to be a flexible way of running ESO data reduction recipes along with other legacy applications and user-written tools. ESO Reflex can also readily use the Taverna Web Services features that are based on the Apache Axis SOAP implementation. Taverna is a general purpose Web Service client, and requires no programming to use such services. However, Taverna also has some restrictions: for example, no numerical types such integers. In addition the preferred binding style is document/literal wrapped, but most astronomical services publish the Axis default WSDL using RPC/encoded style. Despite these minor limitations we have created simple but very promising test VO workflow using the Sesame name resolver service at CDS Strasbourg, the Hubble SIAP server at the Multi-Mission Archive at Space Telescope (MAST) and the WESIX image cataloging and catalogue cross-referencing service at the University of Pittsburgh. ESO Reflex can also pass files and URIs via the PLASTIC protocol to visualisation tools and has its own viewer for VOTables. We picked these three Web Services to try to set up a realistic and useful ESO Reflex workflow. They also demonstrate ESO Reflex abilities to use many kind of Web Services because each of them requires a different interface. We describe each of these services in turn and comment on how it was used

  1. UK Announces Intention to Join ESO

    NASA Astrophysics Data System (ADS)

    2000-11-01

    Summary The Particle Physics and Astronomy Research Council (PPARC) , the UK's strategic science investment agency, today announced that the government of the United Kingdom is making funds available that provide a baseline for this country to join the European Southern Observatory (ESO) . The ESO Director General, Dr. Catherine Cesarsky , and the ESO Community warmly welcome this move towards fuller integration in European astronomy. "With the UK as a potential member country of ESO, our joint opportunities for front-line research and technology will grow significantly", she said. "This announcement is a clear sign of confidence in ESO's abilities, most recently demonstrated with the construction and operation of the unique Very Large Telescope (VLT) on Paranal. Together we will look forward with confidence towards new, exciting projects in ground-based astronomy." It was decided earlier this year to place the 4-m UK Visible and Infrared Survey Telescope (VISTA) at Paranal, cf. ESO Press Release 03/00. Following negotiations between ESO and PPARC, a detailed proposal for the associated UK/ESO Agreement with the various entry modalities will now be presented to the ESO Council for approval. Before this Agreement can enter into force, the ESO Convention and associated protocols must also be ratified by the UK Parliament. Research and key technologies According to the PPARC press release, increased funding for science, announced by the UK government today, will enable UK astronomers to prepare for the next generation of telescopes and expand their current telescope portfolio through membership of the European Southern Observatory (ESO). The uplift to its baseline budget will enable PPARC to enter into final negotiations for UK membership of the ESO. This will ensure that UK astronomers, together with their colleagues in the ESO member states, are actively involved in global scale preparations for the next generation of astronomy facilities. among these are ALMA

  2. Czech Republic to Become Member of ESO

    NASA Astrophysics Data System (ADS)

    2006-12-01

    Today, an agreement was signed in Prague between ESO and the Czech Republic, aiming to make the latter become a full member of ESO as of 1 January 2007. "The future membership of the Czech Republic in ESO opens for the Czech astronomers completely new opportunities and possibilities. It will foster this discipline on the highest quality level and open new opportunities for Czech industry to actively cooperate in research and development of high-tech instruments for astronomical research," said Miroslava Kopicová, Minister of Education, Youth and Sports of the Czech Republic. ESO PR Photo 52/06 ESO PR Photo 52/06 Signing Ceremony "We warmly welcome the Czech Republic as the thirteenth member of ESO," said Catherine Cesarsky, ESO's Director General. "The timing couldn't be better chosen: with the Very Large Telescope, Europe is now at the forefront of ground-based astronomy, and with the construction of ALMA and the final studies for the European Extremely Large Telescope, we will ensure that this will remain so for several decades. We look forward to working together with our Czech colleagues towards these successes." The signing event took place at the Czech Ministry of Education, Youth and Sports in Prague. Following ratification by the Czech Parliament, the Czech Republic with thus join the twelve present member states of ESO, the European Organisation for Astronomical Research in the Southern Hemisphere: Belgium, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. The Czech Republic is the first country from Central and Eastern Europe to join ESO. Astronomy in the Czech Republic has a very long tradition that dates from as far back as 3500 BC. Four centuries ago, Tycho Brahe and Johannes Kepler established themselves in Prague at the invitation of the emperor Rudolph II, laying the ground for the first golden age in astronomy. Later, eminent scientists such as Christian Doppler, Ernst Mach and

  3. ESO Delegation to Visit Chile: the Chile-Eso Treaty and Paranal

    NASA Astrophysics Data System (ADS)

    1994-05-01

    The ESO Council, in its extraordinary session on 28 April 1994, among other matters discussed the relations with the Republic of Chile and the situation around Paranal mountain [1], the designated site for the ESO Very Large Telescope (VLT). Council decided to send a high ranking delegation to Santiago de Chile to discuss with Chilean authorities the pending problems, including the finalisation of the new Treaty between the Republic of Chile and ESO and the legal aspects of the Paranal location. The ESO delegation will consist of Dr. Peter Creola (President of ESO Council), Dr. Catherine Cesarsky (Vice-President of ESO Council), Dr. Henrik Grage (Former Vice-President of ESO Council) and Professor Riccardo Giacconi (ESO Director General), the latter accompanied by his advisers. The delegation will arrive in Chile during the second half of May 1994. The ESO delegation will meet with the Chilean Minister of Foreign Affairs, Mr. Carlos Figueroa, and the Secretary of State in the Ministry of Foreign Affairs, Mr. Jose Miguel Insulza. Other meetings at high level are being planned. The delegation will report about these discussions to the ESO Council during its ordinary session on 7 - 8 June 1994. FOUR PARANAL PHOTOS AVAILABLE A series of four photos which show the current status of the work at Paranal has been prepared. Photographic colour prints for use by the media can be requested from the ESO Information and Photographic Service (please remember to indicate the identification numbers). [1] See ESO Press Release 07/94 of 21 April 1994. PHOTO CAPTIONS ESO PR PHOTO 08/94-1: CERRO PARANAL This aerial photo of the Paranal mountain, the designated site for the ESO Very Large Telescope (VLT), was obtained on 22 March 1994. Paranal is situated in the driest part of the Chilean Atacama desert, approx. 130 km south of the city of Antofagasta, and about 12 km from the Pacific Ocean. In this view towards the West, the ocean is seen in the background. The altitude is 2650 metres

  4. On the possibility of designing a high-resolution heterodyne spectrometer for near-IR range on the basis of a tunable diode laser

    SciTech Connect

    Klimchuk, A Yu; Nadezhdinskii, Aleksandr I; Ponurovskii, Ya Ya; Shapovalov, Yu P; Rodin, A V

    2012-03-31

    The results of heterodyning of broadband radiation in the near-IR range are presented. A stabilised DFB laser was used as a local oscillator, while the role of a broadband radiation source was played by another DFB laser, excited by the pump current below its threshold value. A fibre-optical Y-coupler based on the single-mode silica fibre served as a diplexer. The radiation mixed in the singlemode fibre was incident on the photodetector, the role of which was played by a p - i - n photodiode. The signal from the photodiode was amplified by the preamplifier with the feedback resistance 240 k{Omega} and the bandwidth {approx}1 MHz and then digitised using a 16-digit ADC. The frequency scanning was implemented via the variation of the local oscillator frequency. The developed registration system provides the sensitivity {approx}1.4 % of the shot noise value at the acquisition time {approx}40 min.

  5. APPLICATION OF LASERS AND LASER-OPTICAL METHODS IN LIFE SCIENCES Non-invasive, MRI-compatible fibreoptic device for functional near-IR reflectometry of human brain

    NASA Astrophysics Data System (ADS)

    Sorvoja H. S., S.; Myllylä, T. S.; Kirillin, M. Yu; Sergeeva, Ekaterina A.; Myllylä, Risto A.; Elseoud, A. A.; Nikkinen, J.; Tervonen, O.; Kiviniemi, V.

    2011-01-01

    A non-invasive device for measuring blood oxygen variations in human brain is designed, implemented, and tested for MRI compatibility. The device is based on principles of near-IR reflectometry; power LEDs serve as sources of probing radiation delivered to patient skin surface through optical fibres. Numerical Monte Carlo simulations of probing radiation propagation in a multilayer brain model are performed to evaluate signal levels at different source — detector separations at three operation wavelengths and an additional wavelength of 915 nm. It is shown that the device can be applied for brain activity studies using power LEDs operating at 830 and 915 nm, while employment of wavelength of 660 nm requires an increased probing power. Employment of the wavelength of 592 nm in the current configuration is unreasonable.

  6. Catherine Cesarsky - ESO's Next Director General

    NASA Astrophysics Data System (ADS)

    1999-01-01

    The ESO Council has appointed Dr. Catherine Cesarsky as Director General for a five year period, succeeding Professor Riccardo Giacconi, whose term ends this year. Dr. Cesarsky will take up her duties on September 1, 1999, at the ESO Headquarters in Garching (Germany). Dr. Cesarsky was born in France in 1943. She received a degree in Physical Sciences at the University of Buenos Aires and graduated with a PhD in Astronomy in 1971 from Harvard University (Cambridge, Mass., USA). Afterwards she worked at the California Institute of Technology (CALTECH). In 1974, she became a staff member of the Service d'Astrophysique (SAp) , Direction des Sciences de la Matière (DSM), Commissariat à l'Energie Atomique (CEA) (France). She headed the theoretical group of the SAp (1978-1985), was Head of SAp (1985-1993) and has been Director of DSM since 1994. The DSM encompasses, at the CEA, activities of basic research in physics, chemistry, astrophysics and earth sciences and comprises about 3000 scientists, engineers, technicians, etc. Dr. Cesarsky is known for her successful research activities in several central areas of modern astrophysics. The first part of her career was devoted to the high-energy domain. This has involved studies of the propagation and composition of galactic cosmic rays, of matter and fields in the diffuse interstellar medium, as well as the acceleration of particles in astrophysical shocks, e.g. in connection with supernovae. She then turned to infrared astronomy. She is the Principal Investigator of the ISOCAM camera onboard the Infrared Space Observatory (ISO) of the European Space Agency (ESA) and, as such, she leads the ISOCAM central programme. It studies, in a coordinated way, the infrared emission from a variety of galactic and extragalactic sources and is yielding new and exciting results on star formation and galactic evolution. Dr. Cesarsky received the COSPAR (Committee on Space Research) Space Science Award in 1998. She is a member of many

  7. ESO and Fokker Space Sign Contract about VLTI Delay Line

    NASA Astrophysics Data System (ADS)

    1998-03-01

    variations due to atmospheric disturbances and/or mechanical vibrations along the optical path length. The VLTI Delay Line system consists of a retro-reflector mounted on a moving base. The optical design of this `Cat's Eye' is of the Ritchey-Chretien type that reflects the light very effectively. For this particular application, the `Cat's Eye' is not a corner cube with 3 perpendicular mirrors as is the case in the reflectors on cars and bicycles; it is in fact a telescope with a mirror at the focus that sends a light beam back in a direction parallel to the one it came from. The moving base enables the Cat's Eye to travel along a 60 metres long rail track, thereby providing optical path difference corrections of up to 120 metres, as required for the VLT telescope configurations at Paranal. The necessary, rapid path length corrections are performed by a fine positioning loop in which a piezo crystal (mounted on the backside of the Variable Curvature Mirror M3) is used to correct the fast optical path variations as measured by a Fringe Sensing Unit (FSU). The latter provides a signal to the Delay Line system via a fast link to the Delay Line Local Control Unit. An optical datalink to the Cat's Eye on the carriage ensures the transfer of data to the Piezo controller. The carriage is driven by a Linear Induction Motor. The coils for the motor are mounted on the floor of the Delay Line Long Support Bench and the magnets are mounted on the bottom of the carriage. The metrology system (to measure the carriage position) consists of a laser-interferometer whose beam follows the same path as the light beams from the telescopes via the Cat's Eye. The main design parameters are shown here: Optical Path range above 120 m Optical Path resolution better than 20 nm Optical Path stability better than 14 nm over any 0.01 sec (in the visible spectral range) better than 50 nm over any 0.05 sec (in Near-IR spectral range) better than 225 nm over any 0.3 sec (in Thermal-IR spectral range

  8. Tragic Car Accident Involves ESO Employees

    NASA Astrophysics Data System (ADS)

    2000-06-01

    Saturday, May 27, turned into a tragic day for ESO. The team installing TIMMI2 at La Silla, went on an excursion to the Elqui valley, 70 km east of the city of La Serena and suffered a serious car accident, crashing against another car driving from the opposite direction.

  9. ESO telbib: Linking In and Reaching Out

    NASA Astrophysics Data System (ADS)

    Grothkopf, U.; Meakins, S.

    2015-04-01

    Measuring an observatory's research output is an integral part of its science operations. Like many other observatories, ESO tracks scholarly papers that use observational data from ESO facilities and uses state-of-the-art tools to create, maintain, and further develop the Telescope Bibliography database (telbib). While telbib started out as a stand-alone tool mostly used to compile lists of papers, it has by now developed into a multi-faceted, interlinked system. The core of the telbib database is links between scientific papers and observational data generated by the La Silla Paranal Observatory residing in the ESO archive. This functionality has also been deployed for ALMA data. In addition, telbib reaches out to several other systems, including ESO press releases, the NASA ADS Abstract Service, databases at the CDS Strasbourg, and impact scores at Altmetric.com. We illustrate these features to show how the interconnected telbib system enhances the content of the database as well as the user experience.

  10. ESO Helps Antofagasta Region after the Earthquake

    NASA Astrophysics Data System (ADS)

    2007-11-01

    On November 14 at 12:41 local time, a major earthquake with magnitude 7.7 on the Richter scale affected the north of Chile. The epicentre was located 35 km from the city of Tocopilla and 170 km of Antofagasta. Two persons died and tens were injured, while buildings were damaged in several cities. In the Maria Elena-Tocopilla area, several thousand homes were destroyed or damaged. In an act of solidarity with the local community and its authorities, ESO immediately announced a donation of 30 millions Chilean pesos (around 40,000 euros) to Antofagasta's Regional Government to support reconstruction in the Region II. ESO and its staff have been shocked by the earthquake and its impact on local communities, especially on the people of Tocopilla. The ESO Representation in Chile formally contacted the regional authorities to explore with them possible ways to collaborate in this difficult moment. In addition, many of ESO staff are personally cooperating with the victims, under the coordination of Cruz Roja, the organisation currently in charge of implementing individual efforts.

  11. The ESO Product Data Management System — A New Home for ESO's Technical Documents

    NASA Astrophysics Data System (ADS)

    Kraus, M.; Tamai, R.; Jolley, P.; Hess, G.

    2013-09-01

    Originally the technical archives at ESO grew organically and lacked a single coherent storage and access system. A search for a powerful product data management (PDM) system to unify the document archives of observatory, telescope and instrument technical material was initiated. After a careful assessment of the possible systems, it was decided to implement the Kronodoc system and its recent introduction as the ESO PDM system is described.

  12. Phobos Near-IR Photometry

    NASA Technical Reports Server (NTRS)

    Erard, S.; Poulet, F.

    2002-01-01

    Unusual values of the opposition effect on Phobos derived by Simonelli et al. are tested using ISM observations in the NIR, and do not appear consistent. A Deimos-like opposition surge provides acceptable values for the other Hapke parameters. Additional information is contained in the original extended abstract.

  13. Next Generation Bibliometrics and the Evolution of the ESO Telescope Bibliography

    NASA Astrophysics Data System (ADS)

    Erdmann, C.; Grothkopf, U.

    2010-10-01

    Bibliometric studies typically focus on citation and publication analysis. Due to recent advances in web technology along with greater access to web content, bibliometric research can include statistics and measures that were once difficult to obtain. The European Southern Observatory's Telescope Bibliography (ESO telbib), a content management system for refereed articles containing ESO data, provides an excellent test-bed for exploring next generation bibliometrics. Through web services provided by the NASA Astrophysics Data System (ADS) Abstract Service among others, previously unavailable information can be imported into telbib where it can be analyzed in further detail. Though some telbib features are still in their infancy, some interesting trends can already be derived.

  14. All-solid-state electrochromic device integrated with near-IR blocking layer for image sensor and energy-saving glass application

    NASA Astrophysics Data System (ADS)

    Wang, Min-Chuan; Hsieh, Ming-Hao; Chen, Yung-Chih; Wang, Jen-Yuan

    2016-09-01

    The all-solid-state electrochromic device (ECD) integrated with near-IR (NIR) blocking layer fabricated by reactive DC magnetron sputtering technique has been developed for image sensor and energy-saving glass applications. The all-solid-state ECD with the single-substrate structure of glass/NIR-blocking transparent conductive oxide (TCO)/NiO/Ta2O5/WO3/ITO could potentially modulate the optical transmittance between 81.9% and 17.5% at 550 nm in the visible region and between 38.0% and 9.5% at the NIR wavelength larger than 1100 nm. The better energy-saving and light blocking performance, including the larger optical density difference (ΔOD) and lower solar heat-gain coefficient (SHGC) could be achieved in the NIR-blocking ECD structure, even with the general criteria SHGC(bleach)/SHGC(colored) < 3. With the application of ECDs, it is possible to directly apply the device onto an image sensor and energy-saving glass with the NIR rejection function even in the bleached state. Furthermore, the NIR-blocking TCO with the low sheet resistance and high transparency characteristics also provides the lower power consumption in the switching cycle at voltages as low as 5 V, and makes ECDs the ideal components for applications of large area and battery powered devices.

  15. A Red to Near-IR Fluorogen: Aggregation-Induced Emission, Large Stokes Shift, High Solid Efficiency and Application in Cell-Imaging.

    PubMed

    Wang, Yi Jia; Shi, Yang; Wang, Zhaoyang; Zhu, Zhenfeng; Zhao, Xinyuan; Nie, Han; Qian, Jun; Qin, Anjun; Sun, Jing Zhi; Tang, Ben Zhong

    2016-07-01

    A tetraphenylethene (TPE) derivative modified with the strong electron acceptor 2-dicyano-methylene-3-cyano-4,5,5-trimethyl-2,5-dihydrofuran (TCF) was obtained in high yield by a simple two-step reaction. The resultant TPE-TCF showed evident aggregation-induced emission (AIE) features and pronounced solvatochromic behavior. Changing the solvent from apolar cyclohexane to highly polar acetonitrile, the emission peak shifted from 560 to 680 nm (120 nm redshift). In an acetonitrile solution and in the solid powder, the Stokes shifts are as large as 230 and 190 nm, respectively. The solid film emits red to near-IR (red-NIR) fluorescence with an emission peak at 670 nm and a quantum efficiency of 24.8 %. Taking the advantages of red-NIR emission and high efficiency, nanoparticles (NPs) of TPE-TCF were fabricated by using tat-modified 1,2-distearoylsn-glycero-3-phosphor-ethanol-amine-N-[methoxy-(polyethyl-eneglycol)-2000] as the encapsulation matrix. The obtained NPs showed perfect membrane penetrability and high fluorescent imaging quality of cell cytoplasm. Upon co-incubation with 4,6-diamidino-2-phenylindole (DAPI) in the presence of tritons, the capsulated TPE-TCF nanoparticles could enter into the nucleus and displayed similar staining properties to those of DAPI.

  16. Relaxation dynamics of the LH2 complex from a photosynthetic purple bacterium Thiorhodospira sibirica studied by the near-IR femtosecond pump-probe method

    SciTech Connect

    Razjivin, A P; Pishchal'nikov, R Yu; Kozlovskii, V S; Kompanets, V O; Chekalin, Sergei V; Moskalenko, A A; Makhneva, Z K

    2005-01-31

    Photoinduced changes in the absorption spectrum of the LH2 (B800-830-850) complex from a Thiorhodospira sibirica (Trs. sibirica) bacterium are studied by the pump-probe method. The complex has the anomalous absorption spectrum exhibiting three bands in the near-IR region at 793, 826.5, and 846.5 nm. At room temperature, the excitation energy transfer from the B800, B830, and B859 bands was detected with the time constants {tau}{sub 1{approx}}0.5 ps, {tau}{sub 2{approx}}2.5 ps, and {tau}{sub 3} of the order of a few hundreds of picoseconds, respectively. A rapid energy transfer from the B830 band compared to energy transfer from the B850 band ({tau}{sub 2}||{tau}{sub 3}) suggests that all the three bands belong to the same complex (i.e., that the LH2 complex from Trs. sibirica is homogeneous). A slower energy transfer (by three - five times) from the B830 band of the LH2 complex from Trs. sibirica compared to energy transfer from the B800 band of the LH2 complexes (B800-850 and especially B800-820) from other purple bacteria suggests that the electronic structures of ensembles of bacteriochlorophyll molecules in these complexes are substantially different. (laser applications and other topics in quantum electronics)

  17. The near-IR spectrum of NO(X˜ 2Π )-Ne detected through excitation into the Östate continuum: A joint experimental and theoretical study

    NASA Astrophysics Data System (ADS)

    Kłos, J.; Zhang, S. G.; Meyer, H.

    2016-03-01

    We present new measurements of the near IR spectrum of NO-Ne in the region of the first NO overtone transition. The IR absorption is detected by exciting the vibrationally excited complex to the A ˜ -state dissociation continuum. The resulting NO(A) fragment is subsequently ionized in the same laser pulse. Spectra of the two lowest bands, A and B, are recorded. The spectra are compared with calculated spectra based on bound states derived from a new set of high level ab initio potential energy surfaces (PESs). For the calculation, the PESs are used with either fixed NO intermolecular distance or averaged for the vibrational states of NO (X ˜ , v = 0 or 2). Spectra based on the new PESs reproduce the experimental spectra better than theoretical spectra based on the older PESs of M. H. Alexander et al. [J. Chem. Phys. 114, 5588 (2001)]. Especially, spectra based on the two different vibrationally averaged PESs show a marked improvement in comparison to the one based on the fixed internuclear NO-distance. A fitted set of spectroscopic constants allows to reproduce most of the finer details of the measured spectra. Monitoring simultaneously the NO fragment ion and the parent ion channels while scanning the UV wavelength through the NO A-X hot-band region enabled us to confirm the NO-Ne A ˜ -state dissociation limit of 44233 ± 5 cm-1. These measurements also confirm the absence of a structured NO-Ne spectrum involving the A ˜ -state.

  18. Non-Destructive and Discriminating Identification of Illegal Drugs by Transient Absorption Spectroscopy in the Visible and Near-IR Wavelength Range

    NASA Astrophysics Data System (ADS)

    Sato, Chie; Furube, Akihiro; Katoh, Ryuzi; Nonaka, Hidehiko; Inoue, Hiroyuki

    2008-11-01

    We have tested the possibility of identifying illegal drugs by means of nanosecond transient absorption spectroscopy with a 10-ns UV-laser pulse for the excitation light and visible-to-near-IR light for the probe light. We measured the transient absorption spectra of acetonitrile solutions of d-methamphetamine, dl-3,4-methylenedioxymethamphetamine hydrochloride (MDMA), and dl-N-methyl-1-(1,3-benzodioxol-5-yl)-2-butanamine hydrochloride (MBDB), which are illegal drugs widely consumed in Japan. Transient absorption signals of these drugs were observed between 400 and 950 nm, a range in which they are transparent in the ground state. By analyzing the spectra in terms of exponential and Gaussian functions, we could identify the drugs and discriminate them from chemical substances having similar structures. We propose that transient absorption spectroscopy will be a useful, non-destructive method of inspecting for illegal drugs, especially when they are dissolved in liquids. Such a method may even be used for drugs packed in opaque materials if it is further extended to utilize intense femtosecond laser pulses.

  19. A Red to Near-IR Fluorogen: Aggregation-Induced Emission, Large Stokes Shift, High Solid Efficiency and Application in Cell-Imaging.

    PubMed

    Wang, Yi Jia; Shi, Yang; Wang, Zhaoyang; Zhu, Zhenfeng; Zhao, Xinyuan; Nie, Han; Qian, Jun; Qin, Anjun; Sun, Jing Zhi; Tang, Ben Zhong

    2016-07-01

    A tetraphenylethene (TPE) derivative modified with the strong electron acceptor 2-dicyano-methylene-3-cyano-4,5,5-trimethyl-2,5-dihydrofuran (TCF) was obtained in high yield by a simple two-step reaction. The resultant TPE-TCF showed evident aggregation-induced emission (AIE) features and pronounced solvatochromic behavior. Changing the solvent from apolar cyclohexane to highly polar acetonitrile, the emission peak shifted from 560 to 680 nm (120 nm redshift). In an acetonitrile solution and in the solid powder, the Stokes shifts are as large as 230 and 190 nm, respectively. The solid film emits red to near-IR (red-NIR) fluorescence with an emission peak at 670 nm and a quantum efficiency of 24.8 %. Taking the advantages of red-NIR emission and high efficiency, nanoparticles (NPs) of TPE-TCF were fabricated by using tat-modified 1,2-distearoylsn-glycero-3-phosphor-ethanol-amine-N-[methoxy-(polyethyl-eneglycol)-2000] as the encapsulation matrix. The obtained NPs showed perfect membrane penetrability and high fluorescent imaging quality of cell cytoplasm. Upon co-incubation with 4,6-diamidino-2-phenylindole (DAPI) in the presence of tritons, the capsulated TPE-TCF nanoparticles could enter into the nucleus and displayed similar staining properties to those of DAPI. PMID:27265326

  20. Ethynyl-linked push-pull porphyrin hetero-dimers for near-IR dye-sensitized solar cells: photovoltaic performances versus excited-state dynamics.

    PubMed

    Liu, Yizhu; Lin, Hong; Li, Jianbao; Dy, Joanne Ting; Tamaki, Koichi; Nakazaki, Jotaro; Nakayama, Daisuke; Nishiyama, Chie; Uchida, Satoshi; Kubo, Takaya; Segawa, Hiroshi

    2012-12-28

    Ethynyl-linked porphyrin hetero-dimers substituted by a series of electron donors, namely, bis(4-methoxyphenyl)amino (BMPA), bis(4-tert-butylphenyl)amino (BTBPA) and 3,6-di-tert-butylcarbazol-9-yl (DTBC) as well as a reference dimer with a non-donor moiety (3,5-di-tert-butylphenyl, DTBP) have been synthesized to systematically investigate the influence of donor introduction on the photovoltaic performances of near-IR dye-sensitized solar cells (DSCs) with these sensitizers incorporated. Despite the expected bathochromic shift and intensification of long-wavelength absorption bands as well as elevated LUMO levels and thus increased electron injection driving forces, the substitution of diphenylamino groups (BMPA and BTBPA) with stronger electron-donating abilities gave rise to surprising mediocrity in the short-circuit photocurrent densities (J(sc)), leading to overall energy conversion efficiencies in the order BMPA (3.94%) < DTBP (4.57%) < BTBPA (4.83%) < DTBC (5.21%). A study of the in situ fluorescent behavior of these sensitizers revealed that for all the sensitizers, excited-state lifetimes were significantly shortened in the simulated DSC environment compared to those in a free solution. BMPA showed the shortest intrinsic in situ lifetime while DTBC showed the longest one. These results were correlated with the photovoltaic performances, which is required for a better understanding and further design of porphyrin array sensitizers.

  1. Ultrafast Photochemistry of Copper(II) Monochlorocomplexes in Methanol and Acetonitrile by Broadband Deep-UV-to-Near-IR Femtosecond Transient Absorption Spectroscopy.

    PubMed

    Mereshchenko, Andrey S; Olshin, Pavel K; Myasnikova, Olesya S; Panov, Maxim S; Kochemirovsky, Vladimir A; Skripkin, Mikhail Yu; Moroz, Pavel N; Zamkov, Mikhail; Tarnovsky, Alexander N

    2016-03-24

    Photochemistry of copper(II) monochlorocomplexes in methanol and acetonitrile solutions is studied by UV-pump/broadband deep-UV-to-near-IR probe femtosecond transient absorption spectroscopy. Upon 255 and 266 nm excitation, the complexes in acetonitrile and methanol, respectively, are promoted to the excited ligand-to-metal charge transfer (LMCT) state, which has a short (sub-250 fs) lifetime. From the LMCT state, the complexes decay via internal conversion to lower-lying ligand field (LF) d-d excited states or the vibrationally hot ground electronic state. A minor fraction of the excited complexes relaxes to the LF electronic excited states, which are relatively long-lived with lifetimes >1 ns. Also, in methanol solutions, about 3% of the LMCT-excited copper(II) monochlorocomplexes dissociate forming copper(I) solvatocomplexes and chlorine atoms, which then further react forming long-lived photoproducts. In acetonitrile, about 50% of the LMCT-excited copper(II) monochlorocomplexes dissociate forming radical and ionic products in a ratio of 3:2. Another minor process observed following excitation only in methanol solutions is the re-equilibration between several forms of the copper(II) ground-state complexes present in solutions. This re-equilibration occurs on a time scale from sub-nanoseconds to nanoseconds.

  2. Visible and Near-IR Reflectance Spectra for Smectite, Sulfate And Perchlorate under Dry Conditions for Interpretation of Martian Surface Mineralogy

    NASA Technical Reports Server (NTRS)

    Morris, R.V.; Ming, W.; Golden, D.C.; Arvidson, R.E.; Wiseman, S.M.; Lichtenberg, K.A.; Cull, S.; Graff, T.G.

    2009-01-01

    Visible and near-IR (VNIR) spectral data for the martian surface obtained from orbit by the MRO-CRISM and OMEGA instruments are interpreted as having spectral signatures of H2O/OH-bearing phases, including smectites and other phyllosilicates, sulfates, and high-SiO2 phases [e.g., 1-4]. Interpretations of martian spectral signatures are based on and constrained by spectra that are obtained in the laboratory on samples with known mineralogical compositions and other physicochemical characteristics under, as appropriate, Mars-like environmental conditions (e.g., temperature, pressure, and humidity). With respect to environmental conditions, differences in the absolute concentration of atmospheric H2O can effect the hydration state and therefore the spectra signatures of smectite phyllosilicates (solvation H2O) and certain sulfates (hydration H2O) [e.g., 5-7]. We report VNIR spectral data acquired under humid (laboratory air) and dry (dry N2 gas) environments for two natural smectites (nontronite API-33A and saponite SapCa-1) to characterize the effect of solvation H2O on spectral properties. We also report spectral data for the thermal dehydration products of (1) melanterite (FeSO4.7H2O) in both air and dry N2 gas and (2) Mg-perchlorate (Mg(ClO4)2.6H2O) in dry N2 environments. Spectral measurements for samples dehydrated in dry N2 were made without exposing them to humid laboratory air.

  3. Wavelength dependence of ocular damage thresholds in the near-ir to far-ir transition region: proposed revisions to MPES.

    PubMed

    Zuclich, Joseph A; Lund, David J; Stuck, Bruce E

    2007-01-01

    This report summarizes the results of a series of infrared (IR) laser-induced ocular damage studies conducted over the past decade. The studies examined retinal, lens, and corneal effects of laser exposures in the near-IR to far-IR transition region (wavelengths from 1.3-1.4 mum with exposure durations ranging from Q-switched to continuous wave). The corneal and retinal damage thresholds are tabulated for all pulsewidth regimes, and the wavelength dependence of the IR thresholds is discussed and contrasted to laser safety standard maximum permissible exposure limits. The analysis suggests that the current maximum permissible exposure limits could be beneficially revised to (1) relax the IR limits over wavelength ranges where unusually high safety margins may unintentionally hinder applications of recently developed military and telecommunications laser systems; (2) replace step-function discontinuities in the IR limits by continuously varying analytical functions of wavelength and pulsewidth which more closely follow the trends of the experimental retinal (for point-source laser exposures) and corneal ED50 threshold data; and (3) result in an overall simplification of the permissible exposure limits over the wavelength range from 1.2-2.6 mum. A specific proposal for amending the IR maximum permissible exposure limits over this wavelength range is presented.

  4. Czochralski growth of Sr2Tb8(SiO4)6O2 crystals for visible-near IR magneto-optical applications

    NASA Astrophysics Data System (ADS)

    Chen, Xin; Zhang, Wenhui; Wan, Qiping; Guo, Feiyun; Zhuang, Naifeng; Fu, Hao; Xie, Xitong; Chen, Jianzhong

    2014-11-01

    Sr2Tb8(SiO4)6O2 crystals have been grown and investigated for the first time for magneto-optical applications. The X-ray powder diffraction confirms that the compound crystallizes in the hexagonal system, with a common oxyapatite structure. The as-grown crystal exhibits low thermal expansion anisotropy (αa/αc ≈ 1.1), and the hardness is about 5.0 Moh. The temperature dependence of the magnetic susceptibility indicated that the Sr2Tb8(SiO4)6O2 crystal exhibits paramagnetic behavior over the experimental temperature-range 2-300 K. The present investigations demonstrate that Sr2Tb8(SiO4)6O2 crystals show a higher visible transparency and a larger Faraday rotation than terbium gallium garnet (TGG) crystals. Sr2Tb8(SiO4)6O2 is therefore a very promising material in particular for new magneto-optical applications in the visible-near IR wavelength region.

  5. CERN, ESA and ESO Launch "Physics On Stage"

    NASA Astrophysics Data System (ADS)

    2000-03-01

    Physics is everywhere . The laws of physics govern the Universe, the Sun, the Earth and even our own lives. In today's rapidly developing society, we are becoming increasingly dependent on high technology - computers, transport, and communication are just some of the key areas that are the result of discoveries by scientists working in physics. But how much do the citizens of Europe really know about physics? Here is a unique opportunity to learn more about this elusive subject! [Go to Physics On Stage Website] Beginning in February 2000, three major European research organisations are organising a unique Europe-wide programme to raise the public awareness of physics and related sciences. "Physics on Stage" is launched by the European Laboratory for Particle Physics (CERN) , the European Space Agency (ESA) and the European Southern Observatory (ESO) , with support from the European Union. Other partners are the European Physical Society (EPS) and the European Association for Astronomy Education (EAAE). This exciting programme is part of the European Week for Science and Technology and will culminate in a Science Festival during November 6-11, 2000, on the CERN premises at the French-Swiss border near Geneva. Why "Physics on Stage"? The primary goal of "Physics on Stage" is to counteract the current decline in interest and knowledge about physics among Europe's citizens by means of a series of highly visible promotional activities. It will bring together leading scientists and educators, government bodies and the media, to confront the diminishing attraction of physics to young people and to develop strategies to reverse this trend. The objective in the short term is to infuse excitement and to provide new educational materials. In the longer term, "Physics on Stage" will generate new developments by enabling experts throughout Europe to meet, exchange and innovate. "Physics on Stage" in 22 European Countries "Physics on Stage" has been initiated in 22 European

  6. ESO Demonstration Project with the NRAO 12-m Antenna

    NASA Astrophysics Data System (ADS)

    Heald, R.; Karban, R.

    2000-03-01

    During the months of September through November 1999, an ALMA joint demonstration project between the European Southern Observatory (ESO) and the National Radio Astronomy Observatory (NRAO) was carried out in Socorro/New Mexico. During this period, Robert Karban (ESO) and Ron Heald (NRAO) worked together on the ESO Demonstration Project. The project integrated ESO software and existing NRAO software (a prototype for the future ALMA control software) to control the motion of the Kitt Peak 12-m antenna. ESO software from the VLT provided the operator interface and coordinate transformation software, while Pat Wallace's TPOINT provided the pointing- model software.

  7. Data products in the ESO Science Archive Facility

    NASA Astrophysics Data System (ADS)

    Retzlaff, Jörg; Arnaboldi, Magda; Romaniello, Martino; Ballester, Pascal; Carson, Paul; Delmotte, Nausicaa; Forchi, Vincenzo; Freudling, Wolfram; Gabasch, Armin; Garcia-Dabo, Cesar Enrique; Hanuschik, Reinhard; Hummel, Wolfgang; Klein Gebbinck, Maurice; Lockhart, John; Micol, Alberto; Modigliani, Andrea; Percheron, Isabelle; Szostak, Artur; Vera Sequeiros, Ignacio

    2014-07-01

    The European Southern Observatory Science Archive Facility is evolving from an archive containing predominantly raw data into a resource also offering science-grade data products for immediate analysis and prompt interpretation. New products originate from two different sources. On the one hand Principal Investigators of Public Surveys and other programmes reduce the raw observational data and return their products using the so-called Phase 3 - a process that extends the Data Flow System after proposal submission (Phase 1) and detailed specification of the observations (Phase 2). On the other hand raw data of selected instruments and modes are uniformly processed in-house, independently of the original science goal. Current data products assets in the ESO science archive facility include calibrated images and spectra, as well as catalogues, for a total volume in excess of 16 TB and increasing. Images alone cover more than 4500 square degrees in the NIR bands and 2400 square degrees in the optical bands; over 85000 individually searchable spectra are already available in the spectroscopic data collection. In this paper we review the evolution of the ESO science archive facility content, illustrate the data access by the community, give an overview of the implemented processes and the role of the associated data standard.

  8. Relaxation mechanism of β-carotene from S2 (1Bu(+)) state to S1 (2Ag(-)) state: femtosecond time-resolved near-IR absorption and stimulated resonance Raman studies in 900-1550 nm region.

    PubMed

    Takaya, Tomohisa; Iwata, Koichi

    2014-06-12

    Carotenoids have two major low-lying excited states, the second lowest (S2 (1Bu(+))) and the lowest (S1 (2Ag(-))) excited singlet states, both of which are suggested to be involved in the energy transfer processes in light-harvesting complexes. Studying vibrational dynamics of S2 carotenoids requires ultrafast time-resolved near-IR Raman spectroscopy, although it has much less sensitivity than visible Raman spectroscopy. In this study, the relaxation mechanism of β-carotene from the S2 state to the S1 state is investigated by femtosecond time-resolved multiplex near-IR absorption and stimulated Raman spectroscopy. The energy gap between the S2 and S1 states is estimated to be 6780 cm(-1) from near-IR transient absorption spectra. The near-IR stimulated Raman spectrum of S2 β-carotene show three bands at 1580, 1240, and 1050 cm(-1). When excess energy of 4000 cm(-1) is added, the S1 C═C stretch band shows a large upshift with a time constant of 0.2 ps. The fast upshift is explained by a model that excess energy generated by internal conversion from the S2 state to the S1 state is selectively accepted by one of the vibronic levels of the S1 state and is redistributed among all the vibrational modes.

  9. The ESO VLT as fischertechnick-Model

    NASA Astrophysics Data System (ADS)

    1988-12-01

    The first fully steerable VLT has already been built! Early in 1988, the well-known German firm "fischerwerke" approached ESO with an interesting suggestion. Having read in the local press about the decision to build the VLT, one of their engineers thought that a model of the VLT, built with the "fischertechnik" building blocks, might become an eye-catching centre on the next toy-fairs in Germany.

  10. The ESO Scientific and Technical Committee.

    NASA Astrophysics Data System (ADS)

    Léna, P.

    1982-03-01

    Since 1978, the structure of ESO involves a Scientific and Technical Committee (STC) which advises the Council on scientific and technical matters. This committee meets twice a year, usually at Garehing; its members are nominated by the Council and their term is 4 years. The STC has 10 members, who are as evenly distributed as possible among member countries, although indeed mainly chosen for their scientific abilities. The chairman is invited to attend Council meetings and to report to the members.

  11. NEVEC: the NOVA ESO VLTI Expertise Center

    NASA Astrophysics Data System (ADS)

    Le Poole, Rudolf S.; Miley, George; Jaffe, Walter; Glindemann, Andreas; Bakker, Eric J.; Waters, Rens; Roettgering, Huub J. A.; Cotton, Bill; Percheron, Isabelle; Meisner, Jeffrey A.; de Jong, Jeroen; D'Arcio, Luigi; Heijligers, Bjoern

    2003-02-01

    The start of NEVEC was initiated by the opportunity in the Netherlands to reinstate instrumental efforts in astronomy through a funding program for 'Top Research Schools,’ which brought about the creation of NOVA. The fact that considerable experience exists in Radio Astronomical imaging through interferometry (the Westerbork Synthesis Radio Telescope started in 1970), and the relatively small size at the time of ESO's VLTI Team made it opportune to aim for a win-win situation through collaboration. So presently an MOU between ESO and NOVA is in force, which stipulates that 10 out of the 18 man-years funded by NOVA for NEVEC until 2005 [new personnel, in university setting (Leiden) but on project money] shall be used on tasks that are mutually agreed between NOVA and ESO. The tasks presently are found in the domain of observing modes, calibration and modeling, as well as contributing to the commissioning of new instruments and thinking about future instruments. Another task, outside these 10 FTE, has been the data handling and analysis software for MIDI, and again contributing to its commissioning. Delivery of the first operational version in Heidelberg has just taken place (summer 2002) contributing to the successful Preliminary Acceptance in Europe for MIDI on September 10, 2002. The actual state of 'products and deliveries' and the future outlook are reviewed.

  12. First detection of Mars atmospheric hydroxyl: CRISM Near-IR measurement versus LMD GCM simulation of OH Meinel band emission in the Mars polar winter atmosphere

    NASA Astrophysics Data System (ADS)

    Clancy, R. Todd; Sandor, Brad J.; García-Muñoz, Antonio; Lefèvre, Franck; Smith, Michael D.; Wolff, Michael J.; Montmessin, Franck; Murchie, Scott L.; Nair, Hari

    2013-09-01

    Visible and near-IR Meinel band emissions originate from excited OH in the terrestrial upper atmosphere (Meinel, I.A.B. [1950]. Astrophys. J. 111, 555. http://dx.doi.org/10.1086/145296), and have recently been detected in the Venus nightside upper mesosphere (Piccioni, G. et al. [2008]. Astron. Astrophys. 483, L29-L33. http://dx.doi.org/10.1051/0004-6361:200809761). Meinel band observations support key studies of transport and photochemistry in both of these atmospheres. In the case of Mars, OH regulates the basic stability of the CO2 atmosphere to photolytic decomposition (to CO and O2, e.g. Parkinson, T.D., Hunten, D.M. [1972]. J. Atmos. Sci. 29, 1380-1390. http://dx.doi.org/10.1175/1520-0469(1972)029<1380:SAAOOO>2.0.CO;2), and yet has never been measured. We present the first detection of Mars atmospheric OH, associated with CRISM near-IR spectral limb observations of polar night Meinel band emissions centered at 1.45 and 2.9 μm. Meinel band (1-0), (2-1), and (2-0) average limb intensities of 990 ± 280, 1060 ± 480, and 200 ± 100 kiloRayleighs (kR), respectively, are determined for 70-90 NS polar winter latitudes over altitudes of 40-56 km. Additional OH bands, such as (3-2), (3-1), and (4-2), present ⩽1σ measurements. Uncertainty in the (4-2) band emission rate contributes to increased uncertainty in the determination of the O2(1Δg) (0-0)/(0-1) band emission ratio A00/A01=47-12+26. An average profile retrieval for Mars OH polar nightglow indicates 45-55 km altitude levels for volume emission rates (VER) of 0.4 (2-0) to 2 (1-0, 2-1) × 104 photons/(cm3 s). Similar to polar night O2(1Δg) emission (e.g. Clancy, R.T. et al. [2012]. J. Geophys. Res. (Planets) 117, E00J10. http://dx.doi.org/10.1029/2011JE004018), Meinel OH band emission is supported by upper level, winter poleward transport of O and H in the deep Hadley solsticial circulations of Mars. The retrieved OH emission rates are compared to polar winter OH nightglow simulated by the LMD (Laboratoire

  13. First detection of Mars atmospheric hydroxyl: CRISM Near-IR measurement versus LMD GCM simulation of OH Meinel band emission in the Mars polar winter atmosphere

    NASA Astrophysics Data System (ADS)

    Todd Clancy, R.; Sandor, Brad J.; García-Muñoz, Antonio; Lefèvre, Franck; Smith, Michael D.; Wolff, Michael J.; Montmessin, Franck; Murchie, Scott L.; Nair, Hari

    2013-09-01

    Visible and near-IR Meinel band emissions originate from excited OH in the terrestrial upper atmosphere (Meinel, I.A.B. [1950]. Astrophys. J. 111, 555. http://dx.doi.org/10.1086/145296), and have recently been detected in the Venus nightside upper mesosphere (Piccioni, G. et al. [2008]. Astron. Astrophys. 483, L29-L33. http://dx.doi.org/10.1051/0004-6361:200809761). Meinel band observations support key studies of transport and photochemistry in both of these atmospheres. In the case of Mars, OH regulates the basic stability of the CO2 atmosphere to photolytic decomposition (to CO and O2, e.g. Parkinson, T.D., Hunten, D.M. [1972]. J. Atmos. Sci. 29, 1380-1390. http://dx.doi.org/10.1175/1520-0469(1972)029<1380:SAAOOO>2.0.CO;2), and yet has never been measured. We present the first detection of Mars atmospheric OH, associated with CRISM near-IR spectral limb observations of polar night Meinel band emissions centered at 1.45 and 2.9 μm. Meinel band (1-0), (2-1), and (2-0) average limb intensities of 990 ± 280, 1060 ± 480, and 200 ± 100 kiloRayleighs (kR), respectively, are determined for 70-90 NS polar winter latitudes over altitudes of 40-56 km. Additional OH bands, such as (3-2), (3-1), and (4-2), present ⩽1σ measurements. Uncertainty in the (4-2) band emission rate contributes to increased uncertainty in the determination of the O2(1Δg) (0-0)/(0-1) band emission ratio A00/A01=47-12+26. An average profile retrieval for Mars OH polar nightglow indicates 45-55 km altitude levels for volume emission rates (VER) of 0.4 (2-0) to 2 (1-0, 2-1) × 104 photons/(cm3 s). Similar to polar night O2(1Δg) emission (e.g. Clancy, R.T. et al. [2012]. J. Geophys. Res. (Planets) 117, E00J10. http://dx.doi.org/10.1029/2011JE004018), Meinel OH band emission is supported by upper level, winter poleward transport of O and H in the deep Hadley solsticial circulations of Mars. The retrieved OH emission rates are compared to polar winter OH nightglow simulated by the LMD (Laboratoire

  14. Hybrid Theranostic Platform for Second Near-IR Window Light Triggered Selective Two-Photon Imaging and Photothermal Killing of Targeted Melanoma Cells.

