Science.gov

Sample records for public eso near-ir

  1. VISTA Variables in the Via Lactea (VVV): The public ESO near-IR variability survey of the Milky Way

    NASA Astrophysics Data System (ADS)

    Minniti, D.; Lucas, P. W.; Emerson, J. P.; Saito, R. K.; Hempel, M.; Pietrukowicz, P.; Ahumada, A. V.; Alonso, M. V.; Alonso-Garcia, J.; Arias, J. I.; Bandyopadhyay, R. M.; Barbá, R. H.; Barbuy, B.; Bedin, L. R.; Bica, E.; Borissova, J.; Bronfman, L.; Carraro, G.; Catelan, M.; Clariá, J. J.; Cross, N.; de Grijs, R.; Dékány, I.; Drew, J. E.; Fariña, C.; Feinstein, C.; Fernández Lajús, E.; Gamen, R. C.; Geisler, D.; Gieren, W.; Goldman, B.; Gonzalez, O. A.; Gunthardt, G.; Gurovich, S.; Hambly, N. C.; Irwin, M. J.; Ivanov, V. D.; Jordán, A.; Kerins, E.; Kinemuchi, K.; Kurtev, R.; López-Corredoira, M.; Maccarone, T.; Masetti, N.; Merlo, D.; Messineo, M.; Mirabel, I. F.; Monaco, L.; Morelli, L.; Padilla, N.; Palma, T.; Parisi, M. C.; Pignata, G.; Rejkuba, M.; Roman-Lopes, A.; Sale, S. E.; Schreiber, M. R.; Schröder, A. C.; Smith, M.; , L. Sodré, Jr.; Soto, M.; Tamura, M.; Tappert, C.; Thompson, M. A.; Toledo, I.; Zoccali, M.; Pietrzynski, G.

    2010-07-01

    We describe the public ESO near-IR variability survey (VVV) scanning the Milky Way bulge and an adjacent section of the mid-plane where star formation activity is high. The survey will take 1929 h of observations with the 4-m VISTA telescope during 5 years (2010-2014), covering ˜10 9 point sources across an area of 520 deg 2, including 33 known globular clusters and ˜350 open clusters. The final product will be a deep near-IR atlas in five passbands (0.9-2.5 μm) and a catalogue of more than 10 6 variable point sources. Unlike single-epoch surveys that, in most cases, only produce 2-D maps, the VVV variable star survey will enable the construction of a 3-D map of the surveyed region using well-understood distance indicators such as RR Lyrae stars, and Cepheids. It will yield important information on the ages of the populations. The observations will be combined with data from MACHO, OGLE, EROS, VST, Spitzer, HST, Chandra, INTEGRAL, WISE, Fermi LAT, XMM-Newton, GAIA and ALMA for a complete understanding of the variable sources in the inner Milky Way. This public survey will provide data available to the whole community and therefore will enable further studies of the history of the Milky Way, its globular cluster evolution, and the population census of the Galactic Bulge and center, as well as the investigations of the star forming regions in the disk. The combined variable star catalogues will have important implications for theoretical investigations of pulsation properties of stars.

  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. 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.

  9. 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.

  10. Near-IR Spectroscopy of CEMP Stars with SOAR/OSIRIS

    NASA Astrophysics Data System (ADS)

    Kennedy, Catherine R.; Sivarani, Thirupathi; Beers, Timothy C.; Rossi, Silvia; Placco, Vinicius M.; Johnson, J.; Masseron, T.

    2010-03-01

    We report on medium-resolution near-IR spectroscopy of a sample of over 60 Carbon-Enhanced Metal-Poor (CEMP) stars observed with SOAR/OSIRIS, selected from the HK survey of Beers and colleagues and the Hamburg/ESO Survey of Christlieb and colleagues. Oxygen abundances from the molecular CO lines as well as rough estimates of 12C/13C ratios are estimated from the near-IR spectra of these stars. Near-IR model spectra with varying oxygen abundances, in combination with previously determined parameters from optical spectra are used for the estimation of abundances for this sample. As both oxygen abundances and 12C/13C ratios are tracers of nucleosynthesis, we hope to gain information about Galactic nucleosynthesis through the analysis of this sample.

  11. Report on the ESO-ESA-IAU Conference Communicating Astronomy with the Public 2005

    NASA Astrophysics Data System (ADS)

    Robson, I.; Christensen, L. L.

    2005-09-01

    Over one hundred astronomers, public information officers, planetarium specialists and image-processing gurus descended on ESO Garching in June for CAP 2005 - Communicating Astronomy with the Public 2005. This was the third international conference addressing astronomy outreach; the previous venues being La Palma and Washington DC. The main aim was to bring together the specialists from the various strands of astronomy undertaking outreach in the broadest sense. The four-day conference was a resounding success, much was achieved and the work of ESO was better appreciated (especially from the non- European perspective) through a tour of the facility. Some of the highlights of the local environs were much enjoyed through the conference dinner at the Deutsche Museum's aviation museum “Flugwerft Schleißheim” - (including cockpit tours of an F4 Phantom) and a splendid (and well liquid refreshed) evening at the Augustinerkeller, one of the largest Munich Biergartens.

  12. 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.

  13. 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

  14. 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.

  15. The jet of the BL Lacertae object PKS 0521-365 in the near-IR: MAD adaptive optics observations

    NASA Astrophysics Data System (ADS)

    Falomo, R.; Pian, E.; Treves, A.; Giovannini, G.; Venturi, T.; Moretti, A.; Arcidiacono, C.; Farinato, J.; Ragazzoni, R.; Diolaiti, E.; Lombini, M.; Tavecchio, F.; Brast, R.; Donaldson, R.; Kolb, J.; Marchetti, E.; Tordo, S.

    2009-07-01

    Context: BL Lac objects are low-power active nuclei exhibiting a variety of peculiar properties caused by the presence of a relativistic jet and orientation effects. Aims: We present adaptive optics near-IR images at high spatial resolution of the nearby BL Lac object PKS 0521-365, which is known to display a prominent jet both at radio and optical frequencies. Methods: The observations were obtained in Ks-band using the ESO multi-conjugated adaptive optics demonstrator at the Very Large Telescope. This allowed us to obtain images with 0.1 arcsec effective resolution. We performed a detailed analysis of the jet and its related features from the near-IR images, and combined them with images previously obtained with HST in the R band and by a re-analysis of VLA radio maps. Results: We find a remarkable similarity in the structure of the jet at radio, near-IR, and optical wavelengths. The broad-band emission of the jet knots is dominated by synchrotron radiation, while the nucleus also exhibits a significant inverse Compton component. We discovered the near-IR counterpart of the radio hotspot and found that the near-IR flux is consistent with being a synchrotron emission from radio to X-ray wavelengths. The bright red object (red-tip), detached but well aligned with the jet, is well resolved in the near-IR and has a linear light profile. Since it has no radio counterpart, we propose that it is a background galaxy not associated with the jet. Conclusions: The new adaptive optics near-IR images and previous observations at other frequencies allow us to study the complex environment around the remarkable BL Lac object PKS 0521-365. These data exemplify the capabilities of multi conjugate adaptive optics observations of extragalactic extended sources. Based on observations collected at ESO, Paranal, Chile, as part of MAD Guaranteed Time Observations.

  16. The GOODS-MUSIC sample: a multicolour catalog of near-IR selected galaxies in the GOODS-South field

    NASA Astrophysics Data System (ADS)

    Grazian, A.; Fontana, A.; de Santis, C.; Nonino, M.; Salimbeni, S.; Giallongo, E.; Cristiani, S.; Gallozzi, S.; Vanzella, E.

    2006-04-01

    Aims. We present a high quality multiwavelength (from 0.3 to 8.0 μm) catalog of the large and deep area in the GOODS Southern Field covered by the deep near-IR observations obtained with the ESO VLT. Methods. The catalog is entirely based on public data: in our analysis, we have included the F435W, F606W, F775W and F850LP ACS images, the JHKs VLT data, the Spitzer data provided by IRAC instrument (3.6, 4.5, 5.8 and 8.0 μm), and publicly available U-band data from the 2.2ESO and VLT-VIMOS. We describe in detail the procedures adopted to obtain this multiwavelength catalog. In particular, we developed a specific software for the accurate "PSF-matching" of space and ground-based images of different resolution and depth (ConvPhot), of which we analyse performances and limitations. We have included both z-selected, as well as Ks-selected objects, yielding a unique, self-consistent catalog. The largest fraction of the sample is 90% complete at z≃ 26 or Ks≃ 23.8 (AB scale). Finally, we cross-correlated our data with all the spectroscopic catalogs available to date, assigning a spectroscopic redshift to more than 1000 sources. Results. The final catalog is made up of 14 847 objects, at least 72 of which are known stars, 68 are AGNs, and 928 galaxies with spectroscopic redshift (668 galaxies with reliable redshift determination). We applied our photometric redshift code to this data set, and the comparison with the spectroscopic sample shows that the quality of the resulting photometric redshifts is excellent, with an average scatter of only 0.06. The full catalog, which we named GOODS-MUSIC (MUltiwavelength Southern Infrared Catalog), including the spectroscopic information, is made publicly available, together with the software specifically designed to this end.

  17. 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

  18. 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.

  19. 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.

  20. Near-IR Spectroscopy of CEMP Stars with SOAR/OSIRIS

    NASA Astrophysics Data System (ADS)

    Kennedy, Catherine R.; Sivarani, T.; Beers, T.; Rossi, S.; Placco, V.; Johnson, J.; Masseron, T.

    2009-01-01

    We report on medium-resolution near-IR spectroscopy of a sample of over 70 Carbon-Enhanced Metal-Poor (CEMP) stars observed with SOAR/OSIRIS, selected from the HK survey of Beers and colleagues and the Hamburg/ESO Survey of Christlieb and colleagues. Oxygen abundances from the molecular CO lines as well as 12C/13C ratios are estimated from the near-IR spectra of these stars. Near-IR model spectra with varying oxygen abundances, in combination with previously determined parameters from optical spectra, are used for the estimation of abundances for this sample. There are two categories of CEMP stars: those with neutron-capture enhancement (CEMP-s, CEMP-r, CEMP-r/s), and those without (CEMP-no). Abundance patterns of those stars with neutron-capture enhancement are posited to be the result of mass transer from AGB companion stars. The origin of the abundance patterns in CEMP-no stars is less certain. Proposed models include low-metallicity AGB mass-transfer (in which the s-process is supressed), mass loss by rapidly rotating mega metal-poor stars ([Fe/H]< -6.0), or pollution by early supernovae. As both oxygen abundances and 12C/13C ratios are tracers of nucleosynthesis, we hope to gain information about Galactic nucleosynthesis through the analysis of this sample. This work was supported in part by grants PHY 02-16783 and PHY 08-22648: Physics Frontiers Center / Joint Institute for Nuclear Astrophysics (JINA), awarded by the U.S. National Science Foundation.

  1. Filling the gap --near UV, optical and near IR extinction

    NASA Astrophysics Data System (ADS)

    Massa, Derck

    2014-10-01

    We propose a SNAP program to obtain STIS low resolution near-UV, optical and near-IR (G430L and G750L) spectra for a set of O7-B7 class III-V stars in the Galaxy and Magellanic Clouds with available IUE or HST/STIS UV spectropotometry, optical photometry and 2MASS IR photometry. Together with the existing data, the new observations will provide complete photometric and spectrophotometric coverage from 1150 to 10000 A and enable us to produce complete extinction curves from the far-UV to the near-IR, with well-determined values of R(V). The proposed set of 150 program sight lines includes the full range of interstellar extinction curve types from both the Galaxy and the Magellanic Clouds. The new data will allow us to examine variability in the near-UV through near-IR spectral regions, including the UV-optical "knee", and the "Very Broad Structure" and to verify the applicability of the near IR extinction law recently derived by Fitzpatrick and Massa (2009). We will examine the response of these features to different interstellar environments and their relationship to other curve features. These are largely unexplored aspects of the extinction curves which will provide additional constraints on the properties of interstellar grains. The curves will be derived using model atmospheres for the program stars, eliminating the need for standard stars.

  2. Near-IR imaging of cracks in teeth

    NASA Astrophysics Data System (ADS)

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

    2014-02-01

    Dental enamel is highly transparent at near-IR wavelengths and several studies have shown that these wavelengths are well suited for optical transillumination for the detection and imaging of tooth decay. We hypothesize that these wavelengths are also well suited for imaging cracks in teeth. Extracted teeth with suspected cracks were imaged at several wavelengths in the near-IR from 1300-1700-nm. Extracted teeth were also examined with optical coherence tomography to confirm the existence of suspected cracks. Several teeth of volunteers were also imaged in vivo at 1300-nm to demonstrate clinical potential. In addition we induced cracks in teeth using a carbon dioxide laser and imaged crack formation and propagation in real time using near-IR transillumination. Cracks were clearly visible using near-IR imaging at 1300-nm in both in vitro and in vivo images. Cracks and fractures also interfered with light propagation in the tooth aiding in crack identification and assessment of depth and severity.

  3. 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

  4. Chemical abundances of 11 bulge stars from high-resolution, near-IR spectra

    NASA Astrophysics Data System (ADS)

    Ryde, N.; Gustafsson, B.; Edvardsson, B.; Meléndez, J.; Alves-Brito, A.; Asplund, M.; Barbuy, B.; Hill, V.; Käufl, H. U.; Minniti, D.; Ortolani, S.; Renzini, A.; Zoccali, M.

    2010-01-01

    Context. It is debated whether the Milky Way bulge has characteristics more similar to those of a classical bulge than those of a pseudobulge. Detailed abundance studies of bulge stars are important when investigating the origin, history, and classification of the bulge. These studies provide constraints on the star-formation history, initial mass function, and differences between stellar populations. Not many similar studies have been completed because of the large distance and high variable visual extinction along the line-of-sight towards the bulge. Therefore, near-IR investigations can provide superior results. Aims: To investigate the origin of the bulge and study its chemical abundances determined from near-IR spectra for bulge giants that have already been investigated with optical spectra. The optical spectra also provide the stellar parameters that are very important to the present study. In particular, the important CNO elements are determined more accurately in the near-IR. Oxygen and other α elements are important for investigating the star-formation history. The C and N abundances are important for determining the evolutionary stage of the giants and the origin of C in the bulge. Methods: High-resolution, near-infrared spectra in the H band were recorded using the CRIRES spectrometer mounted on the Very Large Telescope. The CNO abundances are determined from the numerous molecular lines in the wavelength range observed. Abundances of the α elements Si, S, and Ti are also determined from the near-IR spectra. Results: The abundance ratios [O/Fe], [Si/Fe], and [S/Fe] are enhanced to metallicities of at least [Fe/H] = -0.3, after which they decline. This suggests that the Milky Way bulge experienced a rapid and early burst of star formation similar to that of a classical bulge. However, a similarity between the bulge trend and the trend of the local thick disk seems to be present. This similarity suggests that the bulge could have had a pseudobulge

  5. Design and adjustment of a near-IR camera system

    NASA Astrophysics Data System (ADS)

    Liu, Tingyu; Zhang, Jingxu; Li, Yapeng

    2013-01-01

    In order to achieve a large field of view for a 1.23m large telescope, the design and assembly of a near-IR telescope has been done in this paper. First, an on-axis reflected system was designed based on the optical theory. Secondly, by designing and analyzing the deformation of different support structures for the secondary mirror and the deformation of cylinder type and truss structure, the three-beam secondary mirror support structure and the truss structure were chosen. Last, the adjustment was done by a proper secondary mirror adjusting device and a proper CCD counter-rail. A test was done after the assembly and adjustment, with the result of RMS=0.10618 λ, PV=0.55362 λ(λ=632nm). It is proved that the design of the near-IR system can satisfy the requirements of the optical design and imaging according to the test result.

  6. 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

  7. 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

  8. The K20 survey. V. The evolution of the near-IR Luminosity Function

    NASA Astrophysics Data System (ADS)

    Pozzetti, L.; Cimatti, A.; Zamorani, G.; Daddi, E.; Menci, N.; Fontana, A.; Renzini, A.; Mignoli, M.; Poli, F.; Saracco, P.; Broadhurst, T.; Cristiani, S.; D'Odorico, S.; Giallongo, E.; Gilmozzi, R.

    2003-05-01

    We present the galaxy rest-frame near-IR Luminosity Function (LF) and its cosmic evolution to z ~ 1.5 based on a spectroscopic survey of a magnitude limited sample of galaxies with Ks<20 (the K20 survey, Cimatti et al. \\cite{Cimatti2002b}). The LFs have been derived in the rest-frame J and Ks bands. Their evolution is traced using three different redshift bins (zmean =~ 0.5, 1, 1.5) and comparing them to the Local near-IR Luminosity Function. The luminosity functions at different redshifts are fairly well fitted by Schechter functions at z<1.3. The faint-end of the LFs (Lnear-IR colors with near-IR luminosities, the most luminous/massive galaxies being red/old, the low-luminous galaxies being instead dominated by blue young stellar populations. We also investigate the evolution of the near-IR comoving luminosity density to z =~ 1.5, finding a slow evolution with redshift (rholambda (z)= rholambda (z=0) (1+z)beta (lambda ) with beta (J

  9. INGRID: A New Near-IR Camera for the WHT

    NASA Astrophysics Data System (ADS)

    Packham, C.

    1999-09-01

    The new near-IR camera to be operated at the WHT is now nearing completion ready for its commissioning date, now set for January 2000. INGRID (the Isaac Newton Group Red Imaging Device) was designed and partially built by the RGO and finished at the ING during the last year. At INGRID's heart is a 1024*1024 pixel HgCdTe array developed by Rockwell International Science Centre and the University of Hawaii, which features good sensitivity from 0.8 to 2.5mm.

  10. 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.

  11. IRTF Near-IR Spectroscopy of Asteroids V2.0

    NASA Astrophysics Data System (ADS)

    Bus, S. J.

    2011-08-01

    This data set contains low-resolution, near-infrared (0.8 - 2.5 micron) spectra of asteroids obtained with SpeX at the NASA Infrared Telescope Facility (IRTF) on Mauna Kea. Since it was commissioned in June 2000, SpeX has been the premier instrument for producing high quality near-IR spectra of asteroids. These spectra have been used for both taxonomic studies of asteroids, and for more detailed mineralogical and compositional investigations. This data set archives the reduced, calibrated spectra that have been published in the peer-reviewed literature, and will be regularly updated as more data become publicly available.

  12. IRTF Near-IR Spectroscopy of Asteroids V1.0

    NASA Astrophysics Data System (ADS)

    Bus, S. J.

    2009-06-01

    This data set contains low-resolution, near-infrared (0.8 - 2.5 micron) spectra of asteroids obtained with SpeX at the NASA Infrared Telescope Facility (IRTF) on Mauna Kea. Since it was commissioned in June 2000, SpeX has been the premier instrument for producing high quality near-IR spectra of asteroids. These spectra have been used for both taxonomic studies of asteroids, and for more detailed mineralogical and compositional investigations. This data set archives the reduced, calibrated spectra that have been published in the peer-reviewed literature, and will be regularly updated as more data become publicly available.

  13. Retrieval of Atmospheric CO2 Column from Ground-based Near IR Spectra of the Sun

    NASA Technical Reports Server (NTRS)

    Wennberg, Paul

    2005-01-01

    This grant has supported a graduate research assistant stipend for Zhonghua Yang, a geochemistry Ph.D. student at Caltech. In this project, we have significantly improved the retrieval of atmospheric column CO2 (and molecular oxygen) from ground-based, high resolution near-IR solar transmission spectra. This work has greatly benefited from interactions with Dr. Geoffrey Toon and Stan Sander of NASA's Jet Propulsion Laboratory and with James T. Randerson, University of California - Irvine. The results from this study are summarized in three publications, reprints of which are enclosed in with this report.

  14. 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.

  15. 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.

  16. Tunable graphene near-IR dielectric loaded waveguides

    NASA Astrophysics Data System (ADS)

    Liu, Chunlin; He, Xiaoyong; Zhao, Zhenyu; Lin, Fangting; Liu, Feng; Shi, Wangzhou

    2016-07-01

    By integrating the graphene layer with the dielectric loaded surface plasmon waveguides, the tunable propagation properties have been investigated in the near-IR region, including the influences of operation frequency, the Fermi level of the graphene layer, and dielectric layer thickness. To improve the modulation properties, multiple unit cell (graphene-Al2O3) structure has been adopted. The results manifest that as the period number of the unit cell increases, the modulation depths of the propagation properties increase obviously. For instance, the modulation depth of propagation length can reach about 80% if the Fermi level changes in the range of 0.1–0.5 eV. As frequency increases, the effective index of the hybrid mode increases, while the propagation length shows a peak. The results are very helpful in understanding the tunable mechanisms of graphene plasmonic devices and designing novel waveguide structures, e.g. resonators and modulators.

  17. On Structural Features Necessary for Near-IR-Light Photocatalysts.

    PubMed

    Wang, Gang; Huang, Baibiao; Li, Zhujie; Wang, Zeyan; Qin, Xiaoyan; Zhang, Xiaoyang; Dai, Ying; Whangbo, Myung-Hwan

    2015-09-21

    In the search for photocatalysts that can directly utilize near-IR (NIR) light, we investigated three oxides Cu3(OH)4SO4 (antlerite), Cu4(OH)6SO4, and Cu2(OH)3Cl by photodecomposing 2,4-dichlorophenol over them under NIR irradiation and by comparing their electronic structures with that of the known NIR photocatalyst Cu2(OH)PO4. Both Cu3(OH)4SO4 and Cu4(OH)6SO4 are NIR photocatalysts, but Cu2(OH)3Cl is not. Thus, in addition to the presence of two different CuOm and Cu'On polyhedra linked with Cu-O-Cu' bridges, the presence of acceptor groups (e.g., SO4, PO4) linked to the metal oxygen polyhedra is necessary for NIR photocatalysts. PMID:26235723

  18. 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).

  19. 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

  20. 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.

  1. 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

  2. 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.

  3. Saturn's Atmospheric Structure from Visible and Near-IR Observations

    NASA Astrophysics Data System (ADS)

    Chanover, N.

    1999-09-01

    The vertical structure of Saturn's atmosphere is determined using an adding-doubling code to model observed center-to-limb brightness variations. The imaging data sets consist of a) Hubble Space Telescope WF/PC and WFPC2 images taken in continuum and narrow-band methane absorption filters, and b) near-IR (1--2.5 mu m) ground-based images taken in narrow-band methane and continuum filters with the Apache Point Observatory 3.5 meter telescope. A standard two-cloud model is employed, in which layers of clear gas interleave a stratospheric haze layer, an ammonia cloud deck, and a lower, semi-infinite cloud deck. Our code, which has heretofore been used to characterize the Jovian atmosphere, has been modified to incorporate physical conditions more appropriate for Saturn. The global, longitudinally-averaged atmospheric structure as a function of latitude is discussed; vertical structure in anomalous convective regions will be presented elsewhere. This work was funded by NASA Grant NAG5-7904. Additional support was provided by NASA through grant number AR-08363.01-97A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.

  4. Near-IR Observations Of Carbon-Enhanced Metal-Poor Stars With SOAR/OSIRIS

    NASA Astrophysics Data System (ADS)

    Kennedy, Catherine R.; Sivarani, T.; Beers, T.; Lee, Y.; Rossi, S.; Placco, V.

    2007-12-01

    We report on medium-resolution near-IR spectroscopy, obtained with SOAR/OSIRIS, of a sample of over 50 Carbon-Enhanced Metal-Poor (CEMP) stars selected from the HK survey of Beers and colleagues and the Hamburg/ESO Survey of Christlieb and colleagues. These stars are primarily cool (4000 K < Teff < 5000 K), metal-poor objects with previous optical observations that indicate carbon enhancement [C/Fe] > +1.0. The observations are used, in combination with information available from optical spectra, to derive estimates of the O abundance and 12C/13C ratios from the molecular lines of CO, which are very sensitive to oxygen abundances in such stars. The results are compared with abundances determined from high-resolution observations for a subset of these stars. Based the O abundances from CO lines, we revisit the estimation of C and N abundances from optical observations. The origin of the elemental abundance pattern for CEMP stars with s-process enhancement (CEMP-s stars) is very likely to be mass transfer from (now extinct) AGB companions. However, the [C/N] and 12C/13C ratios of CEMP-s stars are very different from solar-metallicity AGB stars. The [O/Fe] measurements provide additional constraints on the mass of these AGB companions. Another class, the CEMP-no stars (CEMP stars with no n-capture enhancement), could have either been polluted by AGB mass-transfer, winds from massive stars, or early supernovae. The 12C/13C and [O/Fe] abundances are crucial to distinguish their origin, and they are not easily available through optical observations due to the weakness of the [OI] 6300 A lines. TCB, YSL, CK, and TS acknowledge support from grant PHY 02-16783; Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA), awarded by the U.S. National Science Foundation.

  5. ESO PR Highlights in 2001

    NASA Astrophysics Data System (ADS)

    2002-01-01

    The year 2001 brought further success to European Astronomy and ESO. All of the four 8.2-m Unit Telescopes of the Very Large Telescope (VLT) are now in regular use and the VLT Interferometer (VLTI) had "first fringes" early in the year. The first tests were made with two small telescopes and later the light beams from two of the large telescopes were combined. The first scientific observations proved the extraordinary stability of the complex VLTI system and already produced excellent results. The Adaptive Optics technique was introduced at the VLT when the new NAOS-CONICA instrument had "First Light" in November. The sharpest-ever VLT images were obtained and immediately demonstrated the enormous potential for exciting front-line research programmes with this new facility. An extraordinary amount of first-class data were obtained by the astronomical communities in the ESO member countries and beyond from the VLT and other ESO telescopes. They resulted in numerous new discoveries and hundreds of articles in the professional literature - some of them were also presented to the public in ESO Press Releases. Portugal became the ninth ESO member country. The UK decided to join ESO by mid-2002 and other countries expressed interest. Japan moved closer to the intercontinental ALMA project and ESO continued its concept studies for a future 100-metre optical/IR telescope (OWL). The ESO Educational Office was established in July 2001. The aim is to provide support for astronomical and astrophysical education, especially at the secondary level. The Europe-wide, EU-sponsored "Life in the Universe" educational project was successfully accomplished, in collaboration with CERN, ESA and other international research organisations. At the end of a hectic and fruitful year, ESO and its staff in Europe and Chile can be optimistic about the future. New state-of-the-art astronomical instruments will be mounted on the ESO telescopes at La Silla and Paranal in 2002, further enhancing the

  6. 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.

  7. 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.

  8. 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.

  9. 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.

  10. 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.

  11. A novel algorithm to attack the problem of pattern recognition with near-IR spectroscopy

    SciTech Connect

    Zou, Yi.

    1993-01-01

    Near-infrared (near-IR) spectroscopy is a rapid, nondestructive analytical technique that has wide application in industry as well as in academic research. In general, near-IR analysis uses reflectance or absorbance signals to determine chemical information from samples. Near-IR is also a very good technique for differentiating samples from different sources using pattern recognition analysis. In this dissertation, a novel algorithm of the quantile BEST (Boot-strap Error-adjusted Sample Technique) for pattern recognition analysis has been extensively tested with hypothetical data and real samples. A modified model is proposed to improve the system performance in higher dimensional space. The applications to real samples include: (1) the identification of the points of origin of soil samples; (2) near-IR spectrophotometric monitoring of stroke-related changes in the protein and lipid composition of whole gerbil brains; and (3) determination of cholesterol concentration in aqueous and serum samples with principal component analysis. In addition, a new laser spectroscopic system is designed and tested. This system uses Nd-YAG and dye lasers are primary sources. Powerful near-IR radiation is obtained from stimulated Raman scattering. The stability, accuracy, and precision of the system is investigated and an application to known samples is shown.

  12. 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.

  13. 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

  14. 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

  15. 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.

  16. 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.

  17. 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

  18. Electrochromic poly(acetylene)s with switchable visible/near-IR absorption characteristics.

    PubMed

    Pauly, Anja C; Varnado, C Daniel; Bielawski, Christopher W; Theato, Patrick

    2014-01-01

    Ferrocene is incorporated into a poly(acetylene) derivative via the postpolymerization amidation of a polymer precursor bearing pentafluorophenyl ester-leaving groups with aminoferrocene. While the neutral polymer exhibits a strong absorbance at 553 nm due to its conjugated backbone, oxidation of the ferrocene moieties with silver tetrafluoroborate causes the material to absorb in the near-IR (λ max ≈ 1215 nm). Subsequent reduction of the oxidized polymer with decamethylferrocene restores the initial absorbance profile, demonstrating that the material features switchable visible/near-IR absorption characteristics. PMID:23996218

  19. 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.

  20. Finland to Join ESO

    NASA Astrophysics Data System (ADS)

    2004-03-01

    Finland will become the eleventh member state of the European Southern Observatory. In a ceremony at the ESO Headquarters in Garching on 9 February 2004, an Agreement to this effect 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.

  1. 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.

  2. 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.

  3. 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.

  4. 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.

  5. Near-IR absorbing phthalocyanine derivatives as materials for organic solar cells

    NASA Astrophysics Data System (ADS)

    Mayukh, Mayank

    2011-12-01

    Phthalocyanines (Pcs) are highly conjugated synthetic porphyrin analogs that exhibit high extinction coefficients and hole mobilities, and strong pi-pi interactions. We have developed a general method for the synthesis of peripherally functionalized Pc chromophores using 'click' chemistry, wherein an alkynyl substituted Pc is reacted with an azide, providing an elegant route to the creation of a library of numerous Pcs. We have also developed a simple route to the synthesis of tri- and tetravalent metal Pc derivatives such as titanyl phthalocyanine (TiO Pc) involving solvent-free conditions. Solvent-free conditions are environmentally friendly and industrially economical, and in the present context effectively eliminate the formation of non-metallated phthalocyanine (H 2Pc), a side product often seen in other routes that interferes with their purification. We have also prepared and characterized thin-films of some of these Pcs, TiOPcs in particular, wherein we have developed an easy route to various TiO Pc polymorphs exhibiting different near-IR sensitivities via spin-coating whose optical properties are reminiscent of Phase-I and Phase-II polymorphs of the unmodified TiOPc. Phase-II is particularly interesting as it is photoelectrically active in the near-IR region with a Q-band maximum at ca. 890 nm. We have also fabricated and characterized organic solar cells in both planar heterojunction (PHJ) and bulk heterojunction (BHJ) architectures based on one of these materials, which exhibited good near-IR photoactivity with the absorption spectrum extending up to 1 micrometer in the near-IR. The incident and absorbed photon to current efficiency (IPCE and APCE) spectra showed contributions from the TiOPc in the near-IR region with local maxima around 680 nm and 920 nm, corresponding to the Frenkel and the charge-transfer (CT) bands of the TiOPc, respectively.

  6. 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

  7. 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.

  8. ESO PR Highlights in 2004

    NASA Astrophysics Data System (ADS)

    2005-01-01

    Last year proved again a wonderful one for astronomy in general and for ESO in particular. Certainly the most important astronomical event for a large public was the unique Transit of Venus : on June 8, 2004, Venus - the Earth's sister planet - passed in front of the Sun. This rare event - the last one occurred in 1882 - attracted the attention of millions of people all over the world. ESO in cooperation with several other institutes and with support from the European Commission organised through the whole year the Venus Transit 2004 (VT-2004) public education programme that successfully exposed the broad public to a number of fundamental issues at the crucial interface between society and basic science. The web site experienced a record 55 million webhits during a period of 8 hours around the transit. The programme also re-enacted the historical determination of the distance to the Sun (the "Astronomical Unit") by collecting 4550 timings of the four contacts made by more than 1500 participating group of observers and combining them in a calculation of the AU. This resulted in an astonishing accurate value of the Astronomical Unit. More details are available at the VT-2004 website, whose wealth of information will certainly make it a useful tool until the next transit in 2012! For ESO also, 2004 proved a very special year. Finland officially joined as eleventh member state and in December, the Chilean President, Ricardo Lagos, visited the Paranal Observatory. Last year was also the Fifth anniversary of the Very Large Telescope, ESO's flagship facility, as on April 1, 1999 the first 8.2-m VLT Unit Telescope, Antu (UT1), was "handed over" to the astronomers. On this occasion, ESO released several products, including a selection of the best astronomical images taken with the VLT, the VLT Top 20. But there is no doubt that the numerous high quality images published last year are all contenders to top the charts of best astronomical pictures. The year 2004 also saw many

  9. 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

  10. 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

  11. 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.

  12. ARCONS: A 2024 Pixel Optical through Near-IR Cryogenic Imaging Spectrophotometer

    NASA Astrophysics Data System (ADS)

    Mazin, B. A.; Meeker, S. R.; Strader, M. J.; Szypryt, P.; Marsden, D.; van Eyken, J. C.; Duggan, G. E.; Walter, A. B.; Ulbricht, G.; Johnson, M.; Bumble, B.; O'Brien, K.; Stoughton, C.

    2013-11-01

    We present the design, construction, and commissioning results of ARCONS, the Array Camera for Optical to Near-IR Spectrophotometry. ARCONS is the first ground-based instrument in the optical through near-IR wavelength range based on microwave kinetic inductance detectors (MKIDs). MKIDs are revolutionary cryogenic detectors, capable of detecting single photons and measuring their energy without filters or gratings, similar to an X-ray microcalorimeter. MKIDs are nearly ideal, noiseless photon detectors, as they do not suffer from read noise or dark current and have nearly perfect cosmic ray rejection. ARCONS is an integral field spectrograph (IFS) containing a lens-coupled 2024 pixel MKID array yielding a 20'' × 20'' field of view and has been deployed on the Palomar 200 inch and Lick 120 inch telescopes for 24 nights of observing. We present initial results showing that ARCONS and its MKID arrays are now a fully operational and powerful tool for astronomical observations.

  13. 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.

  14. Near IR spectra and real and imaginary indicies of refraction of ices of relevance to KBOs

    NASA Astrophysics Data System (ADS)

    Bernstein, M. P.; Mastrapa, R.; Sandford, S.

    2006-12-01

    Fitting spectra of outer Solar System bodies requires lab spectra of real mixtures at appropriate temperatures because the mathematical addition of spectra of pure materials is not equivalent to those of actual mixtures, and spectra are often temperature dependant. IR spectra of outer Solar System objects are primarily in the near-IR (i.e., below 3 microns) where reflected sunlight is greatest, but there has been a dearth of near IR spectra of ice mixtures relevant to Solar System environments, and almost no indices of refraction at all. We shall present new near IR spectra and real and imaginary indicies of amorphous and crystalline H2O at various temperatures and also H2O ice mixtures. Methane (CH4) is of interest because it is present on a number of outer Solar System objects, including Triton and Pluto, KBOs Quaoar, 90377 Sedna, 2003 UB313, and FY9 and CH4 is known to be present in a number of comets. Carbon dioxide (CO2) has been observed in many comets, the Uranian satellite Ariel, Jupiter's satellites Europa, Ganymede and Callisto, Saturn's satellites Phoebe and Iapetus etc. Since H2O is nearly ubiquitous in the outer Solar System, CH4 and CO2 on icy planetesimals is likely to come into contact with H2O, potentially changing its spectral properties. So, we shall present near IR spectra of H2O-CH4 and H2O-CO2 ice mixtures at various concentrations and temperatures. For H2O-CH4 see http://www.astrochem.org/H2OCH4.html and Bernstein, Cruikshank, and Sandford, 2006 Icarus, 181, 302-308 for more information. For H2O-CO2 mixtures, see http://www.astrochem.org/CO2H2O.html and Bernstein, Cruikshank, and Sandford 2005 Icarus, 179, 527-534. This work was supported by NASA's Planetary Geology and Geophysics program (NRA-02-OSS-01-PGG).

  15. 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).

  16. 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

  17. Polarization resolved near-IR imaging of sound and carious dental enamel

    NASA Astrophysics Data System (ADS)

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

    2011-03-01

    A thorough understanding of how polarized near-IR light is reflected from and transmitted through sound and carious dental hard tissues is important for the development of optical imaging devices. New optical imaging tools employing non-ionizing radiation are needed for the detection and assessment of dental caries. 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 is reflected from the occlusal surface or transmitted through thin sections of extracted human whole teeth. Previous near-IR imaging studies suggest that polarization imaging can be exploited to obtain higher contrast images of early dental caries due to the rapid depolarization of incident polarized light by the highly scattering areas of decay. In this study, the reflectance from tooth occlusal surfaces with demineralization and transmitted light through tooth thin sections with caries lesions were investigated. Major differences in the Mueller matrix elements were observed in both sound and demineralized enamel. This study suggests that polarization resolved optical imaging can be exploited to obtain higher contrast images of dental decay.

  18. 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/.

  19. 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

  20. 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.

  1. Interpretation of the Near-IR Spectra of the Kuiper Belt Object

    NASA Technical Reports Server (NTRS)

    Eluszkiewicz, Janusz; Cady-Pereira, Karen; Brown, Michael E.; Stansberry, John A.

    2007-01-01

    Visible and near-IR observations of the Kuiper Belt Object (136472) 2005 FY(9) have indicated the presence of unusually long (1 cm or more) optical path lengths in a layer of methane ice. Using microphysical and radiative transfer modeling, we show that even at the frigid temperatures in the outer reaches of the solar system, a slab of low porosity methane ice can indeed form by pressureless sintering of micron-sized grains, and it can qualitatively reproduce the salient features of the measured spectra. A good semiquantitative match with the near-IR spectra can be obtained with a realistic slab model, provided the spectra are scaled to a visible albedo of 0.6, at the low end of the values currently estimated from Spitzer thermal measurements. Consistent with previous modeling studies, matching spectra scaled to higher albedos requires the incorporation of strong backscattering effects. The albedo may become better constrained through an iterative application of the slab model to the analysis of the thermal measurements from Spitzer and the visible/near-IR reflectance spectra. The slab interpretation offers two falsifiable predictions (1) Absence of an opposition surge, which is commonly attributed to the fluffiness of the optical surface. This prediction is best testable with a spacecraft, as Earth-based observations at true opposition will not be possible until early next century. (2) Unlikelihood of the simultaneous occurrence of very long spectroscopic path lengths in both methane and nitrogen ice on the surface of any Kuiper Belt Object, as the more volatile nitrogen would hinder densification in methane ice.

  2. 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.

  3. 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)

  4. Remote sensing of water vapor in the near IR from EOS/MODIS

    NASA Technical Reports Server (NTRS)

    Kaufman, Yoram J.; Gao, Bo-Cai

    1992-01-01

    Consideration is given to the selection of spectral channels in the near-infrared IR which are to be employed for the derivation of total column water vapor using the MODIS instrument on the NASA's Earth Observing System. Data obtained show that the three near-IR water vapor channels on the MODIS instrument enable remote sensing of the total column water vapor with an absolute accuracy of +/- 13 percent. An absolute accuracy of +/-7 percent can be obtained if additional MODIS channels are used to decrease the effect of uncertainty in the spectral reflectance of the surface, subpixel clouds, haze, and temperature profile on the derived water vapor.

  5. 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

  6. Genetic variation near IRS1 associates with reduced adiposity and an impaired metabolic profile.

    PubMed

    Kilpeläinen, Tuomas O; Zillikens, M Carola; Stančákova, Alena; Finucane, Francis M; Ried, Janina S; Langenberg, Claudia; Zhang, Weihua; Beckmann, Jacques S; Luan, Jian'an; Vandenput, Liesbeth; Styrkarsdottir, Unnur; Zhou, Yanhua; Smith, Albert Vernon; Zhao, Jing-Hua; Amin, Najaf; Vedantam, Sailaja; Shin, So-Youn; Haritunians, Talin; Fu, Mao; Feitosa, Mary F; Kumari, Meena; Halldorsson, Bjarni V; Tikkanen, Emmi; Mangino, Massimo; Hayward, Caroline; Song, Ci; Arnold, Alice M; Aulchenko, Yurii S; Oostra, Ben A; Campbell, Harry; Cupples, L Adrienne; Davis, Kathryn E; Döring, Angela; Eiriksdottir, Gudny; Estrada, Karol; Fernández-Real, José Manuel; Garcia, Melissa; Gieger, Christian; Glazer, Nicole L; Guiducci, Candace; Hofman, Albert; Humphries, Steve E; Isomaa, Bo; Jacobs, Leonie C; Jula, Antti; Karasik, David; Karlsson, Magnus K; Khaw, Kay-Tee; Kim, Lauren J; Kivimäki, Mika; Klopp, Norman; Kühnel, Brigitte; Kuusisto, Johanna; Liu, Yongmei; Ljunggren, Osten; Lorentzon, Mattias; Luben, Robert N; McKnight, Barbara; Mellström, Dan; Mitchell, Braxton D; Mooser, Vincent; Moreno, José Maria; Männistö, Satu; O'Connell, Jeffery R; Pascoe, Laura; Peltonen, Leena; Peral, Belén; Perola, Markus; Psaty, Bruce M; Salomaa, Veikko; Savage, David B; Semple, Robert K; Skaric-Juric, Tatjana; Sigurdsson, Gunnar; Song, Kijoung S; Spector, Timothy D; Syvänen, Ann-Christine; Talmud, Philippa J; Thorleifsson, Gudmar; Thorsteinsdottir, Unnur; Uitterlinden, André G; van Duijn, Cornelia M; Vidal-Puig, Antonio; Wild, Sarah H; Wright, Alan F; Clegg, Deborah J; Schadt, Eric; Wilson, James F; Rudan, Igor; Ripatti, Samuli; Borecki, Ingrid B; Shuldiner, Alan R; Ingelsson, Erik; Jansson, John-Olov; Kaplan, Robert C; Gudnason, Vilmundur; Harris, Tamara B; Groop, Leif; Kiel, Douglas P; Rivadeneira, Fernando; Walker, Mark; Barroso, Inês; Vollenweider, Peter; Waeber, Gérard; Chambers, John C; Kooner, Jaspal S; Soranzo, Nicole; Hirschhorn, Joel N; Stefansson, Kari; Wichmann, H-Erich; Ohlsson, Claes; O'Rahilly, Stephen; Wareham, Nicholas J; Speliotes, Elizabeth K; Fox, Caroline S; Laakso, Markku; Loos, Ruth J F

    2011-08-01

    Genome-wide association studies have identified 32 loci influencing body mass index, but this measure does not distinguish lean from fat mass. To identify adiposity loci, we meta-analyzed associations between ∼2.5 million SNPs and body fat percentage from 36,626 individuals and followed up the 14 most significant (P < 10(-6)) independent loci in 39,576 individuals. We confirmed a previously established adiposity locus in FTO (P = 3 × 10(-26)) and identified two new loci associated with body fat percentage, one near IRS1 (P = 4 × 10(-11)) and one near SPRY2 (P = 3 × 10(-8)). Both loci contain genes with potential links to adipocyte physiology. Notably, the body-fat-decreasing allele near IRS1 is associated with decreased IRS1 expression and with an impaired metabolic profile, including an increased visceral to subcutaneous fat ratio, insulin resistance, dyslipidemia, risk of diabetes and coronary artery disease and decreased adiponectin levels. Our findings provide new insights into adiposity and insulin resistance. PMID:21706003

  7. X-shooter near-IR spectrograph arm: design and manufacturing methods

    NASA Astrophysics Data System (ADS)

    Navarro, Ramon; Elswijk, Eddy; de Haan, Menno; Hanenburg, Hiddo; ter Horst, Rik; Kleszcz, Pawel; Kragt, Jan; Pragt, Johan; Rigal, Florence; Roelfsema, Ronald; Schoenmaker, Ton; Tromp, Niels; Venema, Lars; Groot, Paul; Kaper, Lex

    2006-06-01

    X-shooter, the first 2nd generation VLT instrument, is a new high-efficiency echelle spectrograph. X-shooter operates at the Cassegrain focus and covers an exceptionally wide spectral range from 300 to 2500 nm in a single exposure, with an intermediate spectral resolving power R~5000. The instrument consists of a central structure and three prism cross-dispersed echelle spectrographs optimized for the UV-blue, visible and near-IR wavelength ranges. The design of the near-IR arm of the X-shooter instrument employs advanced design methods and manufacturing techniques. Integrated system design is done at cryogenic working temperatures, aiming for an almost alignment-free integration. ASTRON Extreme Light Weighting is used for high stiffness at low mass. Bare aluminium is post-polished to optical quality mirrors, preserving high shape accuracy at cryogenic conditions. Cryogenic optical mounts compensate for CTE differences of various materials, while ensuring high thermal contact. This paper addresses the general design and the application of these specialized techniques.

  8. Determination of cell culture medium components with overlapping near-IR absorbance peaks

    NASA Astrophysics Data System (ADS)

    McShane, Michael J.; Cote, Gerard L.

    1998-04-01

    A noninvasive method to measure levels of important tissue culture nutrients and metabolic by-products would provide the potential for computer control of the growth process, decreasing the amount of human attention necessary while improving efficiency and repeatability of experiments by precise maintenance of important parameters without contaminating the culture environment. Our approach to meeting this need is the development of optical sensor that extract chemical information based on the absorbance of near-IR radiation. Near-IR spectroscopy of the 2.0-2.5 micrometers region was used to collect absorbance data of aqueous mixtures containing glucose, lactate, ammonia, glutamate, and glutamine, as well as cell culture media samples from a three-day growth period. Multivariate calibration was used with these data to prove that complicated spectra can yield reasonable prediction errors. Calibration models using different combinations of spectra from aqueous mixtures and culture media were built and evaluated for glucose, ammonia, and lactate. Prediction errors of 2 percent, 8 percent, and 15 percent were obtained for glucose, lactate, and ammonia, respectively.

  9. Panchromatic Light Capture and Efficient Excitation Transfer Leading to Near-IR Emission of BODIPY Oligomers.

    PubMed

    Sharma, Ritambhara; Gobeze, Habtom B; D'Souza, Francis; Ravikanth, Mangalampalli

    2016-08-18

    All-BODIPY-based (BODIPY=boron-dipyrromethene) donor-acceptor systems capable of wide-band absorbance leading to efficient energy transfer in the near-IR region are reported. A covalently linked 3-pyrrolyl BODIPY-BODIPY dimer building block bearing an ethynyl group at the meso-aryl position is synthesized and coupled with three different monomeric BODIPY/pyrrolyl BODIPY building blocks with a bromo/iodo group under Pd(0) coupling conditions to obtain three covalently linked 3-pyrrolyl-BODIPY-based donor-acceptor oligomers in 19-29 % yield. The oligomers are characterized in detail by 1D and 2D NMR spectroscopy, high-resolution mass spectrometry, and optical spectroscopy. Due to the presence of different functionalized BODIPY derivatives in the oligomers, panchromatic light capture (300-725 nm) is witnessed. Fluorescence studies reveal singlet-singlet energy transfer from BODIPY monomer to BODIPY dimer leading to emission in the 700-800 nm range. Theoretical modeling according to the Förster mechanism predicts ultrafast energy transfer due to good spectral overlap of the donor and acceptor entities. Femtosecond transient absorption studies confirm this to be the case and thus show the relevance of the currently developed all-BODIPY-based energy-funneling supramolecular sytems with near-IR emission to solar-energy harvesting applications. PMID:27168532

  10. Near IR interband transitions and optical parameters of metal-germanium contacts.

    PubMed

    Chan, E Y; Card, H C

    1980-04-15

    A theoretical and experimental study of the zero-bias quantum efficiency eta(0) for metal (Au, Cu, Ag)-Ge Schottky barrier photodetectors in the near IR range (1.1 microm < lambda < 1.8 microm) has been performed. By an interactive computer programming technique, the optical parameters of the metal thin film electrodes (index of refraction n and extinction coefficient k) as a function of wavelength and of film thickness are determined. Starting with a two-layer calculation of the reflectance R, transmittance T, and absorptance A of the metal electrode, it is found that the eta(0) in this near IR range is dominated by the band-to-band excitation of electrons in the Ge substrate. Using the minority carrier diffusion length L(p) as an adjustable parameter, good agreement between theoretical and experimental results was found for L(p) approximately 150 microm; this value was obtained independent of choice of metal or metal thickness justifying the above procedure. PMID:20221033

  11. 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).

  12. Enhancing near IR luminescence of thiolate Au nanoclusters by thermo treatments and heterogeneous subcellular distributions.

    PubMed

    Conroy, Cecil V; Jiang, Jie; Zhang, Chen; Ahuja, Tarushee; Tang, Zhenghua; Prickett, Cherish A; Yang, Jenny J; Wang, Gangli

    2014-07-01

    A five-to-ten fold enhancement, up to ca. 5-10% quantum efficiency, of near IR luminescence from monothiolate protected gold nanoclusters was achieved by heating in the presence of excess ligand thiols. An emission maximum in the 700-900 nm range makes these Au nanoclusters superior for bioimaging applications over other emissions centered below 650 nm due to reduced background interference, albeit visible emissions could have higher quantum efficiency. The heating procedure is shown to be effective to improve the luminescence of Au nanoclusters synthesized under a variety of conditions using two types of monothiols: mercaptosuccinic acid and tiopronin. Therefore, this heating method is believed to be a generalizable approach to improve the near IR luminescence of aqueous soluble Au nanoclusters, which enables better bioimaging applications. The high quantum yield is found relatively stable over a wide pH range. PEGylation of the Au nanoclusters reduces their quantum efficiency but improves their permeation into the cytoplasm. Interestingly, z-stack confocal analysis clearly reveals the presence of Au nanoclusters inside the cell nucleus in single cell imaging. The finding addresses controversial literature reports and demonstrates the internalization and heterogeneous subcellular distributions, particularly inside the nucleus. The high luminescence intensity, small overall dimension, cell and nuclear distribution, chemical stability and low-to-non toxicity make these Au nanoclusters promising probes for broad cell dynamics and imaging applications. PMID:24879334

  13. Sidecar Asic at ESO

    NASA Astrophysics Data System (ADS)

    Dorn, Reinhold J.; Eschbaumer, Siegfried; Finger, Gert; Ives, Derek; Meyer, Manfred; Stegmeier, Joerg

    2010-07-01

    Teledyne Imaging Sensors (TIS) has developed a CMOS device known as the SIDECAR application-specific integrated circuit (ASIC). This single chip provides all the functionality of FPA drive electronics to operate visible and infrared imaging detectors with a fully digital interface. A Teledyne 2K ×2K silicon PIN diode array hybridized to a Hawaii-2RG multiplexer, the Hybrid Visible Silicon Imager (HyViSI) was read out with the ESO standard IR detector controller IRACE, which delivers detector limited performance. We have tested the H2RG HyViSI detector with the TIS SIDECAR ASIC in 32 channel readout mode at cryogenic temperatures. The SIDECAR has been evaluated down to 105 Kelvin operating temperature and performance results have been compared to those obtained with external electronics. Furthermore ESO has developed its own interface card to replace the JADE USB card provided by Teledyne. The ASIC controller is now being embedded in the ESO standard VLT hard and software environment. This paper provides an update on the recent development of the new ESO ASIC interface card. We find that the SIDECAR ASIC provides performance equal to external electronics.

  14. Perspectives for High-Energy Astrophysics at ESO.

    NASA Astrophysics Data System (ADS)

    Mainieri, V.

    2016-06-01

    Synergies between XMM-Newton and Optical-NIR facilities at ESO are proven by the large number of publications using data from the two observatories. I will review the the current synergies and highlight the future prospects along the evolution of the instrumentation plan at ESO.

  15. Volunteer Outreach Activities at ESO Chile

    NASA Astrophysics Data System (ADS)

    ESO-Chile Outreach Volunteer Team

    2012-06-01

    ESO staff in Chile are often asked to disseminate astronomical knowledge to schools and to the general public. A significant number of volunteers are now involved in these activities and the most recent projects in low-income schools and neighbourhoods are described and possible perspectives discussed.

  16. 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.

  17. 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

  18. ATLAST detector needs for direct spectroscopic biosignature characterization in the visible and near-IR

    NASA Astrophysics Data System (ADS)

    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.

    2015-09-01

    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; λ= 0.4 - 1.8 μm) 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.

  19. 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.

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

    PubMed Central

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

    2014-01-01

    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. PMID:24817803

  1. 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.

  2. UV, visible, and near-IR reflectivity data for magnetic soils/rocks from Brazil

    NASA Technical Reports Server (NTRS)

    Vempati, R. K.; Morris, R. V.; Lauer, H. V., Jr.; Coey, J. M. D.

    1991-01-01

    The objective is to obtain UV, visible, and near-IR reflectivity spectra for several magnetic Brazilian soils/rocks and compare them to corresponding data for Mars to see if these materials satisfy both magnetic and spectral constraints for Mars. Selected physical properties of the magnetic Brazilian soils/rocks are presented. In general, the spectral features resulting from ferric crystal-field transitions are much better defined in the spectra of the magnetic Brazilian soils/rocks than in Martian spectral data. Presumably, this results from a relatively higher proportion of crystalline ferric oxides for the former. The apparent masking of the spectral signature of maghemite by hematite or goethite for the Brazilian samples implies the magnetic and spectral constraints for Mars can be decoupled. That is, maghemite may be present in magnetically-significant but optically-insignificant amounts compared to crystalline hematite.

  3. Analyzing Structure in Star Forming Region AFGL 490 Using Spitzer and Near-IR Photometry

    NASA Astrophysics Data System (ADS)

    Masiunas, Lauren; Gutermuth, R.; Pipher, J.; Meyers, P.; Megeath, T.; Allen, L.

    2011-01-01

    We present an analysis of expanded Spitzer IRAC and MIPS imaging of the AFGL 490 star forming region and deep SQIID near-IR imaging of its central cluster. Using the combined 1-24 micron photometric catalog derived from these data, we have identified 56 class I and 283 class II young stellar objects (YSOs) forming in this region. We isolated several locally over-dense cluster cores from the spatial distribution of YSOs via analysis of the Minimal Spanning Tree of their positions (Gutermuth et al. 2009). The most populated group contains 215 YSOs (63% of the cluster's members) and has an area of 12 square parsecs. The intermediate mass YSO, AFGL 490, contained within this group, resides 0.73-0.98 parsecs away from the center of the group. We compare these statistics to similarly analyzed clusters (Gutermuth et al. 2009), and briefly explore the mass segregation implications of AFGL 490's position within its cluster.

  4. ARCONS: a Highly Multiplexed Superconducting UV-to-Near-IR Camera

    NASA Astrophysics Data System (ADS)

    O'Brien, Kieran; Mazin, Ben; McHugh, Sean; Meeker, Seth; Bumble, Bruce

    2012-04-01

    ARCONS, the Array Camera for Optical to Near-infrared Spectrophotometry, was recently commissioned at the coudé focus of the 200-inch Hale Telescope at the Palomar Observatory. At the heart of this unique instrument is a 1024-pixel Microwave Kinetic Inductance Detector (MKID), exploiting the Kinetic Inductance effect to measure the energy of the incoming photon to better than several percent. The ground-breaking instrument is lens-coupled with a pixel scale of 0''.23/pixel, each pixel recording the arrival time (< 2 μ sec) and energy of a photon (~10%) in the optical to near-IR (0.4-1.1 microns) range. The scientific objectives of the instrument include the rapid follow-up and classification of transient phenomena.

  5. 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

  6. 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.

  7. An Empirical Decomposition of Near-IR Emission into Galactic and Extragalactic Components

    NASA Technical Reports Server (NTRS)

    Dwek, Eli; Arendt, Richard G.

    2002-01-01

    We decompose the COBE/DIRBE observations of the near-IR sky brightness (minus zodiacal light) into Galactic stellar and interstellar medium (ISM) components and an extragalactic background. This empirical procedure allows us to estimate the 4.9 micron cosmic infrared background (CIB) as a function of the CIB intensity at shorter wavelengths. A weak indication of a rising CIB intensity at wavelengths greater than 3.5$ microns hints at interesting astrophysics in the CIB spectrum, or warns that the foreground zodiacal emission may be incompletely subtracted. Subtraction of only the stellar component from the zodiacal-light-subtracted all--sky map reveals the clearest 3.5 micron ISM emission map, which is found to be tightly correlated with the ISM emission at far-IR wavelengths.

  8. An Atomically Precise Au10 Ag2 Nanocluster with Red-Near-IR Dual Emission.

    PubMed

    Lei, Zhen; Guan, Zong-Jie; Pei, Xiao-Li; Yuan, Shang-Fu; Wan, Xian-Kai; Zhang, Jin-Yuan; Wang, Quan-Ming

    2016-08-01

    A red-near-IR dual-emissive nanocluster with the composition [Au10 Ag2 (2-py-C≡C)3 (dppy)6 ](BF4 )5 (1; 2-py-C≡C is 2-pyridylethynyl, dppy=2-pyridyldiphenylphosphine) has been synthesized. Single-crystal X-ray structural analysis reveals that 1 has a trigonal bipyramidal Au10 Ag2 core that contains a planar Au4 (2-py-C≡C)3 unit sandwiched by two Au3 Ag(dppy)3 motifs. Cluster 1 shows intense red-NIR dual emission in solution. The visible emission originates from metal-to-ligand charge transfer (MLCT) from silver atoms to phosphine ligands in the Au3 Ag(dppy)3 motifs, and the intense NIR emission is associated with the participation of 2-pyridylethynyl in the frontier orbitals of the cluster, which is confirmed by a time-dependent density functional theory (TD-DFT) calculation. PMID:27305386

  9. 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

  10. Enhancing near IR luminescence of thiolate Au nanoclusters by thermo treatments and heterogeneous subcellular distributions

    NASA Astrophysics Data System (ADS)

    Conroy, Cecil V.; Jiang, Jie; Zhang, Chen; Ahuja, Tarushee; Tang, Zhenghua; Prickett, Cherish A.; Yang, Jenny J.; Wang, Gangli

    2014-06-01

    A five-to-ten fold enhancement, up to ca. 5-10% quantum efficiency, of near IR luminescence from monothiolate protected gold nanoclusters was achieved by heating in the presence of excess ligand thiols. An emission maximum in the 700-900 nm range makes these Au nanoclusters superior for bioimaging applications over other emissions centered below 650 nm due to reduced background interference, albeit visible emissions could have higher quantum efficiency. The heating procedure is shown to be effective to improve the luminescence of Au nanoclusters synthesized under a variety of conditions using two types of monothiols: mercaptosuccinic acid and tiopronin. Therefore, this heating method is believed to be a generalizable approach to improve the near IR luminescence of aqueous soluble Au nanoclusters, which enables better bioimaging applications. The high quantum yield is found relatively stable over a wide pH range. PEGylation of the Au nanoclusters reduces their quantum efficiency but improves their permeation into the cytoplasm. Interestingly, z-stack confocal analysis clearly reveals the presence of Au nanoclusters inside the cell nucleus in single cell imaging. The finding addresses controversial literature reports and demonstrates the internalization and heterogeneous subcellular distributions, particularly inside the nucleus. The high luminescence intensity, small overall dimension, cell and nuclear distribution, chemical stability and low-to-non toxicity make these Au nanoclusters promising probes for broad cell dynamics and imaging applications.A five-to-ten fold enhancement, up to ca. 5-10% quantum efficiency, of near IR luminescence from monothiolate protected gold nanoclusters was achieved by heating in the presence of excess ligand thiols. An emission maximum in the 700-900 nm range makes these Au nanoclusters superior for bioimaging applications over other emissions centered below 650 nm due to reduced background interference, albeit visible emissions

  11. 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.

  12. 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.

  13. 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.

  14. Possible near-IR channels for remote sensing precipitable water vapor from geostationary satellite platforms

    NASA Technical Reports Server (NTRS)

    Gao, B.-C.; Goetz, A. F. H.; Westwater, Ed R.; Conel, J. E.; Green, R. O.