    PubMed

    Tchounwou, Christine; Sinha, Sudarson Sekhar; Viraka Nellore, Bhanu Priya; Pramanik, Avijit; Kanchanapally, Rajashekhar; Jones, Stacy; Chavva, Suhash Reddy; Ray, Paresh Chandra

    2015-09-23

    Despite advances in the medical field, even in the 21st century cancer is one of the leading causes of death for men and women in the world. Since the second near-infrared (NIR) biological window light between 950 and 1350 nm offers highly efficient tissue penetration, the current article reports the development of hybrid theranostic platform using anti-GD2 antibody attached gold nanoparticle (GNP) conjugated, single-wall carbon nanotube (SWCNT) for second near-IR light triggered selective imaging and efficient photothermal therapy of human melanoma cancer cell. Reported results demonstrate that due to strong plasmon-coupling, two-photon luminescence (TPL) intensity from theranostic GNP attached SWCNT materials is 6 orders of magnitude higher than GNP or SWCNT alone. Experimental and FDTD simulation data indicate that the huge enhancement of TPL intensity is mainly due to strong resonance enhancement coupled with the stronger electric field enhancement. Due to plasmon coupling, the theranostic material serves as a local nanoantennae to enhance the photothermal capability via strong optical energy absorption. Reported data show that theranostic SWCNT can be used for selective two-photon imaging of melanoma UACC903 cell using 1100 nm light. Photothermal killing experiment with 1.0 W/cm(2) 980 nm laser light demonstrates that 100% of melanoma UACC903 cells can be killed using theranostic SWCNT bind melanoma cells after just 8 min of exposure. These results demonstrate that due to plasmon coupling, the theranostic GNP attached SWCNT material serves as a two-photon imaging and photothermal source for cancer cells in biological window II.

  15. Relative Throughput of the Near-IR Science Instruments of the James Webb Space Telescope as Measured in the Ground Testing of the Integrated Science Instrument Module

    NASA Astrophysics Data System (ADS)

    Malumuth, Eliot; Birkmann, Stephan; Kelly, Douglas M.; Kimble, Randy A.; Lindler, Don; Martel, Andre; Ohl, Raymond George; Rieke, Marcia J.; Rowlands, Neil; Te Plate, Maurice

    2016-06-01

    Data were obtained for the purpose of measuring the relative throughput of the Near-IR Science Instruments (SIs) of the James Webb Space Telescope (JWST) as part of the second and third cryogenic-vacuum tests (CV2/CV3) of the Integrated Science Instrument Module (ISIM) conducted at the Goddard Space Flight Center (GSFC) in 2014 and 2015/2016, at the beginning and end of the environmental test program, respectively. In this work we focus on data obtained as part of the Initial Optical Baseline and as part of the Final Performance test -- two epochs that roughly bracket the CV3 test.The purpose of the test is to trend relative throughput to monitor for any potential changes from gross problems such as contamination or degradation of an optical element. Point source data were taken at a variety of wavelengths for NIRCam Module A and Module B, NIRSpec, NIRISS, Guider 1 and Guider 2 using the Laser Diode (LD) 1.06 micron, LD 1.55 micron, 2.1 micron LED and 3.5 micron LED, as well as for NIRCam Mod A and B and NIRISS using a tungsten source and the F277W, and F480M filters. Spectra were taken using the G140M, G235M, and G395M gratings for NIRSpec, the GRISMR grism for NIRCam Mod A and B and the GR150C grism for NIRISS. The results of these measurements will be compared to what would be expected given the efficiency of each of the optical elements in each SI.Although these data were taken as a check against gross problems, they can also be used to provide the first relative throughput estimate for each SI through the various filters/source wavelengths measured in their flight-like configurations.The data, the reduction steps and the resulting cross calibration are presented.

  16. Determination of organic additives in mortars by near-IR spectroscopy. A novel approach to designing a sample set with high-variability components.

    PubMed

    Blanco, Marcelo; Peguero, Anna

    2007-02-01

    Industrial mortars consist primarily of a mixture of cement and an aggregate plus a small amount of additives that are used to modify specific properties. Using too high or too low additive rates usually results in the loss of desirable properties in the end product. This entails carefully controlling the amounts of additives added to mortar in order to ensure correct dosing and/or adequate homogeneity in the final mixture. Near-IR (NIR) spectroscopy has proved effective for this purpose as it requires no sample pretreatment and affords expeditious analyses. The purpose of this work was to determine two organic additives (viz. Ad1 and Ad2) in mortars by using partial least squares regression multivariate calibration models constructed from NIR spectroscopic data. The additives are used to expedite setting and increase cohesion between particles in the mortar. In order to ensure that the sample set contained natural variability in the samples, we used a methodology based on experimental design to construct a representative set of samples. This novel design is based on a hexagonal antiprism that encompasses the concentration ranges spanned by the analytes and the variability inherent in each additive. The D-optimality criterion was used to obtain various combinations between Ad1 and Ad2 additive classes. The partial least squares calibration models thus constructed for each additive provided accurate predictions: the intercept and the slope of the plots of predicted values versus reference values for each additive were close to 0 and 1, respectively, and their confidence ranges included the respective value. The ensuing analytical methods were validated by using an external sample set.

  17. Relative Throughput of the Near-IR Science Instruments for the James Webb Space Telescope as Measured During Ground Testing the Integrated Science Instrument Module

    NASA Technical Reports Server (NTRS)

    Malumuth, Eliot; Birkmann, Stephan; Kelly, Douglas M.; Kimble, Randy A.; Lindler, Don; Martel, Andre; Ohl, Raymond G.; Rieke, Marcia J.; Rowlands, Neil; Te Plate, Maurice

    2016-01-01

    Data were obtained for the purpose of measuring the relative throughput of the Near-IR Science Instruments (SIs) of the James Webb Space Telescope (JWST) as part of the second and third cryogenic-vacuum tests (CV2CV3) of the Integrated Science Instrument Module (ISIM) conducted at the Goddard Space Flight Center (GSFC) in 2014 and 20152016, at the beginning and end of the environmental test program, respectively. This Poster focuses on data obtained as part of the Initial Optical Baseline and as part of the Final Performance test -- two epochs that roughly bracket the CV3 test. The purpose of the test is to trend relative throughput to monitor for any potential changes from gross problems such as contamination or degradation of an optical element. Point source data were taken at a variety of wavelengths for NIRCam Module A and Module B, NIRSpec, NIRISS, Guider 1 and Guider 2 using the Laser Diode (LD) 1.06 micron, LD 1.55 micron, 2.1 micron LED and 3.5 micron LED, as well as for NIRCam Mod A and B and NIRISS using a tungsten source and the F277W, and F480M filters. Spectra were taken using the G140M, G235M, and G395M gratings for NIRSpec, the GRISMR grism for NIRCam Mod A and B and the GR150C grism for NIRISS. The results of these measurements are compared to what would be expected given the efficiency of each of the optical elements in each SI. Although these data were taken as a check against gross problems, they can also be used to provide the first relative throughput estimate for each SI through the various filters source wavelengths measured in their flight-like configurations.

  18. Hybrid Theranostic Platform for Second Near-IR Window Light Triggered Selective Two-Photon Imaging and Photothermal Killing of Targeted Melanoma Cells.

    PubMed

    Tchounwou, Christine; Sinha, Sudarson Sekhar; Viraka Nellore, Bhanu Priya; Pramanik, Avijit; Kanchanapally, Rajashekhar; Jones, Stacy; Chavva, Suhash Reddy; Ray, Paresh Chandra

    2015-09-23

    Despite advances in the medical field, even in the 21st century cancer is one of the leading causes of death for men and women in the world. Since the second near-infrared (NIR) biological window light between 950 and 1350 nm offers highly efficient tissue penetration, the current article reports the development of hybrid theranostic platform using anti-GD2 antibody attached gold nanoparticle (GNP) conjugated, single-wall carbon nanotube (SWCNT) for second near-IR light triggered selective imaging and efficient photothermal therapy of human melanoma cancer cell. Reported results demonstrate that due to strong plasmon-coupling, two-photon luminescence (TPL) intensity from theranostic GNP attached SWCNT materials is 6 orders of magnitude higher than GNP or SWCNT alone. Experimental and FDTD simulation data indicate that the huge enhancement of TPL intensity is mainly due to strong resonance enhancement coupled with the stronger electric field enhancement. Due to plasmon coupling, the theranostic material serves as a local nanoantennae to enhance the photothermal capability via strong optical energy absorption. Reported data show that theranostic SWCNT can be used for selective two-photon imaging of melanoma UACC903 cell using 1100 nm light. Photothermal killing experiment with 1.0 W/cm(2) 980 nm laser light demonstrates that 100% of melanoma UACC903 cells can be killed using theranostic SWCNT bind melanoma cells after just 8 min of exposure. These results demonstrate that due to plasmon coupling, the theranostic GNP attached SWCNT material serves as a two-photon imaging and photothermal source for cancer cells in biological window II. PMID:26327304

  19. The Swift GRB Host Galaxy Legacy Survey. II. Rest-frame Near-IR Luminosity Distribution and Evidence for a Near-solar Metallicity Threshold

    NASA Astrophysics Data System (ADS)

    Perley, D. A.; Tanvir, N. R.; Hjorth, J.; Laskar, T.; Berger, E.; Chary, R.; de Ugarte Postigo, A.; Fynbo, J. P. U.; Krühler, T.; Levan, A. J.; Michałowski, M. J.; Schulze, S.

    2016-01-01

    We present rest-frame near-IR (NIR) luminosities and stellar masses for a large and uniformly selected population of gamma-ray burst (GRB) host galaxies using deep Spitzer Space Telescope imaging of 119 targets from the Swift GRB Host Galaxy Legacy Survey spanning 0.03 < z < 6.3, and we determine the effects of galaxy evolution and chemical enrichment on the mass distribution of the GRB host population across cosmic history. We find a rapid increase in the characteristic NIR host luminosity between z ˜ 0.5 and z ˜ 1.5, but little variation between z ˜ 1.5 and z ˜ 5. Dust-obscured GRBs dominate the massive host population but are only rarely seen associated with low-mass hosts, indicating that massive star-forming galaxies are universally and (to some extent) homogeneously dusty at high redshift while low-mass star-forming galaxies retain little dust in their interstellar medium. Comparing our luminosity distributions with field surveys and measurements of the high-z mass-metallicity relation, our results have good consistency with a model in which the GRB rate per unit star formation is constant in galaxies with gas-phase metallicity below approximately the solar value but heavily suppressed in more metal-rich environments. This model also naturally explains the previously reported “excess” in the GRB rate beyond z ≳ 2 metals stifle GRB production in most galaxies at z < 1.5 but have only minor impact at higher redshifts. The metallicity threshold we infer is much higher than predicted by single-star models and favors a binary progenitor. Our observations also constrain the fraction of cosmic star formation in low-mass galaxies undetectable to Spitzer to be small at z < 4.

  20. ESO Reflex: a graphical workflow engine for data reduction

    NASA Astrophysics Data System (ADS)

    Hook, Richard; Ullgrén, Marko; Romaniello, Martino; Maisala, Sami; Oittinen, Tero; Solin, Otto; Savolainen, Ville; Järveläinen, Pekka; Tyynelä, Jani; Péron, Michèle; Ballester, Pascal; Gabasch, Armin; Izzo, Carlo

    ESO Reflex is a prototype software tool that provides a novel approach to astronomical data reduction by integrating a modern graphical workflow system (Taverna) with existing legacy data reduction algorithms. Most of the raw data produced by instruments at the ESO Very Large Telescope (VLT) in Chile are reduced using recipes. These are compiled C applications following an ESO standard and utilising routines provided by the Common Pipeline Library (CPL). Currently these are run in batch mode as part of the data flow system to generate the input to the ESO/VLT quality control process and are also exported for use offline. ESO Reflex can invoke CPL-based recipes in a flexible way through a general purpose graphical interface. ESO Reflex is based on the Taverna system that was originally developed within the UK life-sciences community. Workflows have been created so far for three VLT/VLTI instruments, and the GUI allows the user to make changes to these or create workflows of their own. Python scripts or IDL procedures can be easily brought into workflows and a variety of visualisation and display options, including custom product inspection and validation steps, are available. Taverna is intended for use with web services and experiments using ESO Reflex to access Virtual Observatory web services have been successfully performed. ESO Reflex is the main product developed by Sampo, a project led by ESO and conducted by a software development team from Finland as an in-kind contribution to joining ESO. The goal was to look into the needs of the ESO community in the area of data reduction environments and to create pilot software products that illustrate critical steps along the road to a new system. Sampo concluded early in 2008. This contribution will describe ESO Reflex and show several examples of its use both locally and using Virtual Observatory remote web services. ESO Reflex is expected to be released to the community in early 2009.

  1. The AstroMundus-ESO Connection

    NASA Astrophysics Data System (ADS)

    Humphreys, E.; Hussain, G.; Biggs, A.; Lu, H.-Y.; Emsellem, E.; De Cia, A.; Lavail, A.; Spyromilio, J.

    2016-03-01

    The AstroMundus Programme is an E+ Erasmus Mundus Joint Masters Degree course in astronomy and astrophysics offered by a consortium of European universities and research institutes. In 2014 and 2016, AstroMundus Masters students visited ESO and participated in proposal-writing sessions, during which groups of students speed-wrote complete ALMA proposals, before presenting them to a pseudo Time Allocation Committee providing on-the-spot feedback. The AstroMundus visit of 25-26 January 2016 is described.

  2. ESO 50th Anniversary Gala Dinner

    NASA Astrophysics Data System (ADS)

    Sirey, R.

    2012-12-01

    To formally mark the 50th anniversary of the signing of the ESO Convention, a gala dinner was held in the Munich Residenz. A brief report of the event is presented and the speeches are reproduced. The speakers were the President of the Council, Xavier Barcons; the German Minister for Education and Research, Prof. Dr Annette Schavan; the Bavarian State Minister for Science, Research and the Arts, Dr Wolfgang Heubisch; physics Nobel Laureate, Brian Schmidt; the current Director General, Tim de Zeeuw and the Chilean Minister of Foreign Affairs, Alfredo Moreno Charme.

  3. Blockbuster starring ESO Paranal opens tomorrow

    NASA Astrophysics Data System (ADS)

    2008-10-01

    The 22nd James Bond adventure is due for release tomorrow, 31 October 2008, in the UK and a week later in the rest of the world. A key location in the movie is the Residencia, the hotel for astronomers and staff at ESO's Paranal Observatory. Blockbuster starring ESO Paranal opens tomorrow ESO PR Photo 38/08 The James Bond "Quantum of Solace" filmmakers Quantum of Solace is the latest film in one of most successful movie franchises -- that of renowned 007 Agent James Bond of the British Secret Service MI6. The agent "on Her Majesty's secret service" is once again played by Daniel Craig. Key scenes of the movie were filmed at Paranal, the home of ESO's Very Large Telescope, and the most advanced optical telescope in the world. Usually occupied by no more than 100 astronomers, engineers and technicians, Paranal welcomed the 300-strong film crew for several days of shooting at the end of March 2008. The crew travelled from their hotel base in Antofagasta for up to two hours each morning to reach the filming locations. "We are delighted to have a movie like this filmed at Paranal and it was extremely good to see how careful the crew were with the surroundings and how mindful they were of the fact that they were in an operating, working observatory", says Tim de Zeeuw, ESO Director General. "Paranal is a unique observatory in a unique setting and it is no real surprise that it plays a major part in a James Bond movie", he adds. The filmmakers were mostly interested in filming exterior scenes at the Paranal Residencia, the accommodation for staff operating the Very Large Telescope. In the movie, the Residencia is supposedly the "Perla de Las Dunas", a unique hotel in the desert. Cerro Paranal is a 2600 m high mountain in the Chilean Atacama Desert, perhaps the driest on Earth. The high altitude site and extreme dryness make excellent conditions for astronomical observations. To make it possible for people to live and work here, a hotel, or Residencia, was built at the

  4. ESO and NSF Sign Agreement on ALMA

    NASA Astrophysics Data System (ADS)

    2003-02-01

    Green Light for World's Most Powerful Radio Observatory On February 25, 2003, the European Southern Observatory (ESO) and the US National Science Foundation (NSF) are signing a historic agreement to construct and operate the world's largest and most powerful radio telescope, operating at millimeter and sub-millimeter wavelength. The Director General of ESO, Dr. Catherine Cesarsky, and the Director of the NSF, Dr. Rita Colwell, act for their respective organizations. Known as the Atacama Large Millimeter Array (ALMA), the future facility will encompass sixty-four interconnected 12-meter antennae at a unique, high-altitude site at Chajnantor in the Atacama region of northern Chile. ALMA is a joint project between Europe and North America. In Europe, ESO is leading on behalf of its ten member countries and Spain. In North America, the NSF also acts for the National Research Council of Canada and executes the project through the National Radio Astronomy Observatory (NRAO) operated by Associated Universities, Inc. (AUI). The conclusion of the ESO-NSF Agreement now gives the final green light for the ALMA project. The total cost of approximately 650 million Euro (or US Dollars) is shared equally between the two partners. Dr. Cesarsky is excited: "This agreement signifies the start of a great project of contemporary astronomy and astrophysics. Representing Europe, and in collaboration with many laboratories and institutes on this continent, we together look forward towards wonderful research projects. With ALMA we may learn how the earliest galaxies in the Universe really looked like, to mention but one of the many eagerly awaited opportunities with this marvellous facility". "With this agreement, we usher in a new age of research in astronomy" says Dr. Colwell. "By working together in this truly global partnership, the international astronomy community will be able to ensure the research capabilities needed to meet the long-term demands of our scientific enterprise, and

  5. Blockbuster starring ESO Paranal opens tomorrow

    NASA Astrophysics Data System (ADS)

    2008-10-01

    The 22nd James Bond adventure is due for release tomorrow, 31 October 2008, in the UK and a week later in the rest of the world. A key location in the movie is the Residencia, the hotel for astronomers and staff at ESO's Paranal Observatory. Blockbuster starring ESO Paranal opens tomorrow ESO PR Photo 38/08 The James Bond "Quantum of Solace" filmmakers Quantum of Solace is the latest film in one of most successful movie franchises -- that of renowned 007 Agent James Bond of the British Secret Service MI6. The agent "on Her Majesty's secret service" is once again played by Daniel Craig. Key scenes of the movie were filmed at Paranal, the home of ESO's Very Large Telescope, and the most advanced optical telescope in the world. Usually occupied by no more than 100 astronomers, engineers and technicians, Paranal welcomed the 300-strong film crew for several days of shooting at the end of March 2008. The crew travelled from their hotel base in Antofagasta for up to two hours each morning to reach the filming locations. "We are delighted to have a movie like this filmed at Paranal and it was extremely good to see how careful the crew were with the surroundings and how mindful they were of the fact that they were in an operating, working observatory", says Tim de Zeeuw, ESO Director General. "Paranal is a unique observatory in a unique setting and it is no real surprise that it plays a major part in a James Bond movie", he adds. The filmmakers were mostly interested in filming exterior scenes at the Paranal Residencia, the accommodation for staff operating the Very Large Telescope. In the movie, the Residencia is supposedly the "Perla de Las Dunas", a unique hotel in the desert. Cerro Paranal is a 2600 m high mountain in the Chilean Atacama Desert, perhaps the driest on Earth. The high altitude site and extreme dryness make excellent conditions for astronomical observations. To make it possible for people to live and work here, a hotel, or Residencia, was built at the

  6. ESO Reflex: A Graphical Workflow Engine for Astronomical Data Reduction

    NASA Astrophysics Data System (ADS)

    Hook, Richard; Romaniello, Martino; Ullgrén, Marko; Maisala, Sami; Solin, Otto; Oittinen, Tero; Savolainen, Villa; Järveläinen, Pekka; Tyynelä, Jani; Péron, Michèle; Izzo, Carlo; Ballester, Pascal; Gabasch, Armin

    2008-03-01

    ESO Reflex is a software tool that provides a novel approach to astronomical data reduction. The reduction sequence is rendered and controlled as a graphical workflow. Users can follow and interact with the processing in an intuitive manner, without the need for complex scripting. The graphical interface also allows the modification of existing workflows and the creation of new ones. ESO Reflex can invoke standard ESO data reduction recipes in a flexible way. Python scripts, IDL procedures and shell commands can also be easily brought into workflows and a variety of visualisation and display options, including custom product inspection and validation steps, are available. ESO Reflex was developed in the context of the Sampo project, a three-year effort led by ESO and conducted by a software development team from Finland as an in-kind contribution to joining ESO. It is planned that the software will be released to the community in late 2008.

  7. Conformers, infrared spectrum, UV-induced photochemistry, and near-IR-induced generation of two rare conformers of matrix-isolated phenylglycine

    SciTech Connect

    Borba, Ana Fausto, Rui; Gómez-Zavaglia, Andrea

    2014-10-21

    The conformational space of α-phenylglycine (PG) have been investigated theoretically at both the DFT/B3LYP/6-311++G(d,p) and MP2/6-311++G(d,p) levels of approximation. Seventeen different minima were found on the investigated potential energy surfaces, which are characterized by different dominant intramolecular interactions: type I conformers are stabilized by hydrogen bonds of the type N–H···O=C, type II by a strong O–H···N hydrogen bond, type III by weak N–H···O–H hydrogen bonds, and type IV by a C=O···H–C contact. The calculations indicate also that entropic effects are relevant in determining the equilibrium populations of the conformers of PG in the gas phase, in particular in the case of conformers of type II, where the strong intramolecular O–H···N hydrogen bond considerably diminishes entropy by reducing the conformational mobility of the molecule. In consonance with the relative energies of the conformers and barriers for conformational interconversion, only 3 conformers of PG were observed for the compound isolated in cryogenic Ar, Xe, and N{sub 2} matrices: the conformational ground state (ICa), and forms ICc and IITa. All other significantly populated conformers existing in the gas phase prior to deposition convert either to conformer ICa or to conformer ICc during matrix deposition. The experimental observation of ICc had never been achieved hitherto. Narrowband near-IR irradiation of the first overtone of νOH vibrational mode of ICa and ICc in nitrogen matrices (at 6910 and 6930 cm{sup −1}, respectively) led to selective generation of two additional conformers of high-energy, ITc and ITa, respectively, which were also observed experimentally for the first time. In addition, these experiments also provided the key information for the detailed vibrational characterization of the 3 conformers initially present in the matrices. On the other hand, UV irradiation (λ = 255 nm) of PG isolated in a xenon matrix revealed that

  8. Conformers, infrared spectrum, UV-induced photochemistry, and near-IR-induced generation of two rare conformers of matrix-isolated phenylglycine.

    PubMed

    Borba, Ana; Gómez-Zavaglia, Andrea; Fausto, Rui

    2014-10-21

    The conformational space of α-phenylglycine (PG) have been investigated theoretically at both the DFT/B3LYP/6-311++G(d,p) and MP2/6-311++G(d,p) levels of approximation. Seventeen different minima were found on the investigated potential energy surfaces, which are characterized by different dominant intramolecular interactions: type I conformers are stabilized by hydrogen bonds of the type N-H···O=C, type II by a strong O-H···N hydrogen bond, type III by weak N-H···O-H hydrogen bonds, and type IV by a C=O···H-C contact. The calculations indicate also that entropic effects are relevant in determining the equilibrium populations of the conformers of PG in the gas phase, in particular in the case of conformers of type II, where the strong intramolecular O-H···N hydrogen bond considerably diminishes entropy by reducing the conformational mobility of the molecule. In consonance with the relative energies of the conformers and barriers for conformational interconversion, only 3 conformers of PG were observed for the compound isolated in cryogenic Ar, Xe, and N2 matrices: the conformational ground state (ICa), and forms ICc and IITa. All other significantly populated conformers existing in the gas phase prior to deposition convert either to conformer ICa or to conformer ICc during matrix deposition. The experimental observation of ICc had never been achieved hitherto. Narrowband near-IR irradiation of the first overtone of νOH vibrational mode of ICa and ICc in nitrogen matrices (at 6910 and 6930 cm(-1), respectively) led to selective generation of two additional conformers of high-energy, ITc and ITa, respectively, which were also observed experimentally for the first time. In addition, these experiments also provided the key information for the detailed vibrational characterization of the 3 conformers initially present in the matrices. On the other hand, UV irradiation (λ = 255 nm) of PG isolated in a xenon matrix revealed that PG undergoes facile

  9. Highly sensitive large-area bolometers for scintillation studies below 100 mK (from near IR to soft x rays)

    NASA Astrophysics Data System (ADS)

    Coron, Noel J.; de Marcillac, Pierre; Leblanc, Jacques; Dambier, Gérard; Moalic, Jean-Pierre

    2004-02-01

    At very low temperature large area bolometers may show a better sensitivity than photomultipliers or semiconductor diodes, while allowing fluorescence measurements of cool targets with no window, no infrared background, good optical couplings and a flat response on a large absorption bandpass. The optical absorber of these composite bolometers can be matched to the desired bandpass. Here we present the design, the performances and calibration tests of a new generation of large area (5 cm2) optical bolometers with a pure germanium disk absorbing on a wide spectral band from near-IR to X-rays. Performances obtained at 25 mK are very promising : Noise Equivalent Power as low as 4x10-17 W/√Hz in the photometry mode, energy threshold about 50 eV in the single photon detection mode, and time constant τ~3 ms. These detectors of low mass (0.25 g) have been recently successfully used for detecting the fluorescence emitted by much more massive bolometers, having for example a BGO (92 g), or a CaWO4 (54 g) target. The simultaneous detection of heat and light in these <> permits the identification of each event in the massive target (α decay, or γ cosmic ray interaction, neutron recoil…). Thanks to the consecutive excellent subtraction of the radioactive and cosmic rays background, it is a powerful tool developed by several groups for fundamental research : study of very rare decays of atoms, measurement of internal very low radioactivity content in single crystals, direct detection of dark matter recoils in massive fluorescence targets, detection of solar neutrino fluorescence events in liquid 4He…Recently obtained results which support this new promising field are reminded: the first detection of the rare alpha decay of 209Bi, and new scintillation data on Al2O3 (sapphire), LiF or TeO2 at 20mK. We discuss the ultimate performances at 12 mK of the optical bolometers as a function of their area, as well as the optimisation of their absorbing part to

  10. VLT instrumentation control: the collaboration of OATs with ESO

    NASA Astrophysics Data System (ADS)

    Santin, P.

    The collaboration of the Astrophysics Technology Group (ATG) of the Astronomical Observatory of Trieste with ESO will be presented. It may be considered as an example of a good practice in the collaboration of a peripheral Institute with ESO. Started in 1985, it spans almost all the time since Italy joined ESO in 1982. The Trieste Astrophysics Technology Group (ATG) participated in many technological enterprise of ESO, from Remote Observing to VLT instrumentation and to ALMA ACS, and is now looking for the challenging E-ELT.

  11. Report on the First ESO-EAAE Astronomy Summer School

    NASA Astrophysics Data System (ADS)

    Pierce-Price, Douglas; Ros, Rosa Maria; Madsen, Claus

    2007-12-01

    The 1st ESO-EAAE Astronomy Summer School for teachers took place in the ESO Headquarters in Garching from 19th to 23rd July 2007. This summer school was based on ten years of successful schools organised around Europe by the EAAE (European Association for Astronomy Education), but 2007 marked increased involvement by ESO. In addition, the summer school was recognised as a Socrates course, allowing teachers to apply for funding through the Socrates programme, while some additional support for delegates was made available through ESO.

  12. ESO Science Outreach Network in Poland during 2011-2013

    NASA Astrophysics Data System (ADS)

    Czart, Krzysztof

    2014-12-01

    ESON Poland works since 2010. One of the main tasks of the ESO Science Outreach Network (ESON) is translation of various materials at ESO website, as well as contacts with journalists. We support also science festivals, conferences, contests, exhibitions, astronomy camps and workshops and other educational and outreach activities. During 2011-2013 we supported events like ESO Astronomy Camp 2013, ESO Industry Days in Warsaw, Warsaw Science Festival, Torun Festival of Science and Art, international astronomy olympiad held in Poland and many others. Among big tasks there was also translation of over 60 ESOcast movies.

  13. Europe's Astronomy Teachers Meet at ESO

    NASA Astrophysics Data System (ADS)

    1994-12-01

    European Association for Astronomy Education Formed A joint EU/ESO Workshop (1) on the Teaching of Astronomy in Europe was held at the ESO Headquarters from November 25-30, 1994, under the auspices of the 1994 European Week for Scientific Culture. More than 100 teachers from secondary schools in 17 European countries participated together with representatives of national ministries and local authorities, as well as professional astronomers. This meeting was the first of its kind ever held and was very successful. As a most visible and immediate outcome, the participants agreed to form the "European Association for Astronomy Education (EAAE)", uniting astronomy educators all over Europe into one network. A provisional Executive Committee of the EAAE was elected which will work towards the organisation of a constitutional conference within the next year. The participants unanimously adopted a "Declaration on the Teaching of Astronomy in Europe", specifying the overall aims and initial actions needed to achieve them. Astronomy: Science, Technology and Culture At the beginning of the Workshop the participants listened to lectures by several specialists about some of the most active fields of astronomy. The scientific sessions included topics as diverse as minor bodies in the solar system, nucleosynthesis, interstellar chemistry and cosmology. Then followed overviews of various recent advances in astronomical technology, some of which are already having direct impact on highly specialized sectors of European industry. They included the advanced use of computers in astronomy, for instance within image processing and data archiving, as well as a demonstration of remote observing. Discussing the cultural aspects, Nigel Calder (UK) and Hubert Reeves (France) emphasized the important role of astronomy in modern society, in particular its continuing influence on our perceptions of mankind's unique location in time and space. Teaching of Astronomy in European Countries

  14. A new "turn-on" naphthalenedimide-based chemosensor for mercury ions with high selectivity: successful utilization of the mechanism of twisted intramolecular charge transfer, near-IR fluorescence, and cell images.

    PubMed

    Li, Qianqian; Peng, Ming; Li, Huiyang; Zhong, Cheng; Zhang, Liang; Cheng, Xiaohong; Peng, Xiaoniu; Wang, Ququan; Qin, Jingui; Li, Zhen

    2012-04-20

    For the first time, a new near-IR "turn-on" fluorescent chemosensor with high selectivity for Hg(2+) ions was designed according to the twisted intramolecular charge transfer (TICT) mechanism. The selective fluorescence enhancement effect can be optimized by modulating the solvent systems. And this naphthalenedimide-based sensor with long wavelength absorption and emission can be used to image intracellular Hg(2+) ions in living Hela cells. PMID:22494314

  15. Post-perihelion coma monitoring of comet Hale-Bopp at ESO

    NASA Astrophysics Data System (ADS)

    Boehnhardt, H.; Bonfils, X.; Petit, Y.; Hainaut, O.; Delahodde, C.; Jorda, L.; Rauer, H.; Colas, F.; Manfroid, J.; Marchis, F.; Schulz, R.; Tanabe, R.; Tozzi, G. P.

    2002-11-01

    The post-perihelion coma activity of Comet C/1995 O1 Hale-Bopp is monitored at ESO telescopes in La Silla and Paranal since Sept. 1997. Imaging through broadband filters in the visible and near-IR wavelength ranges allows to investigate the evolution of the dust coma, namely the appearance of jets, fans, shells and clouds. Long-term evolution: the comet had a porcupine-like embedded fan coma in autumn 1997 that evolved into a northern fan plus shell pattern in 1998 and remains like this since. Thus, the evolution of the coma structure post-perihelion was similar to that pre-perihelion at about the same heliocentric distances, but is occurred in reversed order. This long-term evolution can be characterized by quasi-continuous dust emission from a few (minimum 4) active regions (producing the fan structures) on the nucleus that is modulated by occasional, repetitive and short-term activity increases (generating shell features in the coma). Outbursts: a number of outbursts and unusual activity patterns occurred in the coma of the comet post-perihelion that are documented through the appearance of complex "palm-tree-like" structures of temporary nature in association with outbursts in the visual lightcurve of the comet and a series of 3 dust clouds resembling "mini-comets" and passing through the northern coma at projected velocities of 30-50m/s. The similarity of coma patterns and cometary viewing geometry from Earth before and after perihelion suggests that some nuclear regions had enhanced long-term activity, possibly driven by super-volatile ices at larger (>10AU) heliocentric distances and that the orientation of the rotation axis of the nucleus did not change much over the past 7 years.

  16. The Gaia-ESO Survey Astrophysical Calibration

    NASA Astrophysics Data System (ADS)

    Pancino, E.; Gaia-ESO Survey Consortium

    2016-05-01

    The Gaia-ESO Survey is a wide field spectroscopic survey recently started with the FLAMES@VLT in Cerro Paranal, Chile. It will produce radial velocities more accurate than Gaia's for faint stars (down to V ≃ 18), and astrophysical parameters and abundances for approximately 100 000 stars, belonging to all Galactic populations. 300 nights were assigned in 5 years (with the last year subject to approval after a detailed report). In particular, to connect with other ongoing and planned spectroscopic surveys, a detailed calibration program — for the astrophysical parameters derivation — is planned, including well known clusters, Gaia benchmark stars, and special equatorial calibration fields designed for wide field/multifiber spectrographs.

  17. Manufacturing of the ESO adaptive optics facility

    NASA Astrophysics Data System (ADS)

    Arsenault, R.,; Madec, P.-Y.; Hubin, N.; Stroebele, S.; Paufique, J.; Vernet, E.; Hackenberg, W.; Pirard, J.-F.; Jochum, L.; Glindemann, A.; Jost, A.; Conzelmann, R.; Kiekebusch, M.; Tordo, S.; Lizon, J.-L.; Donaldson, R.; Fedrigo, E.; Soenke, C.; Duchateau, M.; Bruton, A.; Delabre, B.; Downing, M.; Reyes, J.; Kolb, J.; Bechet, C.; Lelouarn, M.; Bonaccini Calia, D.; Quattri, M.; Guidolin, I.; Buzzoni, B.; Dupuy, C.; Guzman, R.; Comin, M.; Silber, A.; Quentin, J.; La Penna, P.; Manescau, A.; Jolley, P.; Heinz, V.; Duhoux, P.; Argomedo, J.; Gallieni, D.; Lazzarini, P.; Biasi, R.; Andrighettoni, M.; Angerer, G.; Pescoller, D.; Stuik, R.,; Deep, A.

    2010-07-01

    The ESO Adaptive Optics Facility (AOF) consists in an evolution of one of the ESO VLT unit telescopes to a laser driven adaptive telescope with a deformable mirror in its optical train, in this case the secondary 1.1m mirror, and four Laser Guide Stars (LGSs). This evolution implements many challenging technologies like the Deformable Secondary Mirror (DSM) including a thin shell mirror (1.1 m diameter and 2mm thin), the high power Na lasers (20W), the low Read-Out Noise (RON) WaveFront Sensor (WFS) camera (< 1e-) and SPARTA the new generation of Real Time Computers (RTC) for adaptive control. It also faces many problematic similar to any Extremely Large Telescope (ELT) and as such, will validate many technologies and solutions needed for the European ELT (E-ELT) 42m telescope. The AOF will offer a very large (7 arcmin) Field Of View (FOV) GLAO correction in J, H and K bands (GRAAL+Hawk-I), a visible integral field spectrograph with a 1 arcmin GLAO corrected FOV (GALACSI-MUSE WFM) and finally a LTAO 7.5" FOV (GALACSI-MUSE NFM). Most systems of the AOF have completed final design and are in manufacturing phase. Specific activities are linked to the modification of the 8m telescope in order to accommodate the new DSM and the 4 LGS Units assembled on its Center-Piece. A one year test period in Europe is planned to test and validate all modes and their performance followed by a commissioning phase in Paranal scheduled for 2014.

  18. NY-ESO-1 specific antibody and cellular responses in melanoma patients primed with NY-ESO-1 protein in ISCOMATRIX and boosted with recombinant NY-ESO-1 fowlpox virus.

    PubMed

    Chen, Ji-Li; Dawoodji, Amina; Tarlton, Andrea; Gnjatic, Sacha; Tajar, Abdelouahid; Karydis, Ioannis; Browning, Judy; Pratap, Sarah; Verfaille, Christian; Venhaus, Ralph R; Pan, Linda; Altman, Douglas G; Cebon, Jonathan S; Old, Lloyd L; Nathan, Paul; Ottensmeier, Christian; Middleton, Mark; Cerundolo, Vincenzo

    2015-03-15

    Vaccination strategies based on repeated injections of NY-ESO-1 protein formulated in ISCOMATRIX particles (NY-ESO-1 ISCOMATRIX) have shown to elicit combined NY-ESO-1 specific antibody and T cell responses. However, it remains unclear whether heterologous prime-boost strategies based on the combination with NY-ESO-1 ISCOMATRIX with different NY-ESO-1 boosting reagents could be used to increase NY-ESO-1 CD8(+) or CD4(+) T cell responses. To address this question, we carried out a randomized clinical trial in 39 high-risk, resected melanoma patients vaccinated with NY-ESO-1 ISCOMATRIX, and then boosted with repeated injections of either recombinant fowlpox virus encoding full length NY-ESO-1 (rF-NY-ESO-1) (Arm A) or NY-ESO-1 ISCOMATRIX alone (Arm B). We have comprehensively analyzed NY-ESO-1 specific T cells and B cells response in all patients before and after vaccination for a total of seven time points per patient. NY-ESO-1 ISCOMATRIX alone elicited a strong NY-ESO-1 specific CD4(+) T cell and antibody response, which was maintained by both regiments at similar levels. However, CD8(+) T cell responses were significantly boosted in 3 out of 18 patients in Arm A after the first rF-NY-ESO-1 injection and such responses were maintained until the end of the trial, while no patients in Arm B showed similar CD8(+) T cell responses. In addition, our results clearly identified immunodominant regions in the NY-ESO-1 protein: NY-ESO-179-102 and NY-ESO-1115-138 for CD4+ T cells and NY-ESO-185-108 for CD8+ T cells in a large proportion of vaccinated patients. These regions of NY-ESO-1 protein should be considered in future clinical trials as immunodominant epitopes.

  19. ESO Observations of New Moon of Jupiter

    NASA Astrophysics Data System (ADS)

    2000-08-01

    Two astronomers, both specialists in minor bodies in the solar system, have performed observations with ESO telescopes that provide important information about a small moon, recently discovered in orbit around the solar system's largest planet, Jupiter. Brett Gladman (of the Centre National de la Recherche Scientifique (CNRS) and working at Observatoire de la Cote d'Azur, France) and Hermann Boehnhardt ( ESO-Paranal) obtained detailed data on the object S/1999 J 1 , definitively confirming it as a natural satellite of Jupiter. Seventeen Jovian moons are now known. The S/1999 J 1 object On July 20, 2000, the Minor Planet Center (MPC) of the International Astronomical Union (IAU) announced on IAU Circular 7460 that orbital computations had shown a small moving object, first seen in the sky in 1999, to be a new candidate satellite of Jupiter. The conclusion was based on several positional observations of that object made in October and November 1999 with the Spacewatch Telescope of the University of Arizona (USA). In particular, the object's motion in the sky was compatible with that of an object in orbit around Jupiter. Following the official IAU procedure, the IAU Central Bureau for Astronomical Telegrams designated the new object as S/1999 J 1 (the 1st candidate Satellite of Jupiter to be discovered in 1999). Details about the exciting detective story of this object's discovery can be found in an MPC press release and the corresponding Spacewatch News Note. Unfortunately, Jupiter and S/1999 J 1 were on the opposite side of the Sun as seen from the Earth during the spring of 2000. The faint object remained lost in the glare of the Sun in this period and, as expected, a search in July 2000 through all available astronomical data archives confirmed that it had not been seen since November 1999, nor before that time. With time, the extrapolated sky position of S/1999 J 1 was getting progressively less accurate. New observations were thus urgently needed to "recover

  20. Public Information and Education in Chile

    NASA Astrophysics Data System (ADS)

    Argandona, G.; Mirabel, F.

    2005-09-01

    One of the initiatives of ESO in Chile is the strengthening of the links with Chilean and Latin American media, to provide the information needed to educate the public in Latin America on the latest advancements in astronomy and astrophysics. This initiative has produced a considerable increase in the media coverage of ESO science activities, as described in Figure 1, which shows the evolution in the number of media publications in Chile on recent achievements at ESO.

  1. The Gaia-ESO Survey: Kinematics of seven Galactic globular clusters

    NASA Astrophysics Data System (ADS)

    Lardo, C.; Pancino, E.; Bellazzini, M.; Bragaglia, A.; Donati, P.; Gilmore, G.; Randich, S.; Feltzing, S.; Jeffries, R. D.; Vallenari, A.; Alfaro, E. J.; Allende Prieto, C.; Flaccomio, E.; Koposov, S. E.; Recio-Blanco, A.; Bergemann, M.; Carraro, G.; Costado, M. T.; Damiani, F.; Hourihane, A.; Jofré, P.; de Laverny, P.; Marconi, G.; Masseron, T.; Morbidelli, L.; Sacco, G. G.; Worley, C. C.

    2015-01-01

    The Gaia-ESO survey is a large public spectroscopic survey aimed at investigating the origin and formation history of our Galaxy by collecting spectroscopy of representative samples (about 105 Milky Way stars) of all Galactic stellar populations, in the field and in clusters. The survey uses globular clusters as intra- and inter-survey calibrators, deriving stellar atmospheric parameters and abundances of a significant number of stars in clusters, along with radial velocity determinations. We used precise radial velocities of a large number of stars in seven globular clusters (NGC 1851, NGC 2808, NGC 4372, NGC 4833, NGC 5927, NGC 6752, and NGC 7078) to validate pipeline results and to preliminarily investigate the cluster internal kinematics. Radial velocity measurements were extracted from FLAMES/GIRAFFE spectra processed by the survey pipeline as part of the second internal data release of data products to ESO. We complemented our sample with ESO archival data obtained with different instrument configurations. Reliable radial velocity measurements for 1513 bona fide cluster star members were obtained in total. We measured systemic rotation, estimated central velocity dispersions, and present velocity dispersion profiles of all the selected clusters, providing the first velocity dispersion curve and the first estimate of the central velocitydispersion for the cluster NGC 5927. Finally, we explore the possible link between cluster kinematics and other physical parameters. The analysis we present here demonstrates that Gaia-ESO survey data are sufficiently accurate to be used in studies of kinematics of stellar systems and stellar populations in the Milky Way. Full Table 3 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/573/A115Based on data products from observations made with ESO telescopes at the La Silla Paranal Observatory under programme 188.B-3002 (the

  2. The ESO Adaptive Optics Facility under Test

    NASA Astrophysics Data System (ADS)

    Arsenault, Robin; Madec, Pierre-Yves; Paufique, Jerome; La Penna, Paolo; Stroebele, Stefan; Vernet, Elise; Pirard, Jean-François; Hackenberg, Wolfgang; Kuntschner, Harald; Kolb, Johann; Muller, Nicolas; Le Louarn, Miska; Amico, Paola; Hubin, Norbert; Lizon, Jean-Louis; Ridings, Rob; Abad, Jose; Fischer, Gert; Heinz, Volker; Kiekebusch, Mario; Argomedo, Javier; Conzelmann, Ralf; Tordo, Sebastien; Donaldson, Rob; Soenke, Christian; Duhoux, Philippe; Fedrigo, Enrico; Delabre, Bernard; Jost, Andrea; Duchateau, Michel; Downing, Mark; Moreno, Javier; Manescau, Antonio; Bonaccini Calia, Domenico; Quattri, Marco; Dupuy, Christophe; Guidolin, Ivan; Comin, Mauro; Guzman, Ronald; Buzzoni, Bernard; Quentin, Jutta; Lewis, Steffan; Jolley, Paul; Kraus, Max; Pfrommer, Thomas; Garcia-Rissmann, Aurea; Biasi, Roberto; Gallieni, Daniele; Stuik, Remko

    2013-12-01

    The Adaptive Optics Facility project has received most of its subsystems in Garching and the ESO Integration Hall has become the central operation location for the next phase of the project. The main test bench ASSIST and the 2nd Generation M2-Unit (hosting the Deformable Secondary Mirror) have been granted acceptance late 2012. The DSM will now undergo a series of tests on ASSIST to qualify its optical performance which launches the System Test Phase of the AOF. The tests will validate the AO modules operation with the DSM: first the GRAAL adaptive optics module for Hawk-I in natural guide star AO mode on-axis and then its Ground Layer AO mode. This will be followed by the GALACSI (for MUSE) Wide-Field-Mode (GLAO) and then the more challenging Narrow-Field-Mode (LTAO). We will report on the status of the subsystems at the time of the conference but also on the performance of the delivered ASSIST test bench, the DSM and the 20 Watt Sodium fiber Laser pre-production unit which has validated all specifications before final manufacturing of the serial units. We will also present some considerations and tools to ensure an efficient operation of the Facility in Paranal.