    1993-01-01

    Remote sensing of troposheric water vapor profiles from current geostationary weather satellites is made using a few broadband infrared (IR) channels in the 6-13 micron region. Uncertainties greater than 20% exist in derived water vapor values just above the surface from the IR emission measurements. In this paper, we propose three near-IR channels, one within the 0.94-micron water vapor band absorption region, and the other two in nearby atmospheric windows, for remote sensing of precipitable water vapor over land areas, excluding lakes and rivers, during daytime from future geostationary satellite platforms. The physical principles are as follows. The reflectance of most surface targets varies approximately linearly with wavelength near 1 micron. The solar radiation on the sun-surface-sensor ray path is attenuated by atmospheric water vapor. The ratio of the radiance from the absorption channel with the radiances from the two window channels removes the surface reflectance effects and yields approximately the mean atmospheric water vapor transmittance of the absorption channel. The integrated water vapor amount from ground to space can be obtained with a precision of better than 5% from the mean transmittance. Because surface reflectances vary slowly with time, temporal variation of precipitable water vapor can be determined reliably. High spatial resolution, precipitable water vapor images are derived from spectral data collected by the Airborne Visable-Infrared Imaging Spectrometer, which measures solar radiation reflected by the surface in the 0.4-2.5 micron region in 10-nm channels and has a ground instantaneous field of view of 20 m from its platform on an ER-2 aircraft at 20 km. The proposed near-IR reflectance technique would complement the IR emission techniques for remote sensing of water vapor profiles from geostationary satellite platforms, especially in the boundary layer where most of the water vapor is located.

  15. 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

  16. 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

  17. Eso's Situation in Chile

    NASA Astrophysics Data System (ADS)

    1995-02-01

    ESO, the European Southern Observatory, in reply to questions raised by the international media, as well as an ongoing debate about the so-called "Paranal case" in Chilean newspapers, would like to make a number of related observations concerning its status and continued operation in that country [1]. THE ESO OBSERVATORY SITES IN CHILE The European Southern Observatory, an international organisation established and supported by eight European countries, has been operating more than 30 years in the Republic of Chile. Here ESO maintains one of the world's prime astronomical observatories on the La Silla mountain in the southern part of the Atacama desert. This location is in the Fourth Chilean Region, some 600 km north of Santiago de Chile. In order to protect the La Silla site against dust and light pollution from possible future mining industries, roads and settlements, ESO early acquired the territory around this site. It totals about 825 sq. km and has effectively contributed to the preservation of its continued, excellent "astronomical" quality. Each year, more than 500 astronomers from European countries, Chile and elsewhere profit from this when they come to La Silla to observe with one or more of the 15 telescopes now located there. In 1987, the ESO Council [2] decided to embark upon one of the most prestigious and technologically advanced projects ever conceived in astronomy, the Very Large Telescope (VLT). It will consist of four interconnected 8.2-metre telescopes and will become the largest optical telescope in the world when it is ready. It is safe to predict that many exciting discoveries will be made with this instrument, and it will undoubtedly play a very important role in our exploration of the distant universe and its many mysteries during the coming decades. THE VLT AND PARANAL In order to find the best site for the VLT, ESO performed a thorough investigation of many possible mountain tops, both near La Silla and in Northern Chile. They showed

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

    PubMed

    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

    2014-05-01

    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. PMID:24647752

  19. Near-IR activity of hybrid solar cells: Enhancement of efficiency by dissociating excitons generated in PbS nanoparticles

    NASA Astrophysics Data System (ADS)

    Guchhait, Asim; Rath, Arup K.; Pal, Amlan J.

    2010-02-01

    Photovoltaic devices based on PbS nanoparticles remained inactive in the near-IR region due to a not-so-favorable energy band-diagram that does not allow dissociation of excitons generated in PbS. In this work, with the introduction of TiO2 nanostructures in the PbS-based hybrid system, we show an enhancement of photovoltaic performance in both visible and near-IR regions. The addition of TiO2 increases the power conversion efficiency from 0.006% to 0.12%. With the aid of energy band-diagram, we show that excitons generated in PbS even in the near-IR range can now become dissociated to yield photocurrent in the external circuit.

  20. 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.

  1. 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

  2. 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

  3. 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

  4. 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).

  5. 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.

  6. 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.

  7. 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.

  8. 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.

  9. 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.

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

    NASA Astrophysics Data System (ADS)

    Connor, B. J.; Sherlock, V.; Toon, G.; Wunch, D.; Wennberg, P.

    2015-11-01

    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 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 1.6 μ 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 superior to existing techniques for retrieval of column abundance. We finish by discussing on-going research which may allow CO2 profile retrievals with sufficient accuracy to significantly improve on the results of column retrievals, both in total column abundance and in profile shape.

  11. 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

    2016-04-12

    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

  12. A car-borne highly sensitive near-IR diode-laser methane detector

    SciTech Connect

    Berezin, A G; Ershov, Oleg V; Shapovalov, Yu P

    2003-08-31

    A highly sensitive automated car-borne detector for measuring methane concentration in real time is designed, developed and tested under laboratory and field conditions. Measurements were made with the help of an uncooled tunable near-IR 1.65-{mu}m laser diode. The detector consists of a multipass optical cell with a 45-m long optical path and a base length of 0.5 m. The car-borne detector is intended for monitoring the methane concentration in air from the moving car to reveal the leakage of domestic gas. The sensitivity limit (standard deviation) under field conditions is 1 ppm (20 ppb under laboratory conditions) for a measuring time of 0.4 s. The measuring technique based on the detection of a single methane line ensured a high selectivity of methane detector relative to other gases. The methane detector can be easily modified for measuring other simple-molecule gases (e.g., CO, CO{sub 2}, HF, NO{sub 2}, H{sub 2}O) by replacing the diode laser and varying the parameters of the control program. (special issue devoted to the memory of academician a m prokhorov)

  13. Fluorescence imaging with multifunctional polyglycerol sulfates: novel polymeric near-IR probes targeting inflammation.

    PubMed

    Licha, Kai; Welker, Pia; Weinhart, Marie; Wegner, Nicole; Kern, Sylvia; Reichert, Stefanie; Gemeinhardt, Ines; Weissbach, Carmen; Ebert, Bernd; Haag, Rainer; Schirner, Michael

    2011-12-21

    We present a highly selective approach for the targeting of inflammation with a multivalent polymeric probe. Dendritic polyglycerol was employed to synthesize a polyanionic macromolecular conjugate with a near-infrared fluorescent dye related to Indocyanine Green (ICG). On the basis of the dense assembly of sulfate groups which were generated from the polyol core, the resulting polyglycerol sulfate (molecular weight 12 kD with ~70 sulfate groups) targets factors of inflammation (IC(50) of 3-6 nM for inhibition of L-selectin binding) and is specifically transported into inflammatory cells. The in vivo accumulation studied by near-IR fluorescence imaging in an animal model of rheumatoid arthritis demonstrated fast and selective uptake which enabled the differentiation of diseased joints (score 1-3) with a 3.5-fold higher fluorescence level and a signal maximum at 60 min post injection. Localization in tissues using fluorescence histology showed that the conjugates are deposited in the inflammatory infiltrate in the synovial membrane, whereas nonsulfated control was not detected in association with disease. Hence, this type of polymeric imaging probe is an alternative to current bioconjugates and provides future options for targeted imaging and drug delivery. PMID:22092336

  14. Preliminary Results from the Array Camera for Optical to Near-IR Spectrophotometry (ARCONS)

    NASA Astrophysics Data System (ADS)

    Mazin, Benjamin A.; O'Brien, K.; Bumble, B.; Strader, M.; Meeker, S.; Stoughton, C.; Marsden, D.; Walter, A.; Szypyrt, P.; Ulbricht, G.

    2013-01-01

    In September 2012, the ARray Camera for Optical to Near-IR Spectrophotometry (ARCONS) was deployed at the 120" Shane telescope at Lick Observatory. ARCONS is a photon conuting integral field unit (IFU) that utilizes Microwave Kinetic Inductance Detectors (MKIDs), which are an emerging superconducting detector technology. MKIDs measure the energy (to within several percent) and arrival time (to within a microsecond) of detected photons. ARCONS contains a 2024 (46x44) pixel MKID array and has an operational bandwidth of 400 to 1100 nm. At the Shane telescope's Coudé focus, the array had a field of view of 22"x23". A variety of observations were made to demonstrate the potential applications of ARCONS's ability to do time-resolved low resolution spectro-imaging. Observations were made of short period compact binaries to look for spectral orbital variations. Observations of eclipsing white dwarfs were made to look for transit timing variations in orbital periods that would indicate the presence of additional companions. Observations were also made of faint galaxies to determine their redshifts, and observations of Low-Mass X-ray Binaries were made to probe the IR-emitting region of their jets. In another use of ARCONS's timing resolution, simultaneous optical and radio observations of the Crab pulsar were made, with the help of collaborators. In this talk I will discuss the preliminary results of a subset of these observations.

  15. Compositional information for the Moon: Some characteristics of current near-IR spectra (telescopic and laboratory)

    NASA Astrophysics Data System (ADS)

    Pieters, Carle M.

    1987-05-01

    For the last decade telescopic near infrared spectra have been obtained for small lunar areas. Such spectra, with the ground truth foundation from lunar samples, have been used extensively to address a multitude of problems in lunar science. Much of the near infrared spectral reflectance data from both laboratory and telescopic measurements have recently been compiled in comparable formats and an initial comparative assessment of the available data using selected spectral parameters has been made. The objective is to develop a framework for the systematics of lunar near-IR spectra in order to better interpret spectra of unknown materials in terms of useful compositional information. Each spectrum was first classified according to its general character then a variety of parameters sensitive to mineralogy and alteration products were measured for each spectrum: band width, band strength, absorption band center near 1 micron, band symmetry, continuum slope, etc. The telescopic and laboratory data sets are briefly described. The comparative analysis shows that a few well known lunar spectral properties are evident in both sets, such as the systematic variation in pyroxene composition between the highlands and the mare. However, an additional gabbroic component can be detected in many highland craters.

  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. Retrieval of Surface Lambert Albedos and Aerosols Optical Depths Using OMEGA Near-IR EPF Observations of Mars

    NASA Astrophysics Data System (ADS)

    Vincendon, M.; Langevin, Y.; Poulet, F.; Bibring, J.-P.; Gondet, B.

    2007-03-01

    We have analyzed five EPF sequences acquired by OMEGA/Mars Express in the near-IR over ice-free and ice-covered surfaces to retrieve simultaneously the Lambert albedo of the surface and the optical depth of aerosols.

  18. 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. PMID:24425677

  19. 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.

  20. 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.

  1. 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

  2. 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.

  3. Goniometer-spectrometer for index of refraction measurements from the near UV through the near IR

    NASA Astrophysics Data System (ADS)

    Ulbrich, Gerd J.; Trede, Jens

    1990-10-01

    The Ml I erWede Goni ometer-Spectrometer Model 2 is a medi urn-high accuracy instrument for the determination of prism angles and index of refraction in the visible wavelength range (400-700nrn) With its automatic Heidenhain rotary encoder the instrument is capab''e of absolute accuracy to I O arcsec for prism angle measurements and i x I 05 for index of refraction measurements. Recently we have developed a modified version of this instrument to provide absolute index of refraction measurements in the wavelength range from the UV through the near IR (254nm-2325 nm). The absolute accuracy for index of refraction measurements in the range is j INIRQDILTIQt4 The classical methods of Rudberg and Franhoer are still the most accurate means of determining the absolute index oT refraction or bulk optical materials. Both methods utilize a collimator and telescope pair which are both focused at inflnity. The former is normally flxed and the latter is mounted on a goniometer arm equipped with a precision graduated circle to provide absolute angular position of the telescope. The collimator is used to project the slit image o various spectral lines through a prism made from the material to be tested Usually spectral lamps are used for the light sources but lasers have also been used. The telescope and the sample prism are each rotated about the vertical axis of the goniometer so that each is set at proper angle to produce a minimum angle of deflection of the projected slit image with the desired wavelength. The goniometer arm and telescope are then fine-adjusted so that the slit image 32 / SPIE Vol. 1327 Properties and Characteristics of Optical Glass II (1990)

  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. 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

  6. 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.

  7. 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.

  8. Portugal to Accede to ESO

    NASA Astrophysics Data System (ADS)

    2000-06-01

    The Republic of Portugal will become the ninth 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 Portuguese Minister of Science and Technology, José Mariano Gago and the ESO Director General, Catherine Cesarsky , in the presence of other high officials from Portugal and the ESO member states (see Video Clip 05/00 below). Following subsequent ratification by the Portuguese Parliament of the ESO Convention and the associated protocols [2], it is foreseen that Portugal will formally join this organisation on January 1, 2001. Uniting European Astronomy ESO PR Photo 16/00 ESO PR Photo 16/00 [Preview - JPEG: 400 x 405 pix - 160k] [Normal - JPEG: 800 x 809 pix - 408k] Caption : Signing of the Portugal-ESO Agreement on June 27, 2000, at the ESO Headquarters in Garching (Germany). At the table, the ESO Director General, Catherine Cesarsky , and the Portuguese Minister of Science and Technology, José Mariano Gago . In his speech, the Portuguese Minister of Science and Technology, José Mariano Gago , stated that "the accession of Portugal to ESO is the result of a joint effort by ESO and Portugal during the last ten years. It was made possible by the rapid Portuguese scientific development and by the growth and internationalisation of its scientific community." He continued: "Portugal is fully committed to European scientific and technological development. We will devote our best efforts to the success of ESO". Catherine Cesarsky , ESO Director General since 1999, warmly welcomed the Portuguese intention to join ESO. "With the accession of their country to ESO, Portuguese astronomers will have great opportunities for working on research programmes at the frontiers of modern astrophysics." "This is indeed a good time to join ESO", she added. "The four 8.2-m VLT Unit Telescopes with their many first-class instruments are nearly ready, and the VLT

  9. Decisions by the ESO Council

    NASA Astrophysics Data System (ADS)

    1995-04-01

    Today, Wednesday, 19 April 1995, the ESO Council [1] met in extraordinary session at the ESO Headquarters in Garching (Germany) to discuss the recent developments which have affected the operations of this Organisation in its host state, the Republic of Chile [2]. The delegations were informed about the various events which have impeded ESO's operations in Chile, in particular the construction of the 16-m equivalent Very Large Telescope (VLT) at Cerro Paranal in the Atacama desert. The ESO Council welcomes and appreciates the signature on 18 April 1995 by Mr. Roberto Cifuentes, Plenipotentiary Ambassador representing the Chilean Government and Professor Riccardo Giacconi, Director General of ESO, of the "Interpretative, Supplementary and Amending Agreement" to the ESO/Chile Convention of 1963 for the establishment of an astronomical observatory in Chile and the accompanying assurances by the Chilean Government. Council considers this as a very significant step towards a new level of cooperation between Chile and ESO, and expects to approve this Agreement at the same time as the Chilean Parliament. Council also appreciates the determined efforts of the Chilean Government to guarantee ESO's privileges and immunities on the basis of the 1963 Convention and to solve the issues surrounding private claims to the Paranal site in short order. However, there still exist a number of problems which impede ESO's activities in Chile including the issue of ESO's immunity from national jurisdiction, financial damage incurred to ESO and its VLT project, and the practical implementation of custom clearance and accreditation procedures to permit the continuation of work. Consequently, Council has directed the ESO Management to continue direct negotiations with the Chilean Government to resolve all pending issues, to continue work on Paranal, and also to convene an ad-hoc Working Group to propose alternatives for the possible placement of one VLT telescope or of the entire VLT

  10. 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

  11. Optical and Near-IR Spectral Comparison with Chromophore Candidates in the Jovian Atmosphere

    NASA Astrophysics Data System (ADS)

    Thelen, Alexander; Chanover, Nancy; Miller, Charles; Loeffler, Mark; Hudson, Reggie; Simon, Amy

    2014-11-01

    Large atmospheric features, such as the belts, zones, and storms that make up Jupiter’s atmosphere remain colored by an unidentified chemical compound (or set of compounds). Optical reflectance spectra of Jupiter’s atmosphere in the literature show few spectral features in the blue (shortwards of 500 nm), unlike the red portion of the spectrum which is dominated by the methane absorption spectrum. The prevailing spectral slope and dearth of molecular absorption features in the blue are attributed to absorption by coloring compounds, or chromophores, in the upper Jovian atmosphere. While both organic and inorganic candidate compounds have been proposed, few laboratory studies have been conducted at temperatures and pressures appropriate for local Jupiter conditions to determine the identity of the chromophores responsible for coloring these large atmospheric features such as Jupiter’s Great Red Spot. In this study, we analyzed ground-based optical spectra and near-IR spectral image cubes of Jupiter for comparison with laboratory data of a potential chromophore compound. Optical spectra 330-450 nm in the blue, ~570-690 nm in the red) were obtained between December 2013 and February 2014 with the Dual Imaging Spectrograph, mounted on the Astrophysical Research Consortium 3.5-meter telescope at Apache Point Observatory. Near-infrared (1.25-2.5 μm) spectra of various locations in Jupiter’s atmosphere were obtained from spectral image cubes taken with the New Horizons Linear Etalon Imaging Spectral Array during the early 2007 Jupiter flyby. The combination of these two data sets allowed us to identify specific regions in the Jovian atmosphere with distinct coloration. We compare these ground- and space-based observations to laboratory spectra from the Cosmic Ice Laboratory at NASA’s Goddard Space Flight Center. Thin films of NH4SH were exposed to varying amounts of ionizing radiation at Jovian temperature conditions, thereby enabling us to evaluate NH4SH as a

  12. Interactions of monochromatic visible light and near-IR radiation with cells: currently discussed mechanisms

    NASA Astrophysics Data System (ADS)

    Karu, Tiina I.

    1995-05-01

    Biological responses of cells to visible and near IR (laser) radiation occur due to physical and/or chemical changes in photoacceptor molecules, components of respiratory chains (cyt a/a3 in mitochondria, and cyt d in E. coli). As a result of the photoexcitation of electronic states, the following physical and/or chemical changes can occur: alteration of redox properties and acceleration of electron transfer, changes in biochemical activity due to local transient heating of chromophores, one-electron auto-oxidation and O2- production, and photodynamic action and 1O2 production. Different reaction channels can be activated to achieve the photobiological macroeffect. The primary physical and/or chemical changes induced by light in photoacceptor molecules are followed by a cascade of biochemical reactions in the cell that do not need further light activation and occur in the dark (photosignal transduction and amplification chains). These reactions are connected with changes in cellular homeostasis parameters. The crucial step here is thought to be an alteration of the cellular redox state: a shift towards oxidation is associated with stimulation of cellular vitality, and a shift towards reduction is linked to inhibition. Cells with a lower than normal pH, where the redox state is shifted in the reduced direction, are considered to be more sensitive to the stimulative action of light than those with the respective parameters being optimal or near optimal. This circumstance explains the possible variations in observed magnitudes of low-power laser effects. Light action on the redox state of a cell via the respiratory chain also explains the diversity of low-power laser effects. Beside explaining many controversies in the field of low-power laser effects (i.e., the diversity of effects, the variable magnitude or absence of effects in certain studies), the proposed redox-regulation mechanism may be a fundamental explanation of some clinical effects of irradiation, for

  13. 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.

  14. 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.

  15. Deep Near-IR Observations of the Globular Cluster M4: Hunting for Brown Dwarfs

    NASA Astrophysics Data System (ADS)

    Dieball, A.; Bedin, L. R.; Knigge, C.; Rich, R. M.; Allard, F.; Dotter, A.; Richer, H.; Zurek, D.

    2016-01-01

    We present an analysis of deep Hubble Space Telescope (HST)/Wide Field Camera 3 near-IR (NIR) imaging data of the globular cluster (GC) M4. The best-photometry NIR color-magnitude diagram (CMD) clearly shows the main sequence extending toward the expected end of the hydrogen-burning limit and going beyond this point toward fainter sources. The white dwarf (WD) sequence can be identified. As such, this is the deepest NIR CMD of a GC to date. Archival HST optical data were used for proper-motion cleaning of the CMD and for distinguishing the WDs from brown dwarf (BD) candidates. Detection limits in the NIR are around F110W ≈ 26.5 mag and F160W ≈ 27 mag, and in the optical around F775W ≈ 28 mag. Comparing our observed CMDs with theoretical models, we conclude that we have reached beyond the H-burning limit in our NIR CMD and are probably just above or around this limit in our optical-NIR CMDs. Thus, any faint NIR sources that have no optical counterpart are potential BD candidates, since the optical data are not deep enough to detect them. We visually inspected the positions of NIR sources that are fainter than the H-burning limit in F110W and for which the optical photometry did not return a counterpart. We found in total five sources for which we did not get an optical measurement. For four of these five sources, a faint optical counterpart could be visually identified, and an upper optical magnitude was estimated. Based on these upper optical magnitude limits, we conclude that one source is likely a WD, one source could be either a WD or BD candidate, and the remaining two sources agree with being BD candidates. No optical counterpart could be detected for just one source, which makes this source a good BD candidate. We conclude that we found in total four good BD candidates.

  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. 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

  18. 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

  19. Near-IR Spectroscopic Monitoring of Class I Protostars: Variability of Accretion and Wind Indicators

    NASA Astrophysics Data System (ADS)

    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 H2). 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 H2 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 H2 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 toward understanding

  20. 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

  1. Near-IR Resonance Raman Spectroscopy of Archaerhodopsin 3: Effects of Transmembrane Potential

    PubMed Central

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

    2013-01-01

    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 3–11. 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 (Oall-trans) is found. At higher pH a second 13-cis retinal N-like species (N13-cis) is detected which is attributed to a slowly decaying intermediate in the red-light photocycle of D95N. However, the amount of N13-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 N13-cis to M13-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 potential

  2. 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.

  3. Conformational Changes in Thiazole-2-carboxylic Acid Selectively Induced by Excitation with Narrowband Near-IR and UV Light.

    PubMed

    Halasa, Anna; Reva, Igor; Lapinski, Leszek; Nowak, Maciej J; Fausto, Rui

    2016-04-01

    Conformers and photoinduced conformational transformations were studied for monomers of thiazole-2-carboxylic acid (TCA). The matrix-isolation technique and excitations with narrowband near-IR and UV light, tuned in an optical parametric oscillator, were used for this purpose. Form I, with the carboxylic moiety in the trans orientation and with the hydrogen atom of the OH group directed toward the nitrogen atom of the ring, was the most abundant in low-temperature argon or nitrogen matrixes. Conformer II, differing from I by 180° rotation of the OH group around the C-O bond, was also trapped in the matrixes, but in much smaller amount. The abundance of form II was experimentally determined as ∼6% of the total amount of TCA molecules. Selective excitation of I with narrowband near-IR laser light resulted in I → II transformation. This near-IR-induced conformational change was photoreversible: form II converted back to I upon selective excitation of II with near-IR light of different wavelength. Conformational conversions of I into II, or vice versa, were also induced in TCA monomers by narrowband UV excitations at 300 nm (for I → II transformation) and at 305 nm (for II → I transformation). A spontaneous conversion of photogenerated II into the most stable form I was observed for the compound trapped in the matrix at 15 K and kept in the dark. This process was very slow; the estimated half-life time of conformer II was longer than 50 h. Finally, TCA was shown to thermally decompose at room temperature, yielding CO2 and thiazole. PMID:26986193

  4. 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).

  5. 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.

  6. Conformers of Kojic Acid and Their Near-IR-Induced Conversions: Long-Range Intramolecular Vibrational Energy Transfer.

    PubMed

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

    2016-05-01

    Conformational transformations were investigated for molecules of kojic acid trapped in low-temperature argon and nitrogen matrixes. Two conformers, differing from each other by 120° rotation of the hydroxymethyl (-CH2OH) moiety, were found to be populated in freshly deposited matrixes, prior to any irradiation. Matrixes containing isolated monomers of kojic acid were irradiated with narrowband, tunable near-infrared (near-IR) laser light. Excitations at wavenumbers corresponding to the overtone of the stretching vibration of the OH bond of the hydroxymethyl group led to conversion of one of the observed conformers into another. The direction of this conformational transformation depended on the wavenumber (within the 7126-7115 cm(-1) range) used for irradiation. The same conformational photoconversion was also observed to occur upon narrowband irradiation at much lower wavenumbers (from the 6468-6447 cm(-1) range). Near-IR light from this range selectively excites overtone vibrations of the OH group directly attached to the heterocyclic ring. Such an observation provides a convincing evidence of a long-range vibrational energy transfer from the initially excited OH group (directly attached to the ring) to the remote hydroxymethyl fragment which changes its orientation. Structural changes, occurring in matrix-isolated molecules of kojic acid upon near-IR excitation, were monitored by FTIR spectroscopy. PMID:27070389

  7. Near-IR Photoluminescence of Pr/Cu/Sn Tridoped Phosphate Glass: Nonplasmonic Material System Versus Plasmonic Nanocomposite

    NASA Astrophysics Data System (ADS)

    Jiménez, José A.; Sendova, Mariana

    2015-04-01

    An optical spectroscopy study of Pr2O3, CuO, and SnO tridoped barium phosphate glass prepared by the melt-quenching technique has been carried out, emphasizing near-infrared (IR) emission properties. The material is studied in its nonplasmonic state (as synthesized) and plasmonic form (heat-treated), aiming to elucidate the effects of Cu nanoparticles. The data indicate that Cu+ ions and Sn centers are stabilized in the melt-quenched glass. Broad ultraviolet excitations of both species can lead to near-IR emission of Pr3+ ions via energy transfer. The plasmonic nanocomposite is produced upon heat treatment as Sn2+ reduces Cu+ to Cu0 atoms, ultimately precipitating as Cu nanoparticles sustaining the surface plasmon resonance. Consequently, depletion of primarily Cu+ modified the ultraviolet excitation properties for the sensitized near-IR Pr3+ emission. Further, suppression of the Pr3+ emission from near-IR emitting states 1D2 and 1G4 was observed in the Cu nanocomposite in accord with a "plasmonic diluent" role of the nanoparticles.

  8. Composition of Lunar Crater Central Peaks: Integrating Thermal IR and Near-IR Spectral Measurements

    NASA Astrophysics Data System (ADS)

    Song, E.; Bandfield, J. L.; Lucey, P. G.; Paige, D. A.

    2011-12-01

    This is an ongoing study of lunar complex craters between -30:30 degrees latitude. The main objective for this study is to examine the central peaks of these craters using thermal emission spectra from the Diviner Lunar Radiometer on board the Lunar Reconnaissance Orbiter. Diviner has 3 spectral filters near 8 microns (7.81, 8.28, 8.55) which are used to derive the wavelength location of the Christiansen Feature (CF). The CF occurs as an emissivity maximum located just shortward of the fundamental molecular vibration bands, making it sensitive to the bulk composition of lunar soils. Bulk composition derived from Diviner will be compared with more specific mineralogy identified using VIS-NIR spectra from Kaguya lunar orbiter's Spectral Profiler instrument. Based on several lines of evidence and the crystallization sequence of the early lunar magma ocean, the lunar crust is believed to become more mafic with depth. Previous studies of complex craters attempt to sample composition sourced from a range of depths in the crust using near-IR spectroscopy of central peaks. These studies have reported the presence of mafic minerals in most central peaks (e.g. Pieters 1986; Tompkins & Pieters, 1999). Quantitative radiative transfer modeling of Clementine multispectral imaging located some mafic and ultramafic peaks (Cahill and Lucey, 2009). The standout crater in these works has been the large relatively fresh crater Copernicus, where the central peaks were interpreted to be extremely olivine-rich. Conversely, CF position indicates the presence of about 50% feldspar, consistent with prior suggestions that Copernicus exposes troctolite. We have also found convincing evidence of substantially more mafic olivine exposures in the walls of Copernicus. Because Diviner is sensitive to the ratio of feldspar to mafic mineral abundances, documenting the CF of central peaks should be a sensitive test of the hypothesis that the lunar crust is increasingly mafic with depth. We have been

  9. 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

  10. 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.

  11. 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.

  12. 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.

  13. ESO PR Highlights in 2000

    NASA Astrophysics Data System (ADS)

    2001-01-01

    At the beginning of the new millennium, ESO and its staff are facing the future with confidence. The four 8.2-m Unit Telescopes of the Very Large Telescope (VLT) are in great shape and the VLT Interferometer (VLTI) will soon have "first fringes". The intercontinental ALMA project is progressing well and concepts for extremely large optical/infrared telescopes are being studied. They can also look back at a fruitful and rewarding past year. Perhaps the most important, single development has been the rapid transition of the Very Large Telescope (VLT). From being a "high-tech project under construction" it has now become a highly proficient, world-class astronomical observatory. This trend is clearly reflected in ESO's Press Releases , as more and more front-line scientific results emerge from rich data obtained at this very efficient facility. There were also exciting news from several of the instruments at La Silla. At the same time, the ESO community may soon grow, as steps towards membership are being taken by various European countries. Throughout 2000, a total of 54 PR communications were made, with a large number of Press Photos and Video Clips, cf. the 2000 PR Index. Some of the ESO PR highlights may be accessed directly via the clickable image on the present page. ESO PR Photo 01/01 is also available in a larger (non-clickable) version [ JPEG: 566 x 566 pix - 112k]. It may be reproduced, if credit is given to the European Southern Observatory.

  14. 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.

  15. 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.

  16. 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.

  17. 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).

  18. Mid-IR Photometry and Near-IR Spectroscopy of the FU Ori Protostar V2775 Ori (HOPS 223)

    NASA Astrophysics Data System (ADS)

    Fischer, William J.; Safron, Emily J.; Megeath, S. Thomas; Terebey, Susan; Soto, Edith; Wilson, Thomas L.; Adams, Joseph D.

    2016-02-01

    On 2015 November 20.39, we obtained mid-IR photometry of V2775 Ori (HOPS 223) with the FORCAST instrument aboard SOFIA. This is a low-mass embedded young stellar object that was reported to have undergone a luminosity outburst by Caratti o Garatti et al. (2011, A & A, 526, L1). Fischer et al. (2012, ApJ, 756, 99) dated the beginning of the outburst to between 2005 April and 2007 March and discussed the similarity of its near-IR spectrum to that of FU Orionis.