  3. El sistema ESO 296-IG 11

    NASA Astrophysics Data System (ADS)

    Agüero, E. L.; Paolantonio, S.

    El objeto ESO 296-IG 11 que se presenta en forma de ``V'' y posee destacadas condensaciones a lo largo de cada una de sus dos ramas, las que son de igual extensión (~ 1'), es estudiado en base a material espectroscópico obtenido en el CASLEO. Así se establecen las principales características espectrales, las condiciones físicas y los mecanismos de excitación dominantes de las zonas más notables de su estructura, como así también la distribución de su extinción interna y la variación del grado de excitación de las mismas. Del análisis de las velocidades radiales se determina que se trata de dos galaxias de tipo disco que se están interpenetrando y que conforman un sistema triple junto con una galaxia de contorno elíptico y tamaño considerablemente menor (0.2') que se encuentra a ~ 1.3' del punto de intersección de las dos primeras, ubicada sobre la dirección que contiene a una de éstas y hacia la que se extienden unas débiles y largas prolongaciones de la otra.

  4. President of Czech Republic visits ESO's Paranal Observatory

    NASA Astrophysics Data System (ADS)

    2011-04-01

    On 6 April 2011, the ESO Paranal Observatory was honoured with a visit from the President of the Czech Republic, Václav Klaus, and his wife Livia Klausová, who also took the opportunity to admire Cerro Armazones, the future site of the planned E-ELT. The distinguished visitor was shown the technical installations at the observatory, and was present when the dome of one of the four 8.2-metre Unit Telescopes of ESO's Very Large Telescope opened for a night's observing at Cerro Paranal, the world's most advanced visible-light observatory. "I'm delighted to welcome President Klaus to the Paranal Observatory and to show him first-hand the world-leading astronomical facility that ESO has designed, has built, and operates for European astronomy," said ESO's Director General, Tim de Zeeuw. President Klaus replied, "I am very impressed by the remarkable technology that ESO has built here in the heart of the desert. Czech astronomers are already making good use of these facilities and we look forward to having Czech industry and its scientific community contribute to the future E-ELT." From the VLT platform, the President had the opportunity to admire Cerro Armazones as well as other spectacular views of Chile's Atacama Desert surrounding Paranal. Adjacent to Cerro Paranal, Armazones has been chosen as the site for the future E-ELT (see eso1018). ESO is seeking approval from its governing bodies by the end of 2011 for the go-ahead for the 1-billion euro E-ELT. Construction is expected to begin in 2012 and the start of operations is planned for early in the next decade. President Klaus was accompanied by the Minister of Foreign Affairs of the Czech Republic, Karel Schwarzenberg, the Czech Ambassador in Chile, Zdenek Kubánek, dignitaries of the government, and a Czech industrial delegation. The group was hosted at Paranal by the ESO Director General, Tim de Zeeuw, the ESO Representative in Chile, Massimo Tarenghi, the Director of Operations, Andreas Kaufer, and Jan Palous

  5. ESO Receives Computerworld Honors Program 21st Century Achievement Award in Science Category

    NASA Astrophysics Data System (ADS)

    2005-06-01

    papers in peer-reviewed journals, ESO is now one of the leading astronomical facilities in the world. Coupled with cutting edge optical telescopes and astronomical instruments at the Chile sites, the DFS has contributed to this success by providing the fundamental IT infrastructure for observation and data management." The case study about ESO, together with the case studies from the other winners and laureates of the 2005 Collection, is available on the Computerworld Honors Program Archives On-Line, www.cwheroes.org, and also distributed to more than 134 members of the Computerworld Honors Global Archives. According to Dan Morrow, a founding director and chief historian for the Honors Program, "This year's award recipients exemplify the very best in the creative use of IT in service to mankind. Their work and their stories are outstanding contributions to the history of the information technology revolution in every sense of the word, and, for the archives we serve all over the world, they are, truly, priceless." From more than 250 nominations submitted this year by the industry chairmen and CEO's who serve on the program's Chairmen's Committee, 162 were honoured as laureates at ceremonies in San Francisco, on April 3, 2005, when their case studies officially became part of the Computerworld Honors 2005 Collection. Of these, 48 finalists were chosen by an academy of distinguished judges to attend the June 6 gala in Washington, D.C., at which 10 were announced recipients of the award, one in each of the following categories: Business and Related Services; Education and Academia; Environment, Energy and Agriculture; Finance, Insurance and Real Estate; Government and Non-Profit Organizations; Manufacturing; Media, Arts and Entertainment; Medicine; Science; and Transportation. Additional information about the 2005 Collection is available at www.cwheroes.org, where the entire collection is available to scholars, researchers and the general public. The ESO Data Management and

  6. Young Astronomers' Observe with ESO Telescopes

    NASA Astrophysics Data System (ADS)

    1995-11-01

    Today, forty 16-18 year old students and their teachers are concluding a one-week, educational `working visit' to the ESO Headquarters in Garching (See ESO Press Release 14/95 of 8 November 1995). They are the winners of the Europe-wide contest `Europe Towards the Stars', organised by ESO with the support of the European Union, under the auspices of the Third European Week for Scientific and Technological Culture. From November 14-20, they have worked with professional ESO astronomers in order to get insight into the methods and principles of modern astronomy and astrophysics, as carried out at one of the world's foremost international centres. This included very successful remote observations with the ESO 3.5-m New Technology Telescope (NTT) and the 1.4-m Coude Auxiliary Telescope (CAT) via a satellite link between the ESO Headquarters and the La Silla observatory in Chile, 12,000 kilometres away. After a general introduction to modern astronomy on the first day of the visit, the participants divided into six teams, according to their interests. Some chose to observe distant galaxies, others prefered to have a closer look on binary stars, and one team decided to investigate a star which is thought to be surrounded by a proto-planetary system. Each team was supported by an experienced ESO astronomer. Then followed the observations at the remote consoles during three nights, the first at the NTT and the following at the CAT. Each team had access to the telescope during half a night. Although the work schedule - exactly as in `real' science - was quite hard, especially during the following data reduction and interpretative phase, all teams managed extremely well and in high spirits. The young astronomers' observations were favoured by excellent atmospheric conditions. At the NTT, the seeing was better than 0.5 arcsecond during several hours, an exceptional value that allows very good images to be obtained. All observations represent solid and interesting science, and

  7. ESO Council Resolves to Continue VLT Project at Paranal

    NASA Astrophysics Data System (ADS)

    1995-06-01

    The ESO Council has just met at the ESO Headquarters in Garching during two days of intensive consultations. Among the important items on the agenda were the recent developments around the Very Large Telescope Project at Paranal, and also the possible membership of other countries. RELATIONS WITH CHILE The ESO Council appreciated the continued efforts by the Government of the Republic of Chile to bring to a successful conclusion the various pending matters concerning the relations between the Republic of Chile and this Organisation. It noted the solution of serious problems which have interfered with ESO's operations in its host country, and now awaits formal confirmation from the Chilean Government that also the legal proceedings around the land dispute around the Paranal site are cleared. Council expects that the ratification of the "Intermediate, Supplementary and Amending Agreement" will occur without undue delay and it reiterates its intention to approve this Agreement at the same time as the Chilean Parliament. Meanwhile, Council expressed its pleasure to welcome those Chilean scientists now nominated by the Chilean Government as observers to the ESO committees. Council instructed the ESO Management to continue work at Paranal. Although the delegates were increasingly optimistic that the VLT project can ultimately remain at Paranal, they nevertheless also requested the Management to pursue, until further notice, the ongoing comparative study of first-class astronomical sites in the world. In connection with the pending issues in the relationship with Chile, Council remained preoccupied about the recognition of ESO's immunities by the Chilean judiciary and it requested from the Management that the assessment of the financial and other implications of the recent events which have interfered with the VLT construction work at Paranal be completed. Finally, in order to provide additional avenues for frequent contacts, the ESO Council invited the Chilean Government

  8. Austria to join ESO on 1 July 2008

    NASA Astrophysics Data System (ADS)

    2008-06-01

    Today, at a ceremony in Vienna, the Austrian Minister for Science and Research, Johannes Hahn and the ESO Director General, Tim de Zeeuw, signed the formal Accession Agreement between Austria and ESO, paving the way for Austria to join ESO as its 14th member state by 1 July this year. Signing Austria Agreement ESO PR Photo 20a/08 The Signing Ceremony "This will not only give the high-quality Austrian astronomical community full access to ESO's facilities, it will give Austrian scientists a say, together with their colleagues from the other member-states, in shaping the future of our science," said Tim de Zeeuw. The signing of the Agreement followed the unanimous approval by the ESO Council during its meeting in Prague on 3 June and the decision by the Austrian Government on 25 June. At the ceremony, Minister Hahn emphasised that the accession of Austria to ESO is a strong commitment to fundamental research and particularly to astronomy. "This sustainable investment enables Austrian science to gain access to a leading, international research infrastructure, and provides an important impulse for the attractiveness of Austria as a place for research," he said. "With the signature of the agreement today we bring a long discussion to a happy end and Austrian astronomy to new horizons." Since the Agreement means accession to an international convention, the agreement must now be submitted to the Austrian Parliament for ratification. "It is not possible to plan for radical changes, but ideal conditions will be created by this accession, which will strengthen Austrian and European astronomy. It is now for the scientists to use this opportunity," concluded the Austrian Minister.

  9. Magellan adaptive optics first-light observations of the exoplanet β PIC b. I. Direct imaging in the far-red optical with MagAO+VisAO and in the near-IR with NICI {sup ,}

    SciTech Connect

    Males, Jared R.; Close, Laird M.; Morzinski, Katie M.; Skemer, Andrew J.; Kopon, Derek; Follette, Katherine B.; Hinz, Philip M.; Rodigas, Timothy J.; Wahhaj, Zahed; Liu, Michael C.; Nielsen, Eric L.; Chun, Mark; Puglisi, Alfio; Esposito, Simone; Riccardi, Armando; Pinna, Enrico; Xompero, Marco; Briguglio, Runa; Hayward, Thomas L. [Gemini Observatory, Southern Operations Center, c and others

    2014-05-01

    We present the first ground-based CCD (λ < 1 μm) image of an extrasolar planet. Using the Magellan Adaptive Optics system's VisAO camera, we detected the extrasolar giant planet β Pictoris b in Y-short (Y{sub S} , 0.985 μm), at a separation of 0.470 ± 0.''010 and a contrast of (1.63 ± 0.49) × 10{sup –5}. This detection has a signal-to-noise ratio of 4.1 with an empirically estimated upper limit on false alarm probability of 1.0%. We also present new photometry from the Gemini Near-Infrared Coronagraphic Imager instrument on the Gemini South telescope, in CH {sub 4S,1%} (1.58 μm), K{sub S} (2.18 μm), and K {sub cont} (2.27 μm). A thorough analysis of our photometry combined with previous measurements yields an estimated near-IR spectral type of L2.5 ± 1.5, consistent with previous estimates. We estimate log (L {sub bol}/L {sub ☉}) = –3.86 ± 0.04, which is consistent with prior estimates for β Pic b and with field early-L brown dwarfs (BDs). This yields a hot-start mass estimate of 11.9 ± 0.7 M {sub Jup} for an age of 21 ± 4 Myr, with an upper limit below the deuterium burning mass. Our L {sub bol}-based hot-start estimate for temperature is T {sub eff} = 1643 ± 32 K (not including model-dependent uncertainty). Due to the large corresponding model-derived radius of R = 1.43 ± 0.02 R {sub Jup}, this T {sub eff} is ∼250 K cooler than would be expected for a field L2.5 BD. Other young, low-gravity (large-radius), ultracool dwarfs and directly imaged EGPs also have lower effective temperatures than are implied by their spectral types. However, such objects tend to be anomalously red in the near-IR compared to field BDs. In contrast, β Pic b has near-IR colors more typical of an early-L dwarf despite its lower inferred temperature.

  10. Magellan Adaptive Optics First-light Observations of the Exoplanet β Pic B. I. Direct Imaging in the Far-red Optical with MagAO+VisAO and in the Near-ir with NICI

    NASA Astrophysics Data System (ADS)

    Males, Jared R.; Close, Laird M.; Morzinski, Katie M.; Wahhaj, Zahed; Liu, Michael C.; Skemer, Andrew J.; Kopon, Derek; Follette, Katherine B.; Puglisi, Alfio; Esposito, Simone; Riccardi, Armando; Pinna, Enrico; Xompero, Marco; Briguglio, Runa; Biller, Beth A.; Nielsen, Eric L.; Hinz, Philip M.; Rodigas, Timothy J.; Hayward, Thomas L.; Chun, Mark; Ftaclas, Christ; Toomey, Douglas W.; Wu, Ya-Lin

    2014-05-01

    We present the first ground-based CCD (λ < 1 μm) image of an extrasolar planet. Using the Magellan Adaptive Optics system's VisAO camera, we detected the extrasolar giant planet β Pictoris b in Y-short (YS , 0.985 μm), at a separation of 0.470 ± 0.''010 and a contrast of (1.63 ± 0.49) × 10-5. This detection has a signal-to-noise ratio of 4.1 with an empirically estimated upper limit on false alarm probability of 1.0%. We also present new photometry from the Gemini Near-Infrared Coronagraphic Imager instrument on the Gemini South telescope, in CH 4S,1% (1.58 μm), KS (2.18 μm), and K cont (2.27 μm). A thorough analysis of our photometry combined with previous measurements yields an estimated near-IR spectral type of L2.5 ± 1.5, consistent with previous estimates. We estimate log (L bol/L ⊙) = -3.86 ± 0.04, which is consistent with prior estimates for β Pic b and with field early-L brown dwarfs (BDs). This yields a hot-start mass estimate of 11.9 ± 0.7 M Jup for an age of 21 ± 4 Myr, with an upper limit below the deuterium burning mass. Our L bol-based hot-start estimate for temperature is T eff = 1643 ± 32 K (not including model-dependent uncertainty). Due to the large corresponding model-derived radius of R = 1.43 ± 0.02 R Jup, this T eff is ~250 K cooler than would be expected for a field L2.5 BD. Other young, low-gravity (large-radius), ultracool dwarfs and directly imaged EGPs also have lower effective temperatures than are implied by their spectral types. However, such objects tend to be anomalously red in the near-IR compared to field BDs. In contrast, β Pic b has near-IR colors more typical of an early-L dwarf despite its lower inferred temperature.

  11. Deep Sky Diving with the ESO New Technology Telescope

    NASA Astrophysics Data System (ADS)

    1998-01-01

    Preparations for future cosmological observations with the VLT Within a few months, the first 8.2-meter Unit Telescope of the ESO Very Large Telescope (VLT) array will open its eye towards the sky above the Atacama desert. As documented by recent Press Photos from ESO, the construction work at the Paranal VLT Observatory is proceeding rapidly. Virtually all of the telescope components, including the giant Zerodur mirror (cf. ESO PR Photos 35a-l/97 ), are now on the mountain. While the integration of the telescope and its many optical, mechanical and electronic components continues, astronomers in the ESO member countries and at ESO are now busy defining the observing programmes that will be carried out with the new telescope, soon after it enters into operation. In this context, new and exciting observations have recently been obtained with the 3.5-m New Technology Telescope at the ESO La Silla Observatory, 600 km to the south of Paranal. How to record the faintest and most remote astronomical objects With its very large mirror surface (and correspondingly great light collecting power), as well as an unsurpassed optical quality, the VLT will be able to look exceedingly far out into the Universe, well beyond current horizons. The best technique to record the faintest possible light and thus the most remote celestial objects, is to combine large numbers of exposures of the same field with slightly different telescope pointing. This increases the total number of photons recorded and by imaging the stars and galaxies on different areas (pixels) of the detector, the signal-to-noise ratio and hence the visibility of the faintest objects is improved. The famous Hubble Deep Field Images were obtained in this way by combining over 300 single exposures and they show myriads of faint galaxies in the distant realms of the Universe. The NTT as test bench for the VLT ESO is in the fortunate situation of possessing a `prototype' model of the Very Large Telescope, the 3.5-m New

  12. ESO Council Decides to Continue VLT Project at Paranal

    NASA Astrophysics Data System (ADS)

    1994-08-01

    The Council [1] of the European Southern Observatory has met in extraordinary session at the ESO Headquarters in Garching near Munich on August 8 and 9, 1994. The main agenda items were concerned with the recent developments around ESO's relations with the host state, the Republic of Chile, as well as the status of the organisation's main project, the 16-metre equivalent Very Large Telescope (VLT) which will become the world's largest optical telescope. Council had decided to hold this special meeting [2] because of various uncertainties that have arisen in connection with the implementation of the VLT Project at Cerro Paranal, approx. 130 kilometres south of Antofagasta, capital of the II Region in Chile. Following continued consultations at different levels within the ESO member states and after careful consideration of all aspects of the current situation - including various supportive actions by the Chilean Government as well as the incessive attacks against this international organisation from certain sides reported in the media in that country - Council took the important decision to continue the construction of the VLT Observatory at Paranal, while at the same time requesting the ESO Management to pursue the ongoing studies of alternative solutions. THE COUNCIL DECISIONS In particular, the ESO Council took note of recent positive developments which have occurred since the May 1994 round of discussions with the Chilean authorities in Santiago. The confirmation of ESO's immunities as an International Organization in Chile, contained in a number of important statements and documents, is considered a significant step by the Chilean Government to insure to ESO the unhindered erection and later operation of the VLT on Paranal. Under these circumstances and in order to maintain progress on the VLT project, the ESO Council authorized the ESO Management to continue the on-site work at Paranal. Council also took note of the desire expressed by the Chilean Government

  13. The Challenges in Metadata Management: 20+ Years of ESO Data

    NASA Astrophysics Data System (ADS)

    Vera, I.; Da Rocha, C.; Dobrzycki, A.; Micol, A.; Vuong, M.

    2015-09-01

    The European Southern Observatory Science Archive Facility has been in operations for more than 20 years. It contains data produced by ESO telescopes as well as the metadata needed for characterizing and distributing those data. This metadata is used to build the different archive services provided by the Archive. Over these years, services have been added, modified or even decommissioned creating a cocktail of new, evolved and legacy data systems. The challenge for the Archive is to harmonize the differences of those data systems to provide the community with a homogeneous experience when using ESO data. In this paper, we present ESO experience in three particular challenging areas. First discussion is dedicated to the problem of metadata quality over the time, second discusses how to integrate obsolete data models on the current services and finally we will present the challenges of ever growing databases. We describe our experience dealing with those issues and the solutions adopted to mitigate them.

  14. ESO Archive Operations in support of Services in Garching

    NASA Astrophysics Data System (ADS)

    Fourniol, Nathalie

    2015-12-01

    ESO Science Archive Facility (SAF) is the unique access point to the La Silla Paranal Observatory (LPO) raw data. It also services data products created at ESO with state-of-the-art pipelines, or fed back by the external astronomical community. ESO SAF is a big success in the sense that users access the data every single day, and they want their data fast! A copy of the ALMA Science Archive (ASA) is also accessible at Garching to the European ALMA community via the European ALMA Regional Center. A data portal allows users to get access to the data. In this poster we present the Archive Operations in support of services in Garching, from archiving the data to making them available to the community.

  15. TIMMI, ESO's new 10 μm camera/spectrometer

    NASA Astrophysics Data System (ADS)

    Käufl, H. U.; Jouan, R.; Lagage, P. O.; Masse, P.; Mestreau, P.; Tarrius, A.

    1994-03-01

    TIMMI stands for Thermal Infrared Multi Mode Instrument. TIMMI allows for imaging (at present 16 filters available) with variable magnifications as well as limited long-slit spectroscopy in the l0 μm atmospheric window. The instrument was built by the Service d'Astrophysique (SAP) according to ESO's specification in a period of 2 years. At the telescope the instrument is using the ƒ;35 chopping configuration in conjunction with the special adaptor unit. TIMMI control and primary data-acquisition is performed by an VME-based computer (under OS9) while final data storage and online data processing with ESO's image processing system MIDAS is done using an UNIX workstation. While TIMMI will provide new observational possibilities for the ESO users community it is also supposed to become a test-bed to gain experience for similar instrumentation at the VLT.

  16. TIMMI, ESO's new 10 micron Camera/Spectrometer

    NASA Astrophysics Data System (ADS)

    Kaeufl, H. U.; Jouan, R.; Lagage, P. O.; Masse, P.; Mestreau, P.; Tarrius, A.

    TIMMI stands for Thermal Infrared Multi Mode Instrument. TIMMI allows for imaging (at present 16 filters available) with variable magnifications as well as limited long-slit spectroscopy in the 10micron atmospheric window. The instrument was built by the Service d'Astrophysique (SAP) according to ESO's specification in a period of two years. At the telescope the instrument is using the f35 chopping configuration in conjunction with the special adaptor unit. TIMMI control and primary data-acquisition is performed by an VME-based computer (under OS9) while final data storage and online data processing with ESO's image processing system MIDAS is done using an UNIX workstation. While TIMMI will provide new observational possibilities for the ESO users community it is also supposed to become a test-bed to gain experience for similar instrumentation at the VLT.

  17. hFits: From Storing Metadata to Publishing ESO Data

    NASA Astrophysics Data System (ADS)

    Vera, I.; Dobrzycki, A.; Vuong, M.; Da Rocha, C.

    2012-09-01

    The ESO Archive holds ca. 20 million FITS files: raw observations taken at the La Silla Paranal Observatory in Chile, data from APEX and UKIRT(WFCAM) telescopes, pipeline-processed data generated by the Quality Control and Data Processing Group in ESO Garching and, since recently, reduced data delivered by the PI's through the ESO Phase 3 infrastructure. A metadata repository has been developed at the ESO Archive (Dobrzycki et al. 2007), (Vera et al. 2011), to hold all the FITS file headers with up-to-date information using data warehouse technology. Presently, the repository contains more that 10 billion keywords from headers of all ESO FITS files. We have added to the repository a mechanism for keeping track of header ingestion and modification, allowing to build incremental applications on top of it. The aim is to provide a framework allowing for creation of fast and good quality metadata query services. We present hFits, a tool for data publishing allowing for metadata enhancement. The tool reads from the metadata repository and inserts the metadata into the conventional relational database systems using a simple configuration framework. It utilises the metadata repository tracking mechanism to incrementally refresh the services and transparently propagate any metadata updates. It supports the use of user defined functions where, for example, WCS coordinates can be calculated or related metadata can be extracted from other information systems, and for each new header file it provides to the archived file the access attributes following ESO data access policy, publishing the data to the community.

  18. NGC 3293 revisited by the Gaia-ESO Survey

    NASA Astrophysics Data System (ADS)

    Semaan, Thierry; Morel, Thierry; Gosset, Eric; Zorec, Juan; Frémat, Yves; Blomme, Ronny; Lobel, Alex

    2015-01-01

    In the framework of the Gaia-ESO survey we have determined the fundamental parameters of a large number of B-type stars in the Galactic, young open cluster NGC 3293. The determination of the stellar parameters is based on medium-resolution spectra obtained with FLAMES/GIRAFFE at ESO-VLT. As a second step, we adopted the accurate parameters to determine the chemical abundances of these hot stars. We present a comparison of our results with those obtained by the 'VLT-FLAMES survey of massive stars' (Evans et al. 2005). Our study increases the number of objects analysed and provides an extended view of this cluster.

  19. Dutch Minister of Science Visits ESO Facilities in Chile

    NASA Astrophysics Data System (ADS)

    2005-05-01

    Mrs. Maria van der Hoeven, the Dutch Minister of Education, Culture and Science, who travelled to the Republic of Chile, arrived at the ESO Paranal Observatory on Friday afternoon, May 13, 2005. The Minister was accompanied, among others, by the Dutch Ambassador to Chile, Mr. Hinkinus Nijenhuis, and Mr. Cornelis van Bochove, the Dutch Director of Science. The distinguished visitors were able to acquaint themselves with one of the foremost European research facilities, the ESO Very Large Telescope (VLT), during an overnight stay at this remote site, and later, with the next major world facility in sub-millimetre and millimetre astronomy, the Atacama Large Millimeter Array (ALMA). At Paranal, the guests were welcomed by the ESO Director General, Dr. Catherine Cesarsky; the ESO Council President, Prof. Piet van der Kruit; the ESO Representative in Chile, Prof. Felix Mirabel; the Director of the La Silla Paranal Observatory, Dr. Jason Spyromilio; by one of the Dutch members of the ESO Council, Prof. Tim de Zeeuw; by the renowned astrophysicist from Leiden, Prof. Ewine van Dishoek, as well as by ESO staff members. The visitors were shown the various high-tech installations at the observatory, including many of the large, front-line VLT astronomical instruments that have been built in collaboration between ESO and European research institutes. Explanations were given by ESO astronomers and engineers and the Minister gained a good impression of the wide range of exciting research programmes that are carried out with the VLT. Having enjoyed the spectacular sunset over the Pacific Ocean from the Paranal deck, the Minister visited the VLT Control Room from where the four 8.2-m Unit Telescopes and the VLT Interferometer (VLTI) are operated. Here, the Minister was invited to follow an observing sequence at the console of the Kueyen (UT2) and Melipal (UT3) telescopes. "I was very impressed, not just by the technology and the science, but most of all by all the people involved

  20. The Gaia-ESO Survey: membership and initial mass function of the γ Velorum cluster

    NASA Astrophysics Data System (ADS)

    Prisinzano, L.; Damiani, F.; Micela, G.; Jeffries, R. D.; Franciosini, E.; Sacco, G. G.; Frasca, A.; Klutsch, A.; Lanzafame, A.; Alfaro, E. J.; Biazzo, K.; Bonito, R.; Bragaglia, A.; Caramazza, M.; Vallenari, A.; Carraro, G.; Costado, M. T.; Flaccomio, E.; Jofré, P.; Lardo, C.; Monaco, L.; Morbidelli, L.; Mowlavi, N.; Pancino, E.; Randich, S.; Zaggia, S.

    2016-05-01

    Context. Understanding the properties of young open clusters, such as the initial mass function (IMF), star formation history, and dynamic evolution, is crucial for obtaining reliable theoretical predictions of the mechanisms involved in the star formation process. Aims: We want to obtain a list that is as complete as possible of confirmed members of the young open cluster γ Velorum, with the aim of deriving general cluster properties such as the IMF. Methods: We used all available spectroscopic membership indicators within the Gaia-ESO public archive, together with literature photometry and X-ray data, and for each method, we derived the most complete list of candidate cluster members. Then, we considered photometry, gravity, and radial velocities as necessary conditions for selecting a subsample of candidates whose membership was confirmed by using the lithium and Hα lines and X-rays as youth indicators. Results: We found 242 confirmed and 4 possible cluster members for which we derived masses using very recent stellar evolutionary models. The cluster IMF in the mass range investigated in this study shows a slope of α = 2.6 ± 0.5 for 0.5 ESO/VLT, at Paranal Observatory under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey).Table 5 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/589/A70

  1. Light Phenomena over the ESO Observatories III: Zodiacal Light

    NASA Astrophysics Data System (ADS)

    Horálek, P.; Christensen, L. L.; Nesvorný, D.; Davies, R.

    2016-06-01

    The zodiacal light is often seen at the ESO observatories in the hours after sunset and before sunrise. The origin of the zodiacal light is described and recent research briefly summarised. Some fine images of the zodiacal light from Paranal and La Silla, including the full extent of the night sky are presented.

  2. Elaborated Student Talk in an Elementary ESoL Classroom.

    ERIC Educational Resources Information Center

    Boyd, Maureen P.; Rubin, Donald L.

    2002-01-01

    Examines the discourse in an English as a second or other language (ESoL) classroom in a best-case scenario that contrasted dramatically with more typical school settings. Samples student critical turns (SCTs) across a six-week literature-rich science unit. Shows that the teacher played a crucial role in extended dialogue among students. (SG)

  3. ESDIS Standards Office (ESO): Requirements, Standards and Practices

    NASA Technical Reports Server (NTRS)

    Mitchell, Andrew E.; Mcinerney, Mark Allen; Enloe, Yonsok K.; Conover, Helen T.; Doyle, Allan

    2016-01-01

    The ESDIS Standards Office assists the ESDIS Project in formulating standards policy for NASA Earth Science Data Systems (ESDS), coordinates standards activities within ESDIS, and provides technical expertise and assistance with standards related tasks within the NASA Earth Science Data System Working Groups (ESDSWG). This poster summarizes information found on the earthdata.nasa.gov site that describes the ESO.

  4. VizieR Online Data Catalog: ESO Imaging Survey (EIS) (Arnouts+, 2001)

    NASA Astrophysics Data System (ADS)

    Arnouts, S.; Vandame, B.; Benoist, C.; Groenewegen, M. A. T.; da Costa, L.; Schirmer, M.; Mignani, R. P.; Slijkhuis, R.

    2002-04-01

    This paper presents multi-passband optical data obtained from observations of the Chandra Deep Field South (CDF-S), located at RA=03h32m, Dec=-27{deg}48'. The observations were conducted at the ESO/MPG 2.2 m telescope at La Silla using the 8kx8k Wide-Field Imager (WFI). This data set, taken over a period of one year, represents the first field to be completed by the ongoing Deep Public Survey (DPS) being carried out as a part of the ESO Imaging Survey (EIS) project. The paper describes the optical observations, the techniques employed for un-supervised pipeline processing and the general characteristics of the final data set. Image processing has been performed using multi-resolution image decomposition techniques adapted to the EIS pipeline. The automatic processing steps include standard de-bias and flat-field, automatic removal of satellite tracks, de-fringing/sky-subtraction, image stacking/mosaicking and astrometry. Stacking of dithered images is carried out using pixel-based astrometry which enables the efficient removal of cosmic rays and image defects, yielding remarkably clean final images. The final astrometric calibration is based on a pre-release of the GSC-II catalog and has an estimated intrinsic accuracy of la 0.10 arcsec, with all passbands sharing the same solution. The data are taken in six different filters (U'UBVRI), cover an area of about 0.25 square degrees, and reach the 5{sigma} limiting magnitudes of U'AB=26.0, UAB=25.7, BAB=26.4, VAB=25.4, RAB=25.5 and IAB=24.7 mag, as measured within a 2xFWHM aperture. The optical data covers an area of ~0.1 square degree for which moderately deep observations in two near-infrared bands are also available, reaching 5{sigma} limiting magnitudes of JAB~23.4 and KAB~22.6. The current optical/infrared data also fully encompass the region of the deep X-ray observations recently completed by the Chandra telescope. The optical data presented here, as well as the infrared data released earlier, are publicly

  5. The Gaia-ESO Survey: A globular cluster escapee in the Galactic halo

    NASA Astrophysics Data System (ADS)

    Lind, K.; Koposov, S. E.; Battistini, C.; Marino, A. F.; Ruchti, G.; Serenelli, A.; Worley, C. C.; Alves-Brito, A.; Asplund, M.; Barklem, P. S.; Bensby, T.; Bergemann, M.; Blanco-Cuaresma, S.; Bragaglia, A.; Edvardsson, B.; Feltzing, S.; Gruyters, P.; Heiter, U.; Jofre, P.; Korn, A. J.; Nordlander, T.; Ryde, N.; Soubiran, C.; Gilmore, G.; Randich, S.; Ferguson, A. M. N.; Jeffries, R. D.; Vallenari, A.; Allende Prieto, C.; Pancino, E.; Recio-Blanco, A.; Romano, D.; Smiljanic, R.; Bellazzini, M.; Damiani, F.; Hill, V.; de Laverny, P.; Jackson, R. J.; Lardo, C.; Zaggia, S.

    2015-03-01

    A small fraction of the halo field is made up of stars that share the light element (Z ≤ 13) anomalies characteristic of second generation globular cluster (GC) stars. The ejected stars shed light on the formation of the Galactic halo by tracing the dynamical history of the clusters, which are believed to have once been more massive. Some of these ejected stars are expected to show strong Al enhancement at the expense of shortage of Mg, but until now no such star has been found. We search for outliers in the Mg and Al abundances of the few hundreds of halo field stars observed in the first eighteen months of the Gaia-ESO public spectroscopic survey. One halo star at the base of the red giant branch, here referred to as 22593757-4648029 is found to have [ Mg/Fe ] = -0.36 ± 0.04 and [ Al/Fe ] = 0.99 ± 0.08, which is compatible with the most extreme ratios detected in GCs so far. We compare the orbit of 22593757-4648029 to GCs of similar metallicity andfind it unlikely that this star has been tidally stripped with low ejection velocity from any of the clusters. However, both chemical and kinematic arguments render it plausible that the star has been ejected at high velocity from the anomalous GC ω Centauri within the last few billion years. We cannot rule out other progenitor GCs, because some may have disrupted fully, and the abundance and orbital data are inadequate for many of those that are still intact. Based on data acquired by the Gaia-ESO Survey, programme ID 188.B-3002. Observations were made with ESO Telescopes at the La Silla Paranal Observatory.Appendix A is available in electronic form at http://www.aanda.org

  6. Publications

    Cancer.gov

    Information about NCI publications including PDQ cancer information for patients and health professionals, patient-education publications, fact sheets, dictionaries, NCI blogs and newsletters and major reports.

  7. ESO Council Visits First VLT Unit Telescope Structure in Milan

    NASA Astrophysics Data System (ADS)

    1995-12-01

    As the ESO Very Large Telescope (VLT) rapidly takes on shape, Europe has just come one step closer to the realisation of its 556 million DEM astronomical showcase project. Last week, the ESO Council held its semi-annual meeting in Milan (Italy) [1]. During a break in the long agenda list, Council members had the opportunity to visit the Ansaldo factory in the outskirts of this city and to see for the first time the assembled mechanical structure of one of the four 8.2-metre VLT Unit telescopes. This Press Release is accompanied by a photo that shows the ESO Council delegates in front of the giant telescope. After a long climb up the steep staircase to the large Nasmyth platform at the side of the telescope where the astronomical instruments will later be placed, Dr. Peter Creola (Switzerland) , President of the ESO Council and a mechanics expert, grabbed the handrail and surveyed the structure with a professional eye: `I knew it was going to be big, but not that enormous!', he said. Other delegates experienced similar feelings, especially when they watched the 430 tonnes of steel in the 24-metre tall and squat structure turn smoothly and silently around the vertical axis. The Chairman of the ESO Scientific Technical Committee (STC), Dr. Johannes Andersen (Denmark) , summarized his first, close encounter with the VLT by `This is great fun!' and several of his colleague astronomers were soon seen in various corners of the vast structure, engaged in elated discussions about the first scientific investigations to be done with the VLT in two years' time. The VLT Main Structures The visit by Council took place at the invitation of Ansaldo Energia S.p.A. (Genova), EIE-European Industrial Engineering S.r.I. (Venice) and SOIMI-Societa Impianti Industriale S.p.A. (Milan), the three Italian enterprises responsible for the construction of the main structures of the VLT 8.2-metre Unit telescopes. Short speeches were given on this occasion by Drs. Ferruccio Bressani (Ansaldo

  8. N° 15-2000: ESA, CERN and ESO launch "Physics on Stage"

    NASA Astrophysics Data System (ADS)

    2000-03-01

    But how much do the citizens of Europe really know about physics? Here is a unique opportunity to learn more about this elusive subject! Beginning in February 2000, three major European research establishments [1] are organising a unique Europe-wide programme to raise the public awareness of physics and related sciences. "Physics on Stage" is launched by the European Space Agency (ESA), the European Laboratory for Particle Physics (CERN), and the European Southern Observatory (ESO), with support from the European Union (EU). Other partners include the European Physical Society (EPS) and the European Association for Astronomy Education (EAAE). This exciting programme is part of the European Week for Science and Technology and will culminate in a Science Festival during November 6-11, 2000, at CERN, Geneva. Why "Physics on Stage"? The primary goal of "Physics on Stage" is to counteract the current decline in interest and knowledge of physics among Europe's citizens by means of a series of highly visible promotional activities. It will bring together leading scientists and educators, government bodies and the media, to confront the diminishing attraction of physics to young people and to develop strategies to reverse this trend. The objective in the short term is to infuse excitement and to provide new educational materials. In the longer term, "Physics on Stage" will generate new developments by enabling experts throughout Europe to meet, exchange and innovate. "Physics on Stage" in 22 European Countries. "Physics on Stage" has been initiated in 22 European countries [2]. In each country, a dedicated National Steering Committee (NSC) is being formed which will be responsible for their own national programme. A list of contact addresses is attached below. "Physics on Stage" is based on a series of high-profile physics-related activities that will inform the European public in general, and European high school physics teachers and media representatives in particular

  9. If we build it, will they come? Curation and use of the ESO telescope bibliography

    NASA Astrophysics Data System (ADS)

    Grothkopf, Uta; Meakins, Silvia; Bordelon, Dominic

    2015-12-01

    The ESO Telescope Bibliography (telbib) is a database of refereed papers published by the ESO users community. It links data in the ESO Science Archive with the published literature, and vice versa. Developed and maintained by the ESO library, telbib also provides insights into the organization's research output and impact as measured through bibliometric studies. Curating telbib is a multi-step process that involves extensive tagging of the database records. Based on selected use cases, this talk will explain how the rich metadata provide parameters for reports and statistics in order to investigate the performance of ESO's facilities and to understand trends and developments in the publishing behaviour of the user community.

  10. PIONIER: from a Expert mode to an ESO facility instrument

    NASA Astrophysics Data System (ADS)

    Percheron, Isabelle

    2015-12-01

    The PIONIER (Precision Integrated-Optics Near-infrared Imaging ExpeRiment) at the VLT Interferometer instrument was originally a visitor instrument from IPAG (Institut de Planétologie et d'Astrophysique de Grenoble). It is now offered to the ESO community as a facility instrument. As a Visitor monde instrument, it was operated on selected nights by the instrument team/consortium, the goal is now for the Paranal staff to run and monitor the instrument as any other VLT/VLTI instrument. This is done by fully integrating PIONIER in the ESO scheme. I will present here how this was done for the data reduction and the quality assurance of the science data and their related calibrations.

  11. Participant Perspectives on the ESO Astronomy Camp Programme

    NASA Astrophysics Data System (ADS)

    Olivotto, C.; Cenadelli, D.; Gamal, M.; Grossmann, D.; Teller, L. A. I.; Marta, A. S.; Matoni, C. L.; Taillard, A.

    2015-09-01

    This article describes the experience of attending the European Southern Observatory (ESO) Astronomy Camp from the perspective of its participants - students aged between 16 and 18 years old from around the world. The students shared a week together during the winter of 2014 in the Alpine village of Saint-Barthelemy, Italy. The camp was organised by ESO in collaboration with Sterrenlab and the Astronomical Observatory of the Autonomous Region of the Aosta Valley and offered a rich programme of astronomy and leisure activities. This article focuses on the concept of astronomy camps, and their role as a unique tool to complement formal classroom education, rather than on the astronomy activities and the scientific programme. Thus, it is not an academic review of the implemented methodologies, but rather a reflection on the overall experience. The article was brought together from collaborative accounts by some of the participants who were asked to reflect on the experience. The participants who contributed to this article represent the diversity of the ESO Astronomy Camp's alumni community.

  12. ESO Views of Earth-Approaching Asteroid Toutatis

    NASA Astrophysics Data System (ADS)

    2004-09-01

    Today, September 29, 2004, is undisputedly the Day of Toutatis, the famous "doomsday" asteroid. Not since the year 1353 did this impressive "space rock" pass so close by the Earth as it does today. Visible as a fast-moving faint point of light in the southern skies, it approaches the Earth to within 1,550,000 km, or just four times the distance of the Moon. Closely watched by astronomers since its discovery in January 1989, this asteroid has been found to move in an orbit that brings it close to the Earth at regular intervals, about once every four years. This happened in 1992, 1996, 2000 and now again in 2004. Radar observations during these passages have shown that Toutatis has an elongated shape, measuring about 4.6 x 2.4 x 1.9 km. It tumbles slowly through space, with a rotation period of 5.4 days. The above images of Toutatis were taken with the ESO Very Large Telescope (during a technical test) in the evening of September 28. They were obtained just over 12 hours before the closest approach that happens today at about 15:40 hrs Central European Summer Time (CEST), or 13:40 hrs Universal Time (UT). At the time of these observations, Toutatis was about 1,640,000 km from the Earth, moving with a speed of about 11 km/sec relative to our planet. They show the asteroid as a fast-moving object of magnitude 10, about 40 times fainter than what can be perceived with the unaided, dark-adapted eye. They also prove that Toutatis is right on track, following exactly the predicted trajectory in space and passing the Earth at a safe distance, as foreseen. Detailed calculations, taking into account all available observations of this celestial body, have shown that although Toutatis passes regularly near the Earth, today's passage is the closest one for quite some time, at least until the year 2562. The ESO observations, obtained at a moment when Toutatis was very close to the Earth, will help to further refine the orbital calculations. The "parallax effect" demonstrated! ESO

  13. ESO 603-G21: A strange polar-ring galaxy

    NASA Astrophysics Data System (ADS)

    Reshetnikov, V. P.; Faúndez-Abans, M.; de Oliveira-Abans, M.

    2002-02-01

    We present the results of B, V, R surface photometry of ESO 603-G21 - a galaxy with a possible polar ring. The morphological and photometric features of this galaxy are discussed. The central round object of the galaxy is rather red and presents a nearly exponential surface brightness distribution. This central structure is surrounded by a blue warped ring or disk. The totality of the observed characteristics (optical and NIR colors, strong color gradients, HI and H_2 content, FIR luminosity and star-formation rate, rotation-curve shape, global mass-to-luminosity ratio, the agreement with the Tully-Fisher relation, etc.) shows that ESO 603-G21 is similar to late-type spiral galaxies. We suppose that morphological peculiarities and the possible existence of two large-scale kinematically-decoupled subsystems in ESO 603-G21 can be explained as being a result of dissipative merging of two spiral galaxies or as a consequence of a companion accretion onto a pre-existing spiral host. Based on observations made at the Observatório do Pico dos Dias (OPD), operated by the MCT/Laboratório Nacional de Astrofísica, Brazil.

  14. CERN, ESA and ESO Launch "Physics On Stage"

    NASA Astrophysics Data System (ADS)

    2000-03-01

    Physics is everywhere . The laws of physics govern the Universe, the Sun, the Earth and even our own lives. In today's rapidly developing society, we are becoming increasingly dependent on high technology - computers, transport, and communication are just some of the key areas that are the result of discoveries by scientists working in physics. But how much do the citizens of Europe really know about physics? Here is a unique opportunity to learn more about this elusive subject! [Go to Physics On Stage Website] Beginning in February 2000, three major European research organisations are organising a unique Europe-wide programme to raise the public awareness of physics and related sciences. "Physics on Stage" is launched by the European Laboratory for Particle Physics (CERN) , the European Space Agency (ESA) and the European Southern Observatory (ESO) , with support from the European Union. Other partners are the European Physical Society (EPS) and the European Association for Astronomy Education (EAAE). This exciting programme is part of the European Week for Science and Technology and will culminate in a Science Festival during November 6-11, 2000, on the CERN premises at the French-Swiss border near Geneva. Why "Physics on Stage"? The primary goal of "Physics on Stage" is to counteract the current decline in interest and knowledge about physics among Europe's citizens by means of a series of highly visible promotional activities. It will bring together leading scientists and educators, government bodies and the media, to confront the diminishing attraction of physics to young people and to develop strategies to reverse this trend. The objective in the short term is to infuse excitement and to provide new educational materials. In the longer term, "Physics on Stage" will generate new developments by enabling experts throughout Europe to meet, exchange and innovate. "Physics on Stage" in 22 European Countries "Physics on Stage" has been initiated in 22 European

  15. First Giant Mirror for the ESO VLT Ready at REOSC

    NASA Astrophysics Data System (ADS)

    1995-11-01

    The REOSC Contract In 1989, the European Southern Observatory (ESO), the European Organisation for Astronomy, awarded to REOSC, a subsidiary of the SFIM Group and located in Saint Pierre du Perray (France), a comprehensive contract for the polishing of four 8.2-metre diameter mirrors for the unit telescopes of the ESO Very Large Telescope (VLT) project. These mirrors are the largest ever manufactured and polished. This contract comprises not only the polishing and high-precision optical testing of each giant mirror, but also the safe condition of transportation of the blanks which were manufactured by Schott Glaswerke in Mainz (Germany). In order to fulfill the contract, REOSC conceived, built and equipped a novel, high-tech workshop which would allow to polish and test the mirrors, each of which has a surface area of more than 50 square metres. First 8.2-Metre Mirror is Ready and within Specifications The REOSC polishing facility for giant mirrors was built in Saint Pierre du Perray, just south of Paris. It is equipped with two machines: one for grinding and the other for polishing the mirrors, and both with 150-actuator systems that support the thin and flexible mirrors. All equipment is computer controlled. State-of-the-art interferometers probe the accuracy of the mirror surface as the polishing proceeds; they are installed at the top level of the facility in a 30-metre high tower, at the centre of the mirror's radius of curvature. The success of the work at REOSC is now evident by the fact that careful measurements of the first mirror earlier this month have shown that the final optical surface is correct to within 0.00005 millimetres. For illustration, this corresponds to an accuracy of only 1 millimetre deviation over a surface with a diameter of 165 kilometres (equivalent to the entire Paris area)! ESO Receives the First VLT Mirror After having been carefully placed in a special transport box designed by REOSC, the first mirror blank, weighing 23.5 tons and

  16. Publications.

    ERIC Educational Resources Information Center

    Aviation/Space, 1980

    1980-01-01

    Presents a variety of publications available from government and nongovernment sources. The government publications are from the Federal Aviation Administration (FAA) and the National Aeronautics and Space Administration (NASA) and are designed for educators, students, and the public. (Author/SA)

  17. Near-IR irradiation of the S2 state of the water oxidizing complex of photosystem II at liquid helium temperatures produces the metalloradical intermediate attributed to S1Y(Z*).