  19. VVV DR1: The first data release of the Milky Way bulge and southern plane from the near-infrared ESO public survey VISTA variables in the Vía Láctea

    NASA Astrophysics Data System (ADS)

    Saito, R. K.; Hempel, M.; Minniti, D.; Lucas, P. W.; Rejkuba, M.; Toledo, I.; Gonzalez, O. A.; Alonso-García, J.; Irwin, M. J.; Gonzalez-Solares, E.; Hodgkin, S. T.; Lewis, J. R.; Cross, N.; Ivanov, V. D.; Kerins, E.; Emerson, J. P.; Soto, M.; Amôres, E. B.; Gurovich, S.; Dékány, I.; Angeloni, R.; Beamin, J. C.; Catelan, M.; Padilla, N.; Zoccali, M.; Pietrukowicz, P.; Moni Bidin, C.; Mauro, F.; Geisler, D.; Folkes, S. L.; Sale, S. E.; Borissova, J.; Kurtev, R.; Ahumada, A. V.; Alonso, M. V.; Adamson, A.; Arias, J. I.; Bandyopadhyay, R. M.; Barbá, R. H.; Barbuy, B.; Baume, G. L.; Bedin, L. R.; Bellini, A.; Benjamin, R.; Bica, E.; Bonatto, C.; Bronfman, L.; Carraro, G.; Chenè, A. N.; Clariá, J. J.; Clarke, J. R. A.; Contreras, C.; Corvillón, A.; de Grijs, R.; Dias, B.; Drew, J. E.; Fariña, C.; Feinstein, C.; Fernández-Lajús, E.; Gamen, R. C.; Gieren, W.; Goldman, B.; González-Fernández, C.; Grand, R. J. J.; Gunthardt, G.; Hambly, N. C.; Hanson, M. M.; Hełminiak, K. G.; Hoare, M. G.; Huckvale, L.; Jordán, A.; Kinemuchi, K.; Longmore, A.; López-Corredoira, M.; Maccarone, T.; Majaess, D.; Martín, E. L.; Masetti, N.; Mennickent, R. E.; Mirabel, I. F.; Monaco, L.; Morelli, L.; Motta, V.; Palma, T.; Parisi, M. C.; Parker, Q.; Peñaloza, F.; Pietrzyński, G.; Pignata, G.; Popescu, B.; Read, M. A.; Rojas, A.; Roman-Lopes, A.; Ruiz, M. T.; Saviane, I.; Schreiber, M. R.; Schröder, A. C.; Sharma, S.; Smith, M. D.; Sodré, L.; Stead, J.; Stephens, A. W.; Tamura, M.; Tappert, C.; Thompson, M. A.; Valenti, E.; Vanzi, L.; Walton, N. A.; Weidmann, W.; Zijlstra, A.

    2012-01-01

    Context. The ESO public survey VISTA variables in the Vía Láctea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for about five years. Aims: We describe the progress of the survey observations in the first observing season, the observing strategy, and quality of the data obtained. Methods: The observations are carried out on the 4-m VISTA telescope in the ZYJHKs filters. In addition to the multi-band imaging the variability monitoring campaign in the Ks filter has started. Data reduction is carried out using the pipeline at the Cambridge Astronomical Survey Unit. The photometric and astrometric calibration is performed via the numerous 2MASS sources observed in each pointing. Results: The first data release contains the aperture photometry and astrometric catalogues for 348 individual pointings in the ZYJHKs filters taken in the 2010 observing season. The typical image quality is 0.9 arcsec {-1.0 arcsec}. The stringent photometric and image quality requirements of the survey are satisfied in 100% of the JHKs images in the disk area and 90% of the JHKs images in the bulge area. The completeness in the Z and Y images is 84% in the disk, and 40% in the bulge. The first season catalogues contain 1.28 × 108 stellar sources in the bulge and 1.68 × 108 in the disk area detected in at least one of the photometric bands. The combined, multi-band catalogues contain more than 1.63 × 108 stellar sources. About 10% of these are double detections because of overlapping adjacent pointings. These overlapping multiple detections are used to characterise the quality of the data. The images in the JHKs bands extend typically 4 mag deeper than 2MASS. The magnitude limit and photometric quality depend strongly on crowding in the inner Galactic regions. The astrometry for Ks = 15-18 mag has rms 35-175 mas. Conclusions: The VVV Survey data products offer a unique dataset to map the stellar populations in the

  20. 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

  1. 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.

  2. 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

  3. 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.

  4. 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

  5. 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.

  6. 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

  7. Report on the 2009 ESO Fellows Symposium

    NASA Astrophysics Data System (ADS)

    Emsellem, Eric; West, Michael; Leibundgut, Bruno

    2009-09-01

    The fourth ESO Fellows Symposium took place in Garching from 8-10 June 2009. This year's symposium brought together 28 ESO Fellows from Chile and Germany to meet their colleagues from across the ocean, discuss their research and provide feedback on ESO's Fellowship programme. This year's symposium also included training workshops to enhance the practical skills of ESO Fellows in today's competitive job market.

  8. Colloidal silicon quantum dots: synthesis and luminescence tuning from the near-UV to the near-IR range

    NASA Astrophysics Data System (ADS)

    Ghosh, Batu; Shirahata, Naoto

    2014-02-01

    This review describes a series of representative synthesis processes, which have been developed in the last two decades to prepare silicon quantum dots (QDs). The methods include both top-down and bottom-up approaches, and their methodological advantages and disadvantages are presented. Considerable efforts in surface functionalization of QDs have categorized it into (i) a two-step process and (ii) in situ surface derivatization. Photophysical properties of QDs are summarized to highlight the continuous tuning of photoluminescence color from the near-UV through visible to the near-IR range. The emission features strongly depend on the silicon nanostructures including QD surface configurations. Possible mechanisms of photoluminescence have been summarized to ascertain the future challenges toward industrial use of silicon-based light emitters.

  9. Tunable visible and near-IR emission from sub-10 nm etched single-crystal Si nanopillars.

    PubMed

    Walavalkar, Sameer S; Hofmann, Carrie E; Homyk, Andrew P; Henry, M David; Atwater, Harry A; Scherer, Axel

    2010-11-10

    Visible and near-IR photoluminescence (PL) is reported from sub-10 nm silicon nanopillars. Pillars were plasma etched from single crystal Si wafers and thinned by utilizing strain-induced, self-terminating oxidation of cylindrical structures. PL, lifetime, and transmission electron microscopy were performed to measure the dimensions and emission characteristics of the pillars. The peak PL energy was found to blue shift with narrowing pillar diameter in accordance with a quantum confinement effect. The blue shift was quantified using a tight binding method simulation that incorporated the strain induced by the thermal oxidation process. These pillars show promise as possible complementary metal oxide semiconductor compatible silicon devices in the form of light-emitting diode or laser structures. PMID:20919695

  10. 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.

  11. 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.

  12. 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)

  13. 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

  14. Development of a femtosecond time-resolved near-IR multiplex stimulated Raman spectrometer in resonance with transitions in the 900-1550 nm region.

    PubMed

    Takaya, Tomohisa; Iwata, Koichi

    2016-07-21

    Charge transfer and charge delocalisation processes play key roles in the functions of large biomolecular systems and organic/inorganic devices. Many of the short-lived transients involved in these processes can be sensitively detected by monitoring their low-energy electronic transitions in the near-IR region. Ultrafast time-resolved near-IR Raman spectroscopy is a promising tool for investigating the structural dynamics of the short-lived transients as well as their electronic dynamics. In this study, we have developed a femtosecond time-resolved near-IR multiplex stimulated Raman spectrometer using the Raman pump pulse at 1190 nm and a broadband probe pulse covering the 900-1550 nm region. Spectral and temporal instrument responses of the spectrometer are estimated to be 5 cm(-1) and 120 fs, respectively. Time-resolved near-IR stimulated Raman spectra of poly(3-dodecylthiophene) (P3DDT) are recorded in toluene solution for investigating its structural changes following the photoexcitation. The spectra strongly indicate conformational changes of P3DDT in excited states associated with the elongation of its effective conjugation length. The results on P3DDT fully demonstrate the effectiveness of the newly developed femtosecond time-resolved near-IR stimulated Raman spectrometer. PMID:27327140

  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. Science Data Management at ESO

    NASA Astrophysics Data System (ADS)

    Romaniello, Martino

    2015-12-01

    Providing the best science data is at the core of ESO’s mission to enable major science discoveries from our science community. I will briefly describe the steps that ESO undertakes to fulfill this, namely ensuring that instruments are working properly, that the science content can be extracted from the data and, finally, delivering the science data to our users, PIs and archive researchers alike.Metrics and statistics that gauge the results and impact of these efforts will be discussed.

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

    NASA Astrophysics Data System (ADS)

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

    2009-10-01

    The graphitic layered compound C 6N 9H 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.

  18. 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

  19. 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.

  20. 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

  1. Association study of a common variant near IRS1 with type 2 diabetes mellitus in Chinese Han population.

    PubMed

    Tang, Yong; Han, Xueyao; Sun, Xiuqin; Lv, Chao; Zhang, Xiaomei; Guo, Wulan; Ren, Qian; Luo, Yingying; Zhang, Xiuying; Zhou, Xianghai; Ji, Linong

    2013-02-01

    The insulin receptor substrate-1 (IRS1) plays an important role in insulin signaling. A recent genome-wide association study identified rs2943641C>T as a susceptibility locus for type 2 diabetes mellitus (T2DM) in Caucasian patients. Therefore, we determined whether this common variant near IRS1 is also associated with the risk of T2DM and T2DM-related phenotypes in a Chinese Han population. A total of 2,290 unrelated Chinese Han individuals residing in Beijing were recruited in this study, including 1177 T2DM patients and 1113 subjects with normal glucose tolerance (control group). The single nucleotide polymorphism (SNP) was genotyped using a MassARRAY iPLEX system. The frequency of risk allele C was 0.929 in the control group and 0.939 in patients with T2DM. We found no association between the C allele of rs2943641 and T2DM in a recessive model [OR 1.14, 95 % confidence interval (CI) 0.89-1.45, P = 0.298], or after adjusting for sex, age, and body mass index (BMI) (OR 1.10, 95 % CI 0.85-1.43, P = 0.301). Analysis of the clinical features of the control subjects with normal glucose tolerance revealed that the 30-min plasma glucose level during a 75-g oral glucose tolerance test was significantly different between the CC and CT+TT genotypes (P = 0.017). Linear regression analysis showed that the 30-min plasma glucose levels was significantly and positively associated with the CC genotype after adjusting for sex, age, and BMI (β = 0.065, 95 % CI 0.009-0.654, P = 0.044). In addition, a potential association between this SNP and increased waist circumference (β = 1.337, 95 % CI -0.179 to 2.853, P = 0.084) was observed with adjustment for the sex and age. Our study was not able to demonstrate the association between rs2943641 near IRS1 and T2DM in a Chinese Han population. However, this SNP may be associated with postprandial hyperglycemia. PMID:22576021

  2. 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.

  3. Austria Declares Intent To Join ESO

    NASA Astrophysics Data System (ADS)

    2008-04-01

    At a press conference today at the University of Vienna's Observatory, the Austrian Science Minister Johannes Hahn announced the decision by the Austrian Government to seek membership of ESO from 1 July this year. ESO PR Photo 11/08 ESO PR Photo 11/08 Announcing Austria's Intent to Join ESO Said Minister Hahn: "With membership of ESO, Austria's scientists will receive direct access to the world's leading infrastructure in astronomy. This strengthens Austria as a place for research and provides an opportunity for young researchers to continue their work from here. With this move, Austria takes an important step in the reinforcement of Europe's science and research infrastructure." The decision constitutes a major breakthrough for Austrian scientists who have argued for membership of ESO for many years. Seeking membership in ESO also marks a step towards the further development of the European Research and Innovation Area, an important element of Europe's so-called Lisbon Strategy. "ESO welcomes the Austrian bid to join our organisation. I salute the Austrian Government for taking this important step and look forward to working closely with our Austrian friends and colleagues in the years to come," commented the ESO Director General, Tim de Zeeuw. For Austrian astronomers, ESO membership means not only unrestricted access to ESO's world-leading observational facilities including the world's most advanced optical telescope, the Very Large Telescope, and full participation in the quasi-global ALMA project, but also the possibility to participate on a par with their European colleagues in the future projects of ESO, including the realisation of ESO's Extremely Large Telescope project (E-ELT), which is currently in the design phase. All these projects require some of the most advanced technologies in key areas such as optics, detectors, lightweight structures, etc. Austrian participation in ESO opens the door for Austrian industry and major research institutes of the

  4. Phase 3 process overview and the ESO Science Data Products Standard

    NASA Astrophysics Data System (ADS)

    Mascetti, L.; Arnaboldi, M.; Delmotte, N.; Micol, A.; Retzlaff, J.

    2015-12-01

    The ESO Phase 3 infrastructure provides a channel to submit reduced data products for publication to the astronomical community at large and long-term data preservation in the ESO science archive facility. The ESO archive serves as the central collection point for data reduced by ESO users but also for the products of in-house pipeline data processing. One unique standard data format is associated to each type of product like image, spectrum, IFU cube, etc. Here we present an overview of the Phase 3 process and its key features, the data types supported by the the ESO Science Data Products Standard and the data collections already served by the Phase 3 service.

  5. 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.

  6. 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; Hashimoto, Jun; Kudo, Tomoyuki; Sitko, Michael; Grady, Carol A.; Karr, Jennifer; Mayama, Satoshi; Kusakabe, Nobuyuki; 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.

  7. 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.

  8. 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

    2016-03-16

    We synthesized two novel ultra low bandgap donor-acceptor (D-A) copolymers (Eg ≤ 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 and , 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 :PC71BM and :PC71BM showed overall power conversion efficiencies (PCEs) of 4.32% and 3.48%, respectively. Although possesses a broad absorption coverage of up to 1300 nm, the lower PCE may be attributed to the low Jsc, 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 :PC71BM and :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. PMID:26932684

  9. 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.

  10. Near-IR Electrochromic Film Prepared by Oxidative Electropolymerization of the Cyclometalated Pt(II) Chloride with a Triphenylamine Group.

    PubMed

    Qiu, Dongfang; Bao, Xiaoyu; Zhao, Qian; Yang, Qichao; Feng, Yuquan; Wang, Hongwei; Yang, Chunxia; Liu, Kecheng

    2015-09-01

    A cyclometalated platinum chloride [(L)PtCl] {L = 4-[p-(diphenylamino)phenyl]-6-phenyl-2,2'-bipyridine} was successfully synthesized and characterized by (1)H NMR, (13)C NMR, MALDI-TOF MS, elemental analysis, and X-ray crystallography. Its oxidative electropolymerization proceeds smoothly on the working Pt and ITO electrodes by cyclic voltammetry. The film thickness can be easily tuned by controlling the CV scan number. The orange hybrid polymer film shows the nondiffusion-controlled redox processes and a unusually inverse dependence of ac impedance on its thickness. As a result of switching of the MLCT/ICT and dication absorption transitions, the adherent metallopolymer film exhibits the low-voltage-controlled anodic coloration near-IR electrochromism with significant optical contrast ratio (ΔT% = 88.8% at 820 nm), fast response time (1.9 s for the coloration step and 2.3 s for the bleaching step), and high coloration efficiency (CE = 363.3 C(-1)·cm(2)). PMID:26270128

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

    NASA Astrophysics Data System (ADS)

    de Leon, Jerome; Takami, Michihiro; Karr, Jennifer L.; Hashimoto, Jun; Kudo, Tomoyuki; Sitko, Michael; Mayama, Satoshi; Kusakabe, Nobuyuki; Akiyama, Eiji; Liu, Hauyu Baobab; Usuda, Tomonori; Abe, Lyu; Brandner, Wolfgang; Brandt, Timothy D.; Carson, Joseph; Currie, Thayne; Egner, Sebastian E.; Feldt, Markus; Follette, Katherine; Grady, Carol A.; Goto, Miwa; Guyon, Olivier; Hayano, Yutaka; Hayashi, Masahiko; Hayashi, Saeko; Henning, Thomas; Hodapp, Klaus W.; Ishii, Miki; Iye, Masanori; Janson, Markus; Kandori, Ryo; Knapp, Gillian R.; Kuzuhara, Masayuki; Kwon, Jungmi; Matsuo, Taro; McElwain, Michael W.; Miyama, Shoken; Morino, Jun-Ichi; Moro-Martin, Amaya; Nishimura, Tetsuo; Pyo, Tae-Soo; Serabyn, Eugene; Suenaga, Takuya; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro; Takato, Naruhisa; Terada, Hiroshi; Thalmann, Christian; Tomono, Daigo; Turner, Edwin L.; Watanabe, Makoto; Wisniewski, John P.; Yamada, Toru; Takami, Hideki; Tamura, Motohide

    2015-06-01

    We present new high-resolution (∼ 0\\buildrel{\\prime\\prime}\\over{.} 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 (∼20 AU) to the star. Within our image, we identify bright emission associated with a disk with a minimum radius of ∼90 AU, an inclination of ∼35° from the plane of the sky, and an approximate PA of 15{}^\\circ 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. Based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

  12. Continuous measurements of stable carbon isotopes in CO2 with a near-IR laser absorption spectrometer

    NASA Astrophysics Data System (ADS)

    Tanaka, Kotaro; Kojima, Ryota; Takahashi, Kenshi; Tonokura, Kenichi

    2013-09-01

    A near-IR laser absorption spectrometer using a technique of wavelength modulation spectroscopy is used to measure stable carbon isotope ratios of ambient CO2 (δ13C) via the absorption lines 12CO2 R(17) (2ν1 + ν12 - ν12 + ν3) at 4978.205 cm-1 and 13CO2 P(16) (ν1 + 2ν2 + ν3) at 4978.023 cm-1. The isotope ratios are measured with a reproducibility of 0.02‰ (1σ) in a 130-s integration time over a 12-h period. The humidity effect on δ13C values has been evaluated in laboratory experiments. The δ13C values of CO2 in ambient air were measured continuously over 8 days and agreed well with those from isotope ratio mass spectrometry of canister samples. The spectrometer is thus capable of real-time, in situ measurements of stable carbon isotope ratios of CO2 under ambient conditions.

  13. 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

  14. 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.

  15. Southern Fireworks above ESO Telescopes

    NASA Astrophysics Data System (ADS)

    1999-05-01

    New Insights from Observations of Mysterious Gamma-Ray Burst International teams of astronomers are now busy working on new and exciting data obtained during the last week with telescopes at the European Southern Observatory (ESO). Their object of study is the remnant of a mysterious cosmic explosion far out in space, first detected as a gigantic outburst of gamma rays on May 10. Gamma-Ray Bursters (GRBs) are brief flashes of very energetic radiation - they represent by far the most powerful type of explosion known in the Universe and their afterglow in optical light can be 10 million times brighter than the brightest supernovae [1]. The May 10 event ranks among the brightest one hundred of the over 2500 GRB's detected in the last decade. The new observations include detailed images and spectra from the VLT 8.2-m ANTU (UT1) telescope at Paranal, obtained at short notice during a special Target of Opportunity programme. This happened just over one month after that powerful telescope entered into regular service and demonstrates its great potential for exciting science. In particular, in an observational first, the VLT measured linear polarization of the light from the optical counterpart, indicating for the first time that synchrotron radiation is involved . It also determined a staggering distance of more than 7,000 million light-years to this GRB . The astronomers are optimistic that the extensive observations will help them to better understand the true nature of such a dramatic event and thus to bring them nearer to the solution of one of the greatest riddles of modern astrophysics. A prime example of international collaboration The present story is about important new results at the front-line of current research. At the same time, it is also a fine illustration of a successful collaboration among several international teams of astronomers and the very effective way modern science functions. It began on May 10, at 08:49 hrs Universal Time (UT), when the Burst

  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. A Multi-Wavelength Study of Sgr A*: The Correlation of X-ray, Near-IR and Sub-millimeter Emitting Flares

    NASA Astrophysics Data System (ADS)

    Yusef-Zadeh, F.; Bushouse, H.; Dowell, C. D.; Wardle, M.; Roberts, D.; Heinke, C.; Bower, G. C.; Vila Vilaro, B.; Shapiro, S.; Goldwurm, A.; Belanger, G.

    2005-12-01

    I review highlights of the results of two observing campaigns in 2004, designed to investigate the correlation of flare activity from Sgr A* between radio wavelengths and soft gamma-ray energies. We report the detection of a simultaneous X-ray and near-IR flare, as well as a sub-millimeter and near-IR flare using the NICMOS of HST, XMM-Newton and CSO. We explain the X-ray emission as arising from the population of near-IR-synchrotron-emitting relativistic particles, scattering sub-millimeter seed photons within the inner 10 RSch radius of Sgr A* up to X-rays and soft gamma-rays, detected by INTEGRAL. Using the inverse Compton scattering picture, we explain the lack of one-to-one X-ray counterparts to near-IR flares by the variation of the magnetic field and the spectral index distributions of the nonthermal particles. Lastly, we present a composite spectrum of Sgr A* based on these observing campaigns.

  18. 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.

  19. 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.

  20. 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.

  1. 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

  2. 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

  3. 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

  4. 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)

  5. 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.

  6. Near-IR supercontinuum generation based on a telecom single-mode fibre in an all-fibre format, and its power combining

    SciTech Connect

    Rumao Tao; Xiaolin Wang; Xiao, H; Zhou, P; Jing Hou

    2014-04-28

    Near-IR supercontinuum (SC) is generated based on a standard telecommunication single-mode (SM) fibre in an all-fibre format. The observed spectrum covers the spectral range from 1050 nm to 1700 nm. High-efficiency combining of the SC power is demonstrated for the first time, and the spectral SC properties are shown to be maintained after power combining. The results may find applications in sensing, spectroscopy and medicine. (control of laser radiation parameters)

  7. 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.

  8. Signing of ESO-Poland Accession Agreement

    NASA Astrophysics Data System (ADS)

    2014-12-01

    An agreement was signed by Professor Lena Kolarska-Bobińska, the Polish Minister of Science and Higher Education, and the ESO Director General Tim de Zeeuw in Warsaw on 28 October 2014 that will lead to the country joining ESO. The signing of the agreement followed its unanimous approval by the ESO Council during an extraordinary meeting on 8 October 2014. Poland will be welcomed as a new Member State, following subsequent ratification of the accession agreement by the Polish Parliament. Tim de Zeeuw’s speech at this ceremony is reproduced below.

  9. ESO Welcomes Finland as Eleventh Member State

    NASA Astrophysics Data System (ADS)

    Cesarsky, C.

    2004-09-01

    In early July, Finland joined ESO as the eleventh member state, following the completion of the formal accession procedure. Before this event, however, Finland and ESO had been in contact for a long time. Under an agreement with Sweden, Finnish astronomers had for quite a while enjoyed access to the SEST at La Silla. Finland had also been a very active participant in ESO's educational activities since they began in 1993. It became clear, that science and technology, as well as education, were priority areas for the Finnish government.

  10. Adaptive optics projects at ESO

    NASA Astrophysics Data System (ADS)

    Hubin, Norbert N.; Arsenault, Robin; Bonnet, Henri; Conan, Rodolphe; Delabre, Bernard; Donaldson, Robert; Dupuy, Christophe; Fedrigo, Enrico; Ivanescu, L.; Kasper, Markus E.; Kissler-Patig, Markus; Lizon, Jean-Luis; Le Louarn, Miska; Marchetti, Enrico; Paufique, J.; Stroebele, Stefan; Tordo, Sebastien

    2003-02-01

    Over the past two years ESO has reinforced its efforts in the field of Adaptive Optics. The AO team has currently the challenging objectives to provide 8 Adaptive Optics systems for the VLT in the coming years and has now a world-leading role in that field. This paper will review all AO projects and plans. We will present an overview of the Nasmyth Adaptive Optics System (NAOS) with its infrared imager CONICA installed successfully at the VLT last year. Sodium Laser Guide Star plans will be introduced. The status of the 4 curvature AO systems (MACAO) developed for the VLT interferometer will be discussed. The status of the SINFONI AO module developed to feed the infrared integral field spectrograph (SPIFFI) will be presented. A short description of the Multi-conjugate Adaptive optics Demonstrator MAD and its instrumentation will be introduced. Finally, we will present the plans for the VLT second-generation AO systems and the researches performed in the frame of OWL.

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

    PubMed Central

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

    2016-01-01

    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

  12. 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

  13. Syntheses of asymmetric zinc phthalocyanines as sensitizer of Pt-loaded graphitic carbon nitride for efficient visible/near-IR-light-driven H2 production.

    PubMed

    Yu, Lijuan; Zhang, Xiaohu; Zhuang, Chuansheng; Lin, Li; Li, Renjie; Peng, Tianyou

    2014-03-01

    Zinc phthalocyanine (ZnPc) derivatives with asymmetric (Zn-tri-PcNc-2) or symmetric (Zn-tetrad-Nc) structure, which possess wide spectral response in the visible/near-IR light region, are synthesized and utilized as a sensitizer of graphitic carbon nitride (g-C3N4) with 0.5 wt% Pt-loading for photocatalytic H2 production. The experimental results indicate that Zn-tri-PcNc-2 exhibits much better photosensitization on g-C3N4 than Zn-tetrad-Nc under visible/near-IR light although Zn-tetrad-Nc possesses wider and stronger optical absorption property than Zn-tri-PcNc-2. Zn-tri-PcNc-2-Pt/g-C3N4 exhibits an average H2 production rate of 132 μmol h(-1), which is much better than that (26.1 μmol h(-1)) of Zn-tetrad-Nc-Pt/g-C3N4 under visible-light (λ ≥ 500 nm) irradiation. Moreover, Zn-tri-PcNc-2-Pt/g-C3N4 also shows much higher apparent quantum yield (AQY) than Zn-tetrad-Nc-Pt/g-C3N4 under red/near-IR light irradiation. Especially, Zn-tri-PcNc-2-Pt/g-C3N4 exhibits impressively higher AQY (1.07%) than that (0.22%) of the Zn-tetrad-Nc-Pt/g-C3N4 under 700 nm monochromatic light irradiation. The much better photoactivity of Zn-tri-PcNc-2-Pt/g-C3N4 than Zn-tetrad-Nc-Pt/g-C3N4 is caused by the asymmetric structure of Zn-tri-PcNc-2, which can result in the electronic orbital directionality of its excited state, much faster photogenerated electron transfer to g-C3N4, and higher red/near-IR light utilization efficiency as compared to Zn-tetrad-Nc-Pt/g-C3N4. The present results provide an important insight into the effects of molecular structure and optical absorption property of phthalocyanine derivatives on the photoactivity of the dye-sensitized semiconductor, and also guide us to further improve the solar energy conversion efficiency by optimizing the molecular structure and effectively utilizing the visible/near-IR light of sunlight. PMID:24448755

  14. Report on the ESO Chile Science Days

    NASA Astrophysics Data System (ADS)

    West, Michael

    2008-03-01

    Science Days in Santiago are an annual gathering of ESO's geographically dispersed team in Chile to learn more about each other's research, to celebrate scientific achievements of the past year and to encourage new collaborations.

  15. Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey -- GOODS-North Field, Late Visits of SNe Search

    NASA Astrophysics Data System (ADS)

    Faber, Sandra

    2012-10-01

    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 12060, is part of the GOODS-S Deep survey. Special Deepscience highlights include: * Detection and counts of early galaxies to z 7-8 as revealed by red-sensitive WFC3-IR images beyond the Lya break - Measurement of the luminosity function of infant galaxies down to 10^9 solar masses out to z = 7-8 - Measurement of the faint-end LF slope to assess the contribution of faint galaxies to cosmic reionization * The physics of early star formation - Propertes of the earliest star-forming regions - sizes, star-formation rates, stellar masses and radiation densities, dust contents - In concert with Spitzer

  16. 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

  17. 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

  18. ESO Astronomers Emeriti -- Sandro D'Odorico and Alan Moorwood

    NASA Astrophysics Data System (ADS)

    Primas, F.; Casali, M.; Walsh, J.

    2010-09-01

    In May and June 2010, Sandro D'Odorico and Alan Moorwood, both driving forces behind many ESO instruments and very active in research, retired after three decades at ESO. The ESO Director General, Tim de Zeeuw, elevated both to the newly inaugurated position of ESO Astronomer Emeritus. Celebrations on their transition to these esteemed positions were held and are briefly described.

  19. 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

  20. 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

  1. Optical and near-IR observations of the faint and fast 2008ha-like supernova 2010ae

    NASA Astrophysics Data System (ADS)

    Stritzinger, M. D.; Hsiao, E.; Valenti, S.; Taddia, F.; Rivera-Thorsen, T. J.; Leloudas, G.; Maeda, K.; Pastorello, A.; Phillips, M. M.; Pignata, G.; Baron, E.; Burns, C. R.; Contreras, C.; Folatelli, G.; Hamuy, M.; Höflich, P.; Morrell, N.; Prieto, J. L.; Benetti, S.; Campillay, A.; Haislip, J. B.; LaClutze, A. P.; Moore, J. P.; Reichart, D. E.

    2014-01-01

    A comprehensive set of optical and near-infrared (NIR) photometry and spectroscopy is presented for the faint and fast 2008ha-like supernova (SN) 2010ae. Contingent on the adopted value of host extinction, SN 2010ae reached a peak brightness of -13.8 > MV > -15.3 mag, while modeling of the UVOIR light curve suggests it produced 0.003-0.007 M⊙ of 56Ni, ejected 0.30-0.60 M⊙ of material, and had an explosion energy of 0.04-0.30 × 1051 erg. The values of these explosion parameters are similar to the peculiar SN 2008ha -for which we also present previously unpublished early phase optical and NIR light curves - and places these two transients at the faint end of the 2002cx-like SN population. Detailed inspection of the post-maximum NIR spectroscopic sequence indicates the presence of a multitude of spectral features, which are identified through SYNAPPS modeling to be mainly attributed to Co ii. Comparison with a collection of published and unpublished NIR spectra of other 2002cx-like SNe, reveals that a Co ii footprint is ubiquitous to this subclass of transients, providing a link to Type Ia SNe. A visual-wavelength spectrum of SN 2010ae obtained at +252 days past maximum shows a striking resemblance to a similar epoch spectrum of SN 2002cx. However, subtle differences in the strength and ratio of calcium emission features, as well as diversity among similar epoch spectra of other 2002cx-like SNe indicates a range of physical conditions of the ejecta, highlighting the heterogeneous nature of thispeculiar class of transients. Based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere, Chile (ESO Programs 082.A-0526, 084.D-0719, 088.D-0222, 184.D-1140, and 386.D-0966); the Gemini Observatory, Cerro Pachon, Chile (Gemini Programs GS-2010A-Q-14 and GS-2010A-Q-38); the Magellan 6.5 m telescopes at Las Campanas Observatory; and the SOAR telescope.Tables 1-5 and Appendix A are available in electronic form at http

  2. 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.