    PubMed

    Koulougliotis, Dionysios; Shen, Jian-Ren; Ioannidis, Nikolaos; Petrouleas, Vasili

    2003-03-18

    Near-IR (NIR) excitation at liquid He temperatures of photosystem II (PSII) membranes from the cyanobacterium Synechococcus vulcanus or from spinach poised in the S2 state results in the production of a g = 2.035 EPR resonance, reminiscent of metalloradical signals. The signal is smaller in the spinach preparations, but it is significantly enhanced by the addition of exogenous quinones. Ethanol (2-3%, v/v) eliminates the ability to trap the signal. The g = 2.035 signal is identical to the one recently obtained by Nugent et al. by visible-light illumination of the S1 state, and preferably assigned to S1Y(Z*) [Nugent, J. H. A., Muhiuddin, I. P., and Evans, M. C. W. (2002) Biochemistry 41, 4117-4126]. The production of the g = 2.035 signal by liquid He temperature NIR excitation of the S2 state is paralleled by a significant reduction (typically 40-45% in S. vulcanus) of the S2 state multiline signal. This is in part due to the conversion of the Mn cluster to higher spin states, an effect documented by Boussac et al. [Boussac, A., Un, S., Horner, O., and Rutherford, A. W. (1998) Biochemistry 37, 4001-4007], and in part due to the conversion to the g = 2.035 configuration. Following the decay of the g = 2.035 signal at liquid helium temperatures (decay halftimes in the time range of a few to tens of minutes depending on the preparation), annealing at elevated temperatures (-80 degrees C) results in only partial restoration of the S2 state multiline signal. The full size of the signal can be restored by visible-light illumination at -80 degrees C, implying that during the near-IR excitation and subsequent storage at liquid helium temperatures recombination with Q(A-) (and therefore decay of the S2 state to the S1 state) occurred in a fraction of centers. In support of this conclusion, the g = 2.035 signal remains stable for several hours (at 11 K) in centers poised in the S2...Q(A) configuration before the NIR excitation. The extended stability of the signal under these

  18. V-Band, Near-IR, and TiO Photometry of the Semi-Regular Red Supergiant TV Geminorum: Long-Term Quasi-Periodic Changes in Temperature, Radius, and Luminosity

    NASA Astrophysics Data System (ADS)

    Wasatonic, Richard P.; Guinan, Edward F.; Durbin, Allyn J.

    2015-10-01

    Seventeen years of V-band and intermediate Wing near-IR TiO (λ719-nm to λ1024-nm) time-series photometry of the M1-4 Iab supergiant TV Geminorum are presented. The observations were conducted from 1997 to 2014 with the primary goals of determining both long-term (years) and short-term (months) periodicities and estimating temporal changes in temperature, luminosity, and radius as the star varies in brightness. Our results suggest a dominant short-term V-band period of ~411 days (~1.12 years) that is superimposed on a long-term cycle of ~3137 days (~8.59 years). Over this long-term cycle, the effective temperature varies between ~3500 K to ~3850 K and, at an adopted distance of 1.5 ± 0.2 kpc, the luminosity varies from ~6.2 × 104 Lsolar to ~8.9 × 104 Lsolar and the radius varies from ~620 Rsolar to ~710 Rsolar. Variations in temperature and luminosity are indicative of a semi-regular long-term pulsation with imposed short-term periods similar to the V-band variations. However, the calculated radius variations are apparently not generally inversely correlated with respect to the long-term temperature and luminosity changes as typically found in Cepheids and Mira-type variables. This observation suggests other undetermined mechanisms, such as the formation and subsequent dissipation of supergranules or possible complex pulsations, are taking place in this evolved red supergiant to account for these variations. Like other young, massive luminous red supergiants such as Betelgeuse (α Orionis) and Antares (α Scorpii), TV Gem shows complicated light variations on time scales that range from months to several years. These evolved high massive stars are important to study because they are nearby, bright progenitors of core-collapsed Type II supernovae.

  19. Vaccination with NY-ESO-1 overlapping peptides mixed with Picibanil OK-432 and montanide ISA-51 in patients with cancers expressing the NY-ESO-1 antigen.

    PubMed

    Wada, Hisashi; Isobe, Midori; Kakimi, Kazuhiro; Mizote, Yu; Eikawa, Shingo; Sato, Eiichi; Takigawa, Nagio; Kiura, Katsuyuki; Tsuji, Kazuhide; Iwatsuki, Keiji; Yamasaki, Makoto; Miyata, Hiroshi; Matsushita, Hirokazu; Udono, Heiichiro; Seto, Yasuyuki; Yamada, Kazuhiro; Nishikawa, Hiroyoshi; Pan, Linda; Venhaus, Ralph; Oka, Mikio; Doki, Yuichiro; Nakayama, Eiichi

    2014-01-01

    We conducted a clinical trial of an NY-ESO-1 cancer vaccine using 4 synthetic overlapping long peptides (OLP; peptides #1, 79-108; #2, 100-129; #3, 121-150; and #4, 142-173) that include a highly immunogenic region of the NY-ESO-1 molecule. Nine patients were immunized with 0.25 mg each of three 30-mer and a 32-mer long NY-ESO-1 OLP mixed with 0.2 KE Picibanil OK-432 and 1.25 mL Montanide ISA-51. The primary endpoints of this study were safety and NY-ESO-1 immune responses. Five to 18 injections of the NY-ESO-1 OLP vaccine were well tolerated. Vaccine-related adverse events observed were fever and injection site reaction (grade 1 and 2). Two patients showed stable disease after vaccination. An NY-ESO-1-specific humoral immune response was observed in all patients and an antibody against peptide #3 (121-150) was detected firstly and strongly after vaccination. NY-ESO-1 CD4 and CD8 T-cell responses were elicited in these patients and their epitopes were identified. Using a multifunctional cytokine assay, the number of single or double cytokine-producing cells was increased in NY-ESO-1-specific CD4 and CD8 T cells after vaccination. Multiple cytokine-producing cells were observed in PD-1 (-) and PD-1 (+) CD4 T cells. In conclusion, our study indicated that the NY-ESO-1 OLP vaccine mixed with Picibanil OK-432 and Montanide ISA-51 was well tolerated and elicited NY-ESO-1-specific humoral and CD4 and CD8 T-cell responses in immunized patients.

  20. The primary mirror support system of the ESO-VLT.

    NASA Astrophysics Data System (ADS)

    Schneermann, M.; Cui, X.-Q.

    1988-10-01

    The 8 meter unit telescopes of the ESO very large telescope (VLT) will have primary mirrors of the solid thin meniscus type. Presently various different options concerning material and thickness are still under consideration for the production of the mirror blanks. This paper describes the performance analysis of a glass ceramic mirror with a thickness of 200 mm. This mirror is supported by a functionally separated axial and radial support system. The results of the analytical assessment of the mirror performance under those loading conditions are discussed.

  1. Report on the ESO Workshop ''Satellites and Streams in Santiago''

    NASA Astrophysics Data System (ADS)

    Küpper, A. H. W.; Mieske, S.

    2015-09-01

    Galactic satellites and tidal streams are arguably the two most direct imprints of hierarchical structure formation in the haloes of galaxies. At this ESO workshop we sought to create the big picture of the galactic accretion process, and shed light on the interplay between satellites and streams in the Milky Way, Andromeda and beyond. The Scientific Organising Committee prepared a well-balanced programme with 60 talks and 30 poster contributions, resulting in a meeting which was greatly enjoyed by the more than 110 participants at the venue, and worldwide via Twitter (#SSS15).

  2. Plans for a fast image recording system at ESO

    NASA Technical Reports Server (NTRS)

    Grosboel, P. J.

    1984-01-01

    A 256 diode-array will be installed as detector on the ESO OPTRONICS S-3000 measuring machine in order to increase the acquisition rate. A high intensity LED will be used as light source in a pulse mode. The data will be stored on a random access mass storage device as density values for later education. The scanning time for a 30 cm x 30 cm plate with a step size of 10 micron will be less than 10 hours while the dynamic range of the data is expected to be 2.5 density units with an offset of at least 1 unit.

  3. High-velocity extended molecular outflow in the star-formation dominated luminous infrared galaxy ESO 320-G030

    NASA Astrophysics Data System (ADS)

    Pereira-Santaella, M.; Colina, L.; García-Burillo, S.; Alonso-Herrero, A.; Arribas, S.; Cazzoli, S.; Emonts, B.; Piqueras López, J.; Planesas, P.; Storchi Bergmann, T.; Usero, A.; Villar-Martín, M.

    2016-10-01

    We analyze new high spatial resolution (~60 pc) ALMA CO(2-1) observations of the isolated luminous infrared galaxy ESO 320-G030 (d = 48 Mpc) in combination with ancillary Hubble Space Telescope optical and near infrared (IR) imaging, as well as VLT/SINFONI near-IR integral field spectroscopy. We detect a high-velocity (~450 km s-1) spatially resolved (size~2.5 kpc; dynamical time ~3 Myr) massive (~107 M⊙; Ṁ ~ 2-8 M⊙ yr-1) molecular outflow that has originated in the central ~250 pc. We observe a clumpy structure in the outflowing cold molecular gas with clump sizes between 60 and 150 pc and masses between 105.5 and 106.4 M⊙. The mass of the clumps decreases with increasing distance, while the velocity is approximately constant. Therefore, both the momentum and kinetic energy of the clumps decrease outwards. In the innermost (~100 pc) part of the outflow, we measure a hot-to-cold molecular gas ratio of 7 × 10-5, which is similar to that measured in other resolved molecular outflows. We do not find evidence of an ionized phase in this outflow. The nuclear IR and radio properties are compatible with strong and highly obscured star-formation (Ak ~ 4.6 mag; star formation rate ~ 15 M⊙ yr-1). We do not find any evidence for the presence of an active galactic nucleus. We estimate that supernova explosions in the nuclear starburst (νSN ~ 0.2 yr-1) can power the observed molecular outflow. The kinetic energy and radial momentum of the cold molecular phase of the outflow correspond to about 2% and 20%, respectively, of the supernovae output. The cold molecular outflow velocity is lower than the escape velocity, so the gas will likely return to the galaxy disk. The mass loading factor is ~0.1-0.5, so the negative feedback owing to this star-formation-powered molecular outflow is probably limited. The reduced images and datacubes (FITS files) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc

  4. NY-ESO-1 expression in synovial sarcoma and other mesenchymal tumors: significance for NY-ESO-1-based targeted therapy and differential diagnosis.

    PubMed

    Lai, Jin-Ping; Robbins, Paul F; Raffeld, Mark; Aung, Phyu Phyu; Tsokos, Maria; Rosenberg, Steven A; Miettinen, Markku M; Lee, Chyi-Chia Richard

    2012-06-01

    A promising targeted therapy against NY-ESO-1 (CTAG 1B) using genetically modified T-cells in synovial sarcomas was recently demonstrated in a clinical trial at the NCI. To investigate the role of NY-ESO-1 immunohistochemistry in patient selection and gain better insight into the incidence of NY-ESO-1 expression in synovial sarcomas and other mesenchymal tumors, we evaluated NY-ESO-1 expression by immunohistochemistry in 417 tumors. This collection of samples included: 50 SS18/SSX1/2 fusion positive synovial sarcomas, 155 gastrointestinal stromal tumors (GIST), 135 other spindle cell sarcomas as well as 77 other sarcomas (chondrosarcoma, osteosarcoma, dedifferentiated liposarcoma, alveolar soft part sarcoma, rhabdomyosarcoma, angiosarcoma, malignant mesothelioma, and Ewing's sarcoma). We report that 76% of synovial sarcomas expressed NY-ESO-1 in a strong and diffuse pattern (2-3+, >50-70% of tumor cells). In contrast, only rare cases of other spindle cell mesenchymal tumor expressed NY-ESO-1 (GIST (2/155), malignant peripheral nerve sheath tumors (1/34), and dermatofibrosarcoma protuberans (2/20)). Individual cases of other sarcomas (angiosarcoma, malignant mesothelioma, chondrosarcoma, osteosarcoma, dedifferentiated liposarcoma, alveolar soft part sarcoma, and Ewing's sarcoma) were positive for NY-ESO-1. However, no positive cases were identified amongst our cohort of leiomyosarcomas (0/24), hemangiopericytoma/solitary fibrous tumors (0/40), and cellular schwannomas (0/17). In summary, we find that NY-ESO-1 is strongly and diffusely expressed in a majority of synovial sarcomas, but only rarely in other mesenchymal lesions. Beyond its role in patient selection for targeted therapy, immunohistochemistry for NY-ESO-1 may be diagnostically useful for the distinction of synovial sarcoma from other spindle cell neoplasms.

  5. Increased NY-ESO-1 expression and reduced infiltrating CD3+ T cells in cutaneous melanoma.

    PubMed

    Giavina-Bianchi, Mara; Giavina-Bianchi, Pedro; Sotto, Mirian Nacagami; Muzikansky, Alona; Kalil, Jorge; Festa-Neto, Cyro; Duncan, Lyn M

    2015-01-01

    NY-ESO-1 is a cancer-testis antigen aberrantly expressed in melanomas, which may serve as a robust and specific target in immunotherapy. NY-ESO-1 antigen expression, tumor features, and the immune profile of tumor infiltrating lymphocytes were assessed in primary cutaneous melanoma. NY-ESO-1 protein was detected in 20% of invasive melanomas (16/79), rarely in in situ melanoma (1/10) and not in benign nevi (0/20). Marked intratumoral heterogeneity of NY-ESO-1 protein expression was observed. NY-ESO-1 expression was associated with increased primary tumor thickness (P = 0.007) and inversely correlated with superficial spreading melanoma (P < 0.02). NY-ESO-1 expression was also associated with reduced numbers and density of CD3+ tumor infiltrating lymphocytes (P = 0.017). When NY-ESO-1 protein was expressed, CD3+ T cells were less diffusely infiltrating the tumor and were more often arranged in small clusters (P = 0.010) or as isolated cells (P = 0.002) than in large clusters of more than five lymphocytes. No correlation of NY-ESO-1 expression with gender, age, tumor site, ulceration, lymph node sentinel status, or survival was observed. NY-ESO-1 expression in melanoma was associated with tumor progression, including increased tumor thickness, and with reduced tumor infiltrating lymphocytes.

  6. NY-ESO-1 protein glycosylated by yeast induces enhanced immune responses.

    PubMed

    Wadle, Andreas; Mischo, Axel; Strahl, Sabine; Nishikawa, Hiroyoshi; Held, Gerhard; Neumann, Frank; Wullner, Beate; Fischer, Eliane; Kleber, Sascha; Karbach, Julia; Jager, Elke; Shiku, Hiroshi; Odunsi, Kunle; Shrikant, Protul A; Knuth, Alexander; Cerundolo, Vincenzo; Renner, Christoph

    2010-11-01

    Vaccine strategies that target dendritic cells to elicit potent cellular immunity are the subject of intense research. Here we report that the genetically engineered yeast Saccharomyces cerevisiae, expressing the full-length tumour-associated antigen NY-ESO-1, is a versatile host for protein production. Exposing dendritic cells (DCs) to soluble NY-ESO-1 protein linked to the yeast a-agglutinin 2 protein (Aga2p) protein resulted in protein uptake, processing and MHC class I cross-presentation of NY-ESO-1-derived peptides. The process of antigen uptake and cross-presentation was dependent on the glycosylation pattern of NY-ESO-1-Aga2p protein and the presence of accessible mannose receptors. In addition, NY-ESO-1-Aga2p protein uptake by dendritic cells resulted in recognition by HLA-DP4 NY-ESO-1-specific CD4(+) T cells, indicating MHC class II presentation. Finally, vaccination of mice with yeast-derived NY-ESO-1-Aga2p protein led to an enhanced humoral and cellular immune response, when compared to the bacterially expressed NY-ESO-1 protein. Together, these data demonstrate that yeast-derived full-length NY-ESO-1-Aga2p protein is processed and presented efficiently by MHC class I and II complexes and warrants clinical trials to determine the potential value of S. cerevisiae as a host for cancer vaccine development.

  7. CUBES: cassegrain U-band Brazil-ESO spectrograph

    NASA Astrophysics Data System (ADS)

    Barbuy, B.; Bawden Macanhan, V.; Bristow, P.; Castilho, B.; Dekker, H.; Delabre, B.; Diaz, M.; Gneiding, C.; Kerber, F.; Kuntschner, H.; La Mura, G.; Maciel, W.; Meléndez, J.; Pasquini, L.; Pereira, C. B.; Petitjean, P.; Reiss, R.; Siqueira-Mello, C.; Smiljanic, R.; Vernet, J.

    2014-11-01

    CUBES is a high-efficiency, medium-resolution ( R˜20,000) ground based UV (300-400 nm) spectrograph, to be installed in the cassegrain focus of one of ESO's VLT unit telescopes in 2017/18. The CUBES project is a joint venture between ESO and IAG/USP, and LNA/MCTI. CUBES will provide access to a wealth of new and relevant information for stellar as well as extragalactic sources. Main science cases include the study of beryllium and heavy elements in metal-poor stars, the direct determination of carbon, nitrogen and oxygen abundances by study of molecular bands in the UV range, as well as the study of active galactic nuclei and the quasar absorption lines. With a streamlined modern instrument design, high efficiency dispersing elements and UV-sensitive detectors, it will give a significant gain in sensitivity over existing ground based medium-high resolution spectrographs, enabling vastly increased sample sizes accessible to the astronomical community. We present here a brief overview of the project including the status, science cases and a discussion of the design options.

  8. The Gaia-ESO Survey: Stellar content and elemental abundances in the massive cluster NGC 6705

    NASA Astrophysics Data System (ADS)

    Cantat-Gaudin, T.; Vallenari, A.; Zaggia, S.; Bragaglia, A.; Sordo, R.; Drew, J. E.; Eisloeffel, J.; Farnhill, H. J.; Gonzalez-Solares, E.; Greimel, R.; Irwin, M. J.; Kupcu-Yoldas, A.; Jordi, C.; Blomme, R.; Sampedro, L.; Costado, M. T.; Alfaro, E.; Smiljanic, R.; Magrini, L.; Donati, P.; Friel, E. D.; Jacobson, H.; Abbas, U.; Hatzidimitriou, D.; Spagna, A.; Vecchiato, A.; Balaguer-Nunez, L.; Lardo, C.; Tosi, M.; Pancino, E.; Klutsch, A.; Tautvaisiene, G.; Drazdauskas, A.; Puzeras, E.; Jiménez-Esteban, F.; Maiorca, E.; Geisler, D.; San Roman, I.; Villanova, S.; Gilmore, G.; Randich, S.; Bensby, T.; Flaccomio, E.; Lanzafame, A.; Recio-Blanco, A.; Damiani, F.; Hourihane, A.; Jofré, P.; de Laverny, P.; Masseron, T.; Morbidelli, L.; Prisinzano, L.; Sacco, G. G.; Sbordone, L.; Worley, C. C.

    2014-09-01

    (the public Gaia-ESO spectroscopic survey, PIs Gilmore and Randich) and on the archive data of the programme 083.D-0671.Full Table 2 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/569/A17

  9. Gaia-ESO Survey: Gas dynamics in the Carina nebula through optical emission lines

    NASA Astrophysics Data System (ADS)

    Damiani, F.; Bonito, R.; Magrini, L.; Prisinzano, L.; Mapelli, M.; Micela, G.; Kalari, V.; Maíz Apellániz, J.; Gilmore, G.; Randich, S.; Alfaro, E.; Flaccomio, E.; Koposov, S.; Klutsch, A.; Lanzafame, A. C.; Pancino, E.; Sacco, G. G.; Bayo, A.; Carraro, G.; Casey, A. R.; Costado, M. T.; Franciosini, E.; Hourihane, A.; Lardo, C.; Lewis, J.; Monaco, L.; Morbidelli, L.; Worley, C.; Zaggia, S.; Zwitter, T.; Dorda, R.

    2016-06-01

    Aims: We present observations from the Gaia-ESO Survey in the lines of Hα, [N II], [S II], and He I of nebular emission in the central part of the Carina nebula. Methods: We investigate the properties of the two already known kinematic components (approaching and receding), which account for the bulk of emission. Moreover, we investigate the features of the much less known low-intensity high-velocity (absolute RV >50 km s-1) gas emission. Results: We show that gas giving rise to Hα and He I emission is dynamically well correlated with but not identical to gas seen through forbidden-line emission. Gas temperatures are derived from line-width ratios, and densities from [S II] doublet ratios. The spatial variation of N ionization is also studied, and found to differ between the approaching and receding components. The main result is that the bulk of the emission lines in the central part of Carina arise from several distinct shell-like expanding regions, the most evident found around η Car, the Trumpler 14 core, and the star WR25. These "shells" are non-spherical and show distortions probably caused by collisions with other shells or colder, higher-density gas. Some of them are also partially obscured by foreground dust lanes, while very little dust is found in their interior. Preferential directions, parallel to the dark dust lanes, are found in the shell geometries and physical properties, probably related to strong density gradients in the studied region. We also find evidence that the ionizing flux emerging from η Car and the surrounding Homunculus nebula varies with polar angle. The high-velocity components in the wings of Hα are found to arise from expanding dust reflecting the η Car spectrum. Based on observations collected with the FLAMES spectrograph at VLT/UT2 telescope (Paranal Observatory, ESO, Chile), for the Gaia-ESO Large Public Survey (program 188.B-3002).Full Tables 1-3 are only available at the CDS via anonymous ftp to http

  10. A Multi-wavelength study with the ESO VLT of comet 103P/Hartley2 at the time of the EPOXI encounter

    NASA Astrophysics Data System (ADS)

    Jehin, E.; Hutsemekers, D.; Manfroid, J.; Decock, A.; Weiler, M.; Kawakita, H.; Shinnaka, Y.; Hashimoto, M.; Bockelée-Morvan, D.; Biver, N.; Crovisier, J.; Hartog, P.

    2011-10-01

    We report on simultaneous optical and infrared spectroscopic observations of the Jupiter Family comet 103P/Hartley2 performed with the UT-1 and UT-2 8-m Unit Telescopes of the ESO Very Large Telescope (VLT). These coordinated observations were carried on during several nights (2010 Nov. 5, 9, 10 and 11 UT) around the NASA EPOXI encounter with the comet on Nov. 4 [1] and in support to the key program « Water and related chemistry in the Solar System » (HssO) [2] of the Herschel Space Observatory. From high resolution optical spectroscopy of the CN (0,0) 388 nm band using UVES at UT2 we determined the isotopic ratios 12C/13C = 95 ± 15 and 14N/15N = 155 ± 25 in the CN radical. From the NH2 (0,9,0) and the H2O+ bands around 600 nm, we derived a nuclear spin temperature of 33 ± 3 K for NH3 and 36 +7/-6 K for H2O. These values are similar to those found in Oort- Cloud and Jupiter Family comets. From lowresolution long-slit spectroscopy with FORS2 at UT1 we will determine the CN, C2 and C3 spatial profiles and their production rates. From the high-resolution near-IR spectra that we collected with CRIRES at UT1 we will measure simultaneously the production rates and mixing ratios of the parent molecules H2O, HCN, C2H6, and CH3OH that are well detected in our spectra and we will study the link to the daughter species.

  11. Live Webcasts from CERN and ESO for European Science and Technology Week

    NASA Astrophysics Data System (ADS)

    2002-10-01

    Visit http://www.cern.ch/sci-tech on 7 - 8 November to find out what modern Europeans can't live without. Seven of Europe's leading Research Organizations [1] are presenting three live Webcasts from CERN in a joint outreach programme for the European Science and Technology Week . The aim of Sci-Tech... couldn't be without it! is to show how today's society couldn't be without cutting-edge scientific research. See also ESO Press Release 05/02. Northern Europeans can't imagine their households without ovens, whereas Southern Europeans identify the refrigerator as the most essential household appliance. In the area of communications, cars and motorbikes are clearly the technologies of choice in Italy, but are regarded as less important in countries like Norway and Germany. For entertainment, the personal computer is a clear winner as the device is considered most essential by all Europeans, followed by the TV and the Internet. This hit parade of technological marvels is the result of a phone and online survey conducted by the Sci-Tech... couldn't be without it! team for this year's European Science and Technology Week on 4-10 November. The technologies Europeans could not be without, form the starting point of three entertaining and informative Webcast shows in Italian (Thursday 7 November at 10:00 CET), French (Thursday 7 November at 15:00 CET) and English (Friday 8 November at 15:00 CET), broadcast live on the Internet from a studio at CERN. During these Webcasts scientists from the seven research Organizations and their industrial partners Sun Microsystems, Siemens, L'Oreal and Luminex will engage - from the CERN studio or from remote locations through teleconference links - an audience of Internauts all over the world. The public will be taken inside their most popular gadgets to discover the science that made them possible and how vital fundamental research has been in the creation of modern technology. Fundamental science will be brought as close as possible to

  12. The Gaia-ESO Survey: Empirical determination of the precision of stellar radial velocities and projected rotation velocities

    NASA Astrophysics Data System (ADS)

    Jackson, R. J.; Jeffries, R. D.; Lewis, J.; Koposov, S. E.; Sacco, G. G.; Randich, S.; Gilmore, G.; Asplund, M.; Binney, J.; Bonifacio, P.; Drew, J. E.; Feltzing, S.; Ferguson, A. M. N.; Micela, G.; Neguerela, I.; Prusti, T.; Rix, H.-W.; Vallenari, A.; Alfaro, E. J.; Allende Prieto, C.; Babusiaux, C.; Bensby, T.; Blomme, R.; Bragaglia, A.; Flaccomio, E.; Francois, P.; Hambly, N.; Irwin, M.; Korn, A. J.; Lanzafame, A. C.; Pancino, E.; Recio-Blanco, A.; Smiljanic, R.; Van Eck, S.; Walton, N.; Bayo, A.; Bergemann, M.; Carraro, G.; Costado, M. T.; Damiani, F.; Edvardsson, B.; Franciosini, E.; Frasca, A.; Heiter, U.; Hill, V.; Hourihane, A.; Jofré, P.; Lardo, C.; de Laverny, P.; Lind, K.; Magrini, L.; Marconi, G.; Martayan, C.; Masseron, T.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Sbordone, L.; Sousa, S. G.; Worley, C. C.; Zaggia, S.

    2015-08-01

    Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey at the European Southern Observatory Very Large Telescope. Aims: A key aim is to provide precise radial velocities (RVs) and projected equatorial velocities (vsini) for representative samples of Galactic stars, which will complement information obtained by the Gaia astrometry satellite. Methods: We present an analysis to empirically quantify the size and distribution of uncertainties in RV and vsini using spectra from repeated exposures of the same stars. Results: We show that the uncertainties vary as simple scaling functions of signal-to-noise ratio (S/N) and vsini, that the uncertainties become larger with increasing photospheric temperature, but that the dependence on stellar gravity, metallicity and age is weak. The underlying uncertainty distributions have extended tails that are better represented by Student's t-distributions than by normal distributions. Conclusions: Parametrised results are provided, which enable estimates of the RV precision for almost all GES measurements, and estimates of the vsini precision for stars in young clusters, as a function of S/N, vsini and stellar temperature. The precision of individual high S/N GES RV measurements is 0.22-0.26 km s-1, dependent on instrumental configuration. Based on observations collected with the FLAMES spectrograph at VLT/UT2 telescope (Paranal Observatory, ESO, Chile), for the Gaia- ESO Large Public Survey (188.B-3002).Full Table 2 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/580/A75

  13. VizieR Online Data Catalog: RR Lyrae variables in ESO294-G010 and ESO410-G005 (Yang+, 2014)

    NASA Astrophysics Data System (ADS)

    Yang, S.-C.; Wagner-Kaiser, R.; Sarajedini, A.; Kim, S. C.; Kyeong, J.

    2016-08-01

    The science images of ESO294-G010 and ESO410-G005 used in this study were taken with the Advanced Camera for Surveys Wide Field Channel (ACS/WFC) on board Hubble Space Telescope (HST) as a part of GO-10503 (PI: Da Costa). ESO294-G010 (R.A.=00:26:33.40 (J2000), Decl.=-41:51:19.0 (J2000)) was observed on the HJD (+2453000) range 859.27358-861.13659 with the F606W filter, and on the HJD (+2453000) range 859.40613-861.00342 with the F814W filter. ESO410-G005 (R.A.=00:15:31.40 (J2000), Decl.=-32:10:47.0 (J2000)) was observed on the HJD (+2453000) range 861.40425-863.21702 with the F606W filter, and on the HJD (+2453000) range 861.53711-866.08158 with the filter F814W. The central regions of each galaxy were placed on one of WFC chips so that the imaging covers almost the entire visual extent of the targets. ESO294-G010 was imaged 12 times in the F606W and 24 times in the F814W filter with an exposure time of 1160s during the observing baseline of ~1.86days. The same number of exposures were obtained for the observations of ESO410-G005 with an exposure time of 1120s over the observing baseline of 4.55days. The basic properties of each of these RRL candidates are summarized in Tables 2 and 3. We have also uncovered a significant number of Luminous Variable (LV) candidates in both transition-type dwarf galaxies (22 in ESO294-G010; 19 in ESO410-G005). Their photometric and pulsation properties are summarized in Table4. (4 data files).

  14. ESO-MIDAS: General tools for image processing and data reduction

    NASA Astrophysics Data System (ADS)

    European Southern Observatory

    2013-02-01

    The ESO-MIDAS system provides general tools for image processing and data reduction with emphasis on astronomical applications including imaging and special reduction packages for ESO instrumentation at La Silla and the VLT at Paranal. In addition it contains applications packages for stellar and surface photometry, image sharpening and decomposition, statistics, data fitting, data presentation in graphical form, and more.

  15. Epigenetic potentiation of NY-ESO-1 vaccine therapy in human ovarian cancer.

    PubMed

    Odunsi, Kunle; Matsuzaki, Junko; James, Smitha R; Mhawech-Fauceglia, Paulette; Tsuji, Takemasa; Miller, Austin; Zhang, Wa; Akers, Stacey N; Griffiths, Elizabeth A; Miliotto, Anthony; Beck, Amy; Batt, Carl A; Ritter, Gerd; Lele, Shashikant; Gnjatic, Sacha; Karpf, Adam R

    2014-01-01

    The cancer-testis/cancer-germline antigen NY-ESO-1 is a vaccine target in epithelial ovarian cancer (EOC), but its limited expression is a barrier to vaccine efficacy. As NY-ESO-1 is regulated by DNA methylation, we hypothesized that DNA methyltransferase (DNMT) inhibitors may augment NY-ESO-1 vaccine therapy. In agreement, global DNA hypomethylation in EOC was associated with the presence of circulating antibodies to NY-ESO-1. Pre-clinical studies using EOC cell lines showed that decitabine treatment enhanced both NY-ESO-1 expression and NY-ESO-1-specific CTL-mediated responses. Based on these observations, we performed a phase I dose-escalation trial of decitabine, as an addition to NY-ESO-1 vaccine and doxorubicin liposome (doxorubicin) chemotherapy, in 12 patients with relapsed EOC. The regimen was safe, with limited and clinically manageable toxicities. Both global and promoter-specific DNA hypomethylation occurred in blood and circulating DNAs, the latter of which may reflect tumor cell responses. Increased NY-ESO-1 serum antibodies and T cell responses were observed in the majority of patients, and antibody spreading to additional tumor antigens was also observed. Finally, disease stabilization or partial clinical response occurred in 6/10 evaluable patients. Based on these encouraging results, evaluation of similar combinatorial chemo-immunotherapy regimens in EOC and other tumor types is warranted.

  16. NY-ESO-1-specific immunological pressure and escape in a patient with metastatic melanoma.

    PubMed

    von Boehmer, Lotta; Mattle, Muriel; Bode, Peter; Landshammer, Alexandro; Schäfer, Carolin; Nuber, Natko; Ritter, Gerd; Old, Lloyd; Moch, Holger; Schäfer, Niklaus; Jäger, Elke; Knuth, Alexander; van den Broek, Maries

    2013-01-01

    During cancer progression, malignant cells may evade immunosurveillance. However, evidence for immunological escape in humans is scarce. We report here the clinical course of a melanoma patient whose initial tumor was positive for the antigens NY-ESO-1, MAGE-C1, and Melan-A. Upon immunization with a recombinant vaccinia/fowlpox NY-ESO-1 construct, the patient experienced a mixed clinical response and spreading of the NY-ESO-1 epitopes in the CD4+ T cell compartment. After NY-ESO-1 protein + CpG immunization, the patient's anti-NY-ESO-1 IgG response increased. Over the following years, progressing lesions were resected and found to be NY-ESO-1-negative while being positive for MAGE-C1, Melan-A, and MHC-I. The fatal, inoperable brain metastasis was analyzed after his death and also proved to be NY-ESO-1-negative, while being positive for MAGE-C1 and Melan-A, as well as MHC-I. We propose that cancer control and cancer escape in this patient were governed by NY-ESO-1-specific immunological pressure. Our findings provide evidence for the existence of immunoediting and immunoescape in this cancer patient.

  17. The Gaia-ESO Survey: the Galactic thick to thin disc transition

    NASA Astrophysics Data System (ADS)

    Recio-Blanco, A.; de Laverny, P.; Kordopatis, G.; Helmi, A.; Hill, V.; Gilmore, G.; Wyse, R.; Adibekyan, V.; Randich, S.; Asplund, M.; Feltzing, S.; Jeffries, R.; Micela, G.; Vallenari, A.; Alfaro, E.; Allende Prieto, C.; Bensby, T.; Bragaglia, A.; Flaccomio, E.; Koposov, S. E.; Korn, A.; Lanzafame, A.; Pancino, E.; Smiljanic, R.; Jackson, R.; Lewis, J.; Magrini, L.; Morbidelli, L.; Prisinzano, L.; Sacco, G.; Worley, C. C.; Hourihane, A.; Bergemann, M.; Costado, M. T.; Heiter, U.; Joffre, P.; Lardo, C.; Lind, K.; Maiorca, E.

    2014-07-01

    and, possibly, the azimuthal velocity dispersion decreased. At [M/H] ≈ -0.25 dex and [α/Fe]≈ 0.1 dex, the mean characteristics of the thick disc in vertical distance to the Galactic plane, rotation, rotational dispersion, and stellar orbits' eccentricity agree with that of the thin disc stars of the same metallicity, suggesting a possible connection between these two populations at a certain epoch of the disc evolution. Finally, the results presented here, based only on the first months of the Gaia ESO Survey observations, confirm how crucial large high-resolution spectroscopic surveys outside the solar neighbourhood are today for our understanding of the Milky Way history. Based on observations collected with the FLAMES spectrograph at the VLT/UT2 telescope (Paranal Observatory, ESO, Chile), for the Gaia-ESO Large Public Survey, programme 188.B-3002.Full Table 1 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/567/A5

  18. Antibody responses to NY-ESO-1 in primary breast cancer identify a subtype target for immunotherapy.

    PubMed

    Hamaï, Ahmed; Duperrier-Amouriaux, Karine; Pignon, Pascale; Raimbaud, Isabelle; Memeo, Lorenzo; Colarossi, Cristina; Canzonieri, Vincenzo; Perin, Tiziana; Classe, Jean-Marc; Campone, Mario; Jézéquel, Pascal; Campion, Loïc; Ayyoub, Maha; Valmori, Danila

    2011-01-01

    The highly immunogenic human tumor antigen NY-ESO-1 (ESO) is a target of choice for anti-cancer immune therapy. In this study, we assessed spontaneous antibody (Ab) responses to ESO in a large cohort of patients with primary breast cancer (BC) and addressed the correlation between the presence of anti-ESO Ab, the expression of ESO in the tumors and their characteristics. We found detectable Ab responses to ESO in 1% of the patients. Tumors from patients with circulating Ab to ESO exhibited common characteristics, being mainly hormone receptor (HR)⁻ invasive ductal carcinomas of high grade, including both HER2⁻ and HER2⁺ tumors. In line with these results, we detected ESO expression in 20% of primary HR⁻ BC, including both ESO Ab⁺ and Ab⁻ patients, but not in HR⁺ BC. Interestingly, whereas expression levels in ESO⁺ BC were not significantly different between ESO Ab⁺ and Ab⁻ patients, the former had, in average, significantly higher numbers of tumor-infiltrated lymph nodes, indicating that lymph node invasion may be required for the development of spontaneous anti-tumor immune responses. Thus, the presence of ESO Ab identifies a tumor subtype of HR⁻ (HER2⁻ or HER2⁺) primary BC with frequent ESO expression and, together with the assessment of antigen expression in the tumor, may be instrumental for the selection of patients for whom ESO-based immunotherapy may complement standard therapy.

  19. New Method for Data Treatment Developed at ESO

    NASA Astrophysics Data System (ADS)

    1996-08-01

    How Future Astronomical Observations Will be Done The past four centuries have seen dramatic improvements in astronomical equipment, in terms of better and larger telescopes, more accurate and sensitive detectors and, not the least, by advanced space instruments with access to new spectral regions. However, until recently there has been little progress on another equally important front, that of quantifying the unavoidable influence of this equipment on the astronomical data they produce . For a long time, astronomers have desired to remove efficiently these `instrumental effects' from their data, in order to give them a clearer understanding of the objects in the Universe and their properties. But it is only now that this fundamental problem can finally be tackled efficiently, with the advent of digital imaging techniques and powerful computers. Two researchers at the ESO Headquarters, Michael R. Rosa of the Space Telescope European Co-ordinating Facility (ST/ECF [1]) and Pascal Ballester of the Data Management Division (DMD) are now developing a new approach to this age-old problem. These results are important for the future use of the ESO Very Large Telescope (VLT) , the Hubble Space Telescope (HST) and other large facilities as well [2]. The observational process Observations are crucial to the progress of all natural sciences, including astronomy. Nevertheless, the properties of the observed objects are rarely revealed directly. First, observational data are gathered at the telescopes with instruments such as cameras and spectrophotometers. Then these `raw' data are processed with advanced computer programmes to produce scientifically meaningful data which are finally scrutinized by the astronomers in order to learn more about the observed celestial objects. A basic problem in this chain is the influence of the telescopes and instruments on the data they produce. The `raw' observational data carries the marks, not only of the celestial objects that are

  20. ESO089-G018 and ESO089-G019: long-slit spectroscopy of emission-line galaxies

    NASA Astrophysics Data System (ADS)

    da Rocha-Poppe, P. C.; Faúndez-Abans, M.; Fernandes-Martin, V. A.; Fernandes, I. F.; de Oliveira-Abans, M.; Rodrígues-Ardila, A.

    2010-03-01

    We present the first spectroscopic observations for the galaxies ESO089-G018 (hereafter G18, an Sb(?)-type galaxy seen nearly edge-on) and ESO089-G019 (hereafter G19, an SA(s): a peculiar galaxy), extracted from the sample of ring-shaped galaxies compiled in Faúndez-Abans & de Oliveira-Abans. The main goal of this work is to investigate the spectral classification using the three line-ratio diagrams, called diagnostic diagrams, of Veilleux & Osterbrock. However, in order to separate the different types of galaxies [HII galaxies, Seyfert 2 galaxies and low-ionization nuclear emission-line region galaxies (LINERs)] we have to used empirical boundaries between them. Based on the observed spectra, we suggest G18 is a `weak-[OI] LINER' or even a `transition object' or LINER/HII. In the case of G19, we see Hβ in absorption and no [OIII] lines, impeding the [OIII]/Hβ ratio to be estimated. However, other lines ratios have been evaluated for the discussion. We classify the nature of G19 as ambiguous, because of the difficulty in determining its ionizing source (narrow-line active galactic nuclei or HII galaxies) in different diagnostic diagrams. The errors in the fluxes were mostly caused by uncertainties in the placement of the continuum level. We have estimated nuclear redshift of z = 0.034 (G18) and z = 0.039 (G19), corresponding to a heliocentric velocity of 10246 and 11734kms-1, respectively. Some other physical parameters have been derived whenever possible. All spectra were reduced and analysed in a homogeneous way with the standard IRAF procedures. Based on observations carried out at Observatório do Pico dos Dias (OPD), which operated by the LNA/MCT, Brazil-MG. E-mail: paulopoppe@gmail.com

  1. NY-ESO-1 expression in hepatocellular carcinoma: A potential new marker for early recurrence after surgery.

    PubMed

    Xu, Heng; Gu, Na; Liu, Zhao-Bo; Zheng, Min; Xiong, Fang; Wang, Si-Ying; Li, Ning; Lu, Jun

    2012-01-01

    NY-ESO-1 belongs to the cancer testis antigens (CTA) family, and is identified in a variety of tumors. Certain studies have demonstrated that NY-ESO-1 predicts tumor recurrence and treatment response. No reports are currently available regarding the correlation between NY-ESO-1 and the recurrence of hepatocellular carcinoma (HCC) following surgery. The purpose of the present study was to evaluate the association between NY-ESO-1 and relapse of HCC and to explore the possible mechanisms for this correlation. A total of 120 HCC patients were analyzed for the expression of NY-ESO-1 by immunohistochemistry (IHC). A stable NY-ESO-1 over-expressed HepG2 cell line (ESO-HepG2) was established to determine the biological effects of NY-ESO-1 on cell proliferation, cell cycle and migration by using the xCELLigence DP system, flow cytometry and xCELLigence SP system. NY-ESO-1 was positive in 28 of 120 (23.3%) HCC tumor tissues. NY-ESO-1 was not detectable in adjacent normal liver tissues. A close correlation was found between NY-ESO-1 expression and the recurrence of HCC following surgery (P=0.007). Kaplan-Meier analysis showed a shorter recurrence-free survival (RFS) for patients positive for NY-ESO-1 (log-rank test, P=0.003). The Cox regression model demonstrated that NY-ESO-1 expression was a significant independent predictor for the recurrence of HCC following curative surgery (P=0.022). Compared with HepG2 cells, ESO-HepG2 cells have increased migration but not proliferation ability. In conclusion, NY-ESO-1 expression is associated with worse HCC outcome following surgery, and the mechanism for this finding may be that NY-ESO-1 increases tumor cell migration.

  2. The Gaia-ESO Survey: Inhibited extra mixing in two giants of the open cluster Trumpler 20?

    NASA Astrophysics Data System (ADS)

    Smiljanic, R.; Franciosini, E.; Randich, S.; Magrini, L.; Bragaglia, A.; Pasquini, L.; Vallenari, A.; Tautvaišienė, G.; Biazzo, K.; Frasca, A.; Donati, P.; Delgado Mena, E.; Casey, A. R.; Geisler, D.; Villanova, S.; Tang, B.; Sousa, S. G.; Gilmore, G.; Bensby, T.; François, P.; Koposov, S. E.; Lanzafame, A. C.; Pancino, E.; Recio-Blanco, A.; Costado, M. T.; Hourihane, A.; Lardo, C.; de Laverny, P.; Lewis, J.; Monaco, L.; Morbidelli, L.; Sacco, G. G.; Worley, C. C.; Zaggia, S.; Martell, S.

    2016-06-01

    Aims: We report the discovery of two Li-rich giants, with A(Li) ~ 1.50, in an analysis of a sample of 40 giants of the open cluster Trumpler 20 (with turnoff mass ~1.8 M⊙). The cluster was observed in the context of the Gaia-ESO Survey. Methods: The atmospheric parameters and Li abundances were derived using high-resolution UVES spectra. The Li abundances were corrected for nonlocal thermodynamical equilibrium (non-LTE) effects. Results: Only upper limits of the Li abundance could be determined for the majority of the sample. Two giants with detected Li turned out to be Li rich: star MG 340 has A(Li)non-LTE = 1.54 ± 0.21 dex and star MG 591 has A(Li)non-LTE = 1.60 ± 0.21 dex. Star MG 340 is on average ~0.30 dex more rich in Li than stars of similar temperature, while for star MG 591 this difference is on average ~0.80 dex. Carbon and nitrogen abundances indicate that all stars in the sample have completed the first dredge-up. Conclusions: The Li abundances in this unique sample of 40 giants in one open cluster clearly show that extra mixing is the norm in this mass range. Giants with Li abundances in agreement with the predictions of standard models are the exception. To explain the two Li-rich giants, we suggest that all events of extra mixing have been inhibited. This includes rotation-induced mixing during the main sequence and the extra mixing at the red giant branch luminosity bump. Such inhibition has been suggested in the literature to occur because of fossil magnetic fields in red giants that are descendants of main-sequence Ap-type stars. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey).

  3. The Gaia-ESO Survey: the first abundance determination of the pre-main-sequence cluster gamma Velorum

    NASA Astrophysics Data System (ADS)

    Spina, L.; Randich, S.; Palla, F.; Sacco, G. G.; Magrini, L.; Franciosini, E.; Morbidelli, L.; Prisinzano, L.; Alfaro, E. J.; Biazzo, K.; Frasca, A.; González Hernández, J. I.; Sousa, S. G.; Adibekyan, V.; Delgado-Mena, E.; Montes, D.; Tabernero, H.; Klutsch, A.; Gilmore, G.; Feltzing, S.; Jeffries, R. D.; Micela, G.; Vallenari, A.; Bensby, T.; Bragaglia, A.; Flaccomio, E.; Koposov, S.; Lanzafame, A. C.; Pancino, E.; Recio-Blanco, A.; Smiljanic, R.; Costado, M. T.; Damiani, F.; Hill, V.; Hourihane, A.; Jofré, P.; de Laverny, P.; Masseron, T.; Worley, C.

    2014-07-01

    Context. Knowledge of the abundance distribution of star forming regions and young clusters is critical to investigate a variety of issues, from triggered star formation and chemical enrichment by nearby supernova explosions to the ability to form planetary systems. In spite of this, detailed abundance studies are currently available for relatively few regions. Aims: In this context, we present the analysis of the metallicity of the gamma Velorum cluster, based on the products distributed in the first internal release of the Gaia-ESO Survey. Methods: The gamma Velorum candidate members have been observed with FLAMES, using both UVES and Giraffe, depending on the target brightness and spectral type. In order to derive a solid metallicity determination for the cluster, membership of the observed stars must be first assessed. To this aim, we use several membership criteria including radial velocities, surface gravity estimates, and the detection of the photospheric lithium line. Results: Out of the 80 targets observed with UVES, we identify 14 high-probability members. We find that the metallicity of the cluster is slightly subsolar, with a mean [ Fe/H ] = -0.057 ± 0.018 dex. Although J08095427-4721419 is one of the high-probability members, its metallicity is significantly larger than the cluster average. We speculate about its origin as the result of recent accretion episodes of rocky bodies of ~60 M⊕ hydrogen-depleted material from the circumstellar disk. Based on observations collected at the ESO telescopes under programme 188.B3002, the Gaia-ESO large public spectroscopic survey.Full Tables 1-4 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/567/A55

  4. T cells targeting NY-ESO-1 demonstrate efficacy against disseminated neuroblastoma

    PubMed Central

    Singh, Nathan; Kulikovskaya, Irina; Barrett, David M.; Binder-Scholl, Gwendolyn; Jakobsen, Bent; Martinez, Daniel; Pawel, Bruce; June, Carl H.; Kalos, Michael D.; Grupp, Stephan A.

    2016-01-01

    abstract The cancer-testis antigen NY-ESO-1 is expressed by many solid tumors and has limited expression by mature somatic tissues, making it a highly attractive target for tumor immunotherapy. Targeting NY-ESO-1 using engineered T cells has demonstrated clinical efficacy in the treatment of some adult tumors. Neuroblastoma is a significant cause of cancer mortality in children, and is a tumor type shown to be responsive to immunotherapies. We evaluated a large panel of primarily resected neuroblastoma samples and demonstrated that 23% express NY-ESO-1. After confirming antigen-specific activity of T cells genetically engineered to express an NY-ESO-1 directed high-affinity transgenic T cell receptor in vitro, we performed xenograft mouse studies assessing the efficacy of NY-ESO-1-targeted T cells in both localized and disseminated models of neuroblastoma. Disease responses were monitored by tumor volume measurement and in vivo bioluminescence. After delivery of NY-ESO-1 transgenic TCR T cells, we observed significant delay of tumor progression in mice bearing localized and disseminated neuroblastoma, as well as enhanced animal survival. These data demonstrate that NY-ESO-1 is an antigen target in neuroblastoma and that targeted T cells represent a potential therapeutic option for patients with neuroblastoma. PMID:26942053

  5. Expression of MAGE-A and NY-ESO-1 in Primary and Metastatic Cancers.

    PubMed

    Park, Tristen S; Groh, Eric M; Patel, Krishna; Kerkar, Sid P; Lee, Chyi-Chia Richard; Rosenberg, Steven A

    2016-01-01

    Melanoma-associated antigen-A (MAGE-A) and New York esophageal squamous cell cancer-1 (NY-ESO-1) are 2 cancer testis antigens (CTA) demonstrating potential for use in targeted immunotherapy. Clinical trials in melanoma and synovial sarcomas targeting these antigens in immune-based therapies have demonstrated durable tumor regression. Although protein expression of NY-ESO-1 has been assessed in a variety of cancer types, the expression of MAGE-A has not been studied in depth. In this study we analyzed MAGE-A and NY-ESO-1 expression in 314 melanoma specimens from 301 melanoma patients, 38 patients with squamous cell cancers and 111 patients with adenocarcinomas. Our results demonstrated higher expression of MAGE-A compared with NY-ESO-1 in melanomas (32% vs. 13%) and squamous cell carcinomas (45% vs. 7.9%), and higher expression of both CTAs in metastatic versus primary tumors. CTA expression in adenocarcinomas was low (MAGE-A: 10%, NY-ESO-1: 0.9%). In addition, we looked at concordance of expression among metastatic melanoma lesions within the same patient and found concordant expression in 38 of 47 patients for MAGE-A and 43 of 47 patients for NY-ESO-1. Our study demonstrated that the MAGE-A family may be of greater utility than NY-ESO-1 for targeted immunotherapy in a variety of cancer histologies, in particular metastatic melanomas and squamous cell carcinomas.

  6. The Gaia-ESO Survey: Catalogue of Hα emission stars

    NASA Astrophysics Data System (ADS)

    Traven, G.; Zwitter, T.; Van Eck, S.; Klutsch, A.; Bonito, R.; Lanzafame, A. C.; Alfaro, E. J.; Bayo, A.; Bragaglia, A.; Costado, M. T.; Damiani, F.; Flaccomio, E.; Frasca, A.; Hourihane, A.; Jimenez-Esteban, F.; Lardo, C.; Morbidelli, L.; Pancino, E.; Prisinzano, L.; Sacco, G. G.; Worley, C. C.

    2015-09-01

    We discuss the properties of Hα emission stars across the sample of 22035 spectra from the Gaia-ESO Survey internal data release, observed with the GIRAFFE instrument and largely belonging to stars in young open clusters. Automated fits using two independent Gaussian profiles and a third component that accounts for the nebular emission allow us to discern distinct morphological types of Hα line profiles with the introduction of a simplified classification scheme. All in all, we find 3765 stars with intrinsic emission and sort their spectra into eight distinct morphological categories: single-component emission, emission blend, sharp emission peaks, double emission, P-Cygni, inverted P-Cygni, self-absorption, and emission in absorption. We have more than one observation for 1430 stars in our sample, thus allowing a quantitative discussion of the degree of variability of Hα emission profiles, which is expected for young, active objects. We present a catalogue of stars with properties of their Hα emission line profiles, morphological classification, analysis of variability with time and the supplementary information from the SIMBAD, VizieR, and ADS databases. The records in SIMBAD indicate the presence of Hα emission for roughly 25% of all stars in our catalogue, while at least 305 of them have already been more thoroughly investigated according to the references in ADS. The most frequently identified morphological categories in our sample of spectra are emission blend (23%), emission in absorption (22%), and self-absorption (16%). Objects with repeated observations demonstrate that our classification into discrete categories is generally stable through time, but categories P-Cygni and self-absorption seem less stable, which is the consequence of discrete classification rules, as well as of the fundamental change in profile shape. Such records of emission stars can be valuable for automatic pipelines in large surveys, where it may prove very useful for

  7. A novel human-derived antibody against NY-ESO-1 improves the efficacy of chemotherapy.

    PubMed

    Gupta, Anurag; Nuber, Natko; Esslinger, Christoph; Wittenbrink, Mareike; Treder, Martin; Landshammer, Alexandro; Noguchi, Takuro; Kelly, Marcus; Gnjatic, Sacha; Ritter, Erika; von Boehmer, Lotta; Nishikawa, Hiroyoshi; Shiku, Hiroshi; Old, Lloyd; Ritter, Gerd; Knuth, Alexander; van den Broek, Maries

    2013-01-01

    We investigated whether antibodies against intracellular tumor-associated antigens support tumor-specific immunity when administered together with a treatment that destroys the tumor. We propose that released antigens form immune complexes with the antibodies, which are then efficiently taken up by dendritic cells. We cloned the first human monoclonal antibodies against the Cancer/Testis (CT) antigen, NY-ESO-1. We tested whether the monoclonal anti-NY-ESO-1 antibody (12D7) facilitates cross-presentation of a NY-ESO-1-derived epitope by dendritic cells to human CD8+ T cells, and whether this results in the maturation of dendritic cells in vitro. We investigated the efficacy of 12D7 in combination with chemotherapy using BALB/c mice bearing syngeneic CT26 tumors that express intracellular NY-ESO-1. Human dendritic cells that were incubated with NY-ESO-1:12D7 immune complexes efficiently stimulated NY-ESO-1(157-165)/HLA-A2-specific human CD8+ T cells to produce interferon-γ, whereas NY-ESO-1 alone did not. Furthermore, the incubation of dendritic cells with NY-ESO-1:12D7 immune complexes resulted in the maturation of dendritic cells. Treatment of BALB/c mice that bear CT26/NY-ESO-1 tumors with 5-fluorouracil (5-FU) plus 12D7 was significantly more effective than chemotherapy alone. We propose systemic injection of monoclonal antibodies (mAbs) against tumor-associated antigens plus a treatment that promotes the local release of those antigens resulting in immune complex formation as a novel therapeutic modality for cancer. PMID:23390374

  8. A novel human-derived antibody against NY-ESO-1 improves the efficacy of chemotherapy

    PubMed Central

    Gupta, Anurag; Nuber, Natko; Esslinger, Christoph; Wittenbrink, Mareike; Treder, Martin; Landshammer, Alexandro; Noguchi, Takuro; Kelly, Marcus; Gnjatic, Sacha; Ritter, Erika; von Boehmer, Lotta; Nishikawa, Hiroyoshi; Shiku, Hiroshi; Old, Lloyd; Ritter, Gerd; Knuth, Alexander; van den Broek, Maries

    2013-01-01

    We investigated whether antibodies against intracellular tumor-associated antigens support tumor-specific immunity when administered together with a treatment that destroys the tumor. We propose that released antigens form immune complexes with the antibodies, which are then efficiently taken up by dendritic cells. We cloned the first human monoclonal antibodies against the Cancer/Testis (CT) antigen, NY-ESO-1. We tested whether the monoclonal anti-NY-ESO-1 antibody (12D7) facilitates cross-presentation of a NY-ESO-1-derived epitope by dendritic cells to human CD8+ T cells, and whether this results in the maturation of dendritic cells in vitro. We investigated the efficacy of 12D7 in combination with chemotherapy using BALB/c mice bearing syngeneic CT26 tumors that express intracellular NY-ESO-1. Human dendritic cells that were incubated with NY-ESO-1:12D7 immune complexes efficiently stimulated NY-ESO-1157–165/HLA-A2-specific human CD8+ T cells to produce interferon-γ, whereas NY-ESO-1 alone did not. Furthermore, the incubation of dendritic cells with NY-ESO-1:12D7 immune complexes resulted in the maturation of dendritic cells. Treatment of BALB/c mice that bear CT26/NY-ESO-1 tumors with 5-fluorouracil (5-FU) plus 12D7 was significantly more effective than chemotherapy alone. We propose systemic injection of monoclonal antibodies (mAbs) against tumor-associated antigens plus a treatment that promotes the local release of those antigens resulting in immune complex formation as a novel therapeutic modality for cancer. PMID:23390374

  9. A novel human-derived antibody against NY-ESO-1 improves the efficacy of chemotherapy.

    PubMed

    Gupta, Anurag; Nuber, Natko; Esslinger, Christoph; Wittenbrink, Mareike; Treder, Martin; Landshammer, Alexandro; Noguchi, Takuro; Kelly, Marcus; Gnjatic, Sacha; Ritter, Erika; von Boehmer, Lotta; Nishikawa, Hiroyoshi; Shiku, Hiroshi; Old, Lloyd; Ritter, Gerd; Knuth, Alexander; van den Broek, Maries

    2013-01-01

    We investigated whether antibodies against intracellular tumor-associated antigens support tumor-specific immunity when administered together with a treatment that destroys the tumor. We propose that released antigens form immune complexes with the antibodies, which are then efficiently taken up by dendritic cells. We cloned the first human monoclonal antibodies against the Cancer/Testis (CT) antigen, NY-ESO-1. We tested whether the monoclonal anti-NY-ESO-1 antibody (12D7) facilitates cross-presentation of a NY-ESO-1-derived epitope by dendritic cells to human CD8+ T cells, and whether this results in the maturation of dendritic cells in vitro. We investigated the efficacy of 12D7 in combination with chemotherapy using BALB/c mice bearing syngeneic CT26 tumors that express intracellular NY-ESO-1. Human dendritic cells that were incubated with NY-ESO-1:12D7 immune complexes efficiently stimulated NY-ESO-1(157-165)/HLA-A2-specific human CD8+ T cells to produce interferon-γ, whereas NY-ESO-1 alone did not. Furthermore, the incubation of dendritic cells with NY-ESO-1:12D7 immune complexes resulted in the maturation of dendritic cells. Treatment of BALB/c mice that bear CT26/NY-ESO-1 tumors with 5-fluorouracil (5-FU) plus 12D7 was significantly more effective than chemotherapy alone. We propose systemic injection of monoclonal antibodies (mAbs) against tumor-associated antigens plus a treatment that promotes the local release of those antigens resulting in immune complex formation as a novel therapeutic modality for cancer.

  10. Mechanical thrombectomy in acute ischemic stroke: Consensus statement by ESO-Karolinska Stroke Update 2014/2015, supported by ESO, ESMINT, ESNR and EAN.

    PubMed

    Wahlgren, Nils; Moreira, Tiago; Michel, Patrik; Steiner, Thorsten; Jansen, Olav; Cognard, Christophe; Mattle, Heinrich P; van Zwam, Wim; Holmin, Staffan; Tatlisumak, Turgut; Petersson, Jesper; Caso, Valeria; Hacke, Werner; Mazighi, Mikael; Arnold, Marcel; Fischer, Urs; Szikora, Istvan; Pierot, Laurent; Fiehler, Jens; Gralla, Jan; Fazekas, Franz; Lees, Kennedy R

    2016-01-01

    The original version of this consensus statement on mechanical thrombectomy was approved at the European Stroke Organisation (ESO)-Karolinska Stroke Update conference in Stockholm, 16-18 November 2014. The statement has later, during 2015, been updated with new clinical trials data in accordance with a decision made at the conference. Revisions have been made at a face-to-face meeting during the ESO Winter School in Berne in February, through email exchanges and the final version has then been approved by each society. The recommendations are identical to the original version with evidence level upgraded by 20 February 2015 and confirmed by 15 May 2015. The purpose of the ESO-Karolinska Stroke Update meetings is to provide updates on recent stroke therapy research and to discuss how the results may be implemented into clinical routine. Selected topics are discussed at consensus sessions, for which a consensus statement is prepared and discussed by the participants at the meeting. The statements are advisory to the ESO guidelines committee. This consensus statement includes recommendations on mechanical thrombectomy after acute stroke. The statement is supported by ESO, European Society of Minimally Invasive Neurological Therapy (ESMINT), European Society of Neuroradiology (ESNR), and European Academy of Neurology (EAN).

  11. The Gaia-ESO Survey: New constraints on the Galactic disc velocity dispersion and its chemical dependencies

    NASA Astrophysics Data System (ADS)

    Guiglion, G.; Recio-Blanco, A.; de Laverny, P.; Kordopatis, G.; Hill, V.; Mikolaitis, Š.; Minchev, I.; Chiappini, C.; Wyse, R. F. G.; Gilmore, G.; Randich, S.; Feltzing, S.; Bensby, T.; Flaccomio, E.; Koposov, S. E.; Pancino, E.; Bayo, A.; Costado, M. T.; Franciosini, E.; Hourihane, A.; Jofré, P.; Lardo, C.; Lewis, J.; Lind, K.; Magrini, L.; Morbidelli, L.; Sacco, G. G.; Ruchti, G.; Worley, C. C.; Zaggia, S.

    2015-11-01

    interval and a larger spatial volume. Conclusions: Thanks to the Gaia-ESO Survey data, we confirm the existence of [Mg/Fe]-rich thick-disc stars with cool kinematics in the generally turbulent context of the primitive Galactic disc. This is discussed in the framework of the different disc formation and evolution scenarios. Based on observations collected with the FLAMES spectrograph at the VLT/UT2 telescope (Paranal Observatory, ESO, Chile), for the Gaia-ESO Large Public Survey, programme 188.B-3002

  12. Report on the ESO/IAG/USP Workshop ''Circumstellar Dynamics at High Resolution''

    NASA Astrophysics Data System (ADS)

    Rivinius, T.; Carciofi, A.; Baade, D.

    2012-06-01

    The workshop was jointly sponsored by ESO, the Brazilian National and São Paulo state agencies CAPES and FAPESP, and the University of São Paulo. Nearly 70 participants gathered to discuss the immediate surroundings of stars, mostly those more massive and hotter than the Sun. The venue, near the spectacular Iguaçu waterfalls, and topic proved to be well chosen to attract a balanced crowd: about one third of the participants came from each of Brazil, other ESO member states and Chile, and ESO non-member states.

  13. Gender Systematics in Telescope Time Allocation at ESO

    NASA Astrophysics Data System (ADS)

    Patat, F.

    2016-09-01

    The results of a comprehensive statistical analysis of gender systematics in the time allocation process at ESO are presented. The sample on which the study is based includes more than 13 000 Normal and Short proposals, submitted by about 3000 principal investigators (PI) over eight years. The genders of PIs, and of the panel members of the Observing Programmes Committee (OPC), were used, together with their career level, to analyse the grade distributions and the proposal success rates. Proposals submitted by female PIs show a significantly lower probability of being allocated time. The proposal success rates (defined as number of top ranked runs over requested runs) are 16.0 ± 0.6% and 22.0 ± 0.4% for females and males, respectively. To a significant extent the disparity is related to different input distributions in terms of career level. The seniority of male PIs is significantly higher than that of female PIs, with only 34% of the female PIs being professionally employed astronomers (compared to 53% for male PIs). A small, but statistically significant, gender-dependent behaviour is measured for the OPC referees: both genders show the same systematics, but they are larger for males than females. The PI female/male fraction is very close to 30/70; although far from parity, the fraction is higher than that observed, for instance, among IAU membership.

  14. ESO Receives Computerworld Honors Program 21st Century Achievement Award in Science Category

    NASA Astrophysics Data System (ADS)

    2005-06-01

    In a ceremony held in Washington, D.C. (USA) on June 6, 2005, ESO, the European Organisation for Astronomical Research in the southern Hemisphere, received the coveted 21st Century Achievement Award from the Computerworld Honors Program for its visionary use of information technology in the Science category. Sybase, a main database server vendor and member of the Chairmen's Committee, nominated ESO's Data Flow System in recognition of its contributions to the global information technology revolution and its positive impact on society. The citations reads: "ESO has revolutionized the operations of ground-based astronomical observatories with a new end-to-end data flow system, designed to improve the transmission and management of astronomical observations and data over transcontinental distances." This year's awards, in 10 categories, were presented at a gala event at the National Building Museum, attended by over 250 guests, including leaders of the information technology industry, former award recipients, judges, scholars, and diplomats representing many of the 54 countries from which the 17-year-old program's laureates have come. "The Computerworld Honors Program 21st Century Achievement Awards are presented to companies from around the world whose visionary use of information technology promotes positive social, economic and educational change," said Bob Carrigan, president and CEO of Computerworld and chairman of the Chairmen's Committee of the Computerworld Honors Program. "The recipients of these awards are the true heroes of the information age and have been appropriately recognized by the leading IT industry chairmen as true revolutionaries in their fields." ESO PR Photo 18/05 ESO PR Photo 18/05 ESO Receives the Award in the Science Category [Preview - JPEG: 400 x 496 pix - 53k] [Normal - JPEG: 800 x 992 pix - 470k] [Full Res - JPEG: 1250 x 1550 pix - 1.1M] Caption: ESO PR Photo 18/05: Receiving the Computerworld 21st Century Achievement Award for Science

  15. The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

    NASA Astrophysics Data System (ADS)

    Smiljanic, R.; Korn, A. J.; Bergemann, M.; Frasca, A.; Magrini, L.; Masseron, T.; Pancino, E.; Ruchti, G.; San Roman, I.; Sbordone, L.; Sousa, S. G.; Tabernero, H.; Tautvaišienė, G.; Valentini, M.; Weber, M.; Worley, C. C.; Adibekyan, V. Zh.; Allende Prieto, C.; Barisevičius, G.; Biazzo, K.; Blanco-Cuaresma, S.; Bonifacio, P.; Bragaglia, A.; Caffau, E.; Cantat-Gaudin, T.; Chorniy, Y.; de Laverny, P.; Delgado-Mena, E.; Donati, P.; Duffau, S.; Franciosini, E.; Friel, E.; Geisler, D.; González Hernández, J. I.; Gruyters, P.; Guiglion, G.; Hansen, C. J.; Heiter, U.; Hill, V.; Jacobson, H. R.; Jofre, P.; Jönsson, H.; Lanzafame, A. C.; Lardo, C.; Ludwig, H.-G.; Maiorca, E.; Mikolaitis, Š.; Montes, D.; Morel, T.; Mucciarelli, A.; Muñoz, C.; Nordlander, T.; Pasquini, L.; Puzeras, E.; Recio-Blanco, A.; Ryde, N.; Sacco, G.; Santos, N. C.; Serenelli, A. M.; Sordo, R.; Soubiran, C.; Spina, L.; Steffen, M.; Vallenari, A.; Van Eck, S.; Villanova, S.; Gilmore, G.; Randich, S.; Asplund, M.; Binney, J.; Drew, J.; Feltzing, S.; Ferguson, A.; Jeffries, R.; Micela, G.; Negueruela, I.; Prusti, T.; Rix, H.-W.; Alfaro, E.; Babusiaux, C.; Bensby, T.; Blomme, R.; Flaccomio, E.; François, P.; Irwin, M.; Koposov, S.; Walton, N.; Bayo, A.; Carraro, G.; Costado, M. T.; Damiani, F.; Edvardsson, B.; Hourihane, A.; Jackson, R.; Lewis, J.; Lind, K.; Marconi, G.; Martayan, C.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Zaggia, S.

    2014-10-01

    Context. The ongoing Gaia-ESO Public Spectroscopic Survey is using FLAMES at the VLT to obtain high-quality medium-resolution Giraffe spectra for about 105 stars and high-resolution UVES spectra for about 5000 stars. With UVES, the Survey has already observed 1447 FGK-type stars. Aims: These UVES spectra are analyzed in parallel by several state-of-the-art methodologies. Our aim is to present how these analyses were implemented, to discuss their results, and to describe how a final recommended parameter scale is defined. We also discuss the precision (method-to-method dispersion) and accuracy (biases with respect to the reference values) of the final parameters. These results are part of the Gaia-ESO second internal release and will be part of its first public release of advanced data products. Methods: The final parameter scale is tied to the scale defined by the Gaia benchmark stars, a set of stars with fundamental atmospheric parameters. In addition, a set of open and globular clusters is used to evaluate the physical soundness of the results. Each of the implemented methodologies is judged against the benchmark stars to define weights in three different regions of the parameter space. The final recommended results are the weighted medians of those from the individual methods. Results: The recommended results successfully reproduce the atmospheric parameters of the benchmark stars and the expected Teff-log g relation of the calibrating clusters. Atmospheric parameters and abundances have been determined for 1301 FGK-type stars observed with UVES. The median of the method-to-method dispersion of the atmospheric parameters is 55 K for Teff, 0.13 dex for log g and 0.07 dex for [Fe/H]. Systematic biases are estimated to be between 50-100 K for Teff, 0.10-0.25 dex for log g and 0.05-0.10 dex for [Fe/H]. Abundances for 24 elements were derived: C, N, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Mo, Ba, Nd, and Eu. The typical method

  16. An interferometric study of the post-AGB binary 89 Herculis. I. Spatially resolving the continuum circumstellar environment at optical and near-IR wavelengths with the VLTI, NPOI, IOTA, PTI, and the CHARA Array

    NASA Astrophysics Data System (ADS)

    Hillen, M.; Verhoelst, T.; Van Winckel, H.; Chesneau, O.; Hummel, C. A.; Monnier, J. D.; Farrington, C.; Tycner, C.; Mourard, D.; ten Brummelaar, T.; Banerjee, D. P. K.; Zavala, R. T.

    2013-11-01

    identification of the source of emission/scattering remains inconclusive without further study on this and similar objects, the implications are manifold. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 079.D-0013 and 089.D-0576.Figures 2, 4, 6, 7, 9, 10, and Table 5 are available in electronic form at http://www.aanda.orgFITS files of the calibrated visibilities are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/559/A111

  17. VizieR Online Data Catalog: Velocity precision in the Gaia-ESO Survey (Jackson+, 2015)

    NASA Astrophysics Data System (ADS)

    Jackson, R. J.; Jeffries, R. D.; Lewis, J.; Koposov, S. E.; Sacco, G. G.; Randich, S.; Gilmore, G.; Asplund, M.; Binney, J.; Bonifacio, P.; Drew, J. E.; Feltzing, S.; Ferguson, A. M. N.; Micela, G.; Neguerela, I.; Prusti, T.; Rix, H.-W.; Vallenari, A.; Alfaro, E. J.; Allende Prieto, C.; Babusiaux, C.; Bensby, T.; Blomme, R.; Bragaglia, A.; Flaccomio, E.; Francois, P.; Hambly, N.; Irwin, M.; Korn, A. J.; Lanzafame, A. C.; Pancino, E.; Recio-Blanco, A.; Smiljanic, R.; Van Eck, S.; Walton, N.; Bayo, A.; Bergemann, M.; Carraro, G.; Costado, M. T.; Damiani, F.; Edvardsson, B.; Franciosini, E.; Frasca, A.; Heiter, U.; Hill, V.; Hourihane, A.; Jof, P.; Lardo, C.; de Laverny, P.; Lind, K.; Magrini, L.; Marconi, G.; Martayan, C.; Masseron, T.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Sbordone, L.; Sousa, S. G.; Worley, C. C.; Zaggia, S.

    2015-07-01

    The Gaia-ESO Survey (GES) is a large public spectroscopic survey at the European Southern Observatory Very LargeTelescope. A key aim is to provide precise radial velocities (RVs) and projected equatorial velocities (vsini) for representative samples of Galactic stars, which will complement information obtained by the Gaia astrometry satellite. We present an analysis to empirically quantify the size and distribution of uncertainties in RV and vsini using spectra from repeated exposures of the same stars. We show that the uncertainties vary as simple scaling functions of signal-to-noise ratio (S/N) and vsini, that the uncertainties become larger with increasing photospheric temperature, but that the dependence on stellar gravity, metallicity and age is weak. The underlying uncertainty distributions have extended tails that are better represented by Students t-distributions than by normal distributions. Parametrised results are provided, which enable estimates of the RV precision for almost all GES measurements, and estimates of the vsini precision for stars in young clusters, as a function of S/N, vsini and stellar temperature. The precision of individual high S/N GES RV measurements is 0.22-0.26km/s, dependent on instrumental configuration. (1 data file).

  18. The Gaia-ESO Survey: Dynamical analysis of the L1688 region in Ophiuchus

    NASA Astrophysics Data System (ADS)

    Rigliaco, E.; Wilking, B.; Meyer, M. R.; Jeffries, R. D.; Cottaar, M.; Frasca, A.; Wright, N. J.; Bayo, A.; Bonito, R.; Damiani, F.; Jackson, R. J.; Jiménez-Esteban, F.; Kalari, V. M.; Klutsch, A.; Lanzafame, A. C.; Sacco, G.; Gilmore, G.; Randich, S.; Alfaro, E. J.; Bragaglia, A.; Costado, M. T.; Franciosini, E.; Lardo, C.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Sousa, S. G.; Zaggia, S.

    2016-04-01

    The Gaia ESO Public Spectroscopic Survey (GES) is providing the astronomical community with high-precision measurements of many stellar parameters including radial velocities (RVs) of stars belonging to several young clusters and star-forming regions. One of the main goals of the young cluster observations is to study their dynamical evolution and provide insight into their future, revealing whether they will eventually disperse to populate the field rather than evolve into bound open clusters. In this paper we report the analysis of the dynamical state of L1688 in the ρ Ophiuchi molecular cloud using the dataset provided by the GES consortium. We performed the membership selection of the more than 300 objects observed. Using the presence of the lithium absorption and the location in the Hertzspung-Russell diagram, we identify 45 already known members and two new association members. We provide accurate RVs for all 47 confirmed members. A dynamical analysis, after accounting for unresolved binaries and errors, shows that the stellar surface population of L1688 has a velocity dispersion σ ~ 1.14 ± 0.35 km s-1 that is consistent with being in virial equilibrium and is bound with a ~80% probability. We also find a velocity gradient in the stellar surface population of ~1.0 km s-1 pc-1 in the northwest-southeast direction, which is consistent with that found for the pre-stellar dense cores, and we discuss the possibility of sequential and triggered star formation in L1688.

  19. Gaia-ESO Survey: Analysis of pre-main sequence stellar spectra

    NASA Astrophysics Data System (ADS)

    Lanzafame, A. C.; Frasca, A.; Damiani, F.; Franciosini, E.; Cottaar, M.; Sousa, S. G.; Tabernero, H. M.; Klutsch, A.; Spina, L.; Biazzo, K.; Prisinzano, L.; Sacco, G. G.; Randich, S.; Brugaletta, E.; Delgado Mena, E.; Adibekyan, V.; Montes, D.; Bonito, R.; Gameiro, J. F.; Alcalá, J. M.; González Hernández, J. I.; Jeffries, R.; Messina, S.; Meyer, M.; Gilmore, G.; Asplund, M.; Binney, J.; Bonifacio, P.; Drew, J. E.; Feltzing, S.; Ferguson, A. M. N.; Micela, G.; Negueruela, I.; Prusti, T.; Rix, H.-W.; Vallenari, A.; Alfaro, E. J.; Allende Prieto, C.; Babusiaux, C.; Bensby, T.; Blomme, R.; Bragaglia, A.; Flaccomio, E.; Francois, P.; Hambly, N.; Irwin, M.; Koposov, S. E.; Korn, A. J.; Smiljanic, R.; Van Eck, S.; Walton, N.; Bayo, A.; Bergemann, M.; Carraro, G.; Costado, M. T.; Edvardsson, B.; Heiter, U.; Hill, V.; Hourihane, A.; Jackson, R. J.; Jofré, P.; Lardo, C.; Lewis, J.; Lind, K.; Magrini, L.; Marconi, G.; Martayan, C.; Masseron, T.; Monaco, L.; Morbidelli, L.; Sbordone, L.; Worley, C. C.; Zaggia, S.

    2015-04-01

    Context. The Gaia-ESO Public Spectroscopic Survey is obtaining high-quality spectroscopy of some 100 000 Milky Way stars using the FLAMES spectrograph at the VLT, down to V = 19 mag, systematically covering all the main components of the Milky Way and providing the first homogeneous overview of the distributions of kinematics and chemical element abundances in the Galaxy. Observations of young open clusters, in particular, are giving new insights into their initial structure, kinematics, and their subsequent evolution. Aims: This paper describes the analysis of UVES and GIRAFFE spectra acquired in the fields of young clusters whose population includes pre-main sequence (PMS) stars. The analysis is applied to all stars in such fields, regardless of any prior information on membership, and provides fundamental stellar atmospheric parameters, elemental abundances, and PMS-specific parameters such as veiling, accretion, and chromospheric activity. Methods: When feasible, different methods were used to derive raw parameters (e.g. line equivalent widths) fundamental atmospheric parameters and derived parameters (e.g. abundances). To derive some of these parameters, we used methods that have been extensively used in the past and new ones developed in the context of the Gaia-ESO survey enterprise. The internal precision of these quantities was estimated by inter-comparing the results obtained by these different methods, while the accuracy was estimated by comparison with independent external data, such as effective temperature and surface gravity derived from angular diameter measurements, on a sample of benchmarks stars. A validation procedure based on these comparisons was applied to discard spurious or doubtful results and produce recommended parameters. Specific strategies were implemented to resolve problems of fast rotation, accretion signatures, chromospheric activity, and veiling. Results: The analysis carried out on spectra acquired in young cluster fields during

  20. NASA and ESA astronauts visit ESO. Hubble repair team meets European astronomers in Garching.

    NASA Astrophysics Data System (ADS)

    1994-02-01

    On Wednesday, February 16, 1994, seven NASA and ESA astronauts and their spouses will spend a day at the Headquarters of the European Southern Observatory. They are the members of the STS-61 crew that successfully repaired the Hubble Space Telescope during a Space Shuttle mission in December 1993. This will be the only stop in Germany during their current tour of various European countries. ESO houses the Space Telescope European Coordinating Facility (ST/ECF), a joint venture by the European Space Agency and ESO. This group of astronomers and computer specialists provide all services needed by European astronomers for observations with the Space Telescope. Currently, the European share is about 20 of the total time available at this telescope. During this visit, a Press Conference will be held on Wednesday, February 16, 11:45 - 12:30 at the ESO Headquarters Karl-Schwarzschild-Strasse 2 D-85748 Garching bei Munchen. Please note that participation in this Press Conference is by invitation only. Media representatives may obtain invitations from Mrs. E. Volk, ESO Information Service at this address (Tel.: +49-89-32006276; Fax.: +49-89-3202362), until Friday, February 11, 1994. After the Press Conference, between 12:30 - 14:00, a light refreshment will be served at the ESO Headquarters to all participants. >From 14:00 - 15:30, the astronauts will meet with students and teachers from the many scientific institutes in Garching in the course of an open presentation at the large lecture hall of the Physics Department of the Technical University. It is a 10 minute walk from ESO to the hall. Later the same day, the astronauts will be back at ESO for a private discussion of various space astronomy issues with their astronomer colleagues, many of whom are users of the Hubble Space Telescope, as well as ground-based telescopes at the ESO La Silla Observatory and elsewhere. The astronauts continue to Switzerland in the evening.

  1. ESO Receives Computerworld Honors Program 21st Century Achievement Award in Science Category

    NASA Astrophysics Data System (ADS)

    2005-06-01

    In a ceremony held in Washington, D.C. (USA) on June 6, 2005, ESO, the European Organisation for Astronomical Research in the Southern Hemisphere, received the coveted 21st Century Achievement Award from the Computerworld Honors Program for its visionary use of information technology in the Science category. Sybase, a main database server vendor and member of the Chairmen's Committee, nominated ESO's Data Flow System in recognition of its contributions to the global information technology revolution and its positive impact on society.

  2. Report on the ESO Workshop ''Central Massive Objects: The Stellar Nuclei - Black Hole Connection''

    NASA Astrophysics Data System (ADS)

    Neumayer, N.; Emsellem, E.

    2010-09-01

    An overview of the ESO workshop on black holes and nuclear star clusters is presented. The meeting reviewed the status of our observational and theoretical understanding of central massive objects, as well as the search for intermediate mass black holes in globular clusters. There will be no published proceedings, but presentations are available at http://www.eso.org/sci/meetings/cmo2010/program.html.

  3. The big comet crash of 1994. Intensive observational campaign at ESO

    NASA Astrophysics Data System (ADS)

    1994-01-01

    at shorter wavelengths than those at TIMMI, they will show higher layers of the atmosphere and the possible changes (streaming motions, new whirls and eddies ?) which may result from the impacts. These programmes will therefore complement eachother. A total of no less than 13 half-nights have been allocated at the 3.5 m New Technology Telescope. They will be shared between two groups which will both use the IRSPEC instrument to obtain detailed infrared spectra of the impact sites. One team is headed by Rita Schulz, the other by Therese Encrenaz from Observatoire de Paris. Among many others, they hope to observe some of the molecules which may be present in the deeper layers of the Jovian atmosphere, e.g., water, ammonium and phosphine (PH3). HOW WILL THE MEDIA LEARN ABOUT THE RESULTS FROM ESO ? Together, these programmes add up to a very significant observational effort at ESO in connection with this astronomical event. Although it is difficult to predict at this moment whether all of the above mentioned phenomena will actually be observed, there is an obvious and great interest in these programmes from all sides. To support the public information about the outcome, it is the intention of the ESO Information Service to provide the media with regular and rapid updates about the observational progress at the La Silla telescopes. For this, a special ESO news service will be activated some days before the series of impacts begin - it will be accessible for all interested parties during the critical period. More details about this service will be announced in a later Press Release.

  4. Carbon stars within the Gaia-ESO survey

    NASA Astrophysics Data System (ADS)

    Abia, C.; Van Eck, S.; Masseron, T.; Merle, T.; Worley, C. C.; Zwitter, T.

    2014-07-01

    The overwhelming majority of the astronomical objects are oxygen-rich, showing an abundance ratio C/O < 1 (by number). The so-called intrinsic carbon stars (C/O > 1) are formed during the AGB phase evolution of 1.5 ≤ M/M⊙≤ 3 stars through the mixing of fresh 12C from the interior of the star into the envelope during the 3rd dredge-up after each thermal pulse. They commonly show s-element enhancements produced by slow neutron captures provided by the 13C(α,n)16O reaction. The prototype of these stars are the AGB C-stars. Extrinsic carbon stars on the other hand, are formed in binary systems by mass transfer of carbon rich material from a former AGB star (now a white dwarf) onto the secondary star. Prototype of these class are the CH stars. A zoo of carbon-rich type stars exists, all being tracers of intermediate-age stellar populations. These stars are extremely useful for studies of the star formation history and chemical evolution of the galaxies. We present the detection and chemical analysis of carbon-enriched stars so far discovered within the Gaia-ESO survey. C-enriched candidates are identified from the analysis of a series of enhanced molecular features, measured through photometric and narrow-band spectroscopic filters. Then, the stellar parameters, C/O ratios and s-process element abundances are determined. The nature (intrinsic or extrinsic) of these carbon-enriched stars is discussed together with the expected impact of the Gaia mission on the knowledge of these objects in the Milky Way.

  5. The Properties of Globular Cluster ESO452-SC11

    NASA Astrophysics Data System (ADS)

    Cornish, A. S. M.; Phelps, R. L.; Briley, M. M.; Friel, E. D.

    2005-12-01

    The globular cluster ESO452-SC11 has been observed using Johnson V and Cousin I filters and PSF photometry has been performed. The resulting color-magnitude diagrams were compared to theoretical isochrones to derive the cluster's age, overall chemical composition, and distance modulus. These isochrone models include those published by Girardi et al., Bergbusch & VandenBerg with BVRI color-Teff relations as described by VandenBerg & Clem, and Demarque et al. (known as the Yale isochrones). From the Yale isochrones, it is estimated that the cluster has an age 9-11 Gyr, a metallicity [Fe/H] between -1.4 and -1.0 dex, and a distance modulus (m-M)V =16.10-16.31 mag resulting in a heliocentric distance of 7.3-7.5 kpc. Using the Bergbusch & VandenBerg models, it is estimated that the cluster has an age of 11-13 Gyr, with an iron-to hydrogen ratio between -1.3 and -0.8 dex, a distance modulus (m-M)V =15.87-16.12 mag, and a heliocentric distance between 7.0-7.2 kpc. The Girardi isochrone models yield a derived age of 13-16 Gyr, metallicity between -1.3 and -0.4 dex, distance modulus (m-M)V =15.59-16.19 mag, and heliocentric distance between 6.6-7.1 kpc. The derived parameters from these models are consistent for metallicity [Fe/H] between -1.3 and -1.0 dex, reddening E(V-I) =0.70 - 0.76, and (m-M)V =16.10 - 16.12 mag. A.C. would like to acknowledge the HACU National Internship program for supporting the data analysis portion of this research.

  6. Blasting away a dwarf galaxy: the `tail' of ESO 324-G024

    NASA Astrophysics Data System (ADS)

    Johnson, Megan C.; Kamphuis, Peter; Koribalski, Bärbel S.; Wang, Jing; Oh, Se-Heon; Hill, Alex S.; O'Sullivan, Shane; Haan, Sebastian; Serra, Paolo

    2015-08-01

    We present Australia Telescope Compact Array radio data of the dwarf irregular galaxy ESO 324-G024 which is seen in projection against the giant, northern lobe of the radio galaxy Centaurus A (Cen A, NGC 5128). The distorted morphology and kinematics of ESO 324-G024, as observed in the 21 cm spectral line emission of neutral hydrogen, indicate disruptions by external forces. We investigate whether tidal interactions and/or ram pressure stripping are responsible for the formation of the H I tail stretching to the north-east of ESO 324-G024 with the latter being most probable. Furthermore, we closely analyse the sub-structure of Cen A's polarized radio lobes to ascertain whether ESO 324-G024 is located in front, within or behind the northern lobe. Our multiwavelength, multicomponent approach allows us to determine that ESO 324-G024 is most likely behind the northern radio lobe of Cen A. This result helps to constrain the orientation of the lobe, which is likely inclined to our line of sight by approximately 60° if NGC 5128 and ESO 324-G024 are at the same distance.

  7. NY-ESO-1 (CTAG1B) expression in mesenchymal tumors.

    PubMed

    Endo, Makoto; de Graaff, Marieke A; Ingram, Davis R; Lim, Simin; Lev, Dina C; Briaire-de Bruijn, Inge H; Somaiah, Neeta; Bovée, Judith V M G; Lazar, Alexander J; Nielsen, Torsten O

    2015-04-01

    New York esophageal squamous cell carcinoma 1 (NY-ESO-1, CTAG1B) is a cancer-testis antigen and currently a focus of several targeted immunotherapeutic strategies. We performed a large-scale immunohistochemical expression study of NY-ESO-1 using tissue microarrays of mesenchymal tumors from three institutions in an international collaboration. A total of 1132 intermediate and malignant and 175 benign mesenchymal lesions were enrolled in this study. Immunohistochemical staining was performed on tissue microarrays using a monoclonal antibody for NY-ESO-1. Among mesenchymal tumors, myxoid liposarcomas showed the highest positivity for NY-ESO-1 (88%), followed by synovial sarcomas (49%), myxofibrosarcomas (35%), and conventional chondrosarcomas (28%). Positivity of NY-ESO-1 in the remaining mesenchymal tumors was consistently low, and no immunoreactivity was observed in benign mesenchymal lesions. On the basis of these findings, nearly 90% of myxoid liposarcomas, as well as a significant proportion of synovial sarcomas, myxofibrosarcomas, and conventional chondrosarcomas are good candidates for immunotherapy targeting NY-ESO-1.

  8. Three novel NY-ESO-1 epitopes bound to DRB1*0803, DQB1*0401 and DRB1*0901 recognized by CD4 T cells from CHP-NY-ESO-1-vaccinated patients.

    PubMed

    Mizote, Yu; Taniguchi, Taku; Tanaka, Kei; Isobe, Midori; Wada, Hisashi; Saika, Takashi; Kita, Shoichi; Koide, Yukari; Uenaka, Akiko; Nakayama, Eiichi

    2010-07-19

    Three novel NY-ESO-1 CD4 T cell epitopes were identified using PBMC obtained from patients who were vaccinated with a complex of cholesterol-bearing hydrophobized pullulan (CHP) and NY-ESO-1 protein (CHP-NY-ESO-1). The restriction molecules were determined by antibody blocking and using various EBV-B cells with different HLA alleles as APC to present peptides to CD4 T cells. The minimal epitope peptides were determined using various N- and C-termini truncated peptides deduced from 18-mer overlapping peptides originally identified for recognition. Those epitopes were DRB1*0901-restricted NY-ESO-1 87-100, DQB1*0401-restricted NY-ESO-1 95-107 and DRB1*0803-restricted NY-ESO-1 124-134. CD4 T cells used to determine those epitope peptides recognized EBV-B cells or DC that were treated with recombinant NY-ESO-1 protein or NY-ESO-1-expressing tumor cell lysate, suggesting that the epitope peptides are naturally processed. These CD4 T cells showed a cytokine profile with Th1 characteristics. Furthermore, NY-ESO-1 87-100 peptide/HLA-DRB1*0901 tetramer staining was observed. Multiple Th1-type CD4 T cell responses are beneficial for inducing effective anti-tumor responses after NY-ESO-1 protein vaccination.

  9. Live Webcasts from CERN and ESO for European Science and Technology Week

    NASA Astrophysics Data System (ADS)

    2002-10-01

    Visit http://www.cern.ch/sci-tech on 7 - 8 November to find out what modern Europeans can't live without. Seven of Europe's leading Research Organizations [1] are presenting three live Webcasts from CERN in a joint outreach programme for the European Science and Technology Week . The aim of Sci-Tech... couldn't be without it! is to show how today's society couldn't be without cutting-edge scientific research. See also ESO Press Release 05/02. Northern Europeans can't imagine their households without ovens, whereas Southern Europeans identify the refrigerator as the most essential household appliance. In the area of communications, cars and motorbikes are clearly the technologies of choice in Italy, but are regarded as less important in countries like Norway and Germany. For entertainment, the personal computer is a clear winner as the device is considered most essential by all Europeans, followed by the TV and the Internet. This hit parade of technological marvels is the result of a phone and online survey conducted by the Sci-Tech... couldn't be without it! team for this year's European Science and Technology Week on 4-10 November. The technologies Europeans could not be without, form the starting point of three entertaining and informative Webcast shows in Italian (Thursday 7 November at 10:00 CET), French (Thursday 7 November at 15:00 CET) and English (Friday 8 November at 15:00 CET), broadcast live on the Internet from a studio at CERN. During these Webcasts scientists from the seven research Organizations and their industrial partners Sun Microsystems, Siemens, L'Oreal and Luminex will engage - from the CERN studio or from remote locations through teleconference links - an audience of Internauts all over the world. The public will be taken inside their most popular gadgets to discover the science that made them possible and how vital fundamental research has been in the creation of modern technology. Fundamental science will be brought as close as possible to

  10. Antibody responses against NY-ESO-1 and HER2 antigens in patients vaccinated with combinations of cholesteryl pullulan (CHP)-NY-ESO-1 and CHP-HER2 with OK-432.