  3. Near-IR electrochromism in electropolymerized films of a biscyclometalated ruthenium complex bridged by 1,2,4,5-tetra(2-pyridyl)benzene.

    PubMed

    Yao, Chang-Jiang; Zhong, Yu-Wu; Nie, Hai-Jing; Abruña, Héctor D; Yao, Jiannian

    2011-12-28

    Reductive electropolymerization of the biscyclometalated ruthenium complex [(vtpy)Ru(tpb)Ru(vtpy)](2+) [vtpy = 4'-vinyl-2,2':6',2″-terpyridine; tpb = 1,2,4,5-tetra(2-pyridyl)benzene] proceeded smoothly on electrode surfaces. Thanks to the strong electron coupling between the ruthenium centers of the individual monomeric units and strong intervalence charge-transfer absorption in the mixed valence state, the produced adherent metallopolymeric films exhibited near-IR electrochromism with tricolor switching, good contrast ratio (40% at 1165 nm), short response time, low-switching voltage, and long memory time. PMID:22133035

  4. Differences in visible and near-IR responses, and derived vegetation indices, for the NOAA-9 and NOAA-10 AVHRRs: a case study

    USGS Publications Warehouse

    Gallo, Kevin P.; Eidenshink, Jeffery C.

    1988-01-01

    This study evaluates the differences in the visible and near-IR responses of the Advanced Very High Resolution Radiometers (AVHRR) of the National Oceanic and Atmospheric Administration (NOAA)-9 and -10 satellites for coincident sample locations. The study also evaluates the differences in vegetation indices computed from those data. Data were acquired of the southeast portion of the United States for the 6 December 1986 daylight orbits of NOAA-9 and NOAA-10 satellites. The results suggest that, with appropriate gain and offset, the vegetation indices of the two sensor systems may be interchangeable for assessment of land surfaces.

  5. 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.

  6. Nonlinear optical properties of thick composite media with vanadium dioxide nanoparticles. I. Self-defocusing of radiation in the visible and near-IR regions

    NASA Astrophysics Data System (ADS)

    Ostrosablina, A. A.; Sidorov, A. I.

    2005-07-01

    This paper presents the experimental and theoretical results of a study of the interaction of pulsed laser radiation with thick composite media containing nanoparticles of vanadium dioxide (VO2). It establishes that the reversible semiconductor-metal phase transition that occurs in VO2 nanoparticles under the action of radiation can produce self-defocusing of radiation in the visible and near-IR regions because of the formation of a photoinduced dynamic lens. An analysis is carried out of how the radiation intensity affects the dynamics of these processes. It is shown that photoinduced absorption and scattering play a role in forming the nonlinear optical response.

  7. 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

  8. Visible and near-IR spectroscopic studies of uranium(IV) oxychloride in a MgCl{sub 2}-KCl melt

    SciTech Connect

    Dai, S.; Toth, L.M.; Del Cul, G.D.; Metcalf, D.H.

    1995-01-04

    Although the chemistry of uranium(IV) chloride complexes in molten chloride melts has been widely investigated, no studies of uranium(IV) oxychloride complexes in these melts have appeared, with the exception of a recent paper from this laboratory. In that paper, visible and near-IR absorption bands overlapping with those of the uranium(IV) chloride complex are attributed to oxychloride species. Attempts have been made to prepare solutions containing uranium oxychloride by a direct dissolution of UOCl{sub 2} into solvents such as water, acids, and molten pyridinium chloride. However, only uranium(IV) chloride complex species are recovered. This led Ewing to conclude that the uranium-oxygen bond in UOCl{sub 2} is stabilized only in the solid state probably by the lattice energy of the crystal. Here the authors want to report, for the first time, the visible and near-IR spectra of uranium oxychloride in molten MgCl{sub 2}-KCl without interference from those of uranium(IV) chloride complexes. In addition, experimental evidence is provided to confirm that the new uranium(IV) species is an oxygen-containing chloride complex.

  9. Near IR fluorescent conjugated poly(ethylene glycol)bisphosphonate nanoparticles for in vivo bone targeting in a young mouse model.

    PubMed

    Rudnick-Glick, S; Corem-Salkmon, E; Grinberg, I; Yehuda, R; Margel, S

    2015-01-01

    Bisphosphonate (BP) compounds are widely used in the treatment of bone disorders. This group of drugs with a high affinity to Ca(+2) ions is rapidly attracted to bone mineral, especially in areas of high resorption. We have engineered unique biodegradable BP nanoparticles (NPs) by dispersion co-polymerization of the monomers methacrylate-PEG-BP) and (3-Aminopropyl)mathacrylamide) with the crosslinker monomer tetra ethylene glycol diacrylate. These NPs possess a dual functionality: (1) covalent attachment of a dye (e.g. near IR dye) or a drug to the nanoparticles through the primary amine groups on the surface of the NPs; (2) chelation to the bone mineral hydroxyapatite through the BP on the surface of the NPs. This study describes the uptake of the unique near IR fluorescent Cy 7-conjugated BP NPs in bone of a young mouse model. Blood half-life studies revealed a relatively long half-life (approximately 5 h) due to a high concentration of PEG in the BP NPs as well as a relatively long whole body clearance (approximately 2 weeks). Body distribution studies showed a specific uptake of the BP NPs in bone. These unique engineered BP NPs are planned to be utilized in future work for diagnostic and drug delivery systems that are targeted to bone disorders. PMID:26577112

  10. Estimation of cellulose crystallinity of lignocelluloses using near-IR FT-Raman spectroscopy and comparison of the Raman and Segal-WAXS methods.

    PubMed

    Agarwal, Umesh P; Reiner, Richard R; Ralph, Sally A

    2013-01-01

    Of the recently developed univariate and multivariate near-IR FT-Raman methods for estimating cellulose crystallinity, the former method was applied to a variety of lignocelluloses: softwoods, hardwoods, wood pulps, and agricultural residues/fibers. The effect of autofluorescence on the crystallinity estimation was minimized by solvent extraction or chemical treatment or both. Additionally, when the roles of lignin and hemicellulose in the Raman crystallinity assessment were investigated, it was found that syringyl lignin containing lignocelluloses generated somewhat higher crystallinity, whereas the presence of hemicellulose reduced the crystallinity. Overall, when autofluorescence was minimized and corrections made for hemicellulose and syringyl lignin contributions, the univariate Raman method performed well and estimated cellulose crystallinity accurately. Moreover, when the Raman and Segal-WAXS methods were compared, we observed that in the absence of significant fluorescence, the Raman method was influenced mostly by hemicellulose and syringyl lignin, whereas the Segal-WAXS was affected by various types of lignin and hemicellulose. It was concluded that the near-IR FT-Raman method with corrections for influences of syringyl lignin and hemicellulose can be used to correctly estimate cellulose crystallinity. PMID:23241140

  11. 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

  12. Former ESO DG Adriaan Blaauw Turned 90

    NASA Astrophysics Data System (ADS)

    2004-06-01

    On April 12, former ESO DG professor Adriaan Blaauw reached his 90th birthday. Adriaan, together with many friends, family members, colleagues from The Netherlands and abroad, celebrated this occasion on April 17, during an informal get-together at the 19th-century country-mansion Nienoord in Leek, near Groningen.

  13. 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.

  14. 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.

  15. 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.

  16. 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.

  17. 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

  18. Low-Symmetrical Zinc(II) Benzonaphthoporphyrazine Sensitizers for Light-Harvesting in Near-IR Region of Dye-Sensitized Solar Cells.

    PubMed

    Ikeuchi, Takuro; Mori, Shogo; Kobayashi, Nagao; Kimura, Mutsumi

    2016-05-16

    Two ring-expanded naphthalocyanine-based sensitizers NcS1 and NcS2 have been designed and synthesized to harvest near-IR light energy in dye-sensitized solar cells. Low-symmetrical "push-pull" structures of NcS1 and NcS2 enable the red-shift of absorption spectrum as well as the defined Q-band splitting. The zinc benzonaphthoporphyrazine sensitizer NcS1 possessing one carboxylic acid and six 2,6-diisopropylphenoxy units showed a PCE value of 3.2% when used as a light-harvesting dye on a TiO2 electrode under one sun condition. The NcS1 cell showed a broad photoresponse at wavelengths from 600 to 850 nm. PMID:27120343

  19. 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.

  20. Unifying access to services: ESO's user portal

    NASA Astrophysics Data System (ADS)

    Chavan, A. M.; Tacconi-Garman, L. E.; Peron, M.; Sogni, F.; Canavan, T.; Nass, P.

    2006-06-01

    The European Southern Observatory (ESO) is in the process of creating a central access point for all services offered to its user community via the Web. That gateway, called the User Portal, will provide registered users with a personalized set of service access points, the actual set depending on each user's privileges. Correspondence between users and ESO will take place by way of "profiles", that is, contact information. Each user may have several active profiles, so that an investigator may choose, for instance, whether their data should be delivered to their own address or to a collaborator. To application developers, the portal will offer authentication and authorization services, either via database queries or an LDAP server. The User Portal is being developed as a Web application using Java-based technology, including servlets and JSPs.

  1. 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

  2. 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.

  3. 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.

  4. New observing concepts for ESO survey telescopes

    NASA Astrophysics Data System (ADS)

    Bierwirth, T.; Szeifert, T.; Dorigo, D.; Nunes, P.; Rejkuba, M.; Baugh, K.; Klein Gebbinck, M.; Manning, A.; Muravov, D.; Vera, I.

    2010-07-01

    The start of operations of the VISTA survey telescope will not only offer a new facility to the ESO community, but also a new way of observing. Survey observation programs typically observe large areas of the sky and might span several years, corresponding to the execution of hundreds of observations blocks (OBs) in service mode. However, the execution time of an individual survey OB will often be rather short. We expect that up to twelve OBs may be executed per hour, as opposed to about one OB per hour on ESO's Very Large Telescope (VLT). OBs of different programs are competing for observation time and must be executed with adequate priority. For these reasons, the scheduling of survey OBs is required to be almost fully automated. Two new key concepts are introduced to address these challenges: ESO's phase 2 proposal preparation tool P2PP allows PIs of survey programs to express advanced mid-term observing strategies using scheduling containers of OBs (groups, timelinks, concatenations). Telescope operators are provided with effective short-term decision support based on ranking observable OBs. The ranking takes into account both empirical probability distributions of various constraints and the observing strategy described by the scheduling containers. We introduce the three scheduling container types and describe how survey OBs are ranked. We demonstrate how the new concepts are implemented in the preparation and observing tools and give an overview of the end-to-end workflow.

  5. Interferometry with the ESO Very Large Telescope

    NASA Astrophysics Data System (ADS)

    von der Luehe, Oskar; Derie, Frederic; Koehler, Bertrand; Leveque, Samuel A.; Paresce, Francesco; Verola, Massimo

    1997-03-01

    The interferometric mode of the ESO very large telescope (VLT) permits coherent combination of stellar light beams collected by four telescopes with 8 m diameter and by several auxiliary telescopes of the 2 m class. While the position of the 8 m telescopes is fixed, auxiliary telescopes can be moved on rails, and can operate from 30 stations distributed on the top of the observatory site for efficient UV coverage. Coherent beam combination can be achieved with the 8 m telescopes alone, with the auxiliary telescopes alone, or with any combination, up to eight telescopes in total. A distinct feature of the interferometric mode is the high sensitivity due to the 8 m pupil of the main telescopes, with the potential for adaptive optics compensation in the near- infrared spectral regime. The VLT interferometer is conceived as an evolutionary program where a significant fraction of the interferometer's functionality is initially funded, and more capability may be added later while experience is gained and further funding becomes available. The scientific program is now defined by a team which consists of a VLTI scientist at ESO and fifteen astronomers from the VLT community. ESO has recently decided to resume the construction of the VLTI which was delayed in December 1993, in order to achieve first interferometric fringes with two of the 8 m telescopes around the year 2000, and routine operation with 2 m auxiliary telescopes from 2003 onwards. This paper presents an overview of the recent evolution of the project and its future development.

  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. 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.

  8. 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

  9. 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.

  10. 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.

  11. 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

  12. 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.

  13. Near-IR laser-based spectrophotometer for comparative analysis of isotope content of CO{sub 2} in exhale air samples

    SciTech Connect

    Stepanov, E V; Glushko, A N; Kasoev, S G; Koval', A V; Lapshin, D A

    2011-12-31

    We present a laser spectrophotometer aimed at high-accuracy comparative analysis of content of {sup 12}CO{sub 2} and {sup 13}CO{sub 2} isotope modifications in the exhale air samples and based on a tunable near-IR diode laser (2.05 {mu}m). The two-channel optical scheme of the spectrophotometer and the special digital system for its control are described. An algorithm of spectral data processing aimed at determining the difference in the isotope composition of gas mixtures is proposed. A few spectral regions (near 4880 cm{sup -1}) are determined to be optimal for analysis of relative content of {sup 12}CO{sub 2} and {sup 13}CO{sub 2} in the exhale air. The use of the proposed spectrophotometer scheme and the developed algorithm makes the results of the analysis less susceptible to the influence of the interference in optical elements, to the absorption in the open atmosphere, to the slow drift of the laser pulse envelope, and to the offset of optical channels. The sensitivity of the comparative analysis of the isotope content of CO{sub 2} in exhale air samples, achieved using the proposed scheme, is estimated to be nearly 0.1 Per-Mille-Sign .

  14. Preliminary results of an aircraft system based on near-IR diode lasers for continuous measurements of the concentration of methane, carbon dioxide, water and its isotopes

    NASA Astrophysics Data System (ADS)

    Nadezhdinsky, A. I.; Ponurovsky, Ya. Ya.; Shapovalov, Y. P.; Popov, I. P.; Stavrovsky, D. B.; Khattatov, V. U.; Galaktionov, V. V.; Kuzmichev, A. S.

    2012-11-01

    The Federal Agency for Hydrometeorology of the Russian Federation created the flying laboratory on board the passenger airplane Yak-42D for geophysical monitoring of the environment, including aircraft measurements of vertical concentrations of greenhouse gases in the troposphere. Within the limits of this project, General Physics Institute of the Russian Academy of Science developed airborne tunable diode laser spectrometer (TDLS) on the basis of diode lasers of a near-IR range for measurement of the altitude profiles of CO2, CH4, H2O and its isotopes. TDLS complex was integrated aboard in standard 19-in. rack. Air samples, taken over an aircraft on the pipeline, were injected into the optical cell. Using the system of inflow and heating, the air was set laminar with a flowrate of 0.2 l/s at a reduced pressure of 100 mbar for detecting narrow absorption lines of water vapor isotopes. For registration of the absorption spectra and for the measurement of greenhouse gas concentrations in online mode, modulation-correlation technique was used. Diode laser spectrometer output data were transferred to the airborne central computer. Sensitivity of TDLS measurements was 20-30 ppm for water, 3-4 ppm for CO2 and 20-25 ppb for CH4. Time of one-unit measurement is about 30 ms.

  15. 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.

  16. The nature of the 2014-2015 dim state of RW Aurigae revealed by X-ray, optical, and near-IR observations

    NASA Astrophysics Data System (ADS)

    Schneider, P. C.; Günther, H. M.; Robrade, J.; Facchini, S.; Hodapp, K. W.; Manara, C. F.; Perdelwitz, V.; Schmitt, J. H. M. M.; Skinner, S.; Wolk, S. J.

    2015-12-01

    The binary system RW Aur consists of two classical T Tauri stars (CTTSs). The primary recently underwent its second observed major dimming event (ΔV ~ 2 mag). We present new, resolved Chandra X-ray and UKIRT near-IR (NIR) data as well as unresolved optical photometry obtained in the dim state to study the gas and dust content of the absorber causing the dimming. The X-ray data show that the absorbing column density increased from NH< 0.1 × 1022cm-2 during the bright state to ≈2 × 1022cm-2 in the dim state. The brightness ratio between dim and bright state at optical to NIR wavelengths shows only a moderate wavelength dependence and the NIR color-color diagram suggests no substantial reddening. Taken together, this indicates gray absorption by large grains (≳1 μm) with a dust mass column density of ≳2 × 10-4 g cm-2. Comparison with NH shows that an absorber responsible for the optical/NIR dimming and the X-ray absorption is compatible with the ISM's gas-to-dust ratio, i.e., that grains grow in the disk surface layers without largely altering the gas-to-dust ratio. Lastly, we discuss a scenario in which a common mechanism can explain the long-lasting dimming in RW Aur and recently in AA Tau. Appendix A is available in electronic form at http://www.aanda.org

  17. 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.

  18. 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)

  19. a Theoretical Characterization of Electronic States of CH2IOO and CH2OO Radicals Relevant to the Near IR Region

    NASA Astrophysics Data System (ADS)

    Dawes, Richard; Lolur, Phalgun; Huang, Meng; Kline, Neal; Miller, Terry A.

    2015-06-01

    Criegee intermediates (R1R2COO or CIs) arise from ozonolysis of biogenic and anthropogenic alkenes, which is an important process in the atmosphere. Recent breakthroughs in producing them in the gas phase have resulted in a flurry of experimental and theoretical studies. Producing the simplest CI (CH2OO) in the lab via photolysis of CH2I2 in the presence of O2 yields both CH2OO and CH2IOO with pressure dependent branching. As discussed in the preceding talk, both species might be expected to have electronic transitions in the near IR (NIR). Here we discuss electronic structure calculations used to characterize the electronic states of both systems in the relevant energy range. Using explicitly-correlated multireference configuration interaction (MRCI-F12) and coupled-cluster (UCCSD(T)-F12b) calculations we were first able to exclude CH2OO as the carrier of the observed NIR spectrum. Next, by computing frequencies and relaxed full torsional scans for the ~A and ~X states, we were able to aid in analysis and assignment of the NIR spectrum attributed to CH2IOO.

  20. 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

  1. Excited-state dynamics and enhanced near-IR emission in Nd3+-structurally activated aluminophosphate glass containing silver and tin

    NASA Astrophysics Data System (ADS)

    Jiménez, José A.; Lysenko, Sergiy; Sendova, Mariana; Zhao, Chunqing

    2015-08-01

    The excited state dynamics and near-infrared (IR) luminescent properties of Nd3+-doped melt-quenched aluminophosphate glass containing silver and tin have been investigated under pulsed-laser and steady-state excitation at 266 nm. A comparative emission dynamics assessment was carried out concerning Ag and Sn dopants in the glass matrix with and without neodymium. The data indicates an effective non-radiative energy transfer from single Ag+ ions and Sn centers as donors to neodymium activator ions which ultimately populates the 4F3/2 emitting state in Nd3+. As a result, the near-IR (1.06 μm) emission from the 4F3/2 metastable state in Nd3+ is enhanced about an order of magnitude relative to a purely Nd-doped reference. In addition, the 4F3/2 excited state lifetime becomes significantly longer in the presence of silver and tin. A comparative 31P nuclear magnetic resonance spectroscopy study suggests glass depolymerization upon neodymium doping. It is proposed that a structural alteration might be linked to the established non-radiative energy transfer.

  2. The Effect of Host Galaxy Morphology on the MBH-Lbulge Relation for Reverberation-Mapped AGN in the Near-IR

    NASA Astrophysics Data System (ADS)

    Manne-Nicholas, Emily; Bentz, Misty C.

    2015-01-01

    We present updated and nearly finalized results of our study on the effects of host galaxy morphology on the MBH-Lbulge relation for reverberation mapped AGN in the near-IR. Previous studies have suggested that the MBH-σ* relation may have an offset depending on whether the host galaxy has a bulge or pseudobulge. This would make using the MBH-σ* relation for black hole mass determinations problematic because it would require knowledge of each galaxy's structure, which would be observationally intensive and thus defeat the purpose of such a scaling relation. We have undertaken to determine whether there exists the same morphological offset in the MBH-Lbulge relation. Historically, the optical MBH-Lbulge relation has been known to exhibit a larger scatter than the MBH-σ* relation likely due to star formation regions and dust obscuration. Therefore, we have conducted our study in the H-band in order to mitigate such effects. Our updated results include preliminary measurements for most of the sample, and we also included the NICMOS measurements of Veilleux et al. 2009. If we find that the MBH-Lbulge relation has less intrinsic scatter and is less affected by galaxy morphology than MBH-σ* , then perhaps MBH-Lbulge is the more fundamental scaling relation and is a better predictor of black hole mass when direct mass measurements are not feasible.

  3. 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

  4. 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.

  5. 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.

  6. 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

  7. 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

  8. Uncovering the mechanism for selective control of the visible and near-IR absorption bands in bacteriochlorophylls a, b and g

    PubMed Central

    Fujisawa, Jun-ichi; Nagata, Morio

    2014-01-01

    Bacteriochlorophylls (BChls) play an important role as light harvesters in photosynthetic bacteria. Interestingly, bacteriochlorophylls (BChls) a, b, and g selectively tune their visible (Qx) and near IR (Qy) absorption bands by the substituent changes. In this paper, we theoretically study the mechanism for the selective control of the absorption bands. Density functional theory (DFT) and time-dependent DFT (TD-DFT) and four-orbital model analyses reveal that the selective red-shift of the Qy band with the substituent change from BChl a to b occurs with the lower-energy shift of the (HOMO, LUMO) excited state directly induced by the molecular-orbital energy changes. In contrast, the Qx band hardly shifts by the cancellation between the higher- and lower-energy shifts of the (HOMO-1, LUMO) excited state directly induced by the molecular-orbital energy changes and configuration interaction, respectively. On the other hand, with the substituent changes from BChl a to g, the Qx band selectively blue-shifts by the larger higher-energy shift of the (HOMO-1, LUMO) excited state directly induced by the molecular-orbital energy shifts than the lower-energy shift due to the configuration interaction. In contrast, the Qy band hardly shifts by the cancellation between the higher- and lower-energy shifts of the (HOMO, LUMO) excited state directly induced by the molecular-orbital energy changes and configuration interaction, respectively. Our work provides the important knowledge for understanding how nature controls the light-absorption properties of the BChl dyes, which might be also useful for design of porphyrinoid chromophores. PMID:27493495

  9. Constraining Albedo And Composition Of Potentially-Hazardous Asteroids 2004 XP14 And (100085) 1992 UY4 Via Near-IR Spectroscopy

    NASA Astrophysics Data System (ADS)

    Reddy, Vishnu; Gaffey, M. J.; Hardersen, P. S.; Abell, P. A.; Kumar, S.

    2006-09-01

    Near-infrared spectroscopic observations of potentially-hazardous asteroids (PHAs) 2004 XP14 were obtained on July 5, 2006 and 1992 UY4 on July 31, 2005, using the SpeX instrument at NASA IRTF on Mauna Kea, Hawai'i. Near-IR spectrum of 2004 XP14 has a neutral slope and shows no detectable absorption features. Given its heliocentric distance (1.02 A.U.), a sharp rise in reflectance beyond 2.0-µm due to thermal emission would be expected if the PHA was a low albedo object. No such excess was detected in the spectrum of 2004 XP14 which establishes a lower limit on the albedo. Using Standard Thermal Model and methods developed by Abell (2003), we estimate the lower limit on the albedo to be 20%. A high albedo (>20%) featureless spectrum suggests that 2004 XP14 belongs to the M- or E-type taxonomic class. 1992 UY4 spectrum also shows no detectable absorption features but exhibits a sharp rise in reflectance beyond 2.0-µm due to thermal emission at its heliocentric distance (1.08 A.U.) at the time of observation. Using the same methods, we estimate the albedo from thermal emission to be 6.0±1; %. Based on albedo, the estimated diameter (Flower & Chillemi, 1992) is 1.8±0.2 km, given the limitations in the STM model. We suggest that 1992 UY4 is a dark object with significant low-albedo absorbing species like carbon in its surface assemblage, given its featureless spectrum and 6.0±1; % albedo. The authors would like to thank NASA IRTF for providing Target of Opportunity observing time for observing 2004 XP14 flyby. This research was supported by NASA Near-Earth Objects Observations Program grant NNG04GI17G.

  10. Mergers as triggers for nuclear activity: a near-IR study of the close environment of AGN in the VISTA-VIDEO survey

    NASA Astrophysics Data System (ADS)

    Karouzos, M.; Jarvis, M. J.; Bonfield, D.

    2014-03-01

    There is an ongoing debate concerning the driver of nuclear activity in galaxies, with active galactic nuclei (AGN) either being triggered by major or minor galactic mergers or, alternatively, through secular processes like cold gas accretion and/or formation of bars. We investigate the close environment of active galaxies selected in the X-ray, the radio and the mid-IR. We utilize the first data release of the new near-IR VISTA Deep Extragalactic Observations (VIDEO) survey of the XMM-Large Scale Structure field. We use two measures of environment density, namely counts within a given aperture and a finite redshift slice (pseudo-3D density) and closest neighbour density measures Σ2 and Σ5. We select both AGN and control samples, matching them in redshift and apparent Ks-band magnitude. We find that AGN are found in a range of environments, with a subset of the AGN samples residing in overdense environments. Seyfert-like X-ray AGN and flat-spectrum radio-AGN are found to inhabit significantly overdense environments compared to their control sample. The relation between overdensities and AGN luminosity does not however reveal any positive correlation. Given the absence of an environment density-AGN luminosity relation, we find no support for a scheme where high-luminosity AGN are preferentially triggered by mergers. On the contrary, we find that AGN likely trace over dense environments at high redshift due to the fact that they inhabit the most massive galaxies, rather than being an AGN.

  11. 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

  12. 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.

  13. 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.

  14. 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.

  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. Multi-Threading for ESO Pipelines

    NASA Astrophysics Data System (ADS)

    de Bilbao, L.; Lundin, L. K.; Ballester, P.; Banse, K.; Izzo, C.; Palsa, R.; García-Dabó, C. E.

    2010-12-01

    The second generation of instruments for ESO’s VLT at Paranal Observatory will increase dramatically the volume of raw data per night. This in turn leads to very high computational needs that can be, up to some level, addressed by existing multi-core, shared-memory computers. To fully utilize these multi-processor systems we need to implement a programming environment supporting multi-threaded execution of applications. Such parallel execution needs to be introduced at the level of pipeline recipes as well as within the Common Pipeline Library (CPL) on which all operational VLT pipelines of ESO are based. We describe our approach to providing such a new, multi-threading pipeline setup and evaluate possible implementation solutions with some performance measurements.

  17. 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.

  18. 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.

  19. ESO adaptive optics facility progress report

    NASA Astrophysics Data System (ADS)

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

    2012-07-01

    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. The project has completed the procurement phase and several large structures have been delivered to Garching (Germany) and are being integrated (the AO modules GRAAL and GALACSI and the ASSIST test bench). The 4LGSF Laser (TOPTICA) has undergone final design review and a pre-production unit has been built and successfully tested. The Deformable Secondary Mirror is fully integrated and system tests have started with the first science grade thin shell mirror delivered by SAGEM. The integrated modules will be tested in stand-alone mode in 2012 and upon delivery of the DSM in late 2012, the system test phase will start. A commissioning strategy has been developed and will be updated before delivery to Paranal. A substantial effort has been spent in 2011-2012 to prepare the unit telescope to receive the AOF by preparing the mechanical interfaces and upgrading the cooling and electrical network. This preparation will also simplify the final installation of the facility on the telescope. A lot of attention is given to the system calibration, how to record and correct any misalignment and control the whole facility. A plan is being developed to efficiently operate the AOF after commissioning. This includes monitoring a relevant set of atmospheric parameters for scheduling and a Laser Traffic control system to assist the operator during the night and help/support the observing block preparation.

  20. 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. PMID:25081390

  1. Fe I oscillator strengths for the Gaia-ESO survey

    NASA Astrophysics Data System (ADS)

    Ruffoni, M. P.; Den Hartog, E. A.; Lawler, J. E.; Brewer, N. R.; Lind, K.; Nave, G.; Pickering, J. C.

    2014-07-01

    The Gaia-ESO Public Spectroscopic Survey (GES) is conducting a large-scale study of multi-element chemical abundances of some 100 000 stars in the Milky Way with the ultimate aim of quantifying the formation history and evolution of young, mature and ancient Galactic populations. However, in preparing for the analysis of GES spectra, it has been noted that atomic oscillator strengths of important Fe I lines required to correctly model stellar line intensities are missing from the atomic data base. Here, we present new experimental oscillator strengths derived from branching fractions and level lifetimes, for 142 transitions of Fe I between 3526 and 10 864 Å, of which at least 38 are urgently needed by GES. We also assess the impact of these new data on solar spectral synthesis and demonstrate that for 36 lines that appear unblended in the Sun, Fe abundance measurements yield a small line-by-line scatter (0.08 dex) with a mean abundance of 7.44 dex in good agreement with recent publications.

  2. 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

  3. Probing Heat Transfer Through Infrared (IR), Near-IR, and Visible Spectroscopy of Lattice Modes, Overtones, Hydrogen Species, and Electronic Transitions

    NASA Astrophysics Data System (ADS)

    Hofmeister, A. M.

    2006-05-01

    between the constituent grains down the temperature gradient. This process can only be quantified from absorption spectra as function of T and P simultaneously. Such data are not available. However, using available data in a revised spectroscopic model that accounts for grain size and interface reflections (Hofmeister 2004 PEPI; 2005 J. Geodynamics) reveals that near-IR absorbance, which is governed by overtones of Si-O vibrations, many types of O-H vibrations, and low-lying electronic transitions of Fe2+, largely controls krad,dif in the upper mantle, whereas electronic absorptions in visible and UV regions are important for the lower mantle. Advancing our understanding of deep mantle heat transfer calls for absorption spectroscopy over a wide spectral range at simultaneously high T and P.