    PubMed

    Aoki, Masatoshi; Ueda, Shugo; Nishikawa, Hiroyoshi; Kitano, Shigehisa; Hirayama, Michiko; Ikeda, Hiroaki; Toyoda, Hideki; Tanaka, Kyosuke; Kanai, Michiyuki; Takabayashi, Arimichi; Imai, Hiroshi; Shiraishi, Taizo; Sato, Eiichi; Wada, Hisashi; Nakayama, Eiichi; Takei, Yoshiyuki; Katayama, Naoyuki; Shiku, Hiroshi; Kageyama, Shinichi

    2009-11-16

    Combination vaccines of the NY-ESO-1 protein complexed with cholesteryl pullulan (CHP), CHP-NY-ESO-1, and the truncated 146HER2 protein with CHP, CHP-HER2, were subcutaneously administered with the immuno-adjuvant OK-432 to eight esophageal cancer patients. Vaccination was well-tolerated. NY-ESO-1- and HER2-specific antibody responses were analyzed using the patients' sera and samples from previous single CHP-NY-ESO-1 or CHP-HER2 vaccine trial. The responses to NY-ESO-1 in the combination vaccine study were comparable to the single vaccine. For responses to HER2, there were fewer antibody responses in the combination vaccines. Although there were marked individual variations in the antibody responses to the NY-ESO-1 and HER2 antigens, the reaction patterns to these antigens were comparable within each patient. Antibodies to OK-432 were not augmented. Protein cancer vaccines targeting multiple antigens are feasible.

  11. Heteroclitic serological response in esophageal and prostate cancer patients after NY-ESO-1 protein vaccination.

    PubMed

    Kawada, Junji; Wada, Hisashi; Isobe, Midori; Gnjatic, Sacha; Nishikawa, Hiroyoshi; Jungbluth, Achim A; Okazaki, Nami; Uenaka, Akiko; Nakamura, Yurika; Fujiwara, Shinichi; Mizuno, Naoaki; Saika, Takashi; Ritter, Erika; Yamasaki, Makoto; Miyata, Hiroshi; Ritter, Gerd; Murphy, Roger; Venhaus, Ralph; Pan, Linda; Old, Lloyd J; Doki, Yuichiro; Nakayama, Eiichi

    2012-02-01

    NY-ESO-1 is a prototypic cancer/testis antigen. In a recent phase I clinical trial, we vaccinated 13 patients bearing NY-ESO-1-expressing tumors with a complex of cholesterol-bearing hydrophobized pullulan (CHP) and NY-ESO-1 protein (CHP-NY-ESO-1) and showed efficient induction of NY-ESO-1 antibody, and CD4 and CD8 T cell responses using peripheral blood from the patients. In our study, we analyzed heteroclitic serological responses in those patients after vaccination. Serological response against 11 tumor antigens including MAGE-A1, MAGE-A3, MAGE-A4, CT7/MAGEC1, CT10/MAGEC2, CT45, CT46/HORMAD1, SOX2, SSX2, XAGE1B and p53 was examined by enzyme-linked immunosorbent assay (ELISA) using sera from ten vaccinated patients. Expression of tumor antigens was determined by reverse transcription-polymerase chain reaction or immunohistochemistry. Eight of nine patients who showed antibody responses against NY-ESO-1 also showed an antibody response against at least 1 of these 11 tumor antigens after vaccination. In one patient, seven tumor antigens were recognized. Specificity analysis of the antibody response by ELISA using control recombinant proteins and synthetic peptides and by Western blot showed that the response was not against His6-tag and/or bacterial products included in a preparation of CHP-NY-ESO-1 used for vaccination. Thus, heteroclitic serological responses appear to be indicative of the overall immune response against the tumor, and their analysis could be useful for immune monitoring in cancer vaccine.

  12. NY-ESO-1 expression in meningioma suggests a rationale for new immunotherapeutic approaches.

    PubMed

    Baia, Gilson S; Caballero, Otavia L; Ho, Janelle S Y; Zhao, Qi; Cohen, Tzeela; Binder, Zev A; Salmasi, Vafi; Gallia, Gary L; Quinones-Hinojosa, Alfredo; Olivi, Alessandro; Brem, Henry; Burger, Peter; Strausberg, Robert L; Simpson, Andrew J G; Eberhart, Charles G; Riggins, Gregory J

    2013-11-01

    Meningiomas are the most common primary intracranial tumors. Surgical resection remains the treatment of choice for these tumors. However, a significant number of tumors are not surgically accessible, recur, or become malignant, necessitating the repetition of surgery and sometimes radiation. Chemotherapy is rarely used and is generally not recognized as an effective treatment. Cancer/testis (CT) genes represent a unique class of genes, which are expressed by germ cells, normally silenced in somatic cells, but activated in various cancers. CT proteins can elicit spontaneous immune responses in patients with cancer and this feature makes them attractive targets for immunotherapy-based approaches. We analyzed mRNA expression of 37 testis-restricted CT genes in a discovery set of 18 meningiomas by reverse transcription PCR. The overall frequency of expression of CT genes ranged from 5.6% to 27.8%. The most frequently expressed was NY-ESO-1, in 5 patients (27.8%). We subsequently analyzed NY-ESO-1 protein expression in a larger set of meningiomas by immunohistochemistry and found expression in 108 of 110 cases. In some cases, NY-ESO-1 expression was diffused and homogenous, but in most instances it was heterogeneous. Importantly, NY-ESO-1 expression was positively correlated with higher grade and patients presenting with higher levels of NY-ESO-1 staining had significantly worse disease-free and overall survival. We have also shown that NY-ESO-1 expression may lead to humoral immune response in patients with meningioma. Considering the limited treatment options for patients with meningioma, the potential of NY-ESO-1-based immunotherapy should be explored.

  13. ESO Telescope Designer Raymond Wilson Wins Prestigious Kavli Award for Astrophysics

    NASA Astrophysics Data System (ADS)

    2010-06-01

    Raymond Wilson, whose pioneering optics research at ESO made today's giant telescopes possible thanks to "active optics" technology, has been awarded the 2010 Kavli Prize in astrophysics. The founder and original leader of the Optics and Telescopes Group at ESO, Wilson shares the million-dollar prize with two American scientists, Jerry Nelson and Roger Angel. The biennial prize, presented by the Norwegian Academy of Science and Letters, the Kavli Foundation, and the Norwegian Ministry of Education and Research, was instituted in 2008 and is given to researchers who significantly advance knowledge in the fields of nanoscience, neuroscience, and astrophysics, acting as a complement to the Nobel Prize. The award is named for and funded by Fred Kavli, the Norwegian entrepreneur and phi­lanthropist who later founded the Kavlico Corpora­tion in the US - today one of the world's largest suppliers of sensors for aeronautic, automotive and industrial applications. Wilson, who joined ESO in 1972, strived to achieve optical perfection, developing the concept of active optics as a way to enhance the size of telescopic primary mirrors. It is the size of these mirrors that determines the ability of a telescope to gather light and study faint and distant objects. Before active optics, mirrors over six metres in diameter were impossible, being too heavy, costly, and likely to bend from gravity and temperature changes. The use of active optics, which preserves optimal image quality by continually adjusting the mirror's shape during observations, made lighter, thinner so-called "meniscus mirrors" possible. Wilson first led the implementation of active optics in the revolutionary New Technology Telescope at ESO's La Silla Observatory, and continued to develop and improve the technology until his retirement in 1993. Since then, active optics have become a standard part of modern astronomy, applied in every big telescope including ESO's Very Large Telescope (VLT), a telescope array

  14. CTLA-4 blockade enhances polyfunctional NY-ESO-1 specific T cell responses in metastatic melanoma patients with clinical benefit.

    PubMed

    Yuan, Jianda; Gnjatic, Sacha; Li, Hao; Powel, Sarah; Gallardo, Humilidad F; Ritter, Erika; Ku, Geoffrey Y; Jungbluth, Achim A; Segal, Neil H; Rasalan, Teresa S; Manukian, Gregor; Xu, Yinyan; Roman, Ruth-Ann; Terzulli, Stephanie L; Heywood, Melanie; Pogoriler, Evelina; Ritter, Gerd; Old, Lloyd J; Allison, James P; Wolchok, Jedd D

    2008-12-23

    Blockade of inhibitory signals mediated by cytotoxic T lymphocyte-associated antigen 4 (CTLA-4) has been shown to enhance T cell responses and induce durable clinical responses in patients with metastatic melanoma. The functional impact of anti-CTLA-4 therapy on human immune responses is still unclear. To explore this, we analyzed immune-related adverse events and immune responses in metastatic melanoma patients treated with ipilimumab, a fully human anti-CTLA-4 monoclonal antibody. Fifteen patients were selected on the basis of availability of suitable specimens for immunologic monitoring, and eight of these showed evidence of clinical benefit. Five of the eight patients with evidence of clinical benefit had NY-ESO-1 antibody, whereas none of seven clinical non-responders was seropositive for NY-ESO-1. All five NY-ESO-1 seropositive patients had clearly detectable CD4(+) and CD8(+) T cells against NY-ESO-1 following treatment with ipilimumab. One NY-ESO-1 seronegative clinical responder also had a NY-ESO-1 CD4(+) and CD8(+) T cell response, possibly related to prior vaccination with NY-ESO-1. Among five clinical non-responders analyzed, only one had a NY-ESO-1 CD4(+) T cell response and this patient did not have detectable anti-NY-ESO-1 antibody. Overall, NY-ESO-1-specific T cell responses increased in frequency and functionality during anti-CTLA-4 treatment, revealing a polyfunctional response pattern of IFN-gamma, MIP-1beta and TNF-alpha. We therefore suggest that CTLA-4 blockade enhanced NY-ESO-1 antigen-specific B cell and T cell immune responses in patients with durable objective clinical responses and stable disease. These data provide an immunologic rationale for the efficacy of anti-CTLA-4 therapy and call for immunotherapeutic designs that combine NY-ESO-1 vaccination with CTLA-4 blockade.

  15. Identification of two forms of the Eso1 protein in Schizosaccharomyces pombe.

    PubMed

    Chen, Zhiming; Cao, Hongshi; Guo, Weichao; Lu, Yingqiang

    2014-05-01

    In Schizosaccharomyces pombe, Eso1p is a protein fusion. Two-thirds of its N-terminus is conserved to budding yeast Rad30, which functions in error-free replication of UV-damaged DNA. A third of the C-terminus is highly conserved to budding yeast Eco1, a lysine acetyltransferase, which is essential for the establishment of cohesion. Both Rad30p and Eco1p need to be finely tuned in budding yeast. Given the distinct function existed in Rad30p and Eco1p, it is enigmatic how the Eso1p, the protein fusion regulated in S. pombe, works. We have identified two forms of the Eso1 protein by Western blot, and detected the Eco1-homology fragment by M/S analysis following TAP purification of Eso1 protein. The result raises the possibility that Eso1 might be processed in vivo to release the Eco1-homology fragment, which allows the independent regulation of Rad30-homology and Eco1-homology fragments.

  16. Expression and clinical relevance of NY-ESO-1, MAGE-1 and MAGE-3 in neuroblastoma.

    PubMed

    Söling, A; Schurr, P; Berthold, F

    1999-01-01

    Human genes NY-ESO-1, MAGE-1 and MAGE-3 code for antigens which are expressed in malignancies of various histological types but not in normal tissues except testis. These antigens might therefore represent potential targets for specific immunotherapy. We studied the expression of genes NY-ESO-1, MAGE-1 and MAGE-3 in 98 neuroblastoma tumors by reverse transcription-polymerase chain reaction (RT-PCR). MAGE-1 was expressed in 66%, NY-ESO-1 in 36% and MAGE-3 in 33% of the tumors. NY-ESO-1 gene expression was associated with age older than one year (p = 0.017), more differentiated tumor histology (p = 0.044), elevated urinary vanillylmandelic acid (VMA, p = 0.018) and normal serum ferritin levels (p = 0.023). MAGE-1 expression correlated significantly with normal serum ferritin levels (p = 0.009) and absence of MycN amplification (p = 0.007) while MAGE-3 expression was associated with absence of metastasis (p = 0.027). We conclude that approximately 70% of the neuroblastoma tumors express at least one of the genes coding for NY-ESO-1, MAGE-1 or -3, respectively.

  17. Phaeomelanin synthesis and obesity in mice. Interaction of the viable yellow (Avy) and sombre (eso) mutations.

    PubMed

    Wolff, G L; Galbraith, D B; Domon, O E; Row, J M

    1978-01-01

    Is abnormal regulation of phaeomelanin synthesis, which results in yellow coat color, inextricably linked to the development of obesity in viable yellow (Avy) house mice? To answer this question, black male mice of genotypes Avy/A eso/e+ and A/ae eso/e+ were produced from (DFT/Wf X C3H-1 vyfB/HeWf X SO/LeWf matings. The sombre (eso) mutation prevents phaeomelanin synthesis; therefore, all mice carrying this dominant allele are black regardless of the alleles present at the agouti locus. These black males were weighed weekly to 18 weeks of age. Simultaneously the agouti locus genotype of each male was determined by test matings to a/a e+/e+ females. The results of these test matings indicated that the two genotypes could be classified rather accurately by the intensity of pigmentation of the belly hair. Black Avy mice tended to have more dilute belly pigmentation that black A/ae mice. These gross observations were confirmed by microscopic examination of several hair types. Black Avy males reached a mean body weight of 44.2 +/- 0.6 g at 18 weeks, while black A males had a mean weight of 30.7 +/- 0.4 g at the same age. It is concluded that excessive weight gain resulting in obesity is induced by the Avy gene even when phaeomelanin synthesis is completely inhibited.

  18. REOSC Delivers the Best Astronomical Mirror in the World to ESO

    NASA Astrophysics Data System (ADS)

    1999-12-01

    On December 14, 1999, REOSC , the Optical Department of the SAGEM Group , finished the polishing of the fourth 8.2-m main mirror for the Very Large Telescope (VLT) of the European Southern Observatory. The mirror was today delivered to ESO at a ceremony at the REOSC factory in Saint Pierre du Perray, just south of Paris. The precision of the form of the mirror that was achieved during the polishing process is 8.5 nanometer (1 nanometer = 1 millionth of a millimetre) over the optical surface. This exceptional value corresponds to an optical resolution (theoretical image sharpness) of 0.03 arcseconds in the visible spectrum. This corresponds to distinguishing two objects separated by only 15 cm at a distance of 1000 km and will allow to detect astronomical objects that are 10,000 million times fainter than what can be perceived with the unaided eye. This impressive measure of quality, achieved by the REOSC teams during much painstaking work, implies that this VLT mirror is the most accurate in the world. In fact, all four 8.2-m VLT main mirrors polished by REOSC are well within the very strict specifications set by ESO, but this is the best of them all. The celebration today is the successful highlight of a contract initiated more than ten years ago, during which REOSC has perfected new polishing and control techniques - innovations improved and developed in a unique workshop dedicated to these giant mirrors. These methods and means are directly applicable to the new generations of segmented mirrors that are now being developed for astronomy and space observations. They are, in this sense, at the foremost front of optical technology. REOSC, the Optical Department of the SAGEM Group , is specialised in the study and realisation of high-precision optics for astronomy, space, defence, science and industry. For earlier information about the work on the VLT mirrors, cf. ESO Press Release 15/95 (13 November 1995). The SAGEM Group is a French high-technology group. It

  19. A phase I study of vaccination with NY-ESO-1f peptide mixed with Picibanil OK-432 and Montanide ISA-51 in patients with cancers expressing the NY-ESO-1 antigen.

    PubMed

    Kakimi, Kazuhiro; Isobe, Midori; Uenaka, Akiko; Wada, Hisashi; Sato, Eiichi; Doki, Yuichiro; Nakajima, Jun; Seto, Yasuyuki; Yamatsuji, Tomoki; Naomoto, Yoshio; Shiraishi, Kenshiro; Takigawa, Nagio; Kiura, Katsuyuki; Tsuji, Kazuhide; Iwatsuki, Keiji; Oka, Mikio; Pan, Linda; Hoffman, Eric W; Old, Lloyd J; Nakayama, Eiichi

    2011-12-15

    We conducted a phase I clinical trial of a cancer vaccine using a 20-mer NY-ESO-1f peptide (NY-ESO-1 91-110) that includes multiple epitopes recognized by antibodies, and CD4 and CD8 T cells. Ten patients were immunized with 600 μg of NY-ESO-1f peptide mixed with 0.2 KE Picibanil OK-432 and 1.25 ml Montanide ISA-51. Primary end points of the study were safety and immune response. Subcutaneous injection of the NY-ESO-1f peptide vaccine was well tolerated. Vaccine-related adverse events observed were fever (Grade 1), injection-site reaction (Grade 1 or 2) and induration (Grade 2). Vaccination with the NY-ESO-1f peptide resulted in an increase or induction of NY-ESO-1 antibody responses in nine of ten patients. The sera reacted with recombinant NY-ESO-1 whole protein as well as the NY-ESO-1f peptide. An increase in CD4 and CD8 T cell responses was observed in nine of ten patients. Vaccine-induced CD4 and CD8 T cells responded to NY-ESO-1 91-108 in all patients with various HLA types with a less frequent response to neighboring peptides. The findings indicate that the 20-mer NY-ESO-1f peptide includes multiple epitopes recognized by CD4 and CD8 T cells with distinct specificity. Of ten patients, two with lung cancer and one with esophageal cancer showed stable disease. Our study shows that the NY-ESO-1f peptide vaccine was well tolerated and elicited humoral, CD4 and CD8 T cell responses in immunized patients.

  20. Early Type Galaxies and Structural Parameters from ESO Public Survey KiDS

    NASA Astrophysics Data System (ADS)

    Roy, N.; Napolitano, N. R.; La Barbera, F.; Tortora, C.; Getman, F.; Radovich, M.; Capaccioli, M.

    The Kilo Degree survey (KiDS) is a large-scale optical imaging survey carried out with the VLT Survey Telescope (VST), which is the ideal tool for galaxy evolution studies. We expect to observe millions of galaxies for which we extract the structural parameters in four wavebands (u, g, r and i). This sample will represent the largest dataset with measured structural parameters up to a redshift z = 0. 5. In this paper we will introduce the sample, and describe the 2D fitting procedure using the 2DPHOT environment and the validation of the parameters with an external catalog.

  1. A Fruitful Collaboration between ESO and the Max Planck Computing and Data Facility

    NASA Astrophysics Data System (ADS)

    Fourniol, N.; Zampieri, S.; Panea, M.

    2016-06-01

    The ESO Science Archive Facility (SAF), contains all La Silla Paranal Observatory raw data, as well as, more recently introduced, processed data created at ESO with state-of-the-art pipelines or returned by the astronomical community. The SAF has been established for over 20 years and its current holding exceeds 700 terabytes. An overview of the content of the SAF and the preservation of its content is provided. The latest development to ensure the preservation of the SAF data, provision of an independent backup copy of the whole SAF at the Max Planck Computing and Data Facility in Garching, is described.

  2. The study of rotation curve with MOND for ESO138-G014

    NASA Astrophysics Data System (ADS)

    Hashim, N.; Salucci, P.; Abidin, Z. Z.

    2013-05-01

    This paper is devoted to solve the galactic rotation problem based on Modified Newtonian Dynamics (MOND). It addresses a new fundamental constant a0, called the acceleration constant, at which acceleration scale of Newton's second law fails to hold. It is an indication of a breakdown of classical Newtonian dynamics. In this respect, we choose the HI observations of a late type galaxy, ESO138-G014, to test the rotation curve within the MOND framework which leads to "MOND RC". We ask whether ESO138-G014 is compatible with MOND or dark matter is still favorable for the galactic rotation problem.

  3. ASASSN-16in: Discovery of A Probable Supernova in ESO 422-G 019

    NASA Astrophysics Data System (ADS)

    Brimacombe, J.; Brown, J. S.; Stanek, K. Z.; Holoien, T. W.-S.; Kochanek, C. S.; Shields, J.; Basu, U.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Bose, S.; Chen, Ping; Cruz, I.; Kiyota, S.; Post, R. S.; Stone, G.

    2016-08-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 422-G 019. ASASSN-16in (AT 2016eso) was discovered in images obtained on UT 2016-08-08.41 at V~17.0 mag. We also detect the object in images obtained on UT 2016-08-06.36 (V~17.3).

  4. South America Delegation of the European Parliament Visits ESO's Paranal Observatory

    NASA Astrophysics Data System (ADS)

    2003-10-01

    Chaired by Dr. Rolf Linkohr , Members of the European Parliament Delegation for Relations with the Countries of South America and MERCOSUR visited ESO's Paranal Observatory on October 29-30, 2003. As the world's most advanced optical/infrared astronomical facility, the ESO Very Large Telescope (VLT) at Paranal is the flagship of European astronomy and a powerful expression of Europe's ambitions in this important area of fundamental research. It is also an outstanding example of the capabilities of Europe's high-technology industries. At the same time, the Paranal Observatory provides a model for international, scientific co-operation between Europe and Latin America, based on agreements between ESO and the Republic of Chile. The deputies were accompanied by the ESO Representative in Chile, Mr. Daniel Hofstadt . Upon arrival Wednesday afternoon, the Delegation was welcomed by Dr. Roberto Gilmozzi , Director of ESO Paranal. The distinguished visitors were impressed by the instrumentation park available to astronomical research at Paranal. During a nightly visit to the Control Centre of the observatory, they met with visiting astronomers and ESO staff and experienced some of the exciting research programmes now being carried out with the VLT at the front line of human knowledge. For Dr. Linkohr , Astrophysics means high-tech today and it has many ramifications in other areas of Science and Technology. "Europe cannot be better represented in Latin America - and in Chile in particular - than by such an outstanding scientific and technical achievement as the VLT" , he said. ESO has received support from EU programmes. "Current interactions between ESO and the EU have shown that first-rate windows of opportunities exist in high-tech developments, indispensable for our continued exploration of the unknown" , indicated Dr. Gilmozzi . The deputies are leaving Paranal today (Thursday October 30th), continuing to La Serena before travelling back to Santiago de Chile. The

  5. Three Good Reasons for Celebrating at the ESO/ST-ECF Science Archive Facility

    NASA Astrophysics Data System (ADS)

    2000-12-01

    Great Demand for Data from New "Virtual Observatory" Summary Due to a happy coincidence, the ESO/ST-ECF Science Archive Facility is celebrating three different milestones at the same time: * its 10th anniversary since the establishment in 1991 * the 10,000th request for data , and * the signing-up of active user number 2000 . This Archive contains over 8 Terabytes (1 Terabyte = 1 million million bytes) of valuable observational data from the NASA/ESA Hubble Space Telescope (HST), the ESO Very Large Telescope (VLT) and other ESO telescopes . Its success paves the way for the establishment of "Virtual Observatories" from which first-class data can be obtained by astronomers all over the world. This greatly enhances the opportunities for more (young) scientists to participate in front-line research. PR Photo 34/00 : Front-page of a new brochure, describing the ESO/ST-ECF Science Archive Facility. Just 10 years ago, on the 1st of January 1991, the ESO/ST-ECF (European Southern Observatory/Space Telescope-European Coordinating Facility) Science Archive Facility opened. It has since served the astronomical community with gigabyte after gigabyte of high-quality astronomical data from some of the world's leading telescopes. The Archive, which is located in Garching, just outside Munich (Germany), contains data from the 2.4-m NASA/ESA Hubble Space Telescope , as well as from several ESO telescopes: the four 8.2-m Unit Telescopes of the Very Large Telescope (VLT) at the Paranal Observatory , and the 3.5-m New Technology Telescope (NTT) , the 3.6-m telescope and the MPG/ESO 2.2-m telescope at La Silla. The Archive is a continuously developing project - in terms of amounts of data stored, the number of users and in particular because of the current dramatic development of innovative techniques for data handling and storage. In the year 2000 more than 2 Terabytes (2000 Gigabytes) of data were distributed to users worldwide. The archiving of VLT data has been described in ESO PR

  6. Heritability of strabismus: genetic influence is specific to eso-deviation and independent of refractive error.

    PubMed

    Sanfilippo, Paul G; Hammond, Christopher J; Staffieri, Sandra E; Kearns, Lisa S; Melissa Liew, S H; Barbour, Julie M; Hewitt, Alex W; Ge, Dongliang; Snieder, Harold; Mackinnon, Jane R; Brown, Shayne A; Lorenz, Birgit; Spector, Tim D; Martin, Nicholas G; Wilmer, Jeremy B; Mackey, David A

    2012-10-01

    Strabismus represents a complex oculomotor disorder characterized by the deviation of one or both eyes and poor vision. A more sophisticated understanding of the genetic liability of strabismus is required to guide searches for associated molecular variants. In this classical twin study of 1,462 twin pairs, we examined the relative influence of genes and environment in comitant strabismus, and the degree to which these influences can be explained by factors in common with refractive error. Participants were examined for the presence of latent ('phoria') and manifest ('tropia') strabismus using cover-uncover and alternate cover tests. Two phenotypes were distinguished: eso-deviation (esophoria and esotropia) and exo-deviation (exophoria and exotropia). Structural equation modeling was subsequently employed to partition the observed phenotypic variation in the twin data into specific variance components. The prevalence of eso-deviation and exo-deviation was 8.6% and 20.7%, respectively. For eso-deviation, the polychoric correlation was significantly greater in monozygotic (MZ) (r = 0.65) compared to dizygotic (DZ) twin pairs (r = 0.33), suggesting a genetic role (p = .003). There was no significant difference in polychoric correlation between MZ (r = 0.55) and DZ twin pairs (r = 0.53) for exo-deviation (p = .86), implying that genetic factors do not play a significant role in the etiology of exo-deviation. The heritability of an eso-deviation was 0.64 (95% CI 0.50-0.75). The additive genetic correlation for eso-deviation and refractive error was 0.13 and the bivariate heritability (i.e., shared variance) was less than 1%, suggesting negligible shared genetic effect. This study documents a substantial heritability of 64% for eso-deviation, yet no corresponding heritability for exo-deviation, suggesting that the genetic contribution to strabismus may be specific to eso-deviation. Future studies are now needed to identify the genes associated with eso-deviation and

  7. The Gaia-ESO Survey: Sodium and aluminium abundances in giants and dwarfs. Implications for stellar and Galactic chemical evolution

    NASA Astrophysics Data System (ADS)

    Smiljanic, R.; Romano, D.; Bragaglia, A.; Donati, P.; Magrini, L.; Friel, E.; Jacobson, H.; Randich, S.; Ventura, P.; Lind, K.; Bergemann, M.; Nordlander, T.; Morel, T.; Pancino, E.; Tautvaišienė, G.; Adibekyan, V.; Tosi, M.; Vallenari, A.; Gilmore, G.; Bensby, T.; François, P.; Koposov, S.; Lanzafame, A. C.; Recio-Blanco, A.; Bayo, A.; Carraro, G.; Casey, A. R.; Costado, M. T.; Franciosini, E.; Heiter, U.; Hill, V.; Hourihane, A.; Jofré, P.; Lardo, C.; de Laverny, P.; Lewis, J.; Monaco, L.; Morbidelli, L.; Sacco, G. G.; Sbordone, L.; Sousa, S. G.; Worley, C. C.; Zaggia, S.

    2016-05-01

    cannot simultaneously explain the run of [Al/Fe] with [Fe/H], and vice versa. The comparison with stellar ages is hampered by severe uncertainties. Indeed, reliable age estimates are available for only a half of the stars of the sample. We conclude that Al is underproduced by the models, except for stellar ages younger than about 7 Gyr. In addition, some significant source of late Na production seems to be missing in the models. Either current Na and Al yields are affected by large uncertainties, and/or some important Galactic source(s) of these elements has as yet not been taken into account. Based on observations made with the ESO/VLT, at Paranal Observatory, under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey), and on data obtained from the ESO Archive originally observed under programs 60.A-9143, 076.B-0263 and 082.D-0726.Table 1 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/589/A115

  8. The ESA/ESO/NASA Photoshop FITS Liberator 3: Have your say on new features

    NASA Astrophysics Data System (ADS)

    Nielsen, L. H.; Christensen, L. L.; Hurt, R. L.; Nielsen, K.; Johansen, T.

    2008-06-01

    The popular, free ESA/ESO/NASA Photoshop FITS Liberator image processing software (a plugin for Adobe Photoshop) is about to get simpler, faster and more user-friendly! Here we would like to solicit inputs from the community of users.

  9. PSN J02062253-5201267 is a type Ia supernova in ESO 197-G24

    NASA Astrophysics Data System (ADS)

    Morrell, N.; Contreras, C.; Phillips, M. M.; Parker, S.; Hsia, E. Y.

    2015-07-01

    PSN J02062253-5201267 was discovered by Stu Parker (BOSS collaboration) in the edge-on spiral galaxy ESO 197-G024 at a redshift of 0.0196 (NED). The optical spectroscopic observation (range 360-960 nm) of the supernova was obtained with the 2.5-m du Pont Telescope (+ WFCCD) at Las Campanas on Jul. 19.40 UT.

  10. ASASSN-16cn: Discovery of A Probable Supernova in ESO 579-G018

    NASA Astrophysics Data System (ADS)

    Monard, L. A. G.; Cruz, I.; Brown, J. S.; Dong, Subo; Holoien, T. W.-S.; Stanek, K. Z.; Kochanek, C. S.; Godoy-Rivera, D.; Basu, U.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Chen, Ping; Brimacombe, J.; Bock, G.; Conseil, E.; Fernandez, J. M.; Kiyota, S.; Masi, G.; Wiethoff, W.

    2016-03-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 579-G018.

  11. ASASSN-16aw: Discovery of A Probable Supernova in ESO 306-G016

    NASA Astrophysics Data System (ADS)

    Kiyota, S.; Brown, J. S.; Holoien, T. W.-S.; Stanek, K. Z.; Kochanek, C. S.; Godoy-Rivera, D.; Basu, U.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Chen, Ping; Brimacombe, J.; Bock, G.; Koff, R. A.; Masi, G.

    2016-01-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 306-G016.

  12. ASASSN-16ff: Discovery of A Probable Supernova in ESO 218-G008

    NASA Astrophysics Data System (ADS)

    Brimacombe, J.; Kiyota, S.; Brown, J. S.; Holoien, T. W.-S.; Stanek, K. Z.; Kochanek, C. S.; Godoy-Rivera, D.; Basu, U.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Chen, Ping; Koff, R. A.; Monard, L. A. G.

    2016-05-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 218-G008.

  13. ASASSN-16hp: Discovery of A Probable Supernova in ESO 509-IG064

    NASA Astrophysics Data System (ADS)

    Shappee, B. J.; Holoien, T. W.-S.; Stanek, K. Z.; Kochanek, C. S.; Brown, J. S.; Shields, J.; Godoy-Rivera, D.; Basu, U.; Prieto, J. L.; Bersier, D.; Dong, Subo; Bose, S.; Chen, Ping; Brimacombe, J.

    2016-07-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 509-IG064.

  14. VizieR Online Data Catalog: Gaia-ESO Survey: NGC6705 (Cantat-Gaudin+, 2014)

    NASA Astrophysics Data System (ADS)

    Cantat-Gaudin, T.; Vallenari, A.; Zaggia, S.; Bragaglia, A.; Sordo, R.; Drew, J. E.; Eisloeffel, J.; Farnhill, H. J.; Gonzalez-Solares, E.; Greimel, R.; Irwin, M. J.; Kupcu-Yoldas, A.; Jordi, C.; Blomme, R.; Sampedro, L.; Costado, M. T.; Alfaro, E.; Smiljanic, R.; Magrini, L.; Donati, P.; Friel, E. D.; Jacobson, H.; Abbas, U.; Hatzidimitriou, D.; Spagna, A.; Vecchiato, A.; Balaguer-Nunez, L.; Lardo, C.; Tosi, M.; Pancino, E.; Klutsch, A.; Tautvaisiene, G.; Drazdauskas, A.; Puzeras, E.; Jimenez-Esteban, F.; Maiorca, E.; Geisler, D.; San, I.; Villanova, S.; Gilmore, G.; Randich, S.; Bensby, T.; Flaccomio, E.; Lanzafame, A.; Recio-Blanco, A.; Damiani, F.; Hourihane, A.; Jofre, P.; Delaverny, P.; Masseron, T.; Morbidelli, L.; Prisinzano, L.; Sacco, G. G.; Sbordone, L.; Worley, C. C.

    2014-07-01

    We combine new BV photometry with the spectroscopic observations of the Gaia-ESO Survey to study the open cluster NGC6 705. 1028 stars were observed with the HR15n grating of the GIRAFFE instrument at VLT/UT2. The radial velocities obtained for those stars were used to derive membership probabilities. (1 data file).

  15. ASASSN-16iq: Discovery of A Probable Supernova in ESO 471-G041

    NASA Astrophysics Data System (ADS)

    Brown, J. S.; Stanek, K. Z.; Holoien, T. W.-S.; Kochanek, C. S.; Shields, J.; Basu, U.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Bose, S.; Chen, Ping; Brimacombe, J.

    2016-08-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 471-G041.

  16. ASASSN-16ip: Discovery of A Probable Supernova in ESO_479-G_007

    NASA Astrophysics Data System (ADS)

    Shields, J.; Brown, J. S.; Stanek, K. Z.; Holoien, T. W.-S.; Kochanek, C. S.; Basu, U.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Bose, S.; Chen, Ping; Brimacombe, J.

    2016-08-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 479-G007.

  17. ESO Director General appointed President-Elect of the International Astronomical Union

    NASA Astrophysics Data System (ADS)

    2003-09-01

    The General Assembly of the International Astronomical Union (IAU), meeting in Sydney (Australia) in July, has appointed the ESO Director General, Dr. Catherine Cesarsky, as President-Elect for the three-year period 2003-2006. The IAU is the world's foremost organisation for astronomy, uniting almost 9000 professional scientists on all continents.

  18. ESO Vacancy - Applications are invited for the position of - Head of the Office for Science

    NASA Astrophysics Data System (ADS)

    2001-03-01

    Assignment: A strong research-oriented scientific staff with diverse expertise is essential to fulfil ESO's mandate of providing and maintaining international competitive observatories for its community of users. In this context the Head of the Office for Science will be responsible to the Director General for the science policies, and the main tasks will be:

  19. ASASSN-16kz: Discovery of A Probable Supernova in ESO 555-G029

    NASA Astrophysics Data System (ADS)

    Holoien, T. W.-S.; Stanek, K. Z.; Kochanek, C. S.; Brown, J. S.; Shields, J.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Bose, S.; Chen, Ping; Brimacombe, J.

    2016-09-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 555-G029.

  20. ESO unveils an amazing, interactive, 360-degree panoramic view of the entire night sky

    NASA Astrophysics Data System (ADS)

    2009-09-01

    The first of three images of ESO's GigaGalaxy Zoom project - a new magnificent 800-million-pixel panorama of the entire sky as seen from ESO's observing sites in Chile - has just been released online. The project allows stargazers to explore and experience the Universe as it is seen with the unaided eye from the darkest and best viewing locations in the world. This 360-degree panoramic image, covering the entire celestial sphere, reveals the cosmic landscape that surrounds our tiny blue planet. This gorgeous starscape serves as the first of three extremely high-resolution images featured in the GigaGalaxy Zoom project, launched by ESO within the framework of the International Year of Astronomy 2009 (IYA2009). GigaGalaxy Zoom features a web tool that allows users to take a breathtaking dive into our Milky Way. With this tool users can learn more about many different and exciting objects in the image, such as multicoloured nebulae and exploding stars, just by clicking on them. In this way, the project seeks to link the sky we can all see with the deep, "hidden" cosmos that astronomers study on a daily basis. The wonderful quality of the images is a testament to the splendour of the night sky at ESO's sites in Chile, which are the most productive astronomical observatories in the world. The plane of our Milky Way Galaxy, which we see edge-on from our perspective on Earth, cuts a luminous swath across the image. The projection used in GigaGalaxy Zoom place the viewer in front of our Galaxy with the Galactic Plane running horizontally through the image - almost as if we were looking at the Milky Way from the outside. From this vantage point, the general components of our spiral galaxy come clearly into view, including its disc, marbled with both dark and glowing nebulae, which harbours bright, young stars, as well as the Galaxy's central bulge and its satellite galaxies. The painstaking production of this image came about as a collaboration between ESO, the renowned

  1. Tim de Zeeuw to Become the Next Director General of ESO

    NASA Astrophysics Data System (ADS)

    2007-01-01

    The ESO Council has just appointed Tim de Zeeuw, 50, as the next Director General of ESO, effective as of 1 September 2007, when the current Director General, Catherine Cesarsky will complete her mandate. ESO PR Photo 02/07 ESO PR Photo 03/07 Professor Tim de Zeeuw "ESO is Europe's flagship organisation for ground-based astronomy," said, Richard Wade, President of the ESO Council. "The ESO Council is very pleased that Professor de Zeeuw has accepted the task as its next Director General. He has played a key role over the last few years in developing a strategic vision for ESO, and I have every confidence that he will now lead the organisation in the realisation of that exciting vision." Tim de Zeeuw has an excellent record, both as a highly respected scientist and as a leader of an internationally recognised science institute in the Netherlands. He is Scientific Director of the Leiden Observatory, a research institute in the College of Mathematics and Natural Sciences of Leiden University. Tim de Zeeuw also has considerable experience as regards science policy issues. Catherine Cesarsky, ESO's current Director General commented: "Over the recent years, ESO has developed considerably with more activities and new member states, and with its ambitious project portfolio, ESO is clearly facing an exciting future. I shall be delighted to pass the baton to Tim de Zeeuw, who as a recent Council member is very familiar with our Organisation." "It is a great honour and an exciting challenge to lead this world-class organisation in the years to come in support of one of the most dynamic areas of science today," said de Zeeuw. "I look forward to overseeing the continued upgrading of the Very Large Telescope with the second-generation instrumentation and the completion of the ALMA project, and in particular to help developing the future European Extremely Large Telescope." Tim de Zeeuw's main research interests embrace the formation, structure and dynamics of galaxies

  2. Polymeric structure and host Toll-like receptor 4 dictate immunogenicity of NY-ESO-1 antigen in vivo.

    PubMed

    Liu, Yanan; Tian, Xiaoli; Leitner, Wolfgang W; Aldridge, Michael E; Zheng, Junying; Yu, Zhiya; Restifo, Nicholas P; Weiss, Richard; Scheiblhofer, Sandra; Xie, Chong; Sun, Ren; Cheng, Genhong; Zeng, Gang

    2011-10-28

    In search of intrinsic factors that contribute to the distinctively strong immunogenicity of a non-mutated cancer/testis antigen, we found that NY-ESO-1 forms polymeric structures through disulfide bonds. NY-ESO-1 binding to immature dendritic cells was dependent on its polymeric structure and involved Toll-like receptor-4 (TLR4) on the surface of immature dendritic cells in mouse and human. Gene gun-delivered plasmid encoding the wild-type NY-ESO-1 readily induced T cell-dependent antibody (Ab) responses in wild-type C57BL/10 mice but not TLR4-knock-out C57BL/10ScNJ mice. Disrupting polymeric structures of NY-ESO-1 by cysteine-to-serine (Cys-to-Ser) substitutions lead to diminished immunogenicity and altered TLR4-dependence in the induced Ab response. To demonstrate its adjuvant effect, NY-ESO-1 was fused with a major mugwort pollen allergen Art v 1 and a tumor-associated antigen, carbonic anhydrase 9. Plasmid DNA vaccines encoding the fusion genes generated robust immune responses against otherwise non-immunogenic targets in mice. Polymeric structure and TLR4 may play important roles in rendering NY-ESO-1 immunogenic and thus serve as a potent molecular adjuvant. NY-ESO-1 thus represents the first example of a cancer/testis antigen that is a also damage-associated molecular pattern.

  3. Effector memory and central memory NY-ESO-1-specific re-directed T cells for treatment of multiple myeloma.

    PubMed

    Schuberth, P C; Jakka, G; Jensen, S M; Wadle, A; Gautschi, F; Haley, D; Haile, S; Mischo, A; Held, G; Thiel, M; Tinguely, M; Bifulco, C B; Fox, B A; Renner, C; Petrausch, U

    2013-04-01

    The cancer-testis antigen NY-ESO-1 is a potential target antigen for immune therapy expressed in a subset of patients with multiple myeloma. We generated chimeric antigen receptors (CARs) recognizing the immunodominant NY-ESO-1 peptide 157-165 in the context of HLA-A*02:01 to re-direct autologous CD8(+) T cells towards NY-ESO-1(+) myeloma cells. These re-directed T cells specifically lysed NY-ESO-1(157-165)/HLA-A*02:01-positive cells and secreted IFNγ. A total of 40% of CCR7(-) re-directed T cells had an effector memory phenotype and 5% a central memory phenotype. Based on CCR7 cell sorting, effector and memory CAR-positive T cells were separated and CCR7(+) memory cells demonstrated after antigen-specific re-stimulation downregulation of CCR7 as sign of differentiation towards effector cells accompanied by an increased secretion of memory signature cytokines such as IL-2. To evaluate NY-ESO-1 as potential target antigen, we screened 78 bone marrow biopsies of multiple myeloma patients where NY-ESO-1 protein was found to be expressed by immunohistochemistry in 9.7% of samples. Adoptively transferred NY-ESO-1-specific re-directed T cells protected mice against challenge with endogenously NY-ESO-1-positive myeloma cells in a xenograft model. In conclusion, re-directed effector- and central memory T cells specifically recognized NY-ESO-1(157-165)/ HLA-A*02:01-positive cells resulting in antigen-specific functionality in vitro and in vivo.

  4. Enhancing whole-tumor cell vaccination by engaging innate immune system through NY-ESO-1/dendritic cell interactions.

    PubMed

    Xu, Le; Zheng, Junying; Nguyen, David H; Luong, Quang T; Zeng, Gang

    2013-10-01

    NY-ESO-1 is a cancer/germline antigen (Ag) with distinctively strong immunogenicity. We have previously demonstrated that NY-ESO-1 serves as an endogenous adjuvant by engaging dendritic cell (DC)-surface receptors of calreticulin (CRT) and toll-like receptor (TLR) 4. In the present study, NY-ESO-1 was investigated for its immunomodulatory roles as a molecular adjuvant in whole-tumor cell vaccines using the Renca kidney cancer model. Renca cells were genetically engineered to express NY-ESO-1 on the cell surface to enhance direct interactions with DC. The effect of ectopic cell-surface expression of NY-ESO-1 was investigated on tumor immunogenicity, DC activation, cytotoxic T lymphocytes against model tumor-associated Ags, and the effectiveness of the modified tumor cells as a therapeutic whole-cell vaccine. Cell-surface expression of NY-ESO-1 was able to reduce the tumor growth of Renca cells in BALB/c mice, although the modification did not alter cell proliferation rate in vitro. Directly engaging the innate immune system through NY-ESO-1 facilitated the interaction of tumor cells with DC, leading to enhanced DC activation and subsequent tumor-specific T-cell priming. When used as a therapeutic whole-cell vaccine, Renca cells with NY-ESO-1 on the surface mediated stronger inhibitory effects on tumor growth and metastasis compared with parental Renca or Renca cells expressing a control protein GFP on the surface. Augmented antitumor efficacy correlated with increased CD8 T-cell infiltration into tumors and decreased myeloid-derived suppressor cells and regulatory T cells in the spleen. As a cancer/germline Ag and as an immunomodulatory adjuvant through engaging innate immune receptors, NY-ESO-1 offers a unique opportunity for improved whole-tumor cell vaccinations upon the classic GM-CSF-engineered cell vaccines.

  5. MAGE-A3/4 and NY-ESO-1 antigens expression in metastatic esophageal squamous cell carcinoma.

    PubMed

    Bujas, T; Marusic, Z; Peric Balja, M; Mijic, A; Kruslin, B; Tomas, D

    2011-03-21

    In the present study we analyzed immunohistochemical expression of MAGE-A 3/4 and NY-ESO-1 in 55 samples of esophageal squamous cell carcinomas (ESCC) and their respective lymph node metastases. To our knowledge this is the first study to assess and compare the expression of these antigens in ESCC lymph node metastases. Fifty (90.9%) primary ESCC were positive for MAGE-A 3/4 and 53 (96.6%) were positive for NY-ESO-1. MAGE-A 3/4 was expressed in all lymph node metastases and the intensity of expression was high in a majority of cases. NY-ESO-1 was negative in 2 (7.1%) lymph nodes metastases, while the reaction was predominantly moderate in the positive group. In primary tumors MAGE-A 3/4 showed a significantly higher intensity of expression compared to NY-ESO-1 (P=0.047), while in lymph node metastases the intensity of expression was not significantly different (P=0.387). Primary tumors with and without lymph node metastases showed no significant differences in MAGE-A 3/4 (P=0.672) and NY-ESO-1 (P=0.444) expression. Intensity of MAGE-A 3/4 (P=0.461) and NY-ESO-1 (P=0.414) expression in primary tumors was not significantly different compared to the expression in their respective lymph nodes metastases. Expression of MAGE-A 3/4 in primary tumors showed significant positive correlation with primary tumor expression of NY-ESO-1 (P=0.021) but no significant correlation with the expression of MAGE-A 3/4 in lymph node metastases (P=0.056). Expression of NY-ESO-1 in primary tumors showed significant positive correlation with the expression of NY-ESO-1 in lymph node metastases (P=0.001) and significant negative correlation with patients’ age (P<0.001). Expression of MAGE-A 3/4 and NY-ESO-1 in primary tumors and lymph node metastases showed no significant correlation with prognostic parameters such as tumor grade and TNM stage (P>0.05). We have shown different levels of MAGE-A 3/4 and NY-ESO-1 expression in almost all specimens of primary tumor and lymph node metastases

  6. Near-IR nonlinear optical filter for optical communication window.

    PubMed

    Vanyukov, Viatcheslav V; Mikheev, Gennady M; Mogileva, Tatyana N; Puzyr, Alexey P; Bondar, Vladimir S; Svirko, Yuri P

    2015-04-10

    We report on a high performance nonlinear optical filter for the telecommunication window that employs detonation nanodiamonds (NDs). The nanosecond Z-scan experiments revealed that the heavy water ND suspensions enable strong optical limiting in the wavelength range of 1400-1675 nm. We observed an enhancement of the optical limiting performance in the blue part of the communication window. In particular, at the wavelength of 1400 nm the transmittance of the 2 mm thick sample with 4.5 wt. % ND concentration is suppressed by 45% for the input fluence of 3.8  J/cm(2). The proposed nonlinear optical filter employs the phenomena of the nonlinear absorption and the nonlinear light scattering in ND suspensions.