  4. 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

  5. Long-term monitoring of the archetype Seyfert galaxy MCG-6-30-15: X-ray, optical and near-IR variability of the corona, disc and torus

    NASA Astrophysics Data System (ADS)

    Lira, P.; Arévalo, P.; Uttley, P.; McHardy, I. M. M.; Videla, L.

    2015-11-01

    We present long-term monitoring of MCG-6-30-15 in X-rays, optical and near-IR wavelengths, collected over 5 yr of monitoring. We determine the power spectrum density of all the observed bands and show that after taking into account the host contamination similar power is observed in the optical and near-IR bands. There is evidence for a correlation between the light curves of the X-ray photon flux and the optical B band, but it is not possible to determine a lag with certainty, with the most likely value being around 0 d. Strong correlation is seen between the optical and near-IR bands. Cross-correlation analysis shows some complex probability distributions and lags that range from 10 to 20 d, with the near-IR following the optical variations. Filtering the light curves in frequency space shows that the strongest correlations are those corresponding to the shortest time-scales. We discuss the nature of the X-ray variability and conclude that this is intrinsic and cannot be accounted for by absorption episodes due to material intervening in the line of sight. It is also found that the lags agree with the relation τ ∝ λ4/3, as expected for an optically thick geometrically thin accretion disc, although for a larger disc than that predicted by the estimated black hole mass and accretion rate in MCG-6-30-15. The cross-correlation analysis suggests that the torus is located at ˜20 light-days from the central source and at most at ˜50 light-days from the central region. This implies an active galactic nucleus bolometric luminosity of ˜3 × 1043 erg s-1 cm-2.

  6. 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

  7. 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.

  8. 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.

  9. The ESO Large Programme ``First Stars''

    NASA Astrophysics Data System (ADS)

    Bonifacio, P.; Andersen, J.; Andrievsky, S. M.; Barbuy, B.; Beers, T. C.; Caffau, E.; Cayrel, R.; Depagne, E.; François, P.; González Hernández, J. I.; Hansen, C. J.; Herwig, F.; Hill, V.; Korotin, S. A.; Ludwig, H.-G.; Molaro, P.; Nordström, B.; Plez, B.; Primas, F.; Sivarani, T.; Spite, F.; Spite, M.

    In ESO period 65 (April-September 2000) the large programme 165.N-0276, led by Roger Cayrel, began making use of UVES at the Kueyen VLT telescope. Known within the Team and outside as "First Stars", it was aimed at obtaining high resolution, high signal-to-noise ratio spectra in the range 320 nm-1000 nm for a large sample of extremely metal-poor (EMP) stars identified from the HK objective prism survey [T.C. Beers, G.W. Preston, S.A. Shectman in Astron. J. 90, 2089 (1985); T.C. Beers, G.W. Preston, S.A. Shectman in Astron. J. 103, 1987 (1992)]. The goal was to use these spectra to determine accurate atmospheric parameters and chemical composition of these stars which are among the oldest objects amenable to our detailed study. Although these stars are not the first generation of stars they must be very close descendants of the first generation. One may hope to gain insight on the nature of the progenitors from detailed information on the descendants.

  10. 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

  11. 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

  12. 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

  13. The ESO/Uppsala survey of the ESO /B/ Atlas of the southern sky. IX

    NASA Astrophysics Data System (ADS)

    Lauberts, A.; Holmberg, E. B.; Schuster, H.-E.; West, R. M.

    1981-11-01

    A systematic search has been carried out in the southern sky at declinations from -90 to -20 deg for NGC + IC galaxies, galaxies with a diameter greater than about 1.0 arcmin, disturbed galaxies, star clusters in the Budapest Catalog and planetary nebulae based on the ESO (B) Atlas. The present paper contains the ninth and final list of such objects found on 64 plates, bringing the total of objects found in the search to 18,500 in 606 fields. Included for each object are its sky and galactic coordinates, diameter, position angle, classification, description and previous references.

  14. PyMidas--A Python Interface to ESO-MIDAS

    NASA Astrophysics Data System (ADS)

    Hook, R. N.; Maisala, S.; Oittinen, T.; Ullgren, M.; Vasko, K.; Savolainen, V.; Lindroos, J.; Anttila, M.; Solin, O.; Møller, P. M.; Banse, K.; Peron, M.

    2006-07-01

    Finland joined the European Southern Observatory in 2004, providing a contribution in kind of software expertise as part of its joining fee. This significant resource, called the Sampo project, will be devoted to exploring the options for the future of data reduction and analysis in an ESO context, to understanding user requirements and to performing a series of major pilot projects to investigate different technologies, approaches and architectures. The Sampo project {http://www.eso.org/sampo} will run for three years and aims to prepare the ESO community for the data analysis and reduction challenges of the next decades. The first major Sampo project is PyMidas, an interface from Python to the ESO-MIDAS data analysis and reduction system. This paper describes the motivation for this project, how it has been implemented and gives some examples of PyMidas in action.

  15. ESO Director General to Become President of AUI

    NASA Astrophysics Data System (ADS)

    1998-11-01

    The appointment of Professor Riccardo Giacconi , Director General of the European Southern Observatory (ESO) since January 1, 1993, to the Presidency of Associated Universities, Inc. ( AUI ) in the USA, has been jointly announced by Professor Paul C. Martin, Chair of AUI's Board of Trustees and Mr. Henrik Grage, President of the ESO Council. Professor Giacconi will assume this new position at the end of his term at ESO as of July 1, 1999. AUI is a not-for-profit science management corporation that operates the National Radio Astronomy Observatory ( NRAO) under a Cooperative Agreement with the National Science Foundation (NSF). Corporate headquarters are located in Washington, D.C. The President is its chief executive officer. Nine northeastern universities joined in founding AUI in 1946: Columbia University, Cornell University, Harvard University, The Johns Hopkins University, Massachusetts Institute of Technology, the University of Pennsylvania, Princeton University, the University of Rochester, and Yale University. Over the years, AUI has taken on a broad national character with a diversified Board of Trustees from universities and other institutions across the United States. ESO is an intergovernmental organization, at present with the following member countries: Belgium, Denmark, France, Germany, Italy, The Netherlands, Sweden and Switzerland. Portugal has an agreement with ESO aiming at full membership. ESO was founded in 1962 to establish and operate an astronomical observatory in the southern hemisphere and to promote and organize co-operation in astronomical research in Europe. While the ESO Headquarters are situated in Europe, the observing facilities are located in Chile (South America). The organization's main administrative and technical departments are located at the ESO Headquarters, in Garching near Munich, Germany. They include a number of highly specialized facilities, e.g. the optical, infrared, detector and instrumentation laboratories, all

  16. 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

  17. 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

  18. Precipitable Water Vapour at the ESO Observatories: The Skill of the Forecasts

    NASA Astrophysics Data System (ADS)

    Sarazin, M.; Kerber, F.; De Breuck, C.

    2013-06-01

    Atmospheric precipitable water vapour (PWV) above an observatory is a crucial parameter for the success and quality of submillimetre and mid-infrared science observations. High precision water vapour radiometers are deployed at the ESO observatories on Paranal (VLT) and Chajnantor (APEX and ALMA), providing continuous high time-resolution measurements of PWV. These data have been used to compare the actual conditions with the forecast delivered by the publicly available Global Forecast System provided by the National Oceanographic and Atmospheric Administration. The quality of these predictions has now reached a level at which it can contribute to optimising science operations.

  19. United Kingdom to Join ESO on July 1, 2002

    NASA Astrophysics Data System (ADS)

    2001-12-01

    ESO and PPARC Councils Endorse Terms of Accession [1] The Councils of the European Southern Observatory (ESO) and the UK Particle Physics and Astronomy Research Council (PPARC) , at their respective meetings on December 3 and 5, 2001, have endorsed the terms for UK membership of ESO, as recently agreed by their Negotiating Teams. All members of the Councils - the governing bodies of the two organisations - welcomed the positive spirit in which the extensive negotiations had been conducted and expressed great satisfaction at the successful outcome of a complex process. The formal procedure of accession will now commence in the UK and is expected to be achieved in good time to allow accession from July 2002. The European Southern Observatory is the main European organisation for astronomy and the United Kingdom will become its tenth member state [2]. ESO operates two major observatories in the Chilean Atacama desert where the conditions for astronomical observations are second-to-none on earth and it has recently put into operation the world's foremost optical/infrared telescope, the Very Large Telescope (VLT) at Paranal. With UK membership, British astronomers will join their European colleagues in preparing new projects now being planned on a global scale. They will also be able to pursue their research on some of the most powerful astronomical instruments available. The ESO Director General, Dr. Catherine Cesarsky , is "delighted that we have come this far after the lengthy negotiations needed to prepare properly the admission of another major European country to our organisation. When ESO was created nearly 40 years ago, the UK was planning for its own facilities in the southern hemisphere, in collaboration with Australia, and decided not to join. However, the impressive scientific and technological advances since then and ESOs emergence as a prime player on the European research scene have convinced our UK colleagues of the great advantages of presenting a

  20. 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.

  1. 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.

  2. 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.

  3. 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.

  4. 6th ESO/OHP Summer School in Astrophysical Observations

    NASA Astrophysics Data System (ADS)

    Véron, M.-P.; Meylan, G.

    1998-09-01

    The 6th ESO/OHP Summer School was hosted again at the Observatoire de Haute-Provence (OHP) from 15 to 25 July 1998. The school, held only every second years, selects 18 of Europe's most promising young doctoral students in astronomy. Courses of lectures, observations, and analysis form the intellectual menu which is aimed at teaching the process of extracting astrophysically digestible results from the photons harvested at the telescopes, such as the ESO VLT, whose four telescopes will become available to the community in turn during the next few years.

  5. 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

  6. 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

  7. PHOENIX: the production line for science data products at ESO

    NASA Astrophysics Data System (ADS)

    Hanuschik, Reinhard

    2015-12-01

    In the past two years ESO has installed a production line for level 2 science data products. Focussing on spectroscopic observations, these in-house generated data products are complementary to the externally provided data products from the imaging surveys. The production line combines mass production (more than one million spectra have been generated so far), previews, and quality control.

  8. 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.

  9. ESO Ultra HD Expedition: New clarity for astronomy outreach

    NASA Astrophysics Data System (ADS)

    Laird, R. J. M.; Christensen, L. L.

    2014-12-01

    In the spring of 2014 a team of ESO Photo Ambassadors embarked on a pioneering expedition to the European Southern Observatory's observing sites in Chile. Their mission was to capture time-lapses, stills, videos and panoramas in crisp Ultra High Definition from some of the darkest night skies on Earth.

  10. 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.

  11. Science with ESO's Multi-conjugate Adaptive-optics Demonstrator - MAD

    NASA Astrophysics Data System (ADS)

    Melnick, Jorge; Marchetti, Enrico; Amico, Paola

    2012-07-01

    ESO's Multi-conjugate Adaptive-optics Demonstrator (MAD) was a prototype designed and built to demonstrate wide-field adaptive optics science on large telescopes. The outstanding results obtained during commissioning and guaranteed time observations (GTO) prompted ESO to issue and open call to the community for 23 science demonstration (SD) observing nights distributed in three runs (in order to provide access to the summer an winter skies). Thus, in total MAD was used for science for 33 nights including the 10 nights of GTO time. date, 19 articles in refereed journals (including one in Nature) have been published based fully or partially o MAD data. To the best of our knowledge, these are not only the first, but also the only scientific publication from MCAO instruments world-wide to date (at least in Astronomy). The scientific impact of these publication, as measured by the h-index, is comparable to that of other AO instruments on the VLT, although over the years these instruments have been allocated many more nights than MAD. In this contribution we present an overview of the scientific results from MAD and a more detailed discussion of the most cited papers.

  12. 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

  13. 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.

  14. Towards a VO compliant ESO science archive

    NASA Astrophysics Data System (ADS)

    Padovani, Paolo

    2007-08-01

    Data centres have a major role in the Virtual Observatory (VO), as they are the primary source of astronomical data. The VO cannot (and does not) dictate how a data centre handles its own archive. However, ‘VO-layer’ is needed to ‘translate’ any locally defined parameter to the standard (i.e., International Virtual Observatory Alliance compliant) ones. The longer term vision of the VO is also to hide away any observatory/telescope/instrument specific detail and work in astronomical units, for example, ‘wavelength range’ and not grism or filter name. Data providers are then advised to systematically collect metadata (‘data about data’) about the curation process, assign unique identifiers, describe the general content (e.g., physical coverage) of a collection, and provide interface and capability parameters of public services. Finally, the VO will work at its best with high-level (‘science-ready’) data, so that the VO user is spared as much as possible any complex and time consuming data reduction. Data centres should then make an effort to provide such data.

  15. Bis(mu-oxo)dicopper in Cu-ZSM-5 and its role in the decomposition of NO: a combined in situ XAFS, UV-vis-near-IR, and kinetic study.

    PubMed

    Groothaert, Marijke H; van Bokhoven, Jeroen A; Battiston, Andrea A; Weckhuysen, Bert M; Schoonheydt, Robert A

    2003-06-25

    In situ XAFS combined with UV-vis-near-IR spectroscopy are used to identify the active site in copper-loaded ZSM-5 responsible for the catalytic decomposition of NO. Cu-ZSM-5 was probed with in situ XAFS (i) after O(2) activation and (ii) while catalyzing the direct decomposition of NO into N(2) and O(2). A careful R-space fitting of the Cu K-edge EXAFS data is presented, including the use of different k-weightings and the analysis of the individual coordination shells. For the O(2)-activated overexchanged Cu-ZSM-5 sample a Cu.Cu contribution at 2.87 A with a coordination number of 1 is found. The corresponding UV-vis-near-IR spectrum is characterized by an intense absorption band at 22 700 cm(-1) and a relatively weaker band at 30 000 cm(-1), while no corresponding EPR signal is detected. Comparison of these data with the large databank of well-characterized copper centers in enzymes and synthetic model complexes leads to the identification of the bis(mu-oxo)dicopper core, i.e. [Cu(2)(mu-O)(2)](2+). After dehydration in He, Cu-ZSM-5 shows stable NO decomposition activity and the in situ XAFS data indicate the formation of a large fraction of the bis(mu-oxo)dicopper core during reaction. When the Cu/Al ratio of Cu-ZSM-5 exceeds 0.2, both the bis(mu-oxo)dicopper core is formed and the NO decomposition activity increases sharply. On the basis of the in situ measurements, a reaction cycle is proposed in which the bis(mu-oxo)dicopper core forms the product O(2) on a single active site and realizes the continuous O(2) release and concomitant self-reduction. PMID:12812505

  16. 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

  17. Minor planets discoveries at the GPO, ESO-La Silla - Dependences of stars for catalogue improvement and future perturbation studies

    NASA Astrophysics Data System (ADS)

    Debehogne, H.

    1982-09-01

    In August and September 1981, we have observed with the Grand Prism Objective (GPO) at the ESO-La Silla some Minor Planets. Parts of them were reduced at Uppsala, Turin, Rio de Janeiro (UFRJ = Universidade Federal do Rio de J. = Observatorio de Valongo; Observatorio Nacional), ESO Center at Garching, Feira de Santana (Bahia-Brasil). Here, we give those that we have computed at Uccle on our UNIVAC Computer. The great number of positions is attained owing to the automatic means we have developed at Uccle for more than 15 years and based on more than 70 years of experience. But the measurements remain very long when performed (for the sake of uniformity) by a single person as in this present publication (1614 observations).

  18. Global Near-IR Maps of Io from Gemini-N and Keck Observations in 2010, with a Specific Emphasis on Kanehekili Fluctus, Janus Patera, and Loki Patera

    NASA Astrophysics Data System (ADS)

    De Pater, I.; Davies, A. G.; Adamkovics, M.; McGregor, A.; Observing Team, G.

    2013-12-01

    We have constructed global maps of Io from observations obtained at 1-5 μm in 2010 using the adaptive optics systems on the Keck and Gemini telescopes. We compare these maps with those obtained in 2001 [1]. Although the total emission from all hot spots combined at each wavelength is similar for the two years, the spatial brightness distribution is very different, a reflection of evolving style and magnitude of volcanic activity. In 2010 thermal emission in the near-infrared was dominated by Loki Patera and Kanehekili Fluctus. We also present new timelines of thermal emission from Kanehekili Fluctus and Loki and Janus Paterae, updating timelines in recent publications [2, 3] with additional Keck adaptive optics data obtained between 2003 and 2010. These new timelines are the most comprehensive plots ever produced of the volcanic thermal emission variability for these or any other locations on Io, utilizing data from multiple ground- and space-based assets. The timeline plot shows that in 2010 Kanehekili Fluctus (as seen by Gemini) was briefly exceptionally brighter than ever seen before, evidence of a short-lived but highly-energetic eruption episode. Acknowledgements: AGD is supported by a grant from the NASA OPR Program. References: [1] Marchis et al. (2005) Icarus, 176, 96-122. [2] Davies et al. (2012) Icarus, 221, 466-470. [3] Rathbun and Spencer (2010) Icarus, 209, 625-630.

  19. Chemodynamics of the Milky Way Disk with Gaia-ESO

    NASA Astrophysics Data System (ADS)

    Hayden, Michael R.; Recio-Blanco, Alejandra; De Laverny, Patrick; Hill, Vanessa; Schultheis, Mathias; Gaia-ESO Survey Consortium

    2016-01-01

    The chemodynamic structure of the Milky Way disk provides a window into the evolutionary history of the Galaxy and is a key constraint for models of galaxy formation and evolution. We present results on the chemical and kinematic structure of the Milky Way disk using a sample of more than 20,000 stars from the fourth internal data release (iDR4) of the Gaia-ESO Survey. The Gaia-ESO Survey is a high-resolution spectroscopic survey of the Milky Way disk, bulge, and halo, which provides precision atmospheric parameters (Teff, log g, [Fe/H], [α/Fe]) for each star observed. Combined with proper motions from PPMXL, we probe the chemodynamic structure of the Milky Way disk across a range of radii (3

  20. 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.

  1. The AMBRE Project: Stellar Parameterisation of ESO Archived Spectra

    NASA Astrophysics Data System (ADS)

    de Laverny, P.; Recio-Blanco, A.; Worley, C. C.; De Pascale, M.; Hill, V.; Bijaoui, A.

    2013-09-01

    AMBRE is a Galactic archaeology project set up by ESO and the Observatoire de la Côte d'Azur in order to determine the stellar atmospheric parameters for the archived spectra from the ESO spectrographs FEROS, HARPS, UVES and GIRAFFE. A total of about 230000 spectra have now been homogeneously analysed and, for most (i.e., the slow-rotating FGKM-type stars), parameterised by their effective temperatures, surface gravities, global metallicities, α-element to iron abundance ratios and radial velocities. The determination of the stellar parameters is carried out using a pipeline that has been specifically developed for AMBRE. This pipeline is based on the MATISSE algorithm initially developed for the analysis of the Gaia Radial Velocity Spectrometer data.

  2. 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

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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

  8. The 94NOV Release of ESO-MIDAS

    NASA Astrophysics Data System (ADS)

    Science Data Analysis Group

    1994-12-01

    The new 94NOV release of ESOMIDAS will contain several improvements and new features in the core system as well as in the application areas. In this article you will find a summary of the most interesting new ones. More detailed descriptions can be found in the recent ESO-MIOAS Courier (October 1994). The new release has been tested on a variety of platforms: SUN/SunOS 4.1.n and SUN/Solaris 2.3, HP/HP-UX, SG/IRIX, IBM/AIX, VAXNMS, DEC/OSF1, DEC/Ultrix, VAX/Open-VMS and VAXNMS, and PC/Linux. At the time this Messenger is distributed, the official 94NOV version will be released and all registered sites informed about its availability in the 'midas' ftp account. In order to optimize the distribution of this new release we request that MIDAS sites with Internet connectivity retrieve it from the 'midas' ftp account. Sites with no connectivity can obtain the new release on magnetic media after having sent a completed ESO-MIDAS Request Form to the MIDAS Group (midas@eso.org).

  9. 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

  10. 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

  11. 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

  12. The Gaia-ESO Survey: chemical signatures of rocky accretion in a young solar-type star

    NASA Astrophysics Data System (ADS)

    Spina, L.; Palla, F.; Randich, S.; Sacco, G.; Jeffries, R.; Magrini, L.; Franciosini, E.; Meyer, M. R.; Tautvaišienė, G.; Gilmore, G.; Alfaro, E. J.; Allende Prieto, C.; Bensby, T.; Bragaglia, A.; Flaccomio, E.; Koposov, S. E.; Lanzafame, A. C.; Costado, M. T.; Hourihane, A.; Lardo, C.; Lewis, J.; Monaco, L.; Morbidelli, L.; Sousa, S. G.; Worley, C. C.; Zaggia, S.

    2015-10-01

    It is well known that newly formed planetary systems undergo processes of orbital reconfiguration and planetary migration. As a result, planets or protoplanetary objects may accrete onto the central star, being fused and mixed into its external layers. If the accreted mass is sufficiently high and the star has a sufficiently thin convective envelope, such events may result in a modification of the chemical composition of the stellar photosphere in an observable way, enhancing it with elements that were abundant in the accreted mass. The recent Gaia-ESO Survey observations of the 10-20 Myr old Gamma Velorum cluster have enabled identifying a star that is significantly enriched in iron with respect to other cluster members. In this Letter we further investigate the abundance pattern of this star, showing that its abundance anomaly is not limited to iron, but is also present in the refractory elements, whose overabundances are correlated with the condensation temperature. This finding strongly supports the hypothesis of a recent accretion of rocky material. Based on observations made with the ESO/VLT, at Paranal Observatory, under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey).

  13. The Gaia-ESO survey: Discovery of a spatially extended low-mass population in the Vela OB2 association

    NASA Astrophysics Data System (ADS)

    Sacco, G. G.; Jeffries, R. D.; Randich, S.; Franciosini, E.; Jackson, R. J.; Cottaar, M.; Spina, L.; Palla, F.; Mapelli, M.; Alfaro, E. J.; Bonito, R.; Damiani, F.; Frasca, A.; Klutsch, A.; Lanzafame, A.; Bayo, A.; Barrado, D.; Jiménez-Esteban, F.; Gilmore, G.; Micela, G.; Vallenari, A.; Allende Prieto, C.; Flaccomio, E.; Carraro, G.; Costado, M. T.; Jofré, P.; Lardo, C.; Magrini, L.; Morbidelli, L.; Prisinzano, L.; Sbordone, L.

    2015-02-01

    The nearby (distance ~ 350-400 pc), rich Vela OB2 association, includes γ2 Velorum, one of the most massive binaries in the solar neighbourhood and an excellent laboratory for investigating the formation and early evolution of young clusters. Recent Gaia-ESO survey observations have led to the discovery of two kinematically distinct populations in the young (10-15 Myr) cluster immediately surrounding γ2 Velorum. Here we analyse the results of Gaia-ESO survey observations of NGC 2547, a 35 Myr cluster located two degrees south of γ2 Velorum. The radial velocity distribution of lithium-rich pre-main sequence stars shows a secondary population that is kinematically distinct from and younger than NGC 2547. The radial velocities, lithium absorption lines, and the positions in a colour-magnitude diagram of this secondary population are consistent with those of one of the components discovered around γ2 Velorum. This result shows that there is a young, low-mass stellar population spread over at least several square degrees in the Vela OB2 association. This population could have originally been part of a cluster around γ2 Velorum that expanded after gas expulsion or formed in a less dense environment that is spread over the whole Vela OB2 region. Based on observations made with the ESO/VLT, at Paranal Observatory, under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey).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/574/L7

  14. 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. PMID:24509171

  15. 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)

  16. 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).

  17. Is ESO's adaptive optics facility suited for MCAO?

    NASA Astrophysics Data System (ADS)

    Marchetti, Enrico; Amico, Paola; Fedrigo, Enrico; Glindemann, Andreas; Hubin, Norbert; La Penna, Paolo; Le Louarn, Miska; Madec, Pierre-Yves

    2010-07-01

    As of 2013, the ESO's VLT will be equipped with the Adaptive Optics Facility for Ground Layer and Laser Tomography adaptive optics assisted imaging and spectroscopy, using a Deformable Secondary Mirror and four Laser Guide Stars. Following the successful experience of the MAD demonstrator, we initiated a speculative study to evaluate the performance gain obtained by implementing a type of Multi-Conjugate Adaptive Optics correction that benefits from the unique features provided by the AOF. In this paper we present the basic concept and provide a first estimation of the correction performance obtained in the near infrared.

  18. 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.

  19. Turbulence profiling methods applied to ESO's adaptive optics facility

    NASA Astrophysics Data System (ADS)

    Valenzuela, Javier; Béchet, Clémentine; Garcia-Rissmann, Aurea; Gonté, Frédéric; Kolb, Johann; Le Louarn, Miska; Neichel, Benoît; Madec, Pierre-Yves; Guesalaga, Andrés.

    2014-07-01

    Two algorithms were recently studied for C2n profiling from wide-field Adaptive Optics (AO) measurements on GeMS (Gemini Multi-Conjugate AO system). They both rely on the Slope Detection and Ranging (SLODAR) approach, using spatial covariances of the measurements issued from various wavefront sensors. The first algorithm estimates the C2n profile by applying the truncated least-squares inverse of a matrix modeling the response of slopes covariances to various turbulent layer heights. In the second method, the profile is estimated by deconvolution of these spatial cross-covariances of slopes. We compare these methods in the new configuration of ESO Adaptive Optics Facility (AOF), a high-order multiple laser system under integration. For this, we use measurements simulated by the AO cluster of ESO. The impact of the measurement noise and of the outer scale of the atmospheric turbulence is analyzed. The important influence of the outer scale on the results leads to the development of a new step for outer scale fitting included in each algorithm. This increases the reliability and robustness of the turbulence strength and profile estimations.

  20. 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. PMID:25954764

  1. 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

  2. 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

  3. Molecfit: A general tool for telluric absorption correction. I. Method and application to ESO instruments

    NASA Astrophysics Data System (ADS)

    Smette, A.; Sana, H.; Noll, S.; Horst, H.; Kausch, W.; Kimeswenger, S.; Barden, M.; Szyszka, C.; Jones, A. M.; Gallenne, A.; Vinther, J.; Ballester, P.; Taylor, J.

    2015-04-01

    Context. The interaction of the light from astronomical objects with the constituents of the Earth's atmosphere leads to the formation of telluric absorption lines in ground-based collected spectra. Correcting for these lines, mostly affecting the red and infrared region of the spectrum, usually relies on observations of specific stars obtained close in time and airmass to the science targets, therefore using precious observing time. Aims: We present molecfit, a tool to correct for telluric absorption lines based on synthetic modelling of the Earth's atmospheric transmission. Molecfit is versatile and can be used with data obtained with various ground-based telescopes and instruments. Methods: Molecfit combines a publicly available radiative transfer code, a molecular line database, atmospheric profiles, and various kernels to model the instrument line spread function. The atmospheric profiles are created by merging a standard atmospheric profile representative of a given observatory's climate, of local meteorological data, and of dynamically retrieved altitude profiles for temperature, pressure, and humidity. We discuss the various ingredients of the method, its applicability, and its limitations. We also show examples of telluric line correction on spectra obtained with a suite of ESO Very Large Telescope (VLT) instruments. Results: Compared to previous similar tools, molecfit takes the best results for temperature, pressure, and humidity in the atmosphere above the observatory into account. As a result, the standard deviation of the residuals after correction of unsaturated telluric lines is frequently better than 2% of the continuum. Conclusions: Molecfit is able to accurately model and correct for telluric lines over a broad range of wavelengths and spectral resolutions. The accuracy reached is comparable to or better than the typical accuracy achieved using a telluric standard star observation. The availability of such a general tool for telluric absorption

  4. The Gaia-ESO Survey: Insights into the inner-disc evolution from open clusters

    NASA Astrophysics Data System (ADS)

    Magrini, L.; Randich, S.; Donati, P.; Bragaglia, A.; Adibekyan, V.; Romano, D.; Smiljanic, R.; Blanco-Cuaresma, S.; Tautvaišienė, G.; Friel, E.; Overbeek, J.; Jacobson, H.; Cantat-Gaudin, T.; Vallenari, A.; Sordo, R.; Pancino, E.; Geisler, D.; San Roman, I.; Villanova, S.; Casey, A.; Hourihane, A.; Worley, C. C.; Francois, P.; Gilmore, G.; Bensby, T.; Flaccomio, E.; Korn, A. J.; Recio-Blanco, A.; Carraro, G.; Costado, M. T.; Franciosini, E.; Heiter, U.; Jofré, P.; Lardo, C.; de Laverny, P.; Monaco, L.; Morbidelli, L.; Sacco, G.; Sousa, S. G.; Zaggia, S.

    2015-08-01

    Context. The inner disc, which links the thin disc with the bulge, has been somewhat neglected in the past because of the intrinsic difficulties in its study, among which crowding and high extinction. Open clusters located in the inner disc are among thebest tracers of its chemistry at different ages and distances. Aims: We analyse the chemical patterns of four open clusters located within 7 kpc of the Galactic centre and of field stars to infer the properties of the inner disc with the Gaia-ESO survey idr2/3 data release. Methods: We derive the parameters of the newly observed cluster, Berkeley 81, finding an age of about 1 Gyr and a Galactocentric distance of ~5.4 kpc. We construct the chemical patterns of clusters and we compare them with those of field stars in the solar neighbourhood and in the inner-disc samples. Results: Comparing the three populations we observe that inner-disc clusters and field stars are both, on average, enhanced in [O/Fe], [Mg/Fe], and [Si/Fe]. Using the idr2/3 results of M67, we estimate the non-local thermodynamic equilibrium (NLTE) effect on the abundances of Mg and Si in giant stars. After empirically correcting for NLTE effects, we note that NGC 6705 and Be 81 still have a high [α/Fe]. Conclusions: The location of the four open clusters and of the field population reveals that the evolution of the metallicity [Fe/H] and of [α/Fe] can be explained within the framework of a simple chemical evolution model: both [Fe/H] and [α/Fe] of Trumpler 20 and of NGC 4815 are in agreement with expectations from a simple chemical evolution model. On the other hand, NGC 6705, and to a lesser degree Berkeley 81, have higher [α/Fe] than expected for their ages, location in the disc, and metallicity. These differences might originate from local enrichment processes as explained in the inhomogeneous evolution framework. Based on observations collected with the FLAMES spectrograph at VLT/UT2 telescope (Paranal Observatory, ESO, Chile), for the Gaia-ESO

  5. The Gaia-ESO Survey: Reevaluation of the parameters of the open cluster Trumpler 20 using photometry and spectroscopy

    NASA Astrophysics Data System (ADS)

    Donati, P.; Cantat Gaudin, T.; Bragaglia, A.; Friel, E.; Magrini, L.; Smiljanic, R.; Vallenari, A.; Tosi, M.; Sordo, R.; Tautvaišienė, G.; Blanco-Cuaresma, S.; Costado, M. T.; Geisler, D.; Klutsch, A.; Mowlavi, N.; Muñoz, C.; San Roman, I.; Zaggia, S.; Gilmore, G.; Randich, S.; Bensby, T.; Flaccomio, E.; Koposov, S. E.; Korn, A. J.; Pancino, E.; Recio-Blanco, A.; Franciosini, E.; de Laverny, P.; Lewis, J.; Morbidelli, L.; Prisinzano, L.; Sacco, G.; Worley, C. C.; Hourihane, A.; Jofré, P.; Lardo, C.; Maiorca, E.

    2014-01-01

    Trumpler 20 is an old open cluster (OC) located toward the Galactic centre, at about 3 kpc from the Sun and ~7 kpc from the Galactic centre. Its position makes this cluster particularly interesting in the framework of the chemical properties of the Galactic disc because very few old OCs reside in the inner part of the disc. For this reason it has been selected as a cluster target of the Gaia-ESO Survey, and spectra of many stars in the main-sequence and red-clump phases are now available. Moreover, although it has been studied by several authors in the past, no consensus on the evolutionary status of Tr 20 has been reached. The heavy contamination of field stars (the line of sight of Tr 20 crosses the Carina spiral arm) complicates a correct interpretation. Another interesting aspect of the cluster is that it shows a broadened main-sequence turn-off and a prominent and extended red-clump, characteristics that are not easily explained by classical evolutionary models. Exploiting both spectroscopic information from the Gaia-ESO Survey (and the ESO archive) and literature photometry, weobtain a detailed and accurate analysis of the properties of the cluster. We make use of the first accurate metallicity measurement ever obtained from several spectra of red clump stars, and of cluster membership determination using radial velocities. According to the evolutionary models adopted, we find that Tr 20 has an age in the range 1.35-1.66 Gyr, an average reddening E(B - V) in the range 0.31-0.35 mag, and a distance modulus (m - M)0 between 12.64 and 12.72 mag. The spectroscopic metallicity is [Fe/H] = +0.17 dex. We discuss the structural properties of the object and constrain possible hypotheses for its broadened upper main sequence by estimating the effect of differential reddening and its extended red clump. Based on the data obtained at ESO telescopes under programme 188.B-3002 (the public Gaia-ESO spectroscopic survey, PIs Gilmore & Randich) and on the archive data of the

  6. 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

  7. 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.

  8. 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

  9. 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).

  10. ESO & NOT photometric monitoring of the Cloverleaf quasar

    NASA Astrophysics Data System (ADS)

    Ostensen, R.; Remy, M.; Lindblad, P. O.; Refsdal, S.; Stabell, R.; Surdej, J.; Barthel, P. D.; Emanuelsen, P. I.; Festin, L.; Gosset, E.; Hainaut, O.; Hakala, P.; Hjelm, M.; Hjorth, J.; Hutsemekers, D.; Jablonski, M.; Kaas, A. A.; Kristen, H.; Larsson, S.; Magain, P.; Pettersson, B.; Pospieszalska-Surdej, A.; Smette, A.; Teuber, J.; Thomsen, B.; van Drom, E.

    1997-12-01

    The Cloverleaf quasar, H1413+117, has been photometrically monitored at ESO (La Silla, Chile) and with the NOT (La Palma, Spain) during the period 1987--1994. All good quality CCD frames have been successfully analysed using two independent methods (i.e. an automatic image decomposition technique and an interactive CLEAN algorithm). The photometric results from the two methods are found to be very similar, and they show that the four lensed QSO images vary significantly in brightness (by up to 0.45 mag), nearly in parallel. The lightcurve of the $D$ component presents some slight departures from the general trend which are very likely caused by micro-lensing effects. Upper limits, at the 99% confidence level, of 150 days on the absolute value for the time delays between the photometric lightcurves of this quadruply imaged variable QSO, are derived. This is unfortunately too large to constrain the lens model but there is little doubt that a better sampling of the lightcurves should allow to accurately derive these time delays. Pending a direct detection of the lensing galaxy (position and redshift), this system thus constitutes another good candidate for a direct and independent determination of the Hubble parameter. Based on observations collected at the European Southern Observatory (La Silla, Chile) and with the Nordic Optical Telescope (La Palma, Spain). Table 1. Logbook for the ESO and NOT observations together with photometric results for the Cloverleaf quasar. This long table can be accessed on the WWW at the URL address: http://vela.astro.ulg.ac.be/grav_lens/glp_homepage.html}

  11. 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.

  12. 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. PMID:23882157

  13. 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

  14. 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

  15. 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

  16. 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

  17. 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).

  18. 4MOST - The new wide-field, high-multiplex spectroscopic survey facility for ESO's VISTA telescope

    NASA Astrophysics Data System (ADS)

    de Jong, Roelof S.; Consortium, 4MOST

    2015-08-01

    4MOST is a wide-field, high-multiplex spectroscopic survey facility under development for the VISTA telescope of the European Southern Observatory (ESO), the only facility of its kind planned for the southern sky. Its main science drivers are in the fields of galactic archeology, high-energy physics, galaxy evolution and cosmology. 4MOST will in particular provide the spectroscopic complements to the large area surveys coming from space missions like Gaia, eROSITA, Euclid, and PLATO and from ground-based facilities like VISTA, VST, DECam, LSST and SKA. Surveys are planned to determine the chemo-dynamical structure and evolution of the Milky Way and to characterize Dark Energy as function of time through multiple methods (e.g., BAO, RSD, lensing) and tracers (galaxies, AGN, Ly-α Forest, galaxy clusters, SNe 1a).The 4MOST baseline concept features a 2.7 degree diameter field-of-view with about 2400 fibres in the focal surface that are configured by a fibre positioner based on the tilting spine principle. The fibres feed two types of spectrographs; ˜1600 fibres go to two spectrographs with resolution R>5000 (˜390-930 nm) and ˜800 fibres to a spectrograph with R>18,000 (˜392-437 nm, 515-572 nm and 605-675 nm). Both types of spectrographs are fixed-configuration, three-channel spectrographs.4MOST will have an unique operations concept in which 5 year public surveys from both the consortium and the ESO community will be combined and observed in parallel during each exposure, resulting in more than 25 million spectra of targets spread over a large fraction of the southern sky. The 4MOST Facility Simulator (4FS) was developed to demonstrate the feasibility of this observing concept. 4MOST has been accepted for implementation by ESO and has moved into its construction phase. Operations are expected to start by the early 2021.

  19. 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

  20. 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

  1. 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

  2. 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

  3. 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.

  4. ESO adaptive optics facility progress and first laboratory test results

    NASA Astrophysics Data System (ADS)

    Arsenault, Robin; Madec, Pierre-Yves; Paufique, Jérome; La Penna, Paolo; Stroebele, Stefan; Vernet, Elise; Pirard, Jean-Francois; Hackenberg, Wolfgang; Kuntschner, Harald; Kolb, Johann; Muller, Nicolas; Garcia-Rissmann, Aurea; Le Louarn, Miska; Amico, Paola; Hubin, Norbert; Lizon, Jean-Louis; Ridings, Rob; Haguenauer, Pierre; Abad, Jose A.; Fischer, Gerhard; 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; Reyes Moreno, Javier; Manescau, Antonio; Bonaccini Calia, Domenico; Quattri, Marco; Dupuy, Christophe; Guidolin, Ivan M.; Comin, Mauro; Guzman, Ronald; Buzzoni, Bernard; Quentin, Jutta; Lewis, Steffan; Jolley, Paul; Kraus, Max; Pfrommer, Thomas; Biasi, Roberto; Gallieni, Daniele; Stuik, Remko; Kaenders, Wilhelm; Ernstberger, Bernhard; Friedenauer, Axel

    2014-07-01

    The Adaptive Optics Facility project is completing the integration of its systems at ESO Headquarters in Garching. The main test bench ASSIST and the 2nd Generation M2-Unit (hosting the Deformable Secondary Mirror) have been granted acceptance late 2012. The DSM has undergone a series of tests on ASSIST in 2013 which have validated its optical performance and launched the System Test Phase of the AOF. This has been followed by the performance evaluation of the GRAAL natural guide star mode on-axis and will continue in 2014 with its Ground Layer AO mode. The GALACSI module (for MUSE) Wide-Field-Mode (GLAO) and the more challenging Narrow-Field-Mode (LTAO) will then be tested. The AOF has also taken delivery of the second scientific thin shell mirror and the first 22 Watt Sodium laser Unit. We will report on the system tests status, the performances evaluated on the ASSIST bench and advancement of the 4Laser Guide Star Facility. We will also present the near future plans for commissioning on the telescope and some considerations on tools to ensure an efficient operation of the Facility in Paranal.

  5. The Spanish in-kind contribution to ESO - Pipelines

    NASA Astrophysics Data System (ADS)

    de Bilbao, L.; Ballester, P.

    2011-11-01

    Ever since entering ESO in 2006, Spain has made an in-kind contribution invarious fields. In the Pipeline Systems Department (PSD), this contribution hasbeen made to a number of projects, in particular to the CPL (Common Pipeline Library), to the pipelines of the instruments ISAAC, SofI and FORS, and to theintegration of the pipeline for the new VISTA telescope into the DFS (Data FlowSystem) at Paranal. Some of these projects started with the VLT a decade ago, and have experiencedan evolution since, as a consequence of standardization processes, of thesearch of elements in common and, especially in the last couple of years, ofthe efforts to provide the astronomy community with 'science-ready' dataproducts. At the same time, the PSD faces new challenges today, as the dramatic increase in the data volume of the Paranal Observatory since the start of operations of VISTA, or the needs of the pipelines of the future instruments of the E-ELT. In the latter, more concretely, the current status of the CPL is being analyzed, with the goal of establishing the necessary changes to meet those future needs.In this article we introduce briefly these projects and detail the Spanish in-kind contribution to them.

  6. 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

  7. Minor planets discoveries at the GPO, ESO-La Silla in September 1983 - Dependences of stars for catalogue improvement and future perturbation studies

    NASA Astrophysics Data System (ADS)

    Debehogne, H.

    1985-01-01

    In August and September 1983, we have observed with the Grand Prisme Objectif (GPO) at ESO-La Silla some Minor Planets. Some of the data were reduced at Uppsala, Rio de Janeiro (Observatorio do Valongo - UFRJ = Universidade Federal do Rio de Janeiro, Observatorio Nacional) and at ESO-Garching. Here, we give results obtained at Uccle on our UNIVAC computer. The great number of positions is obtained owing to the automatic means we have developed at Uccle for more than 15 years and based on more than 70 years of experience. But the measurements remain very time-consuming when performed (for the sake of uniformity) by a single person as in this present publication (583 positions).

  8. 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

  9. 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

  10. 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).

  11. 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

  12. The Gaia-ESO Survey: metallicity and kinematic trends in the Milky Way bulge

    NASA Astrophysics Data System (ADS)

    Rojas-Arriagada, A.; Recio-Blanco, A.; Hill, V.; de Laverny, P.; Schultheis, M.; Babusiaux, C.; Zoccali, M.; Minniti, D.; Gonzalez, O. A.; Feltzing, S.; Gilmore, G.; Randich, S.; Vallenari, A.; Alfaro, E. J.; Bensby, T.; Bragaglia, A.; Flaccomio, E.; Lanzafame, A. C.; Pancino, E.; Smiljanic, R.; Bergemann, M.; Costado, M. T.; Damiani, F.; Hourihane, A.; Jofré, P.; Lardo, C.; Magrini, L.; Maiorca, E.; Morbidelli, L.; Sbordone, L.; Worley, C. C.; Zaggia, S.; Wyse, R.

    2014-09-01

    systematic differences in the velocity dispersion between the metal-rich and the metal-poor components of each field. Conclusions: The iDR1 bulge data show chemo-dynamical distributions that are consistent with varying proportions of stars belonging to (i) a metal-rich boxy/peanut X-shaped component, with bar-like kinematics; and (ii) a metal-poor more extended rotating structure with a higher velocity dispersion that dominates far from the Galactic plane. These first GES data already allow studying the detailed spatial dependence of the Galactic bulge populations, thanks to the analysis of individual fields with relatively high statistics. Based on observations made with the ESO/VLT, at Paranal Observatory, under program 188.B-3002, The Gaia-ESO Public Spectroscopic Survey.

  13. 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.

  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.

  15. 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.

  16. Automated data reduction workflows for astronomy. The ESO Reflex environment

    NASA Astrophysics Data System (ADS)

    Freudling, W.; Romaniello, M.; Bramich, D. M.; Ballester, P.; Forchi, V.; García-Dabló, C. E.; Moehler, S.; Neeser, M. J.

    2013-11-01

    Context. Data from complex modern astronomical instruments often consist of a large number of different science and calibration files, and their reduction requires a variety of software tools. The execution chain of the tools represents a complex workflow that needs to be tuned and supervised, often by individual researchers that are not necessarily experts for any specific instrument. Aims: The efficiency of data reduction can be improved by using automatic workflows to organise data and execute a sequence of data reduction steps. To realize such efficiency gains, we designed a system that allows intuitive representation, execution and modification of the data reduction workflow, and has facilities for inspection and interaction with the data. Methods: The European Southern Observatory (ESO) has developed Reflex, an environment to automate data reduction workflows. Reflex is implemented as a package of customized components for the Kepler workflow engine. Kepler provides the graphical user interface to create an executable flowchart-like representation of the data reduction process. Key features of Reflex are a rule-based data organiser, infrastructure to re-use results, thorough book-keeping, data progeny tracking, interactive user interfaces, and a novel concept to exploit information created during data organisation for the workflow execution. Results: Automated workflows can greatly increase the efficiency of astronomical data reduction. In Reflex, workflows can be run non-interactively as a first step. Subsequent optimization can then be carried out while transparently re-using all unchanged intermediate products. We found that such workflows enable the reduction of complex data by non-expert users and minimizes mistakes due to book-keeping errors. Conclusions: Reflex includes novel concepts to increase the efficiency of astronomical data processing. While Reflex is a specific implementation of astronomical scientific workflows within the Kepler workflow

  17. 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.

  18. 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

  19. 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

  20. 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

  1. Strategy for monitoring T cell responses to NY-ESO-1 in patients with any HLA class I allele.

    PubMed

    Gnjatic, S; Nagata, Y; Jager, E; Stockert, E; Shankara, S; Roberts, B L; Mazzara, G P; Lee, S Y; Dunbar, P R; Dupont, B; Cerundolo, V; Ritter, G; Chen, Y T; Knuth, A; Old, L J

    2000-09-26

    NY-ESO-1 elicits frequent antibody responses in cancer patients, accompanied by strong CD8(+) T cell responses against HLA-A2-restricted epitopes. To broaden the range of cancer patients who can be assessed for immunity to NY-ESO-1, a general method was devised to detect T cell reactivity independent of prior characterization of epitopes. A recombinant adenoviral vector encoding the full cDNA sequence of NY-ESO-1 was used to transduce CD8-depleted peripheral blood lymphocytes as antigen-presenting cells. These modified antigen-presenting cells were then used to restimulate memory effector cells against NY-ESO-1 from the peripheral blood of cancer patients. Specific CD8(+) T cells thus sensitized were assayed on autologous B cell targets infected with a recombinant vaccinia virus encoding NY-ESO-1. Strong polyclonal responses were observed against NY-ESO-1 in antibody-positive patients, regardless of their HLA profile. Because the vectors do not cross-react immunologically, only responses to NY-ESO-1 were detected. The approach described here allows monitoring of CD8(+) T cell responses to NY-ESO-1 in the context of various HLA alleles and has led to the definition of NY-ESO-1 peptides presented by HLA-Cw3 and HLA-Cw6 molecules. PMID:11005863

  2. The Gaia-ESO Survey: Stellar radii in the young open clusters NGC 2264, NGC 2547, and NGC 2516

    NASA Astrophysics Data System (ADS)

    Jackson, R. J.; Jeffries, R. D.; Randich, S.; Bragaglia, A.; Carraro, G.; Costado, M. T.; Flaccomio, E.; Lanzafame, A. C.; Lardo, C.; Monaco, L.; Morbidelli, L.; Smiljanic, R.; Zaggia, S.

    2016-02-01

    of both. 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 Tables 1 and 3 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/586/A52

  3. Tests of MATISSE on large spectral datasets from the ESO archive

    NASA Astrophysics Data System (ADS)

    Worley, C. C.; de Laverny, P.; Recio-Blanco, A.; Hill, V.; Bijaoui, A.; Ordenovic, C.; Vernisse, Y.

    2011-02-01

    The automated stellar classification algorithm, MATISSE, has been developed at the Observatoire de la Côte d'Azur (OCA) as a means of determining stellar effective temperatures, surface gravities and chemical abundances for large samples of stellar spectra. MATISSE is one of the key programmes to be used in the analysis of the spectra that will be obtained by the Radial Velocity Spectrometer (RVS) on the European Space Agency's (ESA) Gaia satellite. In preparation for the Gaia mission, rigorous testing of MATISSE is currently being carried out using large datasets of spectra from the European Southern Observatory (ESO) archive (The AMBRE Project, a collaboration between ESO and OCA). The derived stellar parameters will be delivered to ESO in order to make them available to the astronomical community via the Virtual Observatory. This paper presents the preliminary results of the analysis of the archived FEROS spectra.

  4. 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.

  5. 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).

  6. 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.

  7. 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

  8. NY-ESO-1–specific immunological pressure and escape in a patient with metastatic melanoma

    PubMed Central

    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. PMID:23882157

  9. 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.

    2016-04-01

    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

  10. 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

  11. 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).

  12. Positions of Asteroids and Comets Obtained in 1983 with the GPO Telescope at ESO Chile

    NASA Astrophysics Data System (ADS)

    de Sanctis, G.

    283 accurate positions for 25 numbered and 1 unnumbered asteroids and 2 comets are presented, from observations obtained during April 1983 at the GPO telescope of ESO, La Silla, Chile. Reductions were made using the dependence method with 6 reference stars taken from AGK 3 and SAO catalogues.

  13. Visitor instruments in the ESO Very Large Telescope Observatory in Paranal

    NASA Astrophysics Data System (ADS)

    Robert, Pascal

    2008-07-01

    This paper is presenting the implementation of the concept of a Visitor Instrument at the Very Large Telescope observatory of ESO at Paranal. The focus on the Nasmyth A of Melipal UT#3 (8m telescope) is dedicated to receive these Visitor Instruments. This concept consists in the installation of an Instrument at the Visitor focus for an observation run for a limited period of time, and then to remove the instrument. The selection of the instrument is done according to its scientific and innovative outcome compared to the other ESO instruments already existing in the observatory. Once granted an observation run of several nights, the visitor Instrument has to show its compliance with the requirements of Paranal Observatory. Then the implementation and integration of the Visitor Instrument are scheduled according to the needs of the Institute who developed the instrument. The instrument is installed at Paranal with the support of ESO staff. The Visitor Instrument can be operated in 2 different modes according to its level of compliance to the ESO specifications. Immediately after the observation run is finished, the instrument is removed from the Visitor Focus.

  14. Physical studies of asteroids. XXV - Photoelectric photometry of asteroids obtained at ESO and Hoher List Observatory

    NASA Astrophysics Data System (ADS)

    Lagerkvist, C.-I.; Magnusson, P.; Debehogne, H.; Hoffmann, M.; Erikson, A.; de Campos, A.; Cutispoto, G.

    1992-11-01

    Photoelectric photometry of 14 asteroids, carried out at ESO and the Hoher List Observatory during 1990 and 1991, are presented. Composite lightcurves were derived for the asteroids 140 Siwa, 238 Hypatia, 347 Pariana, 389 Industria and 1593 Fagnes. UBV colors are also given for ten of the asteroids.

  15. 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.

  16. 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.

  17. 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.

  18. 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.

  19. 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.

  20. ASAS-SN Discovery of A Probable Supernova in ESO 297-G037

    NASA Astrophysics Data System (ADS)

    Brimacombe, J.; Holoien, T. W.-S.; Stanek, K. Z.; Kochanek, C. S.; Brown, J. S.; Danilet, A. B.; Simonian, G.; Basu, U.; Beacom, J. F.; Thompson, T. A.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Falco, E.; Wozniak, P. R.; Szczygiel, D.; Pojmanski, G.; Conseil, E.; Fernandez, J. M.; Kiyota, S.; Nicholls, B.; Nicolas, J.; Wiethoff, W.

    2015-06-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the double 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 297-G037.

  1. ASAS-SN Discovery of A Probable Supernova in ESO 069-G005

    NASA Astrophysics Data System (ADS)

    Brimacombe, J.; Holoien, T. W.-S.; Stanek, K. Z.; Kochanek, C. S.; Danilet, A. B.; Simonian, G.; Basu, U.; Goss, N.; Beacom, J. F.; Thompson, T. A.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Wozniak, P. R.; Falco, E.; Szczygiel, D.; Pojmanski, G.; Carballo, J. G.; Kiyota, S.; Koff, R. A.; Krannich, G.; Monard, L. A. G.; Nicholls, B.; Nicolas, J.; Wiethoff, W.

    2015-04-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the double 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 069-G005.

  2. ASAS-SN Discovery of A Probable Supernova in ESO 221-G012

    NASA Astrophysics Data System (ADS)

    Brimacombe, J.; Holoien, T. W.-S.; Stanek, K. Z.; Kochanek, C. S.; Brown, J. S.; Danilet, A. B.; Simonian, G.; Basu, U.; Beacom, J. F.; Thompson, T. A.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Falco, E.; Wozniak, P. R.; Szczygiel, D.; Pojmanski, G.; Carballo, J. G.; Conseil, E.; Kiyota, S.; Koff, R. A.; Masi, G.; Nicholls, B.; Nicolas, J.; Wiethoff, W.

    2015-07-01

    During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the double 14-cm "Cassius" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy ESO 221-G012.

  3. ASAS-SN Discovery of A Probable Supernova in ESO 357-G005

    NASA Astrophysics Data System (ADS)

    Brimacombe, J.; Marples, P.; Kiyota, S.; Bock, G.; Brown, J. S.; Stanek, K. Z.; Holoien, T. W.-S.; Kochanek, C. S.; Rivera, D. Godoy; Simonian, G.; Basu, U.; Beacom, J. F.; Thompson, T. A.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Dong, Subo; Chen, Ping; Falco, E.; Wozniak, P. R.; Pojmanski, G.; Cruz, I.; Koff, R. A.; Nicolas, J.

    2015-09-01

    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 357-G005.

  4. 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.

  5. 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.

  6. VizieR Online Data Catalog: FeI oscillator strengths for Gaia-ESO (Ruffoni+, 2014)

    NASA Astrophysics Data System (ADS)

    Ruffoni, M. P.; den Hartog, E. A.; Lawler, J. E.; Brewer, N. R.; Lind, K.; Nave, G.; Pickering, J. C.

    2014-10-01

    The Gaia-ESO Public Spectroscopic Survey (GES) is conducting a large-scale study of multi-element chemical abundances of some 100000 stars in the Milky Way with the ultimate aim of quantifying the formation history and evolution of young, mature and ancient Galactic populations. However, in preparing for the analysis of GES spectra, it has been noted that atomic oscillator strengths of important FeI lines required to correctly model stellar line intensities are missing from the atomic data base. Here, we present new experimental oscillator strengths derived from branching fractions and level lifetimes, for 142 transitions of FeI between 3526 and 10864Å, of which at least 38 are urgently needed by GES. We also assess the impact of these new data on solar spectral synthesis and demonstrate that for 36 lines that appear unblended in the Sun, Fe abundance measurements yield a small line-by-line scatter (0.08dex) with a mean abundance of 7.44dex in good agreement with recent publications. (3 data files).

  7. 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

  8. 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

  9. 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

  10. 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.

  11. 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

  12. An overview of AONGC and the ESO adaptive optics wave front sensing camera

    NASA Astrophysics Data System (ADS)

    Reyes, Javier; Downing, Mark; Conzelmann, Ralf; Mehrgan, Leander; Stegmeier, Joerg; Todorovic, Mirko; Molina-Conde, Ignacio

    2012-07-01

    The detector controller requirements for Adaptive Optics (AO) cameras presents numerous challenges in the design of the electronics, all of which have led to highly customized controller development in order to meet the requirements of high frame rate, low-noise and low image latency in a compact sized camera. This paper presents an overview of the ESO AOWFS camera and AONGC, the Adaptive Optics ESO's new detector controller; the challenges and excellent progress in achieving detector limited performance from the e2v EMCCD CCD220, along with test results demonstrating sub-electron read noise at frame rates in excess of 1500 Hz. Pre-series cameras have been delivered for use in 2nd Generation VLT instruments (AOF and SPHERE).

  13. Galactic archaeology of a thick disc: Excavating ESO 533-4 with VIMOS

    NASA Astrophysics Data System (ADS)

    Comerón, S.; Salo, H.; Janz, J.; Laurikainen, E.; Yoachim, P.

    2015-12-01

    The disc of galaxies is made of the superposition of a thin and a thick disc. Star formation is hosted in the thin discs and contributes to their growth. Thick discs are formed of old stars. The formation mechanisms of thick discs are under discussion. Thick discs might have formed either at high redshift on a short timescale or might have been built slowly over a Hubble-Lemaître time. They may have an internal or an external origin. Here we adopt a galactic archaeology approach to study the thick disc of ESO 533-4, i.e. we study the kinematics and the stellar populations of this galaxy in detail. ESO 533-4 is a Southern, nearby, and almost bulgeless galaxy. We present the first ever Integral Field Unit spectroscopy of an edge-on galaxy with enough depth and quality to study the thick disc. We exposed ESO 533-4 with the blue grism of the VIMOS instrument of the VLT for 6.5 h. The field of view covered an axial extent from ~ 0.1 r25 to ~ 0.7 r25, where r25 is the 25 mag arcsec-2 isophotal radius. This corresponds to the range from ~1 kpc to ~7 kpc. We used pPXF and the MILES library to obtain velocity and stellar population maps. We compared our kinematic data with simple GADGET-2 models. The apparent rotational lag of the thick disc of ESO 533-4 is compatible with that expected from the combinations of two effects: differential asymmetric drift and the projection effects arising from studying a disc a few degrees (2-3°) away from edge-on. Thus, ESO 533-4 contains little or no counter-rotating material. This is compatible with three formation scenarios: the secular dynamical heating of an initially thin disc, the formation of the thick disc at high redshift in an early turbulent disc phase, and the creation of a thick disc in a major merger event. If this last mechanism occurred in all galaxies, it would cause retrograde thick discs in half of them. These retrograde discs have not been observed in the five massive disc galaxies (circular velocity vc ≳ 120 km s-1

  14. The MATISSE analysis of large spectral datasets from the ESO Archive

    NASA Astrophysics Data System (ADS)

    Worley, C.; de Laverny, P.; Recio-Blanco, A.; Hill, V.; Vernisse, Y.; Ordenovic, C.; Bijaoui, A.

    2010-12-01

    The automated stellar classification algorithm, MATISSE, has been developed at the Observatoire de la Côte d'Azur (OCA) in order to determine stellar temperatures, gravities and chemical abundances for large datasets of stellar spectra. The Gaia Data Processing and Analysis Consortium (DPAC) has selected MATISSE as one of the key programmes to be used in the analysis of the Gaia Radial Velocity Spectrometer (RVS) spectra. MATISSE is currently being used to analyse large datasets of spectra from the ESO archive with the primary goal of producing advanced data products to be made available in the ESO database via the Virtual Observatory. This is also an invaluable opportunity to identify and address issues that can be encountered with the analysis large samples of real spectra prior to the launch of Gaia in 2012. The analysis of the archived spectra of the FEROS spectrograph is currently underway and preliminary results are presented.

  15. 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.

  16. The ESO adaptive optics real-time computer platform: a step toward the future

    NASA Astrophysics Data System (ADS)

    Fedrigo, Enrico; Donaldson, Robert; Soenke, Christian; Hubin, Norbert N.

    2004-10-01

    ESO now operates several AO systems in the Paranal observatory. Most of them are the outcome of different and independent efforts resulting in different and incompatible systems with all the problems of maintaining and evolving them. At the same time, industry is now proposing powerful embedded computers and new standard technologies that enable the construction of massive real time parallel computers, with a technology roadmap that looks extremely promising. The ESO AO Platform initiative aims at taking this unique opportunity of gathering all the experience accumulated so far in building and operating AO system and the recent advances offered by the industry to define and build a standard hardware and software platform able to run every AO system of the near future of the VLT with an eye towards OWL. We review the key technologies that enable the design of a common AO-RTC and we discuss the main choices of the AO Platform initiative.

  17. 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.

  18. Assembly and test results of the AOF laser guide star units at ESO

    NASA Astrophysics Data System (ADS)

    Hackenberg, W.; Bonaccini Calia, D.; Buzzoni, B.; Comin, M.; Dupuy, C.; Gago, F.; Guidolin, I. M.; Guzman, R.; Holzloehner, R.; Kern, L.; Kirchbauer, J.-.; Lewis, S.; Lizon, J.-.; McLay, S.; Pfrommer, T.; Quattri, M.; Quentin, J.; Ridings, R.

    2014-08-01

    The Four Laser Guide Star Facility (4LGSF) is part of the ESO Adaptive Optics Facility, in which one of the VLT telescopes, UT4, is transformed in an adaptive telescope-equipped with a deformable secondary mirror, two adaptive optics systems at the Nasmyth focii and four sodium laser guide star modular units. In this paper we present the design, the assembly and validation test performed so far in Europe on the first laser guide star unit.