  7. Near IR observations of η Car: Reaching its critical rotation?

    NASA Astrophysics Data System (ADS)

    Ishibashi, Kazunori; Mehner, Andrea; Nagayama, Takahiro

    2016-07-01

    We report a preliminary result in the monitoring of η Carinae in JHKs bands through the “spectroscopic” event of 2014.5 at InfraRed Survey Facility (IRSF) located in South African Astronomical Observatory (SAAO). The latest photometric data, combined with the data taken with the MK-II photometer [1], show a sign of the same cyclic variation in the J-H vs. H-K diagram reported by Mehner et al.[2]. The change can still be attributed to an apparent increase in black-body temperature, potentially reaching 3,000 to 6,000K as of March 2015.

  8. Light bullets from near-IR filament in fused silica

    NASA Astrophysics Data System (ADS)

    Smetanina, E. O.; Kompanets, V. O.; Dormidonov, A. E.; Chekalin, S. V.; Kandidov, V. P.

    2013-10-01

    The formation of light bullets during femtosecond laser pulse filamentation in the presence of anomalous group velocity dispersion has been recorded for the first time. The minimum experimentally detected width of the light bullet autocorrelation function is 27 fs, which corresponds to a duration of about 13.5 fs. The duration of the light bullet at a wavelength of 1800 nm is about two periods of the light field oscillation. The numerically calculated width of the autocorrelation function for such a light bullet is 23 fs, which is in good agreement with the experimental value.

  9. Composition of the Martian aerosols through near-IR spectroscopy

    NASA Technical Reports Server (NTRS)

    Erard, Stephane; Cerroni, Priscilla; Coradini, Angioletta

    1993-01-01

    Near-infrared spectroscopy is a powerful technique to study the composition of planetary surfaces, as the main minerals exhibit absorption bands in this spectral range. It gave important information on the mineralogy and petrology of Mars in the past twenty years although in this case it is well known that a large fraction of light is scattered by the airborne particles before reaching the surface. The measured signal is thus the sum of two different contributions that should be studied separately: One from the surface and one from the aerosols that depends on their density, size distribution and composition. Data from the ISM imaging spectrometer are used here to derive the aerosols spectrum. They consist in sets of spectra (from 0.76 to 3.16 microns) of approximately 3000 pixels approximately 25x25 sq km in size. The resulting spectrum exhibits both water-ice and clay mineral features superimposed on a scattering continuum.

  10. Thin hollow glass waveguide for near IR radiation delivery

    NASA Astrophysics Data System (ADS)

    Němec, Michal; Jelínková, Helena; Šulc, Jan; Miyagi, Mitsunobu; Iwai, Katsumasa; Shi, Yi-Wei; Matsuura, Yuji

    2008-02-01

    The delivery of the radiation by thin fiber is required for some application, especially in medical internals treatment. Therefore a new 100 μm and 250 μm inner diameter hollow glass waveguides were developed and investigated for the possibility to transport high power near infrared laser radiation without damage of these delivery systems. As laser sources two Nd:YAG laser systems working in Q-switched regime at wavelength 1.06 μm and 1.34 μm were utilized. Delivered radiation characterization was performed. By Alexandrite laser (755 nm) pumped Q-switched Nd:YAG laser has been generating 1.06 μm wavelength radiation with 6 ns length of pulse and maximum output energy 0.7 mJ (116.7 kW). The laser was Q-switched using LiF:F 2- saturable absorber. Second laser system was Nd:YAG/V:YAG microchip pumped by laser diode operating at 808 nm. The radiation at 1.3 μm wavelength has been generated with 250 Hz repetition rate. Pulse length was 6 ns and mean output power 25 mW. Corresponding pulse energy and peak power was 0.1 mJ and 16.7 kW, respectively. Both lasers were operating in fundamental TEM 00 mode (M2 ~ 1). For delivery a special cyclic olefin polymer-coated silver hollow glass waveguides with the inner/outer diameters 100/190 μm and 250/360 μm were used. The delivery system was consisted of lens, protector, and waveguide. As results the transmission more than 55% and reasonable spatial profile of laser output radiation were found. From these measurements it can be recommended using of this system for near infrared powerful radiation delivery as well as for medical treatment.

  11. Near-IR phosphorescent metalloporphyrin as a photochemical upconversion sensitizer.

    PubMed

    Deng, Fan; Sommer, Jonathan R; Myahkostupov, Mykhaylo; Schanze, Kirk S; Castellano, Felix N

    2013-08-28

    The phosphorescent metalloporphyrin sensitizer PtTPTNP (TPTNP = tetraphenyltetranaphtho[2,3]porphyrin) has been successfully coupled with perylenediimide (PDI) or rubrene utilized as triplet acceptors/annihilators to upconvert 690 nm incident photons into yellow fluorescence through sensitized triplet-triplet annihilation at overall efficiencies in the 6-7% range while exhibiting exceptional photostability. PMID:23857114

  12. Molecular Design of Near-IR Harvesting Unsymmetrical Squaraine Dyes

    SciTech Connect

    Kim, Sanghoon; Mor, Gopal K.; Paulose, Maggie; Varghese, Oomman K.; Baik, Chul; Grimes, Craig A.

    2010-08-17

    The functionalized unsymmetrical benzothiazole squaraine organic sensitizers 5-carboxy-2-({3-[(3-hexylbenzothiazol-2(3H)-ylidene)methyl]-2-hydroxy-4-oxo-2-cyclobuten-1-ylidene}methyl)-1-hexyl-3,3-dimethyl-3H-indolium (hereafter named as SK-11) and 5-carboxy-2-({3-[(3-hexyl-5-methoxybenzothiazol-2(3H)-ylidene)methyl]-2-hydroxy-4-oxo-2-cyclobuten-1-ylidene}methyl)-1-hexyl-3,3-dimethyl-3H-indolium (coded as SK-12) are designed and developed to observe an intense and wider absorption band in the red/NIR wavelength region. DFT/TDDFT calculations have been performed on the two unsymmetrical squaraine sensitizers to gain insight into their electronic and optical properties. The utility of these dyes in solid state dye sensitized solar cells (SS-DSSCs) is demonstrated.

  13. Visual and near-IR spectrophotometry of asteroids

    NASA Technical Reports Server (NTRS)

    Lebofsky, Larry A.

    1991-01-01

    We have been continuing our studies of the spectral properties of dark asteroids in the solar system. From these studies we expect to learn about the distribution of volatile materials, such as water in clay materials (water of hydration) and how the asteroids may relate to the comets. Our most recent work has been concentrating on simultaneous visual and near infrared photometry near Earth, main belt, and trojan asteroids. We have made observations of some unusual asteroids such as Chiron, which has recently shown cometary activity, and 944 Hidalgo, which has a comet-like orbit. We have also begun studies of the small, dark satellites of Mars and Jupiter in order to understand better how they may relate to the steroids. Could they actually be captured asteroids or comets?

  14. The AMBRE Project: Stellar parameterisation of the ESO:UVES archived spectra

    NASA Astrophysics Data System (ADS)

    Worley, C. C.; de Laverny, P.; Recio-Blanco, A.; Hill, V.; Bijaoui, A.

    2016-06-01

    Context. The AMBRE Project is a collaboration between the European Southern Observatory (ESO) and the Observatoire de la Côte d'Azur (OCA) that has been established to determine the stellar atmospheric parameters for the archived spectra of four ESO spectrographs. Aims: The analysis of the UVES archived spectra for their stellar parameters was completed in the third phase of the AMBRE Project. From the complete ESO:UVES archive dataset that was received covering the period 2000 to 2010, 51 921 spectra for the six standard setups were analysed. These correspond to approximately 8014 distinct targets (that comprise stellar and non-stellar objects) by radial coordinate search. Methods: The AMBRE analysis pipeline integrates spectral normalisation, cleaning and radial velocity correction procedures in order that the UVES spectra can then be analysed automatically with the stellar parameterisation algorithm MATISSE to obtain the stellar atmospheric parameters. The synthetic grid against which the MATISSE analysis is carried out is currently constrained to parameters of FGKM stars only. Results: Stellar atmospheric parameters are reported for 12 403 of the 51 921 UVES archived spectra analysed in AMBRE:UVES. This equates to ~23.9% of the sample and ~3708 stars. Effective temperature, surface gravity, metallicity, and alpha element to iron ratio abundances are provided for 10 212 spectra (~19.7%), while effective temperature at least is provided for the remaining 2191 spectra. Radial velocities are reported for 36 881 (~71.0%) of the analysed archive spectra. While parameters were determined for 32 306 (62.2%) spectra these parameters were not considered reliable (and thus not reported to ESO) for reasons such as very low S/N, too poor radial velocity determination, spectral features too broad for analysis, and technical issues from the reduction. Similarly the parameters of a further 7212 spectra (13.9%) were also not reported to ESO based on quality criteria and error

  15. Britain Approaches ESO about Installation of Major New Telescope at Paranal

    NASA Astrophysics Data System (ADS)

    2000-02-01

    The Executive Board of the UK Visible and Infrared Survey Telescope (VISTA) project announced today [1] that it is aiming at the installation of a new and powerful astronomical telescope at the ESO Paranal Observatory (Chile). This 4-metre telescope is a specialised wide-angle facility equipped with powerful cameras and efficient detectors that will enable it to obtain deep images of large sky areas in short time. These survey observations will be made in several wavebands in the optical and, in particular, the near-infrared region of the electromagnetic spectrum. VISTA will become the largest and most effective telescope of its type when it enters into operation in 2004. It is a project of a consortium of 18 UK universities [2]. Construction is expected to start in spring 2000. Funding of the project was announced in May 1999, as one of the first allocations from the "Joint Infrastructure Fund (JIF)", an initiative of the UK Government's Department of Trade and Industry, the Wellcome Trust, and the Higher Education Funding Council for England. ESO's Director General, Dr. Catherine Cesarsky , is very pleased with this decision. She received a mandate from the ESO Council in December 1999 to negotiate a contract with the UK Particle Physics and Astronomy Research Council (PPARC) , acting on behalf of the VISTA Executive Board, for the installation of VISTA at Paranal and now looks forward to settle the associated legal and operational details with her British counterparts at good pace. "The installation of VISTA at Paranal will be of great benefit to all European astronomers", she says. "The placement of a survey telescope of this size next to ESO's VLT, the world's largest optical telescope, opens a plethora of exciting opportunities for joint research projects. Deep observations with VISTA, especially in infrared wavebands, will provide a most valuable, first census of large regions of space. This will most certainly lead to the discoveries of many new and

  16. ESO Vacancy - Applications are invited for the position of Head of Administration

    NASA Astrophysics Data System (ADS)

    2001-06-01

    ESO employs in total approximately 500 staff members, and the Administration Division comprises the Administration at the Headquarters in Garching near Munich and the Administration in Santiago in Chile. The successful candidate will be supported by some 50 qualified staff members. As a member of the ESO Management Board the Head of Administration contributes essentially to the development of the overall policy, strategic planning, relations to the members of personnel and maintains professional contacts at highest level outside the Organisation. The main task is to provide efficient administrative services and advice to the Director General, Division Leaders and to staff members in the scientific and technical areas in the fields of financial planning and accounting, personnel management, purchasing, legal and contractual matters, information systems and building and site maintenance.

  17. ESO 103-G35 - A new Seyfert galaxy and possible X-ray source

    NASA Technical Reports Server (NTRS)

    Phillips, M. M.; Feldman, F. R.; Marshall, F. E.; Wamsteker, W.

    1979-01-01

    By means of an objective prism plate, two emission-line galaxies have been identified within the 0.7-sq deg HEAO-A2 error box for the X-ray source H1834-653. Optical spectrophotometric observations are reported for both objects as well as the galaxy NGC 6684, which also lies near the position of H1834-653. These data show that one of the emission-line galaxies, ESO 103-G35, is a Seyfert galaxy with a high-excitation forbidden-line spectrum and weak broad emission wings at H-alpha. Further measurements of this galaxy reveal an infrared excess at wavelengths longer than 2.2 microns. The H-alpha luminosity of ESO 103-G35 is consistent with the X-ray luminosity estimated from the HEAO-A2 data, thus strengthening the likelihood of association of this galaxy with the X-ray emission.

  18. Observing facilities at the European Southern Observatory (ESO) in Chile for cometary observations

    NASA Technical Reports Server (NTRS)

    Schnur, G. F. O.; Kohoutek, L.; Rahe, J.

    1981-01-01

    The (ESO) is located on the mountain La Silla (geographical coordinates: 4h42m55s10 west, -29 deg 15' 25".8 south, 2400 m elevation. The size of the telescopes ranges from a 40 cm Astrograph to the 3.6 m Richey-Chretien telescope. Future telescopes are discussed: a 2.2 m RC-Telescope which will be identical with the German 2.2 m telescope on Calor Alto in SE-Spain, and a 3.5 m telescope, the New Technology Telescope. In addition to these telescopes, a great number of auxiliary instrumentation are operational. Because ESO has to serve all requests of the visiting astronomers these instruments are designed for very different applications. The telescopes and auxiliary instruments that are especially suited for cometary observations are discussed. The dicussion is divided into three parts: photography, photometry-polarimetry and spectroscopy.

  19. Erratum: BeppoSAX Observations of the Maser Seyfert 2 Galaxy ESO 103-G35

    NASA Astrophysics Data System (ADS)

    Wilkes, Belinda J.; Mathur, Smita; Fiore, Fabrizio; Antonelli, Angelo; Nicastro, Fabrizio

    2001-08-01

    In the paper ``BeppoSAX Observations of the Maser Seyfert 2 Galaxy ESO 103-G35'' by Belinda J. Wilkes, Smita Mathur, Fabrizio Fiore, Angelo Antonelli, and Fabrizio Nicastro (ApJ, 549, 248 [2001]), the size of the line-emitting region derived from the line width should read 0.01 pc and not 50 pc as currently listed in the abstract, § 3.4, and § 4.

  20. NY-ESO-1 antigen-reactive T cell receptors exhibit diverse therapeutic capability.

    PubMed

    Sommermeyer, Daniel; Conrad, Heinke; Krönig, Holger; Gelfort, Haike; Bernhard, Helga; Uckert, Wolfgang

    2013-03-15

    The cancer-testis antigen NY-ESO-1 has been used as a target for different immunotherapies like vaccinations and adoptive transfer of antigen-specific cytotoxic T cells, as it is expressed in various tumor types and has limited expression in normal cells. The in vitro generation of T cells with defined antigen specificity by T cell receptor (TCR) gene transfer is an established method to create cells for immunotherapy. However, an extensive characterization of TCR which are candidates for treatment of patients is crucial for successful therapies. The TCR has to be efficiently expressed, their affinity to the desired antigen should be high enough to recognize low amounts of endogenously processed peptides on tumor cells, and the TCR should not be cross-reactive to other antigens. We characterized three NY-ESO-1 antigen-reactive cytotoxic T lymphocyte clones which were generated by different approaches of T cell priming (autologous, allogeneic), and transferred their TCR into donor T cells for more extensive evaluations. Although one TCR most efficiently bound MHC-multimers loaded with NY-ESO-1 peptide, T cells expressing this transgenic TCR were not able to recognize endogenously processed antigen. A second TCR recognized HLA-A2 independent of the bound peptide beside its much stronger recognition of NY-ESO-1 bound to HLA-A2. A third TCR displayed an intermediate but peptide-specific performance in all functional assays and, therefore, is the most promising candidate TCR for further clinical development. Our data indicate that multiple parameters of TCR gene-modified T cells have to be evaluated to identify an optimal TCR candidate for adoptive therapy.

  1. The strange 'barred' spiral galaxy ESO 235-58 - A case of morphological deception

    NASA Astrophysics Data System (ADS)

    Buta, R.; Crocker, D. A.

    1993-09-01

    On the SRC-J southern sky survey, the galaxy ESO 235-58 (alpha = 21 h 03 m, delta = -48 deg 19 arcmin, 1950) looks deceptively like a late-type barred spiral with a weak, broken ring surrounding the bar. However, the bar shows a straight, splitting dust lane, atypical of normal bars but just like what is seen in an edge-on spiral galaxy. In this paper, we use CCD images to show that the apparent bar is indeed likely to be an edge-on galaxy, possibly of Hubble type Sb. The object is part of a group of nine galaxies at a distance of 47 Mpc, and from the photometry we find that the edge-on component has a low luminosity, corresponding to a corrected absolute blue magnitude of M(0)B = -18.0 (for H0 = 100). The outer spiral part is asymmetric and may be perturbed by one or both of the neighboring large spirals, ESO 235-55 and ESO 235-57. Since we can find no evidence for an independent bulge or nucleus of this part, we believe that ESO 235-58 is not simply a case of superposition of two unrelated objects, but instead is an interacting galaxy of the type related to polar rings. This interpretation is supported by preliminary single-dish H I observations and published optical spectroscopy. Here we present mainly B-band images, a B-I color index map, an unsharp-masked image, integrated parameters, and luminosity profiles of the object to highlight its structural properties.

  2. The Gaia-ESO Survey: detailed abundances for thousands of FGK-type stars

    NASA Astrophysics Data System (ADS)

    Smiljanic, R.

    2014-10-01

    The Gaia-ESO Survey is using FLAMES at the VLT to observe more than 10^{5} stars. Giraffe medium-resolution spectra is being obtained for ˜ 10^{5} stars and high-resolution UVES spectra is being obtained for ˜ 5000 stars. Here I present a short summary of the Survey with emphasis on the sample of FGK-type stars being observed with UVES.

  3. A novel murine T-cell receptor targeting NY-ESO-1.

    PubMed

    Rosati, Shannon F; Parkhurst, Maria R; Hong, Young; Zheng, Zhili; Feldman, Steven A; Rao, Mahadev; Abate-Daga, Daniel; Beard, Rachel E; Xu, Hui; Black, Mary A; Robbins, Paul F; Schrump, David A; Rosenberg, Steven A; Morgan, Richard A

    2014-04-01

    Cancer testis antigens, such as NY-ESO-1, are expressed in a variety of prevalent tumors and represent potential targets for T-cell receptor (TCR) gene therapy. DNA encoding a murine anti-NY-ESO-1 TCR gene (mTCR) was isolated from immunized HLA-A*0201 transgenic mice and inserted into a γ-retroviral vector. Two mTCR vectors were produced and used to transduce human PBL. Transduced cells were cocultured with tumor target cell lines and T2 cells pulsed with the NY-ESO-1 peptide, and assayed for cytokine release and cell lysis activity. The most active TCR construct was selected for production of a master cell bank for clinical use. mTCR-transduced PBL maintained TCR expression in short-term and long-term culture, ranging from 50% to 90% efficiency 7-11 days after stimulation and 46%-82% 10-20 days after restimulation. High levels of interferon-γ secretion were observed (1000-12000 pg/mL), in tumor coculture assays and recognition of peptide-pulsed cells was observed at 0.1 ng/mL, suggesting that the new mTCR had high avidity for antigen recognition. mTCR-transduced T cells also specifically lysed human tumor targets. In all assays, the mTCR was equivalent or better than the comparable human TCR. As the functional activity of TCR-transduced cells may be affected by the formation of mixed dimers, mTCRs, which are less likely to form mixed dimers with endogenous hTCRs, may be more effective in vivo. This new mTCR targeted to NY-ESO-1 represents a novel potential therapeutic option for adoptive cell-transfer therapy for a variety of malignancies.

  4. SPARTA: the ESO standard platform for adaptive optics real time applications

    NASA Astrophysics Data System (ADS)

    Fedrigo, Enrico; Donaldson, Robert; Soenke, Christian; Myers, Richard; Goodsell, Stephen; Geng, Deli; Saunter, Chris; Dipper, Nigel

    2006-06-01

    ESO is starting a number of new projects collectively called Second Generation VLT instrumentation. Several of them will use Adaptive Optics (AO). In comparison with today's ESO AO systems, the 2nd Generation VLT AO systems will be much bigger (in terms of degrees of freedom) and faster (in terms of loop frequency). Consequently the Real-Time Computer controlling these AO systems will be significantly bigger and more challenging to build compared with today's AO systems in operation. To support the new requirements ESO started the development of a common flexible platform called SPARTA for Standard Platform for Adaptive optics Real Time Applications. The guidelines along which SPARTA is developed recognize the importance of industry standards over custom development to lower the development costs, ease the maintenance and make the system upgradeable thus delivering the performance required. SPARTA is based on a hybrid architecture that comprises all the major computing architectures available today: the high computational throughput is achieved through the combination of FPGA and DSP usage, where DSP are used as fast coprocessors and FPGA are used as front and as communication infrastructure, thus guaranteeing also the low latency. The flexibility is spread between the usage of both high-end CPUs and again the DSPs. All three technologies are organized in a parallel system interconnected by fast serial fabrics based on standard protocols. External input / output interfaces are also based on industry standard protocols, thus enabling the usage of commercially available tools for development and testing.

  5. Machine-learning-based photometric redshifts for galaxies of the ESO Kilo-Degree Survey data release 2

    NASA Astrophysics Data System (ADS)

    Cavuoti, S.; Brescia, M.; Tortora, C.; Longo, G.; Napolitano, N. R.; Radovich, M.; Barbera, F. La; Capaccioli, M.; de Jong, J. T. A.; Getman, F.; Grado, A.; Paolillo, M.

    2015-09-01

    We have estimated photometric redshifts (zphot) for more than 1.1 million galaxies of the public European Southern Observatory (ESO) Kilo-Degree Survey (KiDS) data release 2. KiDS is an optical wide-field imaging survey carried out with the Very Large Telescope (VLT) Survey Telescope (VST) and the OmegaCAM camera, which aims to tackle open questions in cosmology and galaxy evolution, such as the origin of dark energy and the channel of galaxy mass growth. We present a catalogue of photometric redshifts obtained using the Multi-Layer Perceptron with Quasi-Newton Algorithm (MLPQNA) model, provided within the framework of the DAta Mining and Exploration Web Application REsource (DAMEWARE). These photometric redshifts are based on a spectroscopic knowledge base that was obtained by merging spectroscopic data sets from the Galaxy and Mass Assembly (GAMA) data release 2 and the Sloan Digital Sky Survey III (SDSS-III) data release 9. The overall 1σ uncertainty on Δz = (zspec - zphot)/(1 + zspec) is ˜0.03, with a very small average bias of ˜0.001, a normalized median absolute deviation of ˜0.02 and a fraction of catastrophic outliers (|Δz| > 0.15) of ˜0.4 per cent.

  6. Concurrent Nontuberculous Mycobacteria Infection and High-Grade Anterior Mediastinal Extraskeletal Osteosarcoma (ESOS): Is There a Connection?

    PubMed

    Faz, Gabriel T; Eltorky, Mahmoud; Karnath, Bernard

    2016-01-01

    BACKGROUND Extraskeletal osteosarcomas (ESOS) of the mediastinum are extremely rare and may present with concurrent nontuberculous mycobacteria infection. CASE REPORT We present the second documented case of high-grade anterior mediastinal extraskeletal osteosarcoma in a 59-year-old man with a history of treated, latent tuberculosis (TB). Sputum samples grew Mycoplasma avium complex and Mycobacterium fortuitum. Imaging showed a right-sided 7.6 cm mass with compression of the main bronchus. Subsequent biopsy with vimentin staining established the diagnosis of ESOS. Due to the patient's rapidly declining performance status, he was not deemed a candidate for surgery or chemotherapy. He subsequently expired within one month of presentation. CONCLUSIONS We present a unique case of high-grade anterior mediastinum ESOS and a review of the literature regarding all documented cases of ESOS to date. We suggest there is a possible link between mediastinal masses and nontuberculous mycobacteria infection. PMID:27539718

  7. N° 15-2000: ESA, CERN and ESO launch "Physics on Stage"

    NASA Astrophysics Data System (ADS)

    2000-03-01

    But how much do the citizens of Europe really know about physics? Here is a unique opportunity to learn more about this elusive subject! Beginning in February 2000, three major European research establishments [1] are organising a unique Europe-wide programme to raise the public awareness of physics and related sciences. "Physics on Stage" is launched by the European Space Agency (ESA), the European Laboratory for Particle Physics (CERN), and the European Southern Observatory (ESO), with support from the European Union (EU). Other partners include the European Physical Society (EPS) and the European Association for Astronomy Education (EAAE). This exciting programme is part of the European Week for Science and Technology and will culminate in a Science Festival during November 6-11, 2000, at CERN, Geneva. Why "Physics on Stage"? The primary goal of "Physics on Stage" is to counteract the current decline in interest and knowledge of physics among Europe's citizens by means of a series of highly visible promotional activities. It will bring together leading scientists and educators, government bodies and the media, to confront the diminishing attraction of physics to young people and to develop strategies to reverse this trend. The objective in the short term is to infuse excitement and to provide new educational materials. In the longer term, "Physics on Stage" will generate new developments by enabling experts throughout Europe to meet, exchange and innovate. "Physics on Stage" in 22 European Countries. "Physics on Stage" has been initiated in 22 European countries [2]. In each country, a dedicated National Steering Committee (NSC) is being formed which will be responsible for their own national programme. A list of contact addresses is attached below. "Physics on Stage" is based on a series of high-profile physics-related activities that will inform the European public in general, and European high school physics teachers and media representatives in particular

  8. The Gaia-ESO Survey: characterisation of the [α/Fe] sequences in the Milky Way discs

    NASA Astrophysics Data System (ADS)

    Kordopatis, G.; Wyse, R. F. G.; Gilmore, G.; Recio-Blanco, A.; de Laverny, P.; Hill, V.; Adibekyan, V.; Heiter, U.; Minchev, I.; Famaey, B.; Bensby, T.; Feltzing, S.; Guiglion, G.; Korn, A. J.; Mikolaitis, Š.; Schultheis, M.; Vallenari, A.; Bayo, A.; Carraro, G.; Flaccomio, E.; Franciosini, E.; Hourihane, A.; Jofré, P.; Koposov, S. E.; Lardo, C.; Lewis, J.; Lind, K.; Magrini, L.; Morbidelli, L.; Pancino, E.; Randich, S.; Sacco, G. G.; Worley, C. C.; Zaggia, S.

    2015-10-01

    -resolution spectroscopic surveys. Conclusions: The small variations in the spatial [α/ Fe] - [Fe/H] paths of the thin disc do not allow us to distinguish between formation models of this structure. On the other hand, the lack of radial gradients and [α/ Fe] - [Fe/H] variations for the thick disc indicate that the mechanism responsible for the mixing of metals in the young Galaxy (e.g. radial stellar migration or turbulent gaseous disc) was more efficient before the (present) thin disc started forming. Based on observations collected with the FLAMES spectrograph at the VLT/UT2 telescope (Paranal Observatory, ESO, Chile), for the Gaia-ESO Large Public Survey, programme 188.B-3002.

  9. The AMBRE project: Parameterisation of FGK-type stars from the ESO:HARPS archived spectra

    NASA Astrophysics Data System (ADS)

    De Pascale, M.; Worley, C. C.; de Laverny, P.; Recio-Blanco, A.; Hill, V.; Bijaoui, A.

    2014-10-01

    Context. The AMBRE project is a collaboration between the European Southern Observatory (ESO) and the Observatoire de la Côte d'Azur (OCA). It has been established to determine the stellar atmospheric parameters of the archived spectra of four ESO spectrographs. Aims: The analysis of the ESO:HARPS archived spectra for the determination of their atmospheric parameters (effective temperature, surface gravity, global metallicities, and abundance of α-elements over iron) is presented. The sample being analysed (AMBRE:HARPS) covers the period from 2003 to 2010 and is comprised of 126 688 scientific spectra corresponding to ~17 218 different stars. Methods: For the analysis of the AMBRE:HARPS spectral sample, the automated pipeline developed for the analysis of the AMBRE:FEROS archived spectra has been adapted to the characteristics of the HARPS spectra. Within the pipeline, the stellar parameters are determined by the MATISSE algorithm, which has been developed at OCA for the analysis of large samples of stellar spectra in the framework of galactic archaeology. In the present application, MATISSE uses the AMBRE grid of synthetic spectra, which covers FGKM-type stars for a range of gravities and metallicities. Results: We first determined the radial velocity and its associated error for the ~15% of the AMBRE:HARPS spectra, for which this velocity had not been derived by the ESO:HARPS reduction pipeline. The stellar atmospheric parameters and the associated chemical index [α/Fe] with their associated errors have then been estimated for all the spectra of the AMBRE:HARPS archived sample. Based on key quality criteria, we accepted and delivered the parameterisation of 93 116 (74% of the total sample) spectra to ESO. These spectra correspond to ~10 706 stars; each are observed between one and several hundred times. This automatic parameterisation of the AMBRE:HARPS spectra shows that the large majority of these stars are cool main-sequence dwarfs with metallicities

  10. A cancer vaccine induces expansion of NY-ESO-1-specific regulatory T cells in patients with advanced melanoma.

    PubMed

    Ebert, Lisa M; MacRaild, Sarah E; Zanker, Damien; Davis, Ian D; Cebon, Jonathan; Chen, Weisan

    2012-01-01

    Cancer vaccines are designed to expand tumor antigen-specific T cells with effector function. However, they may also inadvertently expand regulatory T cells (Treg), which could seriously hamper clinical efficacy. To address this possibility, we developed a novel assay to detect antigen-specific Treg based on down-regulation of surface CD3 following TCR engagement, and used this approach to screen for Treg specific to the NY-ESO-1 tumor antigen in melanoma patients treated with the NY-ESO-1/ISCOMATRIX™ cancer vaccine. All patients tested had Treg (CD25(bright) FoxP3(+) CD127(neg)) specific for at least one NY-ESO-1 epitope in the blood. Strikingly, comparison with pre-treatment samples revealed that many of these responses were induced or boosted by vaccination. The most frequently detected response was toward the HLA-DP4-restricted NY-ESO-1(157-170) epitope, which is also recognized by effector T cells. Notably, functional Treg specific for an HLA-DR-restricted epitope within the NY-ESO-1(115-132) peptide were also identified at high frequency in tumor tissue, suggesting that NY-ESO-1-specific Treg may suppress local anti-tumor immune responses. Together, our data provide compelling evidence for the ability of a cancer vaccine to expand tumor antigen-specific Treg in the setting of advanced cancer, a finding which should be given serious consideration in the design of future cancer vaccine clinical trials.

  11. Immune escape from NY-ESO-1-specific T-cell therapy via loss of heterozygosity in the MHC.

    PubMed

    Klippel, Z K; Chou, J; Towlerton, A M; Voong, L N; Robbins, P; Bensinger, W I; Warren, E H

    2014-03-01

    Adoptive immunotherapy of tumors with T cells specific for the cancer-testis antigen NY-ESO-1 has shown great promise in preclinical models and in early stage clinical trials. Tumor persistence or recurrence after NY-ESO-1-specific therapy occurs, however, and the mechanisms of recurrence remain poorly defined. In a murine xenograft model of NY-ESO-1(+) multiple myeloma, we observed tumor recurrence after adoptive transfer of CD8(+) T cells genetically redirected to the prototypic NY-ESO-1157-165 peptide presented by HLA-A*02:01. Analysis of the myeloma cells that had escaped from T-cell control revealed intact expression of NY-ESO-1 and B2M, but selective, complete loss of HLA-A*02:01 expression from the cell surface. Loss of heterozygosity (LOH) in the major histocompatibility complex (MHC) involving the HLA-A locus was identified in the tumor cells, and further analysis revealed selective loss of the allele encoding HLA-A*02:01. Although LOH involving the MHC has not been described in myeloma patients with persistent or recurrent disease after immune therapies such as allogeneic hematopoietic cell transplantation (HCT), it has been described in patients with acute myelogenous leukemia who relapsed after allogeneic HCT. These results suggest that MHC loss should be evaluated in patients with myeloma and other cancers who relapse after adoptive NY-ESO-1-specific T-cell therapy.

  12. MHC class II/ESO tetramer-based generation of in vitro primed anti-tumor T-helper lines for adoptive cell therapy of cancer.

    PubMed

    Poli, Caroline; Raffin, Caroline; Dojcinovic, Danijel; Luescher, Immanuel; Ayyoub, Maha; Valmori, Danila

    2013-02-01

    Generation of tumor-antigen specific CD4(+) T-helper (T(H)) lines through in vitro priming is of interest for adoptive cell therapy of cancer, but the development of this approach has been limited by the lack of appropriate tools to identify and isolate low frequency tumor antigen-specific CD4(+) T cells. Here, we have used recently developed MHC class II/peptide tetramers incorporating an immunodominant peptide from NY-ESO-1 (ESO), a tumor antigen frequently expressed in different human solid and hematologic cancers, to implement an in vitro priming platform allowing the generation of ESO-specific T(H) lines. We isolated phenotypically defined CD4(+) T-cell subpopulations from circulating lymphocytes of DR52b(+) healthy donors by flow cytometry cell sorting and stimulated them in vitro with peptide ESO(119-143), autologous APC and IL-2. We assessed the frequency of ESO-specific cells in the cultures by staining with DR52b/ESO(119-143) tetramers (ESO-tetramers) and TCR repertoire of ESO-tetramer(+) cells by co-staining with TCR variable β chain (BV) specific antibodies. We isolated ESO-tetramer(+) cells by flow cytometry cell sorting and expanded them with PHA, APC and IL-2 to generate ESO-specific T(H) lines. We characterized the lines for antigen recognition, by stimulation with ESO peptide or recombinant protein, cytokine production, by intracellular staining using specific antibodies, and alloreactivity, by stimulation with allo-APC. Using this approach, we could consistently generate ESO-tetramer(+) T(H) lines from conventional CD4(+)CD25(-) naïve and central memory populations, but not from effector memory populations or CD4(+)CD25(+) Treg. In vitro primed T(H) lines recognized ESO with affinities comparable to ESO-tetramer(+) cells from patients immunized with an ESO vaccine and used a similar TCR repertoire. In this study, using MHC class II/ESO tetramers, we have implemented an in vitro priming platform allowing the generation of ESO

  13. Induction of CD8 T-cell responses restricted to multiple HLA class I alleles in a cancer patient by immunization with a 20-mer NY-ESO-1f (NY-ESO-1 91-110) peptide.

    PubMed

    Eikawa, Shingo; Kakimi, Kazuhiro; Isobe, Midori; Kuzushima, Kiyotaka; Luescher, Immanuel; Ohue, Yoshihiro; Ikeuchi, Kazuhiro; Uenaka, Akiko; Nishikawa, Hiroyoshi; Udono, Heiichiro; Oka, Mikio; Nakayama, Eiichi

    2013-01-15

    Immunogenicity of a long 20-mer NY-ESO-1f peptide vaccine was evaluated in a lung cancer patient TK-f01, immunized with the peptide with Picibanil OK-432 and Montanide ISA-51. We showed that internalization of the peptide was necessary to present CD8 T-cell epitopes on APC, contrasting with the direct presentation of the short epitope. CD8 T-cell responses restricted to all five HLA class I alleles were induced in the patient after the peptide vaccination. Clonal analysis showed that B*35:01 and B*52:01-restricted CD8 T-cell responses were the two dominant responses. The minimal epitopes recognized by A*24:02, B*35:01, B*52:01 and C*12:02-restricted CD8 T-cell clones were defined and peptide/HLA tetramers were produced. NY-ESO-1 91-101 on A*24:02, NY-ESO-1 92-102 on B*35:01, NY-ESO-1 96-104 on B*52:01 and NY-ESO-1 96-104 on C*12:02 were new epitopes first defined in this study. Identification of the A*24:02 epitope is highly relevant for studying the Japanese population because of its high expression frequency (60%). High affinity CD8 T-cells recognizing tumor cells naturally expressing the epitopes and matched HLA were induced at a significant level. The findings suggest the usefulness of a long 20-mer NY-ESO-1f peptide harboring multiple CD8 T-cell epitopes as an NY-ESO-1 vaccine. Characterization of CD8 T-cell responses in immunomonitoring using peptide/HLA tetramers revealed that multiple CD8 T-cell responses comprised the dominant response.

  14. Definition of key variables for the induction of optimal NY-ESO-1-specific T cells in HLA transgene mice.

    PubMed

    Johannsen, Alexandre; Genolet, Raphaël; Legler, Daniel F; Luther, Sanjiv A; Luescher, Immanuel F

    2010-09-15

    An attractive treatment of cancer consists in inducing tumor-eradicating CD8(+) CTL specific for tumor-associated Ags, such as NY-ESO-1 (ESO), a strongly immunogenic cancer germ line gene-encoded tumor-associated Ag, widely expressed on diverse tumors. To establish optimal priming of ESO-specific CTL and to define critical vaccine variables and mechanisms, we used HLA-A2/DR1 H-2(-/-) transgenic mice and sequential immunization with immunodominant DR1- and A2-restricted ESO peptides. Immunization of mice first with the DR1-restricted ESO(123-137) peptide and subsequently with mature dendritic cells (DCs) presenting this and the A2-restriced ESO(157-165) epitope generated abundant, circulating, high-avidity primary and memory CD8(+) T cells that efficiently killed A2/ESO(157-165)(+) tumor cells. This prime boost regimen was superior to other vaccine regimes and required strong Th1 cell responses, copresentation of MHC class I and MHC class II peptides by the same DC, and resulted in upregulation of sphingosine 1-phosphate receptor 1, and thus egress of freshly primed CD8(+) T cells from the draining lymph nodes into circulation. This well-defined system allowed detailed mechanistic analysis, which revealed that 1) the Th1 cytokines IFN-gamma and IL-2 played key roles in CTL priming, namely by upregulating on naive CD8(+) T cells the chemokine receptor CCR5; 2) the inflammatory chemokines CCL4 (MIP-1beta) and CCL3 (MIP-1alpha) chemoattracted primed CD4(+) T cells to mature DCs and activated, naive CD8(+) T cells to DC-CD4 conjugates, respectively; and 3) blockade of these chemokines or their common receptor CCR5 ablated priming of CD8(+) T cells and upregulation of sphingosine 1-phosphate receptor 1. These findings provide new opportunities for improving T cell cancer vaccines.

  15. Combination of autoantibodies against NY-ESO-1 and viral capsid antigen immunoglobulin A for improved detection of nasopharyngeal carcinoma.

    PubMed

    Peng, Yu-Hui; Xu, Yi-Wei; Qiu, Si-Qi; Hong, Chao-Qun; Zhai, Tian-Tian; Li, En-Min; Xu, Li-Yan

    2014-09-01

    Nasopharyngeal carcinoma (NPC) is one of the most common malignant tumors in Southern China and Southeast Asia, and early detection remains a challenge. Autoantibodies have been found to precede the manifestations of symptomatic cancer by several months to years, making their identification of particular relevance for early detection. In the present study, the diagnostic value of serum autoantibodies against NY-ESO-1 in NPC patients was evaluated. The study included 112 patients with NPC and 138 normal controls. Serum levels of autoantibodies against NY-ESO-1 and classical Epstein-Barr virus marker, viral capsid antigen immunoglobulin A (VCA-IgA), were measured by enzyme-linked immunosorbent assay. Measurement of autoantibodies against NY-ESO-1 and VCA-IgA demonstrated a sensitivity/specificity of 42.9/94.9% [95% confidence interval (CI), 33.7-52.6/89.4-97.8%] and 55.4/95.7% (95% CI, 45.7-64.7/90.4-98.2%), respectively. The area under receiver operating characteristic curve for autoantibodies against NY-ESO-1 (0.821; 95% CI, 0.771-0.871) was marginally lower than that for VCA-IgA (0.860; 95% CI, 0.810-0.910) in NPC. The combination of autoantibodies against NY-ESO-1 and VCA-IgA yielded an enhanced sensitivity of 80.4% (95% CI, 71.6-87.0%) and a specificity of 90.6% (95% CI, 84.1-94.7%). Moreover, detection of autoantibodies against NY-ESO-1 could differentiate early-stage NPC patients from normal controls. Our results suggest that autoantibodies against NY-ESO-1 may serve as a potential biomarker, as a supplement to VCA-IgA, for the screening and diagnosis of NPC.

  16. ESA/ESO collaboration to track potentially threatening near-Earth objects

    NASA Astrophysics Data System (ADS)

    Hainaut, O.; Koschny, D.; Micheli, M.

    2014-07-01

    A collaboration has been set up between ESA and ESO, within the global effort by the United Nations and its Committee on the Peaceful Uses of Outer Space (UN-COPUOS). The UN-COPUOS Action Team 14 put forward recommendations for an international response to the near-Earth-object (NEO) impact threat to form an International Asteroid Warning Network, which the UN General Assembly approved in October 2013. The NEO Segment of ESA's Space Situational Awareness (SSA) aims to coordinate and combine information from different sources, and analyse them to predict possible impacts with the Earth, and assess danger, and analyse possible mitigations, including the deflection of a menacing asteroid. With the VLT, ESO's capabilities to observe very faint (but still threatening) NEOs complement ESA's efforts to discover and track these objects. The ESA/ESO campaign focuses on faint objects, with a high value on the Palermo scale, which cannot be observed with smaller telescopes, and on recently discovered NEOs, which are rapidly fading below the detection threshold for smaller telescopes before their orbit can be secured. Technically, the campaign is implemented as a 'Target of Opportunity'' program, in which observations can be queued on VLT's UT1 with FORS at short notice. The first observations targeted 2009 FD, which had been ranked among the top five objects on the NEODyS Risk List. The VLT observations, processed by the European NEODyS system and the JPL-based Sentry system, decreased its Palermo index from -1.8 to -2.6. The campaign currently has a telescope time credit corresponding to 15--20 recoveries per year.

  17. Report on the ESO-ESA Workshop ''Science Operations 2015: Science Data Management''

    NASA Astrophysics Data System (ADS)

    Romaniello, M.; Arviset, C.; Leibundgut, B.; Lennon, D.; Sterzik, M.

    2016-03-01

    During four intense days, more than 100 astronomers, software engineers, science operation and data management experts gathered for the second installment of the ESO-ESA workshop series “Science Operations: Working together in support of science”. Two years ago, the inaugural meeting of the series at the European Space Astronomy Centre in Madrid provided an overview of all of the different aspects of Science Operations. This year’s gathering was focused on science data management, and an overview of the presentations and a summary of the discussions is provided.

  18. Chemical tagging with Gaia-ESO Survey and Gaia-RVS data

    NASA Astrophysics Data System (ADS)

    Guiglion, G.; Recio-Blanco, A.; de Laverny, P.

    2014-01-01

    We present a new method devoted to chemical tagging for Galactic Archeology. In the context of the Gaia-ESO Survey (GES) and the Gaia Data Processing and Analysis Consortium (DPAC), we aim at preparing the Gaia-Radial Velocity Spectrograph analysis, which will provide ~ 2×106 spectra covering the IR CaII triplet domain (R ~ 11 500), with sufficient SNR to perform chemical tagging. Our method will be integrated in the Gaia DPAC Apsis pipeline (CU8, Astrophysical Parameters) and we test it with GES GIRAFFE spectra (MEDUSA mode, HR10 & HR21) deriving abundances of MgI in 168 stars.

  19. ASASSN-16jt: Discovery of A Probable Supernova in ESO 344-G 021

    NASA Astrophysics Data System (ADS)

    Brimacombe, J.; Brown, J. S.; Stanek, K. Z.; Holoien, T. W.-S.; Kochanek, C. S.; Shields, J.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Bose, S.; Chen, Ping; Krannich, G.; Masi, G.; Nicholls, B.; Nicolas, J.; Post, R. S.; Stone, G.

    2016-08-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 344-G 021. ASASSN-16jt was discovered in images obtained on UT 2016-08-31.09 at V~16.2 mag. We do not detect (V > 17.8) the object in images taken on UT 2016-08-26.24 and before.

  20. New Results from the McDonald Observatory and ESO/VLT Planet Surveys

    NASA Astrophysics Data System (ADS)

    Endl, M.; Cochran, W. D.; Kürster, M.; Wittenmyer, R. A.; Bean, J. L.

    We discuss the current status of our precision radial velocity surveys at the Hobby-Eberly Telescope (HET) and 2.7 m telescope at McDonald Observatory, as well as at the ESO/VLT in the southern hemisphere. With the HET we have just detected a planetary system, consisting of 2 Jovian-type planets, around a very metal-poor star ([Fe/H] = -0.68). Furthermore, using the VLT data for Barnard's star and Proxima Cen we will demonstrate that our current sensitivity for low-mass planets around mid M dwarfs (M4-M5V) approaches 1 Earth mass.

  1. Gaia benchmark stars and their twins in the Gaia-ESO Survey

    NASA Astrophysics Data System (ADS)

    Jofré, P.

    2016-09-01

    The Gaia benchmark stars are stars with very precise stellar parameters that cover a wide range in the HR diagram at various metallicities. They are meant to be good representative of typical FGK stars in the Milky Way. Currently, they are used by several spectroscopic surveys to validate and calibrate the methods that analyse the data. I review our recent activities done for these stars. Additionally, by applying our new method to find stellar twins on the Gaia-ESO Survey, I discuss how good representatives of Milky Way stars the benchmark stars are and how they distribute in space.

  2. Measurement of serum antibodies against NY-ESO-1 by ELISA: A guide for the treatment of specific immunotherapy for patients with advanced colorectal cancer.

    PubMed

    Long, Yan-Yan; Wang, Yu; Huang, Qian-Rong; Zheng, Guang-Shun; Jiao, Shun-Chang

    2014-10-01

    NY-ESO-1 has been identified as one of the most immunogenic antigens; thus, is a highly attractive target for cancer immunotherapy. The present study analyzed the expression of serum antibodies (Abs) against NY-ESO-1 in patients with advanced colorectal cancer (CRC), with the aim of guiding the treatment of NY-ESO-1-based specific-immunotherapy for these patients. Furthermore, the present study was the first to evaluate the kinetic expression of anti-NY-ESO-1 Abs and investigate the possible influencing factors. A total of 239 serum samples from 155 pathologically confirmed patients with advanced CRC (stages III and IV) were collected. The presence of spontaneous Abs against NY-ESO-1 was analyzed using an enzyme-linked immunosorbent assay (ELISA). The results demonstrated that 24.5% (38/155) of the investigated patients were positive for NY-ESO-1-specific Abs. No statistically significant correlations were identified between the expression of anti-NY-ESO-1 Abs and clinicopathological parameters, including age and gender, location, grading, local infiltration, lymph node status, metastatic status and K-ras mutation status (P>0.05). In 59 patients, the kinetic expression of anti-NY-ESO-1 Abs was analyzed, of which 14 patients were initially positive and 45 patients were initially negative. Notably, 16/59 (27.1%) patients changed their expression status during the study period, and the initially positive patients were more likely to change compared with the initially negative patients (85.7 vs. 8.8%; P<0.001). Therefore, monitoring serum Abs against NY-ESO-1 by ELISA is an easy and feasible method. The high expression rate of NY-ESO-1-specific Abs in CRC patients indicates that measuring the levels of serum Abs against NY-ESO-1 may guide the treatment of NY-ESO-1-based specific immunotherapy for patients with advanced CRC.

  3. ESO's VLT Helps ESA's Rosetta Spacecraft Prepare to Ride on a Cosmic Bullet

    NASA Astrophysics Data System (ADS)

    2002-02-01

    New Images of Comet Wirtanen's Nucleus [1] Summary New images of Comet Wirtanen's 1-km 'dirty snowball' nucleus have been obtained with the ESO Very Large Telescope at Paranal (Chile). They show this object at a distance of approx. 435 million km from the Sun, about the same as when the Rosetta spacecraft of the European Space Agency (ESA) arrives in 2011. The new observations indicate that the comet has a very low degree of activity at this point in its orbit - almost no material is seen around the nucleus. This means that there will not be so much dust near the nucleus as to make the planned landing dramatically difficult. PR Photo 06a/02 : The Nucleus of Comet Wirtanen (composite photo). PR Photo 06b/02 : Comet Wirtanen's motion in the sky (animated). A distant target ESO PR Photo 06a/02 ESO PR Photo 06a/02 [Preview - JPEG: 400 x 445 pix - 120k] [Normal - JPEG: 800 x 890 pix - 1.1M] ESO PR Photo 06b/02 ESO PR Photo 06b/02 [Animated GIF: 400 x 420 pix - 312k] Caption : PR Photo 06a/02 shows a (false-colour) composite image of the nucleus of Comet Wirtanen (the point of light at the centre), recorded on December 9, 2001, with the FORS2 multi-mode instrument at the 8.2-m VLT YEPUN Unit Telescope. It is based on four exposures and since the telescope was set to track the motion of the comet in the sky, the images of stars in the field are seen as four consecutive trails. The measured brightness and the fact that the image of the comet's 'dirty snowball' nucleus is almost star-like indicates that it is surrounded by a very small amount of gas or dust. The diameter of the nucleus is about 1 km and the distance to the comet from the Earth was approx. 534 million km. In PR Photo 06b/02 , the four exposures have been combined to show the motion of the comet during the four exposures. Technical information about the photos is available below. Chase a fast-moving comet, land on it and 'ride' it while it speeds up towards the Sun: not the script of a science-fiction movie

  4. Recombinant Lactobacillus plantarum induces immune responses to cancer testis antigen NY-ESO-1 and maturation of dendritic cells.

    PubMed

    Mobergslien, Anne; Vasovic, Vlada; Mathiesen, Geir; Fredriksen, Lasse; Westby, Phuong; Eijsink, Vincent G H; Peng, Qian; Sioud, Mouldy

    2015-01-01

    Given their safe use in humans and inherent adjuvanticity, Lactic Acid Bacteria may offer several advantages over other mucosal delivery strategies for cancer vaccines. The objective of this study is to evaluate the immune responses in mice after oral immunization with Lactobacillus (L) plantarum WCFS1 expressing a cell-wall anchored tumor antigen NY-ESO-1. And to investigate the immunostimulatory potency of this new candidate vaccine on human dendritic cells (DCs). L. plantarum displaying NY-ESO-1 induced NY-ESO-1 specific antibodies and T-cell responses in mice. By contrast, L. plantarum displaying conserved proteins such as heat shock protein-27 and galectin-1, did not induce immunity, suggesting that immune tolerance to self-proteins cannot be broken by oral administration of L. plantarum. With respect to immunomodulation, immature DCs incubated with wild type or L. plantarum-NY-ESO-1 upregulated the expression of co-stimulatory molecules and secreted a large amount of interleukin (IL)-12, TNF-α, but not IL-4. Moreover, they upregulated the expression of immunosuppressive factors such as IL-10 and indoleamine 2,3-dioxygenase. Although L. plantarum-matured DCs expressed inhibitory molecules, they stimulated allogeneic T cells in-vitro. Collectively, the data indicate that L. plantarum-NY-ESO-1 can evoke antigen-specific immunity upon oral administration and induce DC maturation, raising the potential of its use in cancer immunotherapies.

  5. The Gaia-ESO Survey: the selection function of the Milky Way field stars

    NASA Astrophysics Data System (ADS)

    Stonkutė, E.; Koposov, S. E.; Howes, L. M.; Feltzing, S.; Worley, C. C.; Gilmore, G.; Ruchti, G. R.; Kordopatis, G.; Randich, S.; Zwitter, T.; Bensby, T.; Bragaglia, A.; Smiljanic, R.; Costado, M. T.; Tautvaišienė, G.; Casey, A. R.; Korn, A. J.; Lanzafame, A. C.; Pancino, E.; Franciosini, E.; Hourihane, A.; Jofré, P.; Lardo, C.; Lewis, J.; Magrini, L.; Monaco, L.; Morbidelli, L.; Sacco, G. G.; Sbordone, L.

    2016-07-01

    The Gaia-ESO Survey was designed to target all major Galactic components (i.e. bulge, thin and thick discs, halo and clusters), with the goal of constraining the chemical and dynamical evolution of the Milky Way. This paper presents the methodology and considerations that drive the selection of the targeted, allocated and successfully observed Milky Way field stars. The detailed understanding of the survey construction, specifically the influence of target selection criteria on observed Milky Way field stars is required in order to analyse and interpret the survey data correctly. We present the target selection process for the Milky Way field stars observed with Very Large Telescope/Fibre Large Array Multi Element Spectrograph and provide the weights that characterize the survey target selection. The weights can be used to account for the selection effects in the Gaia-ESO Survey data for scientific studies. We provide a couple of simple examples to highlight the necessity of including such information in studies of the stellar populations in the Milky Way.

  6. ESO Signs Largest-Ever European Industrial Contract For Ground-Based Astronomy Project ALMA

    NASA Astrophysics Data System (ADS)

    2005-12-01

    ESO, the European Organisation for Astronomical Research in the Southern Hemisphere, announced today that it has signed a contract with the consortium led by Alcatel Alenia Space and composed also of European Industrial Engineering (Italy) and MT Aerospace (Germany), to supply 25 antennas for the Atacama Large Millimeter Array (ALMA) project, along with an option for another seven antennas. The contract, worth 147 million euros, covers the design, manufacture, transport and on-site integration of the antennas. It is the largest contract ever signed in ground-based astronomy in Europe. The ALMA antennas present difficult technical challenges, since the antenna surface accuracy must be within 25 microns, the pointing accuracy within 0.6 arc seconds, and the antennas must be able to be moved between various stations on the ALMA site. This is especially remarkable since the antennas will be located outdoor in all weather conditions, without any protection. Moreover, the ALMA antennas can be pointed directly at the Sun. ALMA will have a collecting area of more than 5,600 square meters, allowing for unprecedented measurements of extremely faint objects. The signing ceremony took place on December 6, 2005 at ESO Headquarters in Garching, Germany. "This contract represents a major milestone. It allows us to move forward, together with our American and Japanese colleagues, in this very ambitious and unique project," said ESO's Director General, Dr. Catherine Cesarsky. "By building ALMA, we are giving European astronomers access to the world's leading submillimetre facility at the beginning of the next decade, thereby fulfilling Europe's desire to play a major role in this field of fundamental research." Pascale Sourisse, Chairman and CEO of Alcatel Alenia Space, said: "We would like to thank ESO for trusting us to take on this new challenge. We are bringing to the table not only our recognized expertise in antenna development, but also our long-standing experience in

  7. Introducing CUBES: the Cassegrain U-band Brazil-ESO spectrograph

    NASA Astrophysics Data System (ADS)

    Bristow, Paul; Barbuy, Beatriz; Macanhan, Vanessa B.; Castilho, Bruno; Dekker, Hans; Delabre, Bernard; Diaz, Marcos; Gneiding, Clemens; Kerber, Florian; Kuntschner, Harald; La Mura, Giovanni; Reiss, Roland; Vernet, J.

    2014-07-01

    CUBES is a high-efficiency, medium-resolution (R ≃ 20, 000) spectrograph dedicated to the "ground based UV" (approximately the wavelength range from 300 to 400nm) destined for the Cassegrain focus of one of ESO's VLT unit telescopes in 2018/19. The CUBES project is a joint venture between ESO and Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG) at the Universidade de São Paulo and the Brazilian Laboratório Nacional de Astrofísica (LNA). CUBES will provide access to a wealth of new and relevant information for stellar as well as extra-galactic sources. Principle science cases include the study of heavy elements in metal-poor stars, the direct determination of carbon, nitrogen and oxygen abundances by study of molecular bands in the UV range and the determination of the Beryllium abundance as well as the study of active galactic nuclei and the inter-galactic medium. With a streamlined modern instrument design, high efficiency dispersing elements and UV-sensitive detectors, it will enable a significant gain in sensitivity over existing ground based medium-high resolution spectrographs enabling vastly increased sample sizes accessible to the astronomical community. We present here a brief overview of the project, introducing the science cases that drive the design and discussing the design options and technological challenges.

  8. The Gaia-ESO Survey: Metal-rich Bananas in the Bulge

    NASA Astrophysics Data System (ADS)

    Williams, Angus A.; Evans, N. W.; Molloy, Matthew; Kordopatis, Georges; Smith, M. C.; Shen, J.; Gilmore, G.; Randich, S.; Bensby, T.; Francois, P.; Koposov, S. E.; Recio-Blanco, A.; Bayo, A.; Carraro, G.; Casey, A.; Costado, T.; Franciosini, E.; Hourihane, A.; de Laverny, P.; Lewis, J.; Lind, K.; Magrini, L.; Monaco, L.; Morbidelli, L.; Sacco, G. G.; Worley, C.; Zaggia, S.; Mikolaitis, Š.

    2016-06-01

    We analyze the kinematics of ˜2000 giant stars in the direction of the Galactic bulge, extracted from the Gaia-ESO survey in the region -10^\\circ ≲ {\\ell }≲ 10^\\circ and -11^\\circ ≲ b≲ -3^\\circ . We find distinct kinematic trends in the metal-rich ([{{M}}/{{H}}]\\gt 0) and metal-poor ([{{M}}/{{H}}]\\lt 0) stars in the data. The velocity dispersion of the metal-rich stars drops steeply with latitude, compared to a flat profile in the metal-poor stars, as has been seen previously. We argue that the metal-rich stars in this region are mostly on orbits that support the boxy–peanut shape of the bulge, which naturally explains the drop in their velocity dispersion profile with latitude. The metal-rich stars also exhibit peaky features in their line of sight velocity histograms, particularly along the minor axis of the bulge. We propose that these features are due to stars on resonant orbits supporting the boxy–peanut bulge. This conjecture is strengthened through the comparison of the minor axis data with the velocity histograms of resonant orbits generated in simulations of buckled bars. The “banana” or 2:1:2 orbits provide strongly bimodal histograms with narrow velocity peaks that resemble the Gaia-ESO metal-rich data.

  9. VizieR Online Data Catalog: Surface Photometry of ESO-Uppsala Galaxies (Lauberts+ 1989)

    NASA Astrophysics Data System (ADS)

    Lauberts, A.; Valentijn, E. A.

    2006-04-01

    The 15467 southern galaxies in this catalog were scanned from 407 blue and 407 red original ESO-Schmidt plates using a PDS microdensitometer. The galaxies were selected from the ESO-Uppsala Catalogue (VII/34). The original selection criterion was a minimum visual angular diameter of 1arcmin. The plates were calibrated using a catalog of photo- electric standards of 1700 standard galaxies transformed to a photometric standard system (Cousins) created by the authors. The result is a catalog acquired in a homogeneous fashion for all types of galaxies in various environments. The extracted parameters include radial surface brightness profiles, magnitudes at several isophotal levels, colors, color gradients, effective radius parameters, structural parameters such as axial ratios, position angles, and profile gradients. The full version of the catalog, made of 190 columns, is available as the file "esolv.fit" in FITS table format. The ascii file "esolv1.dat" contains a subset of these columns which includes those parameters listed in the printed book version. Detailed discussion of the catalog creation is given in the published book version (ISBN 3-923524-31-5) (2 data files).

  10. ESO's VLT Helps ESA's Rosetta Spacecraft Prepare to Ride on a Cosmic Bullet

    NASA Astrophysics Data System (ADS)

    2002-02-01

    New Images of Comet Wirtanen's Nucleus [1] Summary New images of Comet Wirtanen's 1-km 'dirty snowball' nucleus have been obtained with the ESO Very Large Telescope at Paranal (Chile). They show this object at a distance of approx. 435 million km from the Sun, about the same as when the Rosetta spacecraft of the European Space Agency (ESA) arrives in 2011. The new observations indicate that the comet has a very low degree of activity at this point in its orbit - almost no material is seen around the nucleus. This means that there will not be so much dust near the nucleus as to make the planned landing dramatically difficult. PR Photo 06a/02 : The Nucleus of Comet Wirtanen (composite photo). PR Photo 06b/02 : Comet Wirtanen's motion in the sky (animated). A distant target ESO PR Photo 06a/02 ESO PR Photo 06a/02 [Preview - JPEG: 400 x 445 pix - 120k] [Normal - JPEG: 800 x 890 pix - 1.1M] ESO PR Photo 06b/02 ESO PR Photo 06b/02 [Animated GIF: 400 x 420 pix - 312k] Caption : PR Photo 06a/02 shows a (false-colour) composite image of the nucleus of Comet Wirtanen (the point of light at the centre), recorded on December 9, 2001, with the FORS2 multi-mode instrument at the 8.2-m VLT YEPUN Unit Telescope. It is based on four exposures and since the telescope was set to track the motion of the comet in the sky, the images of stars in the field are seen as four consecutive trails. The measured brightness and the fact that the image of the comet's 'dirty snowball' nucleus is almost star-like indicates that it is surrounded by a very small amount of gas or dust. The diameter of the nucleus is about 1 km and the distance to the comet from the Earth was approx. 534 million km. In PR Photo 06b/02 , the four exposures have been combined to show the motion of the comet during the four exposures. Technical information about the photos is available below. Chase a fast-moving comet, land on it and 'ride' it while it speeds up towards the Sun: not the script of a science-fiction movie

  11. The Gaia-ESO Survey: Metal-rich Bananas in the Bulge

    NASA Astrophysics Data System (ADS)

    Williams, Angus A.; Evans, N. W.; Molloy, Matthew; Kordopatis, Georges; Smith, M. C.; Shen, J.; Gilmore, G.; Randich, S.; Bensby, T.; Francois, P.; Koposov, S. E.; Recio-Blanco, A.; Bayo, A.; Carraro, G.; Casey, A.; Costado, T.; Franciosini, E.; Hourihane, A.; de Laverny, P.; Lewis, J.; Lind, K.; Magrini, L.; Monaco, L.; Morbidelli, L.; Sacco, G. G.; Worley, C.; Zaggia, S.; Mikolaitis, Š.

    2016-06-01

    We analyze the kinematics of ˜2000 giant stars in the direction of the Galactic bulge, extracted from the Gaia-ESO survey in the region -10^\\circ ≲ {\\ell }≲ 10^\\circ and -11^\\circ ≲ b≲ -3^\\circ . We find distinct kinematic trends in the metal-rich ([{{M}}/{{H}}]\\gt 0) and metal-poor ([{{M}}/{{H}}]\\lt 0) stars in the data. The velocity dispersion of the metal-rich stars drops steeply with latitude, compared to a flat profile in the metal-poor stars, as has been seen previously. We argue that the metal-rich stars in this region are mostly on orbits that support the boxy-peanut shape of the bulge, which naturally explains the drop in their velocity dispersion profile with latitude. The metal-rich stars also exhibit peaky features in their line of sight velocity histograms, particularly along the minor axis of the bulge. We propose that these features are due to stars on resonant orbits supporting the boxy-peanut bulge. This conjecture is strengthened through the comparison of the minor axis data with the velocity histograms of resonant orbits generated in simulations of buckled bars. The “banana” or 2:1:2 orbits provide strongly bimodal histograms with narrow velocity peaks that resemble the Gaia-ESO metal-rich data.

  12. ESO Astronomers Detect a Galaxy at the Edge of the Universe

    NASA Astrophysics Data System (ADS)

    1995-09-01

    Starlight from the Depths of Time Four European astronomers [1] have taken advantage of the superb imaging quality of the ESO 3.5-metre New Technology Telescope (NTT) at the La Silla observatory, to detect a galaxy at an extremely large distance. They conclude that its redshift [2] is z = 4.4; thus, this galaxy is by far the most remote ever detected. In fact, it has taken its light about 90 percent of the age of the Universe to reach us, and we now observe this early object as it appeared, only 1 - 2 billion years [3] after the Universe was created in the Big Bang. Still, the galaxy contains a considerable amount of elements that must have been produced in stars. This proves that stars were formed in normal galaxies, already before this very early epoch. Galaxies in the Very Early Universe Astronomical observations during the past decade indicate that the age of the Universe is probably somewhere between 13 and 17 billion years. It is expected that further studies at the limit of available telescopes during the next years will make it possible to determine this fundamental parameter more accurately. But whatever the actual age, one of the central questions which must answered in order to understand the evolution of the Universe is the time of formation of the first stars and galaxies; its determination is accordingly a prime goal of current cosmological observations. This early process was crucial for the distribution of matter now observed, but how long after the Big Bang did it actually happen? We do not know yet. In order to cast more light on this important question, we must look back to this very early epoch by detecting and measuring objects at the largest possible distances, i.e. at the highest redshifts. However, this is extremely difficult because of the faintness of such objects and so far, progress in this fundamental research field has been slow. An Enriched Hydrogen Cloud at z = 4.4 In 1994, the ESO team obtained a high-resolution, detailed spectrum

  13. Resiquimod as an immunologic adjuvant for NY-ESO-1 protein vaccination in patients with high-risk melanoma.

    PubMed

    Sabado, Rachel Lubong; Pavlick, Anna; Gnjatic, Sacha; Cruz, Crystal M; Vengco, Isabelita; Hasan, Farah; Spadaccia, Meredith; Darvishian, Farbod; Chiriboga, Luis; Holman, Rose Marie; Escalon, Juliet; Muren, Caroline; Escano, Crystal; Yepes, Ethel; Sharpe, Dunbar; Vasilakos, John P; Rolnitzsky, Linda; Goldberg, Judith D; Mandeli, John; Adams, Sylvia; Jungbluth, Achim; Pan, Linda; Venhaus, Ralph; Ott, Patrick A; Bhardwaj, Nina

    2015-03-01

    The Toll-like receptor (TLR) 7/8 agonist resiquimod has been used as an immune adjuvant in cancer vaccines. We evaluated the safety and immunogenicity of the cancer testis antigen NY-ESO-1 given in combination with Montanide (Seppic) with or without resiquimod in patients with high-risk melanoma. In part I of the study, patients received 100 μg of full-length NY-ESO-1 protein emulsified in 1.25 mL of Montanide (day 1) followed by topical application of 1,000 mg of 0.2% resiquimod gel on days 1 and 3 (cohort 1) versus days 1, 3, and 5 (cohort 2) of a 21-day cycle. In part II, patients were randomized to receive 100-μg NY-ESO-1 protein plus Montanide (day 1) followed by topical application of placebo gel [(arm A; n = 8) or 1,000 mg of 0.2% resiquimod gel (arm B; n = 12)] using the dosing regimen established in part I. The vaccine regimens were generally well tolerated. NY-ESO-1-specific humoral responses were induced or boosted in all patients, many of whom had high titer antibodies. In part II, 16 of 20 patients in both arms had NY-ESO-1-specific CD4⁺ T-cell responses. CD8⁺ T-cell responses were only seen in 3 of 12 patients in arm B. Patients with TLR7 SNP rs179008 had a greater likelihood of developing NY-ESO-1-specific CD8⁺ responses. In conclusion, NY-ESO-1 protein in combination with Montanide with or without topical resiquimod is safe and induces both antibody and CD4⁺ T-cell responses in the majority of patients; the small proportion of CD8⁺ T-cell responses suggests that the addition of topical resiquimod to Montanide is not sufficient to induce consistent NY-ESO-1-specific CD8⁺ T-cell responses.

  14. Expression of the cancer/testis antigen NY-ESO-1 in primary and metastatic malignant melanoma (MM) - correlation with prognostic factors

    PubMed Central

    Velazquez, Elsa F.; Jungbluth, Achim A.; Yancovitz, Molly; Gnjatic, Sacha; Adams, Sylvia; O'Neill, David; Zavilevich, Kira; Albukh, Tatyana; Christos, Paul; Mazumdar, Madhu; Pavlick, Anna; Polsky, David; Shapiro, Richard; Berman, Russell; Spira, Joanna; Busam, Klaus; Osman, Iman

    2007-01-01

    Cancer/testis (CT) antigens are potential targets for cancer immunotherapy, with NY-ESO-1 being among the most immunogenic. In several clinical trials in malignant melanoma (MM) patients, NY-ESO-1 protein/peptides showed clear evidence of inducing specific immunity. However, little is known about NY-ESO-1 expression in primary and metastatic MM and its relationship to disease progression. We analyzed NY-ESO-1 expression immunohistochemically in a series of primary and metastatic MMs and its relation to prognostic parameters and survival. We studied 61 primary and 63 metastatic MM specimens (from 61 and 56 patients, respectively). The prevalence of NY-ESO-1 expression was significantly higher in metastatic versus primary tumors [18/56 (32%) versus 8/61 (13%), P = 0.015]. There was a significant association between initial stage at presentation and NY-ESO-1 expression [stage I (3.45%), stage II (9.52%) and stage III (45.45%), P = 0.0014]. Primary MMs expressing NY-ESO-1 were significantly thicker than NY-ESO-1 negative cases (median thickness 4.7 mm versus 1.53 mm respectively, P = 0.03). No significant difference was seen in overall survival. In conclusion, NY-ESO-1 is more frequently expressed in metastatic than in primary MM and its expression is associated with thicker primary lesions and a higher frequency of metastatic disease, indicative of a worse prognosis. Our study suggests that patients with metastatic MM who express NY-ESO-1 may benefit from NY-ESO-1-based immunotherapy. PMID:17625806

  15. Evaluation of LAGE-1 and NY-ESO-1 expression in multiple myeloma patients to explore possible benefits of their homology for immunotherapy.

    PubMed

    de Carvalho, Fabricio; Vettore, Andre L; Inaoka, Riguel J; Karia, Bruno; Andrade, Valéria C C; Gnjatic, Sacha; Jungbluth, Achim A; Colleoni, Gisele W B

    2011-01-20

    Due to the high homology between the LAGE-1 and NY-ESO-1 proteins, we hypothesized that an anti-NY-ESO-1 vaccine might elicit LAGE-1 immunity and hence may be effective in multiple myeloma (MM) patients with LAGE-1-positive/NY-ESO-1-negative tumors. Therefore, we set out to evaluate LAGE-1 and NY-ESO-1 mRNA and protein expression in MM patients in a bid to evaluate possible benefits of their homology for immunotherapy. LAGE-1 (a and b isoforms) and NY-ESO-1 mRNA expression was studied in 18 normal tissues and 50 bone marrow MM samples by RT-PCR. LAGE-1 and NY-ESO-1 protein expression was analyzed by immunohistochemistry (IHC) in 27 MM specimens using mAbs 219-510-23 and E978. Spontaneous serological immune response against both antigens was analyzed by ELISA in sera from 33 MM patients. LAGE-1 (a and b isoforms) was positive in 42% and NY-ESO-1 in 26% of the MM samples analyzed by RT-PCR. Both genes were found to be expressed in 18% of the cases, while at least one of the genes was found to be expressed in 50% of the cases. In LAGE-1 positive samples, 81% were positive for LAGE-1a and 19% were positive for both LAGE-1a and -1b. LAGE-1 and NY-ESO-1 protein expression could only be detected in two cases by IHC and there was a clear strong spontaneous antibody response to LAGE-1 and NY-ESO-1 in only one MM patient. In conclusion, LAGE-1a and NY-ESO-1 homology cannot be easily exploited in an anti-NY-ESO-1 vaccine given the low frequency of protein expression detected by IHC or serum analysis.

  16. Integrated NY-ESO-1 antibody and CD8+ T-cell responses correlate with clinical benefit in advanced melanoma patients treated with ipilimumab.

    PubMed

    Yuan, Jianda; Adamow, Matthew; Ginsberg, Brian A; Rasalan, Teresa S; Ritter, Erika; Gallardo, Humilidad F; Xu, Yinyan; Pogoriler, Evelina; Terzulli, Stephanie L; Kuk, Deborah; Panageas, Katherine S; Ritter, Gerd; Sznol, Mario; Halaban, Ruth; Jungbluth, Achim A; Allison, James P; Old, Lloyd J; Wolchok, Jedd D; Gnjatic, Sacha

    2011-10-01

    Ipilimumab, a monoclonal antibody against cytotoxic T lymphocyte antigen 4 (CTLA-4), has been shown to improve survival in patients with advanced metastatic melanoma. It also enhances immunity to NY-ESO-1, a cancer/testis antigen expressed in a subset of patients with melanoma. To characterize the association between immune response and clinical outcome, we first analyzed NY-ESO-1 serum antibody by ELISA in 144 ipilimumab-treated patients with melanoma and found 22 of 140 (16%) seropositive at baseline and 31 of 144 (22%) seropositive following treatment. These NY-ESO-1-seropositive patients had a greater likelihood of experiencing clinical benefit 24 wk after ipilimumab treatment than NY-ESO-1-seronegative patients (P = 0.02, relative risk = 1.8, two-tailed Fisher test). To understand why some patients with NY-ESO-1 antibody failed to experience clinical benefit, we analyzed NY-ESO-1-specific CD4(+) and CD8(+) T-cell responses by intracellular multicytokine staining in 20 NY-ESO-1-seropositive patients and found a surprising dissociation between NY-ESO-1 antibody and CD8 responses in some patients. NY-ESO-1-seropositive patients with associated CD8(+) T cells experienced more frequent clinical benefit (10 of 13; 77%) than those with undetectable CD8(+) T-cell response (one of seven; 14%; P = 0.02; relative risk = 5.4, two-tailed Fisher test), as well as a significant survival advantage (P = 0.01; hazard ratio = 0.2, time-dependent Cox model). Together, our data suggest that integrated NY-ESO-1 immune responses may have predictive value for ipilimumab treatment and argue for prospective studies in patients with established NY-ESO-1 immunity. The current findings provide a strong rationale for the clinical use of modulators of immunosuppression with concurrent approaches to favor tumor antigen-specific immune responses, such as vaccines or adoptive transfer, in patients with cancer.

  17. Hubble and ESO's VLT provide unique 3D views of remote galaxies

    NASA Astrophysics Data System (ADS)

    2009-03-01

    Astronomers have obtained exceptional 3D views of distant galaxies, seen when the Universe was half its current age, by combining the twin strengths of the NASA/ESA Hubble Space Telescope's acute eye, and the capacity of ESO's Very Large Telescope to probe the motions of gas in tiny objects. By looking at this unique "history book" of our Universe, at an epoch when the Sun and the Earth did not yet exist, scientists hope to solve the puzzle of how galaxies formed in the remote past. ESO PR Photo 10a/09 A 3D view of remote galaxies ESO PR Photo 10b/09 Measuring motions in 3 distant galaxies ESO PR Video 10a/09 Galaxies in collision For decades, distant galaxies that emitted their light six billion years ago were no more than small specks of light on the sky. With the launch of the Hubble Space Telescope in the early 1990s, astronomers were able to scrutinise the structure of distant galaxies in some detail for the first time. Under the superb skies of Paranal, the VLT's FLAMES/GIRAFFE spectrograph (ESO 13/02) -- which obtains simultaneous spectra from small areas of extended objects -- can now also resolve the motions of the gas in these distant galaxies (ESO 10/06). "This unique combination of Hubble and the VLT allows us to model distant galaxies almost as nicely as we can close ones," says François Hammer, who led the team. "In effect, FLAMES/GIRAFFE now allows us to measure the velocity of the gas at various locations in these objects. This means that we can see how the gas is moving, which provides us with a three-dimensional view of galaxies halfway across the Universe." The team has undertaken the Herculean task of reconstituting the history of about one hundred remote galaxies that have been observed with both Hubble and GIRAFFE on the VLT. The first results are coming in and have already provided useful insights for three galaxies. In one galaxy, GIRAFFE revealed a region full of ionised gas, that is, hot gas composed of atoms that have been stripped of

  18. ESO unveils an amazing, interactive, 360-degree panoramic view of the entire night sky

    NASA Astrophysics Data System (ADS)

    2009-09-01

    The first of three images of ESO's GigaGalaxy Zoom project - a new magnificent 800-million-pixel panorama of the entire sky as seen from ESO's observing sites in Chile - has just been released online. The project allows stargazers to explore and experience the Universe as it is seen with the unaided eye from the darkest and best viewing locations in the world. This 360-degree panoramic image, covering the entire celestial sphere, reveals the cosmic landscape that surrounds our tiny blue planet. This gorgeous starscape serves as the first of three extremely high-resolution images featured in the GigaGalaxy Zoom project, launched by ESO within the framework of the International Year of Astronomy 2009 (IYA2009). GigaGalaxy Zoom features a web tool that allows users to take a breathtaking dive into our Milky Way. With this tool users can learn more about many different and exciting objects in the image, such as multicoloured nebulae and exploding stars, just by clicking on them. In this way, the project seeks to link the sky we can all see with the deep, "hidden" cosmos that astronomers study on a daily basis. The wonderful quality of the images is a testament to the splendour of the night sky at ESO's sites in Chile, which are the most productive astronomical observatories in the world. The plane of our Milky Way Galaxy, which we see edge-on from our perspective on Earth, cuts a luminous swath across the image. The projection used in GigaGalaxy Zoom place the viewer in front of our Galaxy with the Galactic Plane running horizontally through the image - almost as if we were looking at the Milky Way from the outside. From this vantage point, the general components of our spiral galaxy come clearly into view, including its disc, marbled with both dark and glowing nebulae, which harbours bright, young stars, as well as the Galaxy's central bulge and its satellite galaxies. The painstaking production of this image came about as a collaboration between ESO, the renowned

  19. Comet Halley passes the halfway mark. Very distant image obtained with the ESO NTT.

    NASA Astrophysics Data System (ADS)

    1994-02-01

    Eight years after the passage of Comet Halley in early 1986, astronomers at the European Southern Observatory have succeeded in obtaining an image [1] of this famous object at a distance of no less than 2,820 million km from the Sun. The comet is now about as far away as giant planet Uranus. It recently passed the halfway mark towards the most distant point of its very elongated 76-year orbit. The image shows the 6 x 15 km avocado-shaped nucleus as an extremely faint point of light without any surrounding dust cloud. It appears that the surface is now completely frozen and the comet has ceased to emit dust and gas. This observation was made with the ESO 3.58 metre New Technology Telescope (NTT). It is by far the faintest and most distant image ever recorded of this comet. A DIFFICULT OBSERVATION The new Halley image was obtained in the course of an observational programme by a small group of astronomers [2], aimed at the investigation of distant solar system objects. The observation was difficult to perform and is close to the limit of what is possible, even with the NTT, one of the technologically most advanced astronomical telescopes. In fact, this observation may be compared to viewing a black golfball, used during a late evening game, from a distance of 12,000 km. At Halley's present, very large distance from the Sun, the intensity of the solar light is over 350 times fainter than here on Earth. The surface of the cometary nucleus is very dark; it reflects only 4 % of the infalling sunlight. The amount of light received from Halley is therefore extremely small: the recorded star-like image of the nucleus is about 160 million times fainter than the faintest star that can be seen with the unaided eye. A long exposure was needed to catch enough light to show the object; even with the very sensitive SuSI CCD camera at the NTT, the shutter had to be kept open for a total of 3 hours 45 minutes. During this time, of the order of 9000 photons from Comet Halley were

  20. Vaccination with a recombinant protein encoding the tumor-specific antigen NY-ESO-1 elicits an A2/157-165-specific CTL repertoire structurally distinct and of reduced tumor reactivity than that elicited by spontaneous immune responses to NY-ESO-1-expressing Tumors.

    PubMed

    Bioley, Gilles; Guillaume, Philippe; Luescher, Immanuel; Bhardwaj, Nina; Mears, Gregory; Old, Lloyd; Valmori, Danila; Ayyoub, Maha

    2009-01-01

    In a recent vaccination trial assessing the immunogenicity of an NY-ESO-1 (ESO) recombinant protein administered with Montanide and CpG, we have obtained evidence that this vaccine induces specific cytolytic T lymphocytes (CTL) in half of the patients. Most vaccine-induced CTLs were directed against epitopes located in the central part of the protein, between amino acids 81 and 110. This immunodominant region, however, is distinct from another ESO CTL region, 157-165, that is a frequent target of spontaneous CTL responses in A2+ patients bearing ESO tumors. In this study, we have investigated the CTL responses to ESO 157-165 in A2+ patients vaccinated with the recombinant protein. Our data indicate that after vaccination with the protein, CTL responses to ESO 157-165 are induced in some, but not all, A2+ patients. ESO 157-165-specific CTLs induced by vaccination with the ESO protein were functionally heterogeneous in terms of tumor recognition and often displayed decreased tumor reactivity as compared with ESO 157-165-specific CTLs isolated from patients with spontaneous immune responses to ESO. Remarkably, protein-induced CTLs used T-cell receptors similar to those previously isolated from patients vaccinated with synthetic ESO peptides (Vbeta4.1) and distinct from those used by highly tumor-reactive CTLs isolated from patients with spontaneous immune responses (Vbeta1.1, Vbeta8.1, and Vbeta13.1). Together, these results demonstrate that vaccination with the ESO protein elicits a repertoire of ESO 157-165-specific CTLs bearing T-cell receptors that are structurally distinct from those of CTLs found in spontaneous immune responses to the antigen and that are heterogeneous in terms of tumor reactivity, being often poorly tumor reactive.

  1. The Gaia-ESO Survey: Probes of the inner disk abundance gradient

    NASA Astrophysics Data System (ADS)

    Jacobson, H. R.; Friel, E. D.; Jílková, L.; Magrini, L.; Bragaglia, A.; Vallenari, A.; Tosi, M.; Randich, S.; Donati, P.; Cantat-Gaudin, T.; Sordo, R.; Smiljanic, R.; Overbeek, J. C.; Carraro, G.; Tautvaišienė, G.; San Roman, I.; Villanova, S.; Geisler, D.; Muñoz, C.; Jiménez-Esteban, F.; Tang, B.; Gilmore, G.; Alfaro, E. J.; Bensby, T.; Flaccomio, E.; Koposov, S. E.; Korn, A. J.; Pancino, E.; Recio-Blanco, A.; Casey, A. R.; Costado, M. T.; Franciosini, E.; Heiter, U.; Hill, V.; Hourihane, A.; Lardo, C.; de Laverny, P.; Lewis, J.; Monaco, L.; Morbidelli, L.; Sacco, G. G.; Sousa, S. G.; Worley, C. C.; Zaggia, S.

    2016-06-01

    Context. The nature of the metallicity gradient inside the solar circle (RGC < 8 kpc) is poorly understood, but studies of Cepheids and a small sample of open clusters suggest that it steepens in the inner disk. Aims: We investigate the metallicity gradient of the inner disk using a sample of inner disk open clusters that is three times larger than has previously been studied in the literature to better characterize the gradient in this part of the disk. Methods: We used the Gaia-ESO Survey (GES) [Fe/H] values and stellar parameters for stars in 12 open clusters in the inner disk from GES-UVES data. Cluster mean [Fe/H] values were determined based on a membership analysis for each cluster. Where necessary, distances and ages to clusters were determined via comparison to theoretical isochrones. Results: The GES open clusters exhibit a radial metallicity gradient of -0.10 ± 0.02 dex kpc-1, consistent with the gradient measured by other literature studies of field red giant stars and open clusters in the range RGC ~ 6-12 kpc. We also measure a trend of increasing [Fe/H] with increasing cluster age, as has also been found in the literature. Conclusions: We find no evidence for a steepening of the inner disk metallicity gradient inside the solar circle as earlier studies indicated. The age-metallicity relation shown by the clusters is consistent with that predicted by chemical evolution models that include the effects of radial migration, but a more detailed comparison between cluster observations and models would be premature. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002 and 193.B-0936. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive

  2. The Asiago-ESO/RASS QSO Survey. III. Clustering Analysis and Theoretical Interpretation

    NASA Astrophysics Data System (ADS)

    Grazian, Andrea; Negrello, Mattia; Moscardini, Lauro; Cristiani, Stefano; Haehnelt, Martin G.; Matarrese, Sabino; Omizzolo, Alessandro; Vanzella, Eros

    2004-02-01

    This is the third paper in a series describing the Asiago-ESO/RASS QSO Survey (AERQS), a project aimed at the construction of an all-sky statistically well-defined sample of relatively bright quasi-stellar objects (QSOs; B<=15) at z<=0.3. We present here the clustering analysis of the full spectroscopically identified database (392 active galactic nuclei [AGNs]). The clustering signal at 0.02ESO P66.A-0277 and ESO P67.A-0537), with the Steward Observatory in Arizona and the National Telescope Galileo (TNG) during period AO3.

  3. Agreement between the Government of the Republic of Chile and ESO for establishing a new centre for observation in Chile - ALMA

    NASA Astrophysics Data System (ADS)

    2002-12-01

    On October 21, 2002, the Minister of Foreign Affairs of the Republic of Chile, Mrs. María Soledad Alvear, and the ESO Director General, Dr. Catherine Cesarsky, signed an Agreement that authorizes ESO to establish a new centre for astronomical observation in Chile.

  4. Allorestricted T lymphocytes with a high avidity T-cell receptor towards NY-ESO-1 have potent anti-tumor activity.

    PubMed

    Krönig, Holger; Hofer, Kathrin; Conrad, Heinke; Guilaume, Philippe; Müller, Julia; Schiemann, Matthias; Lennerz, Volker; Cosma, Antonio; Peschel, Christian; Busch, Dirk H; Romero, Pedro; Bernhard, Helga

    2009-08-01

    The cancer-testis antigen NY-ESO-1 has been targeted as a tumor-associated antigen by immunotherapeutical strategies, such as cancer vaccines. The prerequisite for a T-cell-based therapy is the induction of T cells capable of recognizing the NY-ESO-1-expressing tumor cells. In this study, we generated human T lymphocytes directed against the immunodominant NY-ESO-1(157-165) epitope known to be naturally presented with HLA-A*0201. We succeeded to isolate autorestricted and allorestricted T lymphocytes with low, intermediate or high avidity TCRs against the NY-ESO-1 peptide. The avidity of the established CTL populations correlated with their capacity of lysing HLA-A2-positive, NY-ESO-1-expressing tumor cell lines derived from different origins, e.g. melanoma and myeloma. The allorestricted NY-ESO-1-specific T lymphocytes displayed TCRs with the highest avidity and best anti-tumor recognition activity. TCRs derived from allorestricted, NY-ESO-1-specific T cells may be useful reagents for redirecting primary T cells by TCR gene transfer and, therefore, may facilitate the development of adoptive transfer regimens based on TCR-transduced T cells for the treatment of NY-ESO-1-expressing hematological malignancies and solid tumors.

  5. VizieR Online Data Catalog: Gaia-ESO Survey: Halpha emission stars catalogue (Traven+, 2015)

    NASA Astrophysics Data System (ADS)

    Traven, G.; Zwitter, T.; van Eck, S.; Klutsch, A.; Bonito, R.; Lanzafame, A. C.; Alfaro, E. J.; Bayo, A.; Bragaglia, A.; Costado, M. T.; Damiani, F.; Flaccomio, E.; Frasca, A.; Hourihane, A.; Jimenez-Esteban, F.; Lardo, C.; Morbidelli, L.; Pancino, E.; Prisinzano, L.; Sacco, G. G.; Worley, C. C.

    2015-07-01

    The GES employs the VLT-UT2 FLAMES high-resolution multiobject spectrograph . FLAMES has two instruments, the higher-resolution UVES, fed by 8 fibres, and GIRAFFE, with about 130 fibres. In the present paper we concentrate on the much more numerous GIRAFFE spectra to thoroughly test our classification scheme; a similar analysis of the UVES spectra will follow later. We use only spectra obtained in the wavelength range with Hα line - HR15N setting (6470-6790Å, R=17000), for which the majority of targets selected by GES are open cluster stars. Along with ongoing GES observations, we also use all relevant ESO archive data, which are included to be analysed as part of GES. (3 data files).

  6. First Science with SAMI: A Serendipitously Discovered Galactic Wind in ESO 185-G031

    NASA Astrophysics Data System (ADS)

    Fogarty, Lisa M. R.; Bland-Hawthorn, Joss; Croom, Scott M.; Green, Andrew W.; Bryant, Julia J.; Lawrence, Jon S.; Richards, Samuel; Allen, James T.; Bauer, Amanda E.; Birchall, Michael N.; Brough, Sarah; Colless, Matthew; Ellis, Simon C.; Farrell, Tony; Goodwin, Michael; Heald, Ron; Hopkins, Andrew M.; Horton, Anthony; Jones, D. Heath; Lee, Steve; Lewis, Geraint; López-Sánchez, Ángel R.; Miziarski, Stan; Trowland, Holly; Leon-Saval, Sergio G.; Min, Seong-Sik; Trinh, Christopher; Cecil, Gerald; Veilleux, Sylvain; Kreimeyer, Kory

    2012-12-01

    We present the first scientific results from the Sydney-AAO Multi-Object IFS (SAMI) at the Anglo-Australian Telescope. This unique instrument deploys 13 fused fiber bundles (hexabundles) across a one-degree field of view allowing simultaneous spatially resolved spectroscopy of 13 galaxies. During the first SAMI commissioning run, targeting a single galaxy field, one object (ESO 185-G031) was found to have extended minor axis emission with ionization and kinematic properties consistent with a large-scale galactic wind. The importance of this result is twofold: (1) fiber bundle spectrographs are able to identify low surface brightness emission arising from extranuclear activity and (2) such activity may be more common than presently assumed because conventional multi-object spectrographs use single-aperture fibers and spectra from these are nearly always dominated by nuclear emission. These early results demonstrate the extraordinary potential of multi-object hexabundle spectroscopy in future galaxy surveys.

  7. ASASSN-16km: Discovery of A Supernova in ESO 197-G 010

    NASA Astrophysics Data System (ADS)

    Brown, J. S.; Prieto, J. L.; Ricci, C.; Oh, K.; Stanek, K. Z.; Holoien, T. W.-S.; Kochanek, C. S.; Shields, J.; Shappee, B. J.; Bersier, D.; Dong, Subo; Bose, S.; Chen, Ping; Brimacombe, J.

    2016-09-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a Type Ia supernova in the galaxy ESO 197-G 010. ASASSN-16km (AT 2016ggb) was discovered in images obtained on UT 2016-09-12.34 at V~16.3 mag. We also detect the object in images obtained on UT 2016-09-13.15 (V~16.2), UT 2016-09-10.15 (V~16.3), UT 2016-09-09.15 (V~16.6), UT 2016-09-05.110 (V~17.1), and UT 2016-09-02.41 (V~17.6).

  8. The Gaia-ESO Survey: CNO Abundances in Open Clusters of our Galaxy