  19. TWO-DIMENSIONAL KINEMATICS OF THE EDGE-ON SPIRAL GALAXY ESO 379-006

    SciTech Connect

    Rosado, M.; Gabbasov, R. F.; Repetto, P.; Martos, M.; Fuentes-Carrera, I.; Amram, P.; Hernandez, O.

    2013-05-15

    We present a kinematical study of the nearly edge-on galaxy ESO 379-006 that shows the existence of extraplanar ionized gas. With Fabry-Perot spectroscopy at H{alpha}, we study the kinematics of ESO 379-006 using velocity maps and position-velocity diagrams parallel to the major and to the minor axis of the galaxy. We build the rotation curve of the disk and discuss the role of projection effects due to the fact of viewing this galaxy nearly edge-on. The twisting of the isovelocities in the radial velocity field of the disk of ESO 379-006 as well as the kinematical asymmetries found in some position-velocity diagrams parallel to the minor axis of the galaxy suggest the existence of deviations to circular motions in the disk that can be modeled and explained with the inclusion of a radial inflow probably generated by a bar or by spiral arms. We succeeded in detecting extraplanar diffuse ionized gas in this galaxy. At the same time, from the analysis of position-velocity diagrams, we found some evidence that the extraplanar gas could lag in rotation velocity with respect to the midplane rotation.

  20. Complex Stellar System ESO65SC03: Open Cluster or Remnant?

    NASA Astrophysics Data System (ADS)

    Joshi, Gireesh C.; Joshi, Y. C.; Joshi, S.; Chowdhury, S.; Tyagi, R. K.

    2015-06-01

    We present a complete spatial and dynamical study of the poorly populated stellar system ESO65SC03. The radial distribution of the system gives a core and cluster radii of 1.10±0.63 and 5.36±0.24 arcmin, respectively. The SNDP does not show any clear enhancement of the surface stellar number density between the stars of the system and the field regions. We derive the optimum isochrone solution for a particular grid size in the CMD using the statistical cleaning procedure. Using the statistically cleaned CMDs, we find the distance modulus, (m - M)0, and reddening, E(B - V), of the system to be 11.8±0.2 and 0.45 mag, respectively. The mean proper motion of this system is - 5.37±0.81 mas yr-1 and 0.31±0.40 in RA and DEC directions, respectively. The mean proper motion of this system is found to be almost similar to the field region. The mass function for the brighter stars is found to be too high for the system to be an open cluster. These combined results place constraints on whether stellar system ESO65SC03 is a POCR or an Asterism. Our understanding is that the ESO65SC03 is in a stage of POCR by losing their main-sequence stars in the dynamic evolution processes.

  1. Core network infrastructure supporting the VLT at ESO Paranal in Chile

    NASA Astrophysics Data System (ADS)

    Reay, Harold

    2000-06-01

    In October 1997 a number of projects were started at ESO's Paranal Observatory at Cerro Paranal in Chile to upgrade the communications infrastructure in place at the time. The planned upgrades were to internal systems such as computer data networks and telephone installations and also data links connecting Paranal to other ESO sites. This paper details the installation work carried out on the Paranal Core Network (PCN) during the period of October 1997 to December 1999. These installations were to provide both short term solutions to the requirement for reliable high bandwidth network connectivity between Paranal and ESO HQ in Garching, Germany in time for UTI (Antu) first light and perhaps more importantly, to provide the core systems necessary for a site moving towards operational status. This paper explains the reasons for using particular cable types, network topology, and fiber backbone design and implementation. We explain why it was decided to install the PCN in two distinct stages and how equipment used in temporary installations was re-used in the Very Large Telescope networks. Finally we describe the tools used to monitor network and satellite link performance and will discuss whether network backbone bandwidth meets the expected utilization and how this bandwidth can easily be increased in the future should there be a requirement.

  2. The ESO transportable LGS Unit for measurements of the LGS photon return and other experiments

    NASA Astrophysics Data System (ADS)

    Bonaccini Calia, D.; Guidolin, I.; Friedenauer, A.; Hager, M.; Karpov, V.; Pfrommer, T.; Holzlöhner, R.; Lewis, S.; Hackenberg, W.; Lombardi, G.; Centrone, M.; Pedichini, F.

    2012-09-01

    Sodium laser guide stars (LGS) are used, or planned to be used, as single or multiple artificial beacons for Adaptive Optics in many present or future large and extremely large telescopes projects. In our opinion, several aspects of the LGS have not been studied systematically and thoroughly enough in the past to ensure optimal system designs. ESO has designed and built, with support from industry, an experimental transportable laser guide star unit, composed of a compact laser based on the ESO narrow-band Raman Fiber Amplifier patented technology, attached to a 30cm launch telescope. Besides field tests of the new laser technology, the purpose of the transportable unit is to conduct field experiments related to LGS and LGS-AO, useful for the optimization of future LGS-AO systems. Among the proposed ones are the validation of ESO LGS return flux simulations as a function of CW and pulsed laser properties, the feasibility of line-of-sight sodium profile measurements via partial CW laser modulation and tests of AO operation with elongated LGS in the EELT geometry configuration. After a description of the WLGSU and its main capabilities, results on the WLGSU commissioning and LGS return flux measurements are presented.

  3. 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.

  4. 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

  5. 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

  6. 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.

  7. 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

  8. Tunable Single-Frequency Near IR Lasers for DIAL Applications

    NASA Technical Reports Server (NTRS)

    Henderson, Sammy W.; Marquardt, John H.; Carrig, Timothy J.; Gatt, Phil; Smith, Duane D.; Hale, Charley P.

    2000-01-01

    Tunable single-frequency sources in the 2-4 micron wavelength region are useful for remote DIAL measurements of chemicals and pollutants. We are developing tunable single-frequency transmitters and receivers for both direct and coherent detection lidar measurement applications. We have demonstrated a direct-diode-pumped PPLN-based OPO that operates single frequency, produces greater than 10 mW cw and is tunable over the 2.5 - 3.9 micron wavelength region. This laser has been used to injection seed a pulsed PPLN OPO, pumped by a 1.064 micron Nd:YAG laser, producing 50-100 microJoule single-frequency pulses at 100 Hz PRF near 3.6 micron wavelength. In addition, we have demonstrated a cw Cr:ZnSe laser that is tunable over the 2.1 - 2.8 micron wavelength region. This laser is pumped by a cw diode-pumped Tm:YALO laser and has produced over 1.8 W cw. Tm- and Tm, Ho-doped single-frequency solid-state lasers that produce over 50 mW cw and are tunable over approximately 10 nm in the 2 -2.1 micron band with fast PZT tuning have also been demonstrated. A fast PZT-tunable Tm, Ho:YLF laser was used for a direct-detection column content DIAL measurement of atmospheric CO2. Modeling shows that that all these cw and pulsed sources are useful for column-content coherent DIAL measurements at several km range using topographic targets.

  9. Silicon microspheres for near-IR communication applications

    NASA Astrophysics Data System (ADS)

    Serpengüzel, Ali; Demir, Abdullah

    2008-06-01

    We have performed transverse electric and transverse magnetic polarized elastic light scattering calculations at 90° and 0° in the o-band at 1.3 µm for a 15 µm radius silicon microsphere with a refractive index of 3.5. The quality factors are on the order of 107 and the mode/channel spacing is 7 nm, which correlate well with the refractive index and the optical size of the microsphere. The 90° elastic light scattering can be used to monitor a dropped channel (drop port), whereas the 0° elastic scattering can be used to monitor the transmission channel (through port). The optical resonances of the silicon microspheres provide the necessary narrow linewidths that are needed for high-resolution optical communication applications. Potential telecommunication applications include filters, modulators, switches, wavelength converters, detectors, amplifiers and light sources. Silicon microspheres show promise as potential building blocks for silicon-based electrophotonic integration.

  10. Temporal Variations in the Uranian Near-IR Geometric Albedo

    NASA Astrophysics Data System (ADS)

    Walter, C. M.; Marley, M. S.; Baines, K. H.

    1996-09-01

    Over the period August 1995 -- August 1996 the near-infrared geometric albedo of Uranus showed distinct variation. We obtained images of the planet in 10 broad and narrowband filters using the ARC 3.5 meter telescope at Apache Point Observatory. Along with the albedo variations we saw significant changes in the contrast of the planet. Data acquired in August 1995 (Walter & Marley 1995) show the same high altitude hazes encircling the south polar region as seen by Baines et al. (1995) from the IRTF two days prior to our observations and by HST in August 1994. Followup images from June 1996 no longer contain this asymmetry, instead showing a homogeneous disk with corresponding lower albedos at matching wavelengths. Observations will also be made in late August 1996. We modeled this data by computing theoretical monochromatic albedos which were then integrated over the filter bandpasses. These filters were chosen to best probe a variety of atmospheric levels, with continuum filters probing down to the CH_4 tropospheric cloud and beyond. Filters selected in the deep H_2 and CH_4 absorption bands allow us to examine the structure of hazes in the upper stratosphere, whose small reflection contributions dominate in these dark filters. Preliminary analysis of information from two very different states of Uranian weather shows evidence for temporal variability in the vertical location and thickness of the CH_4 cloud as well as the incompatibility of extrapolating optical stratospheric haze characteristics in the near-infrared. This work was supported by NASA grant NGT-51383. Baines, K. H., Yanamandra-Fisher, P., Lebofsky, L. A., Momary, T. W., & Golisch, W. 1995, BAAS, 27, 1088. Walter, C & Marley, M. S. 1995, BAAS, 27, 1089.

  11. 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.

  12. Near-IR photon number resolving detector design

    NASA Astrophysics Data System (ADS)

    Bogdanski, Jan; Huntington, Elanor H.

    2013-05-01

    Photon-Number-Resolving-Detection (PNRD) capability is crucial for many Quantum-Information (QI) applications, e.g. for Coherent-State-Quantum-Computing, Linear-Optics-Quantum-Computing. In Quantum-Key-Distribution and Quantum-Secret-Sharing over 1310/1550 nm fiber, two other important, defense and information security related, QI applications, it's crucial for the information transmission security to guarantee that the information carriers (photons) are single. Thus a PNRD can provide an additional security level against eavesdropping. Currently, there are at least a couple of promising PNRD technologies in the Near-Infrared, but all of them require cryogenic cooling. Thus a compact, portable PNRD, based on commercial Avalanche-Photo-Diodes (APDs), could be a very useful instrument for many QI experiments. For an APD-based PNRD, it is crucial to measure the APD-current in the beginning of the avalanche. Thus an efficient cancellation of the APD capacitive spikes is a necessary condition for the very weak APD current measurement. The detector's principle is based on two commercial, pair-matched InGaAs/InP APDs, connected in series. It leads to a great cancelation of the capacitive spikes caused by the narrow (300 ps), differential gate-pulses of maximum 4V amplitude assuming that both pulses are perfectly matched in regards to their phases, amplitudes, and shapes. The cancellation scheme could be used for other APD-technologies, e.g. Silicon, extending the detection spectrum from visible to NIR. The design distinguishes itself from other, APD-based, schemes by its scalability feature and its computer controlled cancellation of the capacitive spikes. Furthermore, both APDs could be equally used for the detection purpose, which opens a possibility for the odd-even photon number parity detection.

  13. Near-IR Spectroscopy of V-type Asteroids

    NASA Astrophysics Data System (ADS)

    Hardersen, Paul S.; Genet, Russell M.; Roberts, Rachel

    2013-05-01

    Two nights of observing were conducted at the NASA Infrared Telescope Facility (IRTF), Mauna Kea, Hawaii, January 14/15, 2013 UT to obtain near-infrared (NIR) reflectance spectra of candidate basaltic asteroids associated with mainbelt asteroid (4) Vesta. NIR spectra for eight V-type asteroids were obtained on January 14 with 10-34 spectra being acquired per asteroid, but no data were obtained on January 15 due to fog at the summit. These spectra will be analyzed to confirm the V-type taxonomic classification, constrain the average surface pyroxene mineral chemistry, and associate any basaltic asteroids with the HED meteorite types.

  14. 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.

  15. Near-IR Spectroscopy of the Atmosphere of Jupiter

    NASA Technical Reports Server (NTRS)

    Baines, R. W.

    1997-01-01

    The Galileo Near Infrared Mapping Spectrometer obtains spectral images in the wavelength range 0.7 to 5.2 um with a special resolving power of approximately 200. This spectral range allows NIMS to sense cloud-reflected solar radiation, thermal emission from the deep atmosphere, and auroral bands from the thermosphere of Jupiter.

  16. 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.

  17. 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.

  18. 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?

  19. Frequency stabilized near-IR laser system for optical communications

    NASA Astrophysics Data System (ADS)

    Růžička, B.; Číp, O.; Lazar, J.

    2005-08-01

    We present a design of a stabilized laser system, an etalon of the optical frequency at the 1.5 μm band following the demands of the telecommunication industry in the Czech Republic. Our laser system employs a DFB laser diode in a two stage stabilizing scheme. The linear absorption arrangement with an acetylene filled absorption cell of a pressure about 1 kPa is used to lock the laser to the Doppler-broadened lines. To achieve a reliable and robust stabilization of the laser frequency we arranged a two-loop digital servo-system overcoming the problem of a narrow locking range of the detected transition. The wavelength of the laser is modulated by current and the servo-control and tuning is performed by a fast and precise thermal control. To achieve the resolution of the weak sub-Doppler transitions we assembled a locking scheme via frequency-modulation spectroscopy to the high finesse cavity. The system is assembled using predominantly fibre-optic components. A technology of acetylene absorption cells with AR coated windows is presented as well.

  20. Near IR Spectroscopy of Iapetus : Search for Organic Matter

    NASA Astrophysics Data System (ADS)

    Wittemberg, R.; Coustenis, A.; Schmitt, B.; Cuby, J.-G.; Quirico, E.; Doute, S.

    1997-07-01

    One of the most mysterious among the icy Saturnian satellites, Iapetus, is unique in its range of surface albedos, from 0.5 on the trailing side (typical of icy objects) to 0.02-0.04 in the inner parts of the leading hemisphere. This albedo asymmetry is not unique in the solar system, as Titan and Hyperion present such a property, which might be indicative of a common origin. The nature and the origin of the dark component has not been elucidated yet, but according to some models, this is possibly connected with the presence of organic material on the surface. We have tried to detect organic lines on the leading side of Iapetus with the Infrared Spectrometer (ISIS) at the CFHT in the 1.4-1.8 micron range, where some signatures of most of the expected organic components (Polymers, tholins and other hydrocarbons) are located. The observations were made with R=2000 on 26 & 27 August 1996. We have compared the observations with laboratory measurements made at the L.G.G.E (Grenoble, France) of C_3H_8, C_2H_4, C_2H_6 & C_2H_2 (Quirico and Schmitt, 1997, Icarus, in press). No obvious identification was achieved, but we set constraints on the abundance of some organics on Iapetus' surface.

  1. Groundbased near-IR observations of the surface of Venus

    NASA Technical Reports Server (NTRS)

    Meadows, V. S.; Crisp, D.; Allen, D. A.

    1992-01-01

    We present images of the nightside of Venus taken in the near-infrared windows at 1.0, 1.1, 1.18, 1.28, 1.31, and 2.3 microns with the new infrared camera/spectrometer IRIS on the Anglo-Australian Telescope. These data were taken in spectral-mapping mode. This technique involves scanning the telescope perpendicular to the slit, while collecting spectra at successive slit positions across the planet. We produce data cubes with one spectral and two spatial dimensions. Images can be extracted over any wavelength regions. Each image has square pixels of 0.8 inch resolution. We reduced the scattered light from the sunlit crescent in images extracted from each window by subtracting images taken on either side of the window, where the Venus atmosphere is opaque. Unlike the short wavelength windows, which reveal thermal contrasts that originate primarily from the surface and deep atmosphere, the emission in the 2.3 microns window is produced at much higher altitudes (30-40 km). Emission contrasts seen near 2.3 microns are associated with horizontal variations in the cloud optical depths, and have rotation periods of about six days. We detect large contrasts in infrared emission (20-40 percent) across the disc of Venus in the 1.0-, 1.1-, 1.18-, 1.28-, and 1.31-micron images. Contrasts at these wavelengths may be due to a combination of variations in the optical depths of the overlying sulfuric acid clouds and differences in surface emission. Comparison with the 2.3-micron images show that the patterns seen in the 1.28- and 1.31-micron windows are consistent with cloud optical depth variations alone and require no contribution from the surface. However, images at 1.0, 1.1, and 1.8 microns from July 1991 show a dark feature having a contrast that increases with decreasing wavelength. This behavior is contrary to that expected of cloud absorption. Images taken on three successive days in October show another dark feature that is stationary with respect to the surface. These regions of lower emission correspond closely to the high-altitude surface regions of Beta Regio and Aphrodite Terra. The images can potentially reveal the near-infrared emissiveity of the surface of Venus, thereby complementing Magellan radar reflectivity and ground based radio emissivity measurements. The contrast ratio between highlands and plains is much smaller than would be expected for blackbody radiation from the surface along. Unlike at radio wavelengths, where the atmosphere is essentially transparent, at near-infrared wavelengths the atmosphere emits, absorbs, and scatters radiation, and can modify the observed topographically induced contrasts. The additional radiation from the atmosphere reduces the contrast, and further modification would be expected if terrain at different altitudes has different emissivities. A fit to our data therefore requires, and may constrain, a model of the lowest scale height of the atmosphere.

  2. Effective Sample Size in Diffuse Reflectance Near-IR Spectrometry.

    PubMed

    Berntsson, O; Burger, T; Folestad, S; Danielsson, L G; Kuhn, J; Fricke, J

    1999-02-01

    Two independent methods for determination of the effectively sampled mass per unit area are presented and compared. The first method combines directional-hemispherical transmittance and reflectance measurements. A three-flux approximation of the equation of radiative transfer is used, to separately determine the specific absorption and scattering coefficients of the powder material, which subsequently are used to determine the effective sample size. The second method uses a number of diffuse reflectance measurements on layers of controlled powder thickness in an empirical approach. The two methods are shown to agree well and thus confirm each other. From the determination of the effective sample size at each measured wavelength in the visible-NIR region for two different model powder materials, large differences was found, both between the two analyzed powders and between different wavelengths. As an example, the effective sample size ranges between 15 and 70 mg/cm(2) for microcrystalline cellulose and between 70 and 300 mg/cm(2) for film-coated pellets. However, the contribution to the spectral information obtained from a certain layer decreases rapidly with increasing distance from the powder surface. With both methods, the extent of contribution from various depths of a powder sample to the visible-NIR diffuse reflection signal is characterized. This information is valuable for validation of analytical applications of diffuse reflectance visible-NIR spectrometry. PMID:21662719

  3. 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.

  4. 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.

  5. Gaia discovery of a Supernova candidate in ESO 297- G 008

    NASA Astrophysics Data System (ADS)

    Blagorodnova, N.; Campbell, H.; Delgado, A.; Fraser, M.; Hodgkin, S.; Harrison, D.; Koposov, S.; Rixon, G.; Walton, N.; Wyrzykowski, L.; Kostrzewa-Rutkowska, Z.

    2015-03-01

    We report the Gaia discovery of a bright SN candidate in the galaxy ESO 297- G 008: Object| Discovery TCB| RA (J2000)| DEC (J2000)| Alert G mag| Last non-detection TCB Gaia15aeb| 2015-03-22 22:33:30 | 23.88592| -39.38601| 16.53| 2015-01-16 19:49:26 Gaia15aeb was discovered on 22 Mar 2015, 22:33:30 (TCB) at 16.53 magnitude in Gaia G band (600 nm).

  6. 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.

  7. Announcement - Scientific Importance of High Angular Resolution at Infrared and Optical Wavelengths - ESO Conference

    NASA Astrophysics Data System (ADS)

    1981-03-01

    The European Southern Observatory is organizing an international conference on the subject "SCIENTIFIC IMPORTANCE OF HIGH ANGULAR RESOLUTION AT INFRARED AND OPTICAL WAVELENGTHS", to be held in the ESO building at Garching bei München during the period of 24-27 March 1981. The purpose of this conference is to discuss, on the one hand, the systems in use or under construction and possible future developments to achieve high angular resolution and, on the other hand, to discuss the areas of astrophysics which, in the next decades, will most benefit from observations at high angular resolution.

  8. Delivery of the Second Generation VLT Secondary Mirror (M2) Unit to ESO

    NASA Astrophysics Data System (ADS)

    Arsenault, R.; Vernet, E.; Madec, P.-Y.; Lizon, J.-L.; Duhoux, P.; Conzelmann, R.; Hubin, N.; Biasi, R.; Andrighettoni, M.; Angerer, G.; Pescoller, D.; Mair, C.; Picin, F.; Gallieni, D.; Lazzarini, P.; Anaclerio, E.; Mantegazza, M.; Fumi, L.; Riccardi, A.; Briguglio, R.; Poutriquet, F.; Ruch, E.; Rinchet, A.; Carré, J.-F.; Fappani, D.

    2013-03-01

    The deformable secondary mirror (DSM), one of the key systems of the VLT Adaptive Optics Facility (AOF), has been delivered to ESO. It has been fully qualified in standalone mode and has successfully passed the technical acceptance Europe. Recently it was installed on ASSIST, the test bench for the AOF, and will undergo optical tests, which will complete its preliminary acceptance in Europe. With its 1170 actuators and 1.1-metre thin-shell mirror, it constitutes the largest adaptive optics mirror ever produced. The DSM constitutes a fine accomplishment by European industry and is set to become the "flagship" of the AOF on Paranal.

  9. 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.

  10. 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.

  11. 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

  12. 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

  13. 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.

  14. 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.

  15. 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.

  16. 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

  17. 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.

  18. MACAO-VLTI: An Adaptive Optics system for the ESO VLT interferometer

    NASA Astrophysics Data System (ADS)

    Arsenault, Robin; Alonso, Jaime; Bonnet, Henri; Brynnel, Joar; Delabre, Bernard; Donaldson, Robert; Dupuy, Christophe; Fedrigo, Enrico; Farinato, Jacopo; Hubin, Norbert N.; Ivanescu, L.; Kasper, Markus E.; Paufique, J.; Rossi, S.; Tordo, Sebastien; Stroebele, Stefan; Lizon, Jean-Luis; Gigan, Pierre; Delplancke, Francoise; Silber, A.; Quattri, Marco; Reiss, Roland

    2003-02-01

    MACAO stands for Multi Application Curvature Adaptive Optics. A similar concept is applied to fulfill the need for wavefront correction for several VLT instruments. MACAO-VLTI is one of these built in 4 copies in order to equip the Coude focii of the ESO VLT's. The optical beams will then be corrected before interferometric recombination in the VLTI (Very Large Telescope Interferometer) laboratory. MACAO-VLTI uses a 60 elements bimorph mirror and curvature wavefront sensor. A custom made board processes the signals provided by the wavefront detectors, 60 Avalanche Photo-diodes, and transfer them to a commercial Power PC CPU board for Real Time Calculation. Mirrors Commands are sent to a High Voltage amplifier unit through an optical fiber link. The tip-tilt correction is done by a dedicated Tip-tilt mount holding the deformable mirror. The whole wavefront is located at the Coude focus. Software is developed in house and is ESO compatible. Expected performance is a Strehl ratio sligthly under 60% at 2.2 micron for bright reference sources (star V<10) and a limiting magnitude of 17.5 (Strehl ~0.1). The four systems will be installed in Paranal successively, the first one being planned for June 2003 and the last one for June 2004.

  19. Diffuse Ionized Gas in Irregular Galaxies. I. GR 8 and ESO 245-G05

    NASA Astrophysics Data System (ADS)

    Hidalgo-Gámez, A. M.

    2006-04-01

    We have studied the spectral characteristics of the diffuse ionized gas (DIG) in two irregular galaxies with low metallicities and intermediate star formation rates: ESO 245-G05 and GR 8. The [O III]/Hβ ratio in these galaxies is higher than in the DIG of spiral galaxies but not as high as in other irregular galaxies previously studied, such as IC 10 and NGC 6822. The [N II]/Hα and [S II]/Hα ratios have very small values, indicating the absence of shocks as the ionization source for this gas. This ionization can be explained in both galaxies with photon leakage from the H II regions as the only source. The percentage of photons that have escaped from the H II regions is small in ESO 245-G05, only 35%, but varies from 35% up to 60% in GR 8. We also investigated whether the differences found between spiral and irregular galaxies in the [O III]/Hβ and the [N II]/Hα ratios are due to differences in the metal content between these types of galaxies. Although the number of galaxies studied is not very large, it can be concluded that the [O III]/Hβ ratio is not related to the oxygen content, while the situation is more ambiguous for the [N II]/Hα ratio.

  20. 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.

    2016-04-01

    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 VLT/FLAMES and provide the weights that characterise 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.

  1. 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).

  2. 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

  3. 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

  4. 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

  5. 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

  6. 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

  7. The AMBRE Project: Stellar parameterisation of the ESO:FEROS archived spectra

    NASA Astrophysics Data System (ADS)

    Worley, C. C.; de Laverny, P.; Recio-Blanco, A.; Hill, V.; Bijaoui, A.; Ordenovic, C.

    2012-06-01

    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 in order to carry out the determination of stellar atmospheric parameters for the archived spectra of four ESO spectrographs. Aims: The analysis of the FEROS archived spectra for their stellar parameters (effective temperatures, surface gravities, global metallicities, alpha element to iron ratios and radial velocities) has been completed in the first phase of the AMBRE Project. From the complete ESO:FEROS archive dataset that was received, a total of 21 551 scientific spectra have been identified, covering the period 2005 to 2010. These spectra correspond to 6285 stars. Methods: The determination of the stellar parameters was carried out using the stellar parameterisation algorithm, MATISSE (MATrix Inversion for Spectral SynthEsis), which has been developed at OCA to be used in the analysis of large scale spectroscopic studies in galactic archaeology. An analysis pipeline has been constructed that integrates spectral normalisation, cleaning and radial velocity correction procedures in order that the FEROS spectra could be analysed automatically with MATISSE to obtain the stellar 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, effective temperature, surface gravity, metallicity and alpha element abundances, were determined for 6508 (30.2%) of the FEROS archived spectra (~3087 stars). Radial velocities were determined for 11 963 (56%) of the archived spectra. 2370 (11%) spectra could not be analysed within the pipeline due to very low signal-to-noise ratios or missing spectral orders. 12 673 spectra (58.8%) were analysed in the pipeline but their parameters were discarded based on quality criteria and error analysis determined within the automated process. The majority of

  8. 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

  9. 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).

  10. The super star cluster driven feedback in ESO338-IG04 and Haro 11

    NASA Astrophysics Data System (ADS)

    Bik, Arjan; Adamo, Angela; Östlin, Göran; Hayes, Matthew; Menacho, Veronica; Melinder, Jens; Amram, Philippe

    2015-08-01

    We present high quality integral field spectroscopy taken with VLT/MUSE and VLT/SINFONI of two starburst galaxies: ESO 338-IG04 and Haro 11. This provides us with an unprecedented view of the state and kinematics of the ionized gas in the galaxy allowing us to study the effect of stellar feedback on large (with MUSE) and small (with SINFONI) scales. I will present our recent results on studying the ISM state of these two galaxies. The data of both galaxies show that the mechanical and ionization feedback of the super star clusters in the galaxy modify the state and kinematics of the ISM substancially by creating highly ionized bubbles around the cluster, making the central part of the galaxy highly ionized. This shows that the HII regions around the individual clusters are density bounded, allowing the ionizing photons to escape and ionize the ISM further out.

  11. Geometry of an AGN accretion disk on parsec scales: ESO 269-G012

    NASA Astrophysics Data System (ADS)

    Zaw, Ingyin; Greenhill, Lincoln; Briggs, Frank; Moin, Aquib; Horiuchi, Shinji; Kuiper, Tom; Soni, Ashish

    2014-04-01

    Water maser emission at 22 GHz (lambda 1.35 cm) is the only known tracer of sub-parsec structure in active galactic nuclei (AGN) that has been resolved in position and velocity. Some AGN masers have emission that trace highly inclined accretion disks (``disk masers''). These disk masers are extremely rare, and in particular, only 4 have both maser emission and detected radio continuum emission. ESO 269-G012 is one of the four and previously unmapped with VLBI. We request four 12 h tracks, one K band for the maser, and three tracks in K, X, and S bands for the continuum. We will estimate the disk size and geometry, measure the enclosed mass, determine the SMBH position from combining locations of maser and continuum emission, and measure the spectral index of the continuum emission.

  12. ESO adaptive optics NGSD/LGSD prototype controller for the E-ELT

    NASA Astrophysics Data System (ADS)

    Reyes, Javier; Downing, Mark; Romero, Jorge

    2014-07-01

    This paper presents the development of the ESO prototype detector controller for the Adaptive Optics imager in the EELT which is based on the e2v Natural Guide Star Detector (NGSD) and Laser Guide Star Detector (LGSD). NGSD is a 880×840 pixel CMOS array organized as 44×42 sub-apertures of 20×20 pixel each. NGSD is exactly 1/4 of the LGSD and therefore it is considered a scaled down demonstrator for the LGSD. The detector controller requirements present important challenges in the design of the electronics due to the low-power, low-noise and high parallel data rate of the detectors involved. The general architecture of the controller along with the front-end electronics to drive and read-out the detector are described here. This electronics is based on Xilinx Virtex-7 FPGAs.

  13. VizieR Online Data Catalog: ESO Slice Project (Vettolani+ 1998)

    NASA Astrophysics Data System (ADS)

    Vettolani, G.; Zucca, E.; Merighi, R.; Mignoli, M.; Proust, D.; Zamorani, G.; Cappi, A.; Guzzo, L.; Maccagni, D.; Ramella, M.; Stirpe, G. M.; Blanchard, A.; Cayatte, V.; Collins, C.; McGillivray, H.; Maurogordato, S.; Scaramella, R.; Balkowski, C.; Chincarini, G.; Felenbok, P.

    1998-03-01

    The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&A...325..954V; Zucca et al., 1997A&A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40°15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray & Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies +