Observations of the Crab Nebula, NGC 4151, Cyg X1 and Cyg X3 at medium gamma ray energies

NASA Technical Reports Server (NTRS)

Zanrosso, E. M.; Long, J. L.; Zych, A. D.; Gibbons, R.; White, R. S.; Dayton, B.

1980-01-01

The paper analyzes observations of the Crab Nebula, NGC 4151, Cyg X1, and Cyg X3 taken with the UCR gamma ray telescope at a residual atmospheric depth of about 3.5 g/sq cm on a balloon launched from Palestine, Texas, 4.5 GV, 2000 local time LT (0100 UT), on September 29, 1978. The data consists of continuous observations from 0430 LT (0930 UT) on September 30 to 1800 LT (2300 UT) on October 1, 1979. A flux increase is observed at the right ascension of the Crab Nebula within about a 10 min uncertainty of telescope source position determination, eliminating the SAS-2, CG 195+4, and the two COS-B sources in the antigalactic center direction as the origin of the gamma rays. The total flux of gamma rays for the Crab Nebula from 1.2 to 10 MeV is (6.1 + or - 1.5) x 10 to the -3rd photons/sq cm-s, with an upper limit at 10-20 MeV of 7 x 10 to the -5th photons/sq cm-s. Results for the NGC 4151, Cyg X1, and Cyg X3 are also discussed and flux upper limits are given.

Hubble Space Telescope Discovery of a z = 3.9 Multiply Imaged Galaxy Behind

Science.gov Websites

the SAO/NASA ADS Astronomy Abstract Service Title: Hubble Space Telescope Discovery of a z College, Clinton, NY 13323, USA), AI(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AJ(Institute of Astronomy, Graduate School of Science, University of Tokyo 2-21-1

Happy Anniversary, VLT !

NASA Astrophysics Data System (ADS)

2004-04-01

Five years at the service of Europe's astronomers VLT 5 Years One of the world's most advanced astronomical research facilities, the ESO Very Large Telescope (VLT) at the Paranal Observatory in the Chilean Atacama desert, celebrates an important anniversary today. On April 1, 1999, and following almost one year of extensive tests and careful trimming of its numerous high-tech parts, the first 8.2-m VLT Unit Telescope, Antu (UT1), was "handed over" to the astronomers. Since that date, science operations with this marvellous research tool have been continuous and intensive. Kueyen (UT2) started normal operations exactly one year later. Yepun (UT4) was offered to the scientific community in June 2001, while Melipal (UT3) followed in August 2001 [1]. Ever since, all four VLT Unit Telescopes, with an ever-growing suite of highly specialised, extremely powerful astronomical instruments have been in full operation, 365 nights a year. And this with unequalled success, as demonstrated by a long list of important scientific results, including a substantial number of exciting discoveries that are now opening new horizons in astrophysics. Moreover, thanks to heroic and persistent efforts by the dedicated teams of ESO scientists and engineers, the "downtime" due to technical problems has been very small, about 3 per cent, a number that is unequalled among the world's large telescope facilities. In addition, the weather conditions at the Paranal site in the dry Atacama desert in Northern Chile are truly excellent - this is indeed one of the best locations for astronomical observations on the surface of the Earth - and the corresponding "weather downtime" has only been around 10 per cent. This has resulted in an unbelievably low value of total downtime, most likely a new world record for ground-based 8-10 m class telescopes. VLT strong points The Very Large Telescope (VLT) is the world's largest and most advanced optical telescope. It comprises four 8.2-m reflecting Unit Telescopes (UTs) and will in due time also include four moving 1.8-m Auxiliary Telescopes (ATs), the first one of which successfully passed its first tests in January of this year (see ESO PR 01/04). With unprecedented optical resolution and unsurpassed surface area, the VLT produces extremely sharp images and can record light from the faintest and most remote objects in the Universe. It works at the limit of modern technology, regularly allowing the scientists to peer into new and unknown territories in the immense Universe. Contrary to other large astronomical telescopes, the VLT was designed from the beginning with the use of interferometry as a major goal. For this reason, the four 8.2-m Unit Telescopes were positioned in a quasi-trapezoidal configuration. The light beams from these telescopes, at this moment two-by-two, can be combined in the VLT Interferometer (VLTI). It provides the European scientific community with a ground-based telescope array with collecting power significantly greater than any other facilities available at present or being planned, offering imaging and spectroscopy capabilities at visible and infrared wavelengths. Seven of the planned ten first-generation astronomical instruments are now in operation at the VLT. They cover all major observing modes required to tackle current "hot", front-line research topics: * the multi-mode instrument FORS1 (FOcal Reducer and Spectrograph) and its twin, FORS2, * the Infrared Spectrometer And Array Camera (ISAAC) cryogenic infrared imager and spectrometer, * the UVES (Ultra-violet and Visible Echelle Spectrograph) high-dispersion spectrograph, * the NAOS-CONICA Adaptive Optics facility producing images as sharp as if taken in space [2], * the VIsible Multi-Object Spectrograph (VIMOS) four-channel multiobject spectrograph and imager - allowing to obtain low-resolution spectra of up to 1000 galaxies at a time * the Fibre Large Array Multi-Element Spectrograph (FLAMES) that offers the unique capability to study simultaneously and at high spectral resolution 100 individual stars in nearby galaxies. The remaining instruments - the high-resolution infrared spectrograph CRIRES, the Mid Infrared Spectrometer/Imager VISIR and the integral field spectrograph SINFONI - will be installed in 2004-2005. The observational statistics prove that these instruments are extremely efficient - they have some of the highest "shutter-open times" (i.e. percentage of the maximum possible observing time during which the instruments are collecting light from the astronomical objects) ever achieved. The astronomers are well served in this respect: the ISAAC instrument, for example, continues to be in the highest demand and has now performed smoothly during more than 1000 nights and two others, UVES and FORS, are now approaching the same number. Working together with astronomers and engineers at many research institutes in the ten ESO member countries, ESO is now in the process of defining second generation instruments and feasibility studies are well under way. Among the prime projects in this direction are a cryogenic multi-object spectrometer in the near-infrared 1 to 2.4 μm range ("KMOS"), a medium-resolution wide-band (0.32 to 2.4 μm) spectrometer ("X-shooter"), as well as a wide-field 3D optical spectrometer ("3D deep-field surveyor") and a high-contrast, adaptive optics assisted, imager ("planet finder"). In addition to these highly innovative instruments for the VLT UTs, specific instruments that will work with the combined light from several of the telescopes have also been conceived. The interferometric instrument MIDI will be offered to the astronomical community from today (April 1, 2004), fulfilling the VLTI promise. Great efforts have indeed gone into making observations with this very complex science machine as user-friendly as possible. Contrary to what is normally the case in this technically demanding branch of astronomy, scientists will find interferometric work at the VLTI quite similar to that of using the many other, more conventional VLT instruments. Science with the VLT The impressive battery of top-ranking instruments, coupled with the enormous light-collecting power of the VLT, has already provided a real research bonanza with many outstanding scientific results, some of which have been true breakthroughs. They include the amazing new knowledge about the Black Hole at the Galactic Centre, the farthest galaxy known, the most metal-poor and hence, oldest stars, accurate cosmochronological dating by means of Uranium and Thorium spectral lines, high-redshift galaxy rotation curves, micro-quasars, properties of the optical counterparts of gamma-ray bursts, high-redshift supernovae, etc. [3]. All of these advances attest to the power of the VLT and its mode of operational. Not to be forgotten is also the beauty of many of the stunning images obtained with this telescope, one of which was voted amongst the 10 most inspirational astronomical images of the past century [4]. Look at the numerous and detailed ESO Press Releases for more examples of research achievements from the VLT. This trend is also apparent in the productivity of the telescopes. The number of research publications resulting from VLT work in top ranking astronomical journals is steadily increasing with a total close to 700, hereof 250 in 2003 alone. Moreover, research articles based on VLT data are in the mean quoted twice as often as the average. The very high efficiency of the VLT "science machine" now generates huge amounts of data at a very high rate. These are stored in a permanent Science Archive Facility at ESO headquarters, which is jointly operated by ESO and the Space Telescope European Coordinating Facility (ST-ECF). From here, data are distributed daily to astronomers on DVDs and over the World Wide Web. The archive facility has been conceived and developed to enable astronomers to "mine" very efficiently the enormous volumes of data that is collected from the VLT. The archive now contains more than 1 million images or spectra taken by the four UTs with a total volume of about 50 Terabytes (50,000,000,000,000 bytes) of data. This corresponds to the content of about 25 million books of 1000 pages each; they would occupy more than 1000 kilometres of bookshelves! Looking towards the future Says Catherine Cesarsky, ESO Director General since 1999: " The Paranal Observatory has already given rise to an impressive number of scientific results, many of which could not have been obtained elsewhere. Overall, the VLT has been a most remarkable success, and will contribute to science at the highest level for years to come - a fantastic achievement of which we can all be justifiably proud." The work is now underway at full power to provide second-generation instruments for the VLT, to add three more Auxiliary Telescopes to the VLTI and to complement this unique research facility with the two wide-field survey ("pathfinding") telescopes - one to work in the visible part of the spectrum (the 2.5-m VST), the other in the infrared (the 4-m VISTA) - now being constructed at Paranal. Roberto Gilmozzi, director of Paranal Observatory, looks forward: " Ever more exciting times lie ahead for Paranal with new instruments like VISIR and SINFONI and the laser guide star, all of them coming this year. Five years after the start of operations on UT1, the observatory operates its telescopes with very little time set aside for engineering (less than 10%) and very low technical down time. Combined with excellent weather and great image quality, we provide the European community with unsurpassed observing capabilities. As director of this observatory since 1999, I have been privileged to be part of this adventure." The VLT is a fine example of the vast benefits of pooling resources from several countries and it is a flagship of contemporary European research. There is little doubt that for many years to come, ESO's Paranal Observatory with its powerful and efficient facilities will continue to play a leading role in astronomical research. Information for the media Associated material can be found on the corresponding Press Events webpage.

The Early Spectral Evolution of the Classical Nova ASASSN-15th in M33

NASA Astrophysics Data System (ADS)

Wagner, R. Mark; Neric, Marko; Darnley, Matt J.; Williams, Steven; Starrfield, Sumner; Woodward, Charles E.; Prieto, Jose Luis

2016-06-01

During the course of the All Sky Automated Survey for SuperNovae (ASAS-SN) a new transient source designated ASASSN-15th was identified on images of the nearby galaxy M33 obtained with the 14 cm Brutus telescope in Haleakala, Hawaii on 2015 Dec 1.4 UT at V ~ 16.5 mag. Given the location of the transient in M33 and its apparent V magnitude at discovery, the implied absolute visual magnitude was about -8.5 mag suggesting that the transient was a new classical nova outburst in M33. Optical spectroscopy obtained by us on 2015 Dec 2.3 showed broad emission lines of Balmer, Fe II, and Na I D with P Cygni-type line profiles superposed on a blue continuum. The spectrum was consistent with a Fe II-type classical nova in M33 discovered early in the outburst. Subsequent spectra obtained by us on 2015 Dec 10.9 UT showed significant evolution since our first spectrum in that the deep P Cygni-type line profiles seen earlier were now extremely shallow or had almost completely disappeared with the emission component growing in strength. Additional emission lines from O I, Si II, and possibly He I were also present. We obtained optical spectroscopy of ASASSN-15th on 17 epochs between 2015 Dec 1 and 2016 Feb 11 UT with the 2.4 m Hiltner telescope (+OSMOS) of the MDM Observatory, the 2 m fully robotic Liverpool Telescope (+SPRAT), and the 2 x 8.4 m Large Binocular Telescope (+MODS). We will present our spectroscopy and discuss the early evolution of ASASSN-15th in the context of Galactic Fe II-class novae.

Assessment of the Effects of Plasma Bubbles on GAIM-GM

DTIC Science & Technology

2011-09-01

m / s , 230 m / s was chosen as a realistic upper bound that fit well into the modified IFM grid resolution. The sun...to a second condition where the bubbles would form at 2000 LT and then allowed to super-rotate at 230 m / s , or 7.5 degrees/hr, depicted in Figure 7...moving east at 230 m / s . Units are in TEC electrons per square meter. ( a ) 00UT (b) 01UT (c) 02UT (d) 03 UT (e) 04UT (f) 05UT 1 1 2 1

Optical Spectroscopy of Nova Ophiuchi 2015 (PNV J17291350-1846120)

NASA Astrophysics Data System (ADS)

Danilet, A. B.; Holoien, T. W.-S.; Wagner, R. M.; Woodward, C. E.; Starrfield, S.; Wilber, A.; Walter, F.; Shore, S.

2015-04-01

Following the discovery by Y. Sakurai (Ibaraki-ken, Japan) on 2015 Mar. 29.766 UT of a new stellar object of magnitude 12.2 in Ophiuchus (S. Nakano, CBET 4086) and its subsequent confirmation as a likely He/N classical nova (K Ayani, CBET 4086), we obtained a spectrum (range: 398-685 nm; resolution 0.3 nm) of Nova Oph 2015 on 2015 April 1.459 UT with the 2.4 m Hiltner telescope (+OSMOS) of the MDM Observatory on Kitt Peak.

Classification of PSN J12015272-1852183 as a young type Ic SN

NASA Astrophysics Data System (ADS)

Harutyunyan, A.; Benetti, S.; Pastorello, A.; Cappellaro, E.; Tomasella, L.; Ochner, P.; Turatto, M.

2013-06-01

We report the spectroscopic classification (range 335-785 nm; resolution 1.5 nm) of PSN J12015272-1852183 discovered by the CHASE project on June 22.12 UT. The spectrogram obtained on June 23.88 UT with the TNG Telescope (+Dolores), shows that this is a type-Ic supernova. A good match is found with the type-Ic supernova 1994I (Millard et al 1999, ApJ 527, 746) at about six days before maximum light.

Spectroscopic classification of PSN J12211796+113025

NASA Astrophysics Data System (ADS)

Tomasella, L.; Ochner, P.; Benetti, S.; Pastorello, A.; Cappellaro, E.; Bedin, L.; Turatto, M.; Spiro, S.; Tartaglia, L.; Harutyunyan, A.; Dimai, A.; Botticella, M. T.; Pignata, G.; Bufano, F.; Valenti, S.; Elias-Rosa, N.

2013-02-01

We report that optical spectra of PSN J12211796+113025 obtained on Feb. 14.93 UT with the Asiago 1.82-m Copernico Telescope (+ AFOSC; range 340-820 nm; resolution 1.3 nm) and on Feb. 15.11 UT with the TNG (+Dolores; 320-800 nm, resolution 1.4 nm) shows a blue continuum (Tbb ~ 15300 K) with superimposed narrow, unresolved (FWHM < 600 km/s) emission lines of H, [O II], [O III], [N II] and [S II]. However, we cannot disentangle the intrinsic transient contribution to line emissions because of the heavy contamination from nearby H II regions.

Spectroscopic classification of AT 2017byx as a Type Ia Supernova

NASA Astrophysics Data System (ADS)

Vinko, J.; Wheeler, J. C.; Sarneczky, K.; Szakats, R.; Szalai, T.; Szekely, P.; HETDEX Collaboration

2017-05-01

During the commissioning phase of the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) survey we observed AT 2017byx (ATLAS17bla, PS17bve) at R.A.=14:17:48.36 Dec.=+52:41:54.6 with the Visible Integral-field Replicable Unit Spectrograph (VIRUS) at McDonald Observatory on 2017-04-28.2 UT. The spectrum (range between 3500 and 5500 Angstroms) indicates that AT 2017byx is a Type Ia supernova.

SALT Spectroscopic classification of ASASSN-18lp as a dwarf nova

NASA Astrophysics Data System (ADS)

Buckley, D. A. H.; Gromadzki, M.; Dong, Subo; Stanek, K. Z.

2018-06-01

ASASSN-18lp (AT 2018cex) was discovered by the All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014) on UT 2018-06-05.24 at g 16 mag. It was observed with the Southern African Large Telescope (SALT) using the Robert Stobie Spectrograph on UT 2018-06-05.75 UT (HJD 2458275.2561) employing the PG300 lines/mm grating.

High-resolution maps of H2 regions at far-infrared wavelengths. [balloon-borne cassegrain telescope

NASA Technical Reports Server (NTRS)

Fazio, G. G.; Kleinmann, D. E.; Noyes, R. W.; Wright, E. L.; Zeilik, M., II; Low, F. J.

1974-01-01

The first successful flight of a balloon-borne 1-m telescope for far-infrared (40 micron) astronomy occurred on 4 February 1974 (UT), from Palestine, Texas. During 6 h at float altitude, the gyrostabilized telescope mapped the intensity of far-infrared radiation from the H 2 regions Ori A and W3 with a resolution of 1 prime. Partial maps of these regions were made with a resolution of 0.5 prime. These sources were resolved into several components, some of which were previously unknown. Observations of Mars were used for calibration.

Radio re-brightening of MAXI J1535-571 as it transitions back towards the hard state

NASA Astrophysics Data System (ADS)

Russell, T. D.; Altamirano, D.; Tetarenko, A. J.; Sivakoff, G. R.; Neilsen, J.; Miller-Jones, J. C. A.; van den Eijnden, J.; Jacpot Xrb Collaboration

2017-10-01

As part of an ongoing Australia Telescope Compact Array (ATCA) campaign monitoring the current outburst of MAXI J1535-571, we observed the source on 2017 October 25 between 06:09 UT and 09:24 UT (MJD 58051.32 +/- 0.07).

Discovery and Classification of Optical Transient in M81 : P60- M81-081203

NASA Astrophysics Data System (ADS)

Kasliwal, M. M.; Cenko, S. B.; Quimby, R.; Rau, A.; Ofek, E. O.; Kulkarni, S. R.

2008-12-01

On UT 2008 Dec 3.303, P60-FasTING (Palomar 60-inch Fast Transients In Nearby Galaxies) discovered an optical transient in M81 at RA(J2000) = 09:55:16.920, DEC(J2000)=+69:02:17.68, offset from the nucleus by 87.2"W, 97.4"S. P60-M81-081203 had a brightness of g = 20.5 +/- 0.1 at discovery. It was not detected by P60 to g > 22.3 on Nov 30.410. There is no counterpart in SDSS or SIMBAD. Follow-up spectroscopy with the Double Beam Spectrograph on the Palomar Hale telescope showed a featureless spectrum on Dec 4 UT and Dec 5 UT.

A Preliminary Search for the Progenitor Candidate of PSN J12015272-1852183 in the Antennae Galaxies (NGC 4038)

NASA Astrophysics Data System (ADS)

Elias-Rosa, N.; Pastorello, A.; Benetti, S.; Cappellaro, E.; Pignata, G.; Takats, K.; Valenti, S.; Harutyunyan, A.

2013-06-01

We report the identification of potential candidates for the progenitor star of the Type Ic PSN J12015272-1852183 discovered by the CHASE survey (CBAT TOCP) from archival Hubble Space Telescope (HST) WFPC2 images in F555W (~V), and F814W (~I). These images were obtained from 2008-12-02 to 2009-02-09 UT for the HST proposal 11962, PI: A. Riess. We used a good-quality, acquisition image of the SN obtained at TNG Telescope (+Dolores) on June 23.88 UT to geometrically match the HST mosaics.

Optical and Infrared Spectral Features of Nova Canis Majoris 2018

NASA Astrophysics Data System (ADS)

Rudy, Richard; Mauerhan, Jon; Crawford, Kirk; Russell, Ray; Wiktorowicz, Sloane

2018-04-01

Optical and IR spectra from 0.47-2.5 microns (resolution: 5-30 angstroms) of Nova Canis Majoris (CBET 4499), were obtained 2018 April 21.14 (UT) with the Aerospace Corporation's 1.0 m telescope using its Visible and Infrared Imaging Spectrograph (VNIRIS).

Optical alignment of the VLTI

NASA Astrophysics Data System (ADS)

Guisard, Stephane

2003-02-01

When completed the VLTI project will be composed by four 8.2 m Unit Telescopes (UT) and four 1.8 m Auxiliay Telescopes (AT) with their respective Coude trains and relay optics, two test siderostats, 6 (up to 8) Delay lines and 8 Beam compressors with their corresponding feeding mirrors. There will be more than 200 optical components, mirrors and lenses, with diameters ranging from 5 mm to 8200 mm. Their surface shapes range from flat to off-axis ellipsoid, including also spherical, on and off-axis hyperbolae and parabolas as well as cylindrical surfaces. Depending on the interferometer configuration, the different possible optical path lengths are of the order of 100 to 300 meters. We describe briefly the principles chosen as well as the types of criteria and method used for the alignment. The method can certainly be applied to other optical systems. The explanations given are understandable to the non-optician, this text is not intended to be an alignment procedure.

Spectroscopic Classification of SN 2018bek as a Young Type II Supernova

NASA Astrophysics Data System (ADS)

Xiang, Danfeng; Wang, Xiaofeng; Zhang, Kaicheng; Li, Wenxiong; DerKacy, James; Baron, Eddie; Brink, Thomas; Zheng, Weikang; Filippenko, Alex; Lin, Han; Rui, Liming; Hu, Lei; Hu, Maokai; Zhang, Tianmeng; Zhang, Jujia

2018-05-01

We obtained a few optical spectra of SN 2018bek,discovered by Jaroslaw Grzegorzek,on UT May 05-09 2018 with the 3.5m telescope (+Dual Imaging Spectrograph) at the Apache Point Observatory, the 2.16-m telescope(+BFOSC) at Xinglong Observatory of NAOC, and the Lick 3.0-m telescope (+Kast) at Lick Observatory.

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), Luigi Guiffrida (SOIMI), Gianpietro Marchiori (EIE) and Prof. Massimo Tarenghi (ESO), describing the very successful implementation of this major VLT contract that was awarded by ESO in September 1991 [2]. All speakers praised the good collaboration between ESO and its industrial partners and Prof. Riccardo Giacconi , Director General of ESO, expressed his satisfaction `with the splendid performance of the ESO-Industry team which was bringing us close to the realisation of the premier telescope array in optical ground-based astronomy in the world'. The participants were also pleased to listen to several of the Italian engineers present who commented on the very positive experience of being personally involved in the world's largest telescope project. The VLT telescope structures incorporate many new technological concepts. Thanks to these and careful planning of the many components and their integration, it has been possible to achieve, among others, light weight construction, high mechanical stiffness, good thermal equilibrium with the ambient air (of importance for the seeing during the observations), low electromagnetic emissitivity (i.e. low interference with the sensitive astronomical instruments) and easy maintainability. Of particular interest is also the giant, direct drive system with a diameter of 9 metres and the sophisticated, innovative laser encoder system. In this way, there is no direct contact between the moving parts and the friction during the rotation is kept at an absolute minimum. The Next Steps The ESO VLT project is now entering into a decisive phase and the next years will see an increasing number of telescope parts and instruments from the scientific and industrial laboratories of Europe converging towards the VLT observatory at Cerro Paranal in Chile. It is gratifying that, despite its high degree of complexity and incorporation of a substantial number of new technologies, the project is within schedule and budget. There will be several important milestones in 1996. During the next two months, the mounting of the mechanical structure in Milan will be completed. Following this, a group of ESO hard- and software experts will spend about 6 months next to it, implementing and thoroughly testing all aspects of the very advanced VLT telescope control system. In the meantime, the erection of the first telescope enclosure at Paranal is rapidly proceeding and the outside panelling will soon be put in place. This work will be completed in January 1996, after which the integration of all inside mechanical components will follow. The take-over by ESO of the fully operational, first enclosure is scheduled for May 1996. The other enclosures will become ready at regular intervals thereafter. In Milan, all of the heavy parts of the second telescope structure have already been produced and the third and fourth are about 60 percent complete. While the first structure has now been pre-assembled for tests, the individual parts of the second will not be put together before they are shipped to Paranal in early 1996. Starting in June 1996, they will then be assembled inside the completed, first enclosure. Thus, the `second' structure will become the `first' VLT Unit telescope (UT1). This work will last until early 1997, after which the first 8.2-metre mirror will arrive from Europe and be installed. Finally, after another test and optimisation period, `first light' for UT1 is expected in late 1997. This procedure is very advantageous, because it allows to continue under less time pressure the extensive tests on the `first' structure in Milan until a satisfactory state of debugging and optimisation of the new VLT control system has been reached. In this way, the time necessary for the installation of this system in UT1 at Paranal in 1997 will be significantly shortened. In fact, the structure seen by the ESO Council in Milan will be the last to be shipped to Paranal where it will then become the fourth 8.2-metre Unit telescope (UT4). Mirrors and Instruments As earlier announced, ESO officially received the first 8.2-metre VLT mirror from REOSC in Paris [3] on November 21. The polishing of the second mirror has already started and, based on the experience gained with the first, it is expected that this work will be accomplished in less time. The third blank is already at REOSC and the fourth will soon be ready at Schott Glaswerke in Mainz (Germany). Following extended studies, and as yet another move towards new technology within the VLT project, it has now been decided to make the 1.2-metre secondary VLT mirrors of beryllium, a very light, exotic metal. The contracting firm is Dornier of the DASA group (Germany). This saves much weight and allows these relatively large mirrors to be efficiently used in the `chopping and tilting' mode needed for observations in the infrared wavelength region as well as for the critical, image-sharpening adaptive optics system. Significant progress has also been achieved on the first astronomical instruments which will be installed at the VLT. The integration of the first two of these, ISAAC and CONICA which will be installed on UT1 in the course of 1997, has already started in the ESO laboratories at the Headquarters in Garching. Important advances have also taken place within the FORS (managed by a consortium of Landessternwarte Heidelberg, Universitaets-Sternwarte Goettingen and Institut fuer Astronomie und Astrophysik der Ludwig Maximilians Universitaet Muenchen) and FUEGOS (Paris Observatory, Meudon Observatory, Toulouse Observatory, Geneva Observatory and Bologna Observatory) projects. More details about these and other VLT instruments will be given in later communications. Notes: [1] The Council of ESO consists of two representatives from each of the eight member states. It is the highest legislative authority of the organisation and normally meets twice a year. This time, Council was invited to Milan by the Director of the Osservatorio di Brera (Milan), Prof. Guido Chincarini, and the Italian delegation. [2] See ESO Press Release 08/91 of 24 September 1991. [3] See ESO Press Release 15/95 of 13 November 1995. How to obtain ESO Press Information ESO Press Information is made available on the World-Wide Web (URL: http://www.eso.org../). ESO Press Photos may be reproduced, if credit is given to the European Southern Observatory.

Ground and space-based separate PSF photometry of Pluto and Charon from New Horizons and Magellan

NASA Astrophysics Data System (ADS)

Zangari, Amanda M.; Stern, S. A.; Young, L. A.; Weaver, H. A.; Olkin, C.; Buratti, B. J.; Spencer, J.; Ennico, K.

2013-10-01

While Pluto and Charon are easily resolvable in some space-based telescopes, ground-based imaging of Pluto and Charon can yield separate PSF photometry in excellent seeing. We present B and Sloan g', r', i', and z' separate photometry of Pluto and Charon taken at the Magellan Clay telescope using LDSS-3. In 2011, observations were made on 7, 8, 9, 19, and 20 March, at 9:00 UT, covering sub-Earth longitudes 130°, 74°, 17°, 175° and 118°. The solar phase angle ranged from 1.66-1.68° to 1.76-1.77°. In 2012, observations were made on February 28, 29 and March 1 at 9:00 UT covering longitudes 342°, 110° and 53° and on May 30 and 31 at 9:30 UT and 7:00 UT, covering longitudes 358° and 272°. Solar phase angles were 1.53-1.56° and 0.89°-0.90° degrees. All longitudes use the convention of zero at the sub-Charon longitude and decrease in time. Seeing ranged from 0.46 to 1.26 arcsecond. We find that the mean rotationally-averaged Charon-to-Pluto light ratio is 0.142±0.003 for Sloan r',i' and z'. Charon is brighter in B and g', with a light ratio of 0.182±0.003 and 0.178±0.002 respectively. Additionally, we present separate PSF photometry of Pluto and Charon from New Horizons images taken by the LORRI instrument on 1 and 3 July 2013 at 17:00 UT and 23:00 UT, sub-Earth longitude 251° and 125°. We find that the rotation-dependent variations in the light ratio are consistent with earlier estimates such as those from Buie et al. 2010, AJ 139, 1117-1127. However, at a solar phase angle of 10.9°, Charon appears 0.25 magnitudes fainter relative to Pluto at the same rotational phase than measurements from the ground with the largest possible solar phase angle. Thus we provide the first estimate of a Pluto phase curve beyond 2°. These results represent some of the first Pluto science from New Horizons. This work has been funded in part by NASA Planetary Astronomy Grant NNX10AB27G and NSF Award 0707609 to MIT and by NASA's New Horizons mission to Pluto.

Expectations Increase as VLT First Light Approaches

NASA Astrophysics Data System (ADS)

1998-05-01

Two weeks before the moment of "First Light" of Unit Telescope no. 1 of the Very Large Telescope (VLT) , the ESO Team at the Paranal Observatory reports good progress of the preparatory work. The crucial optimization of the world's first, thin 8.2-metre mirror proceeds according to the established plan. It is thus expected that this important event will take place as foreseen, i.e. during the night of May 25-26, 1998 . If no unforeseen obstacles are encountered, the first scientific images will then be presented during a series of near-simultaneous Press Conferences in the ESO member countries on May 27 . The photos will be published on the WWW the same day, together with explanatory texts. In preliminary optical tests at the first VLT Unit Telescope (UT1), the initial adjustment of the active optics system that controls the telescope optics has demonstrated excellent results. In particular, the first tests have verified the fine optical performance of the 8.2-m primary mirror and of the complex control system that maintains the shape of this thin and flexible Zerodur mirror. In short test exposures with the guide probe (the technical device that is used to steer the telescope) - i.e., not yet with the scientific CCD-camera that will be used for the First Light images - the telescope has been following the external seeing provided by the Paranal site. Image quality of better than 0.5 arcsec has been achieved routinely. "We are pleased with the progress and confident that the telescope will live up to the expectations", says Riccardo Giacconi , Director General of ESO. "The team at Paranal is doing a great job." For more details about the various media activities surrounding the VLT First Light event, please consult the First Light homepage. A list of locations, times and contact addresses for the Press Conferences is available on the web. How to obtain ESO Press Information ESO Press Information is made available on the World-Wide Web (URL: http://www.eso.org ). ESO Press Photos may be reproduced, if credit is given to the European Southern Observatory.

Spectroscopic classification of ASASSN-17rl as type Ib/c

NASA Astrophysics Data System (ADS)

Bose, S.; Chen, P.; Dong, Subo; Bersier, David; Prieto, J. L.

2018-01-01

We report optical spectroscopic observations of supernova candidate ASASSN-17rl / 2017jea (ATel #11103) done on UT 2017-12-28.47 with DBSP mounted on the Hale 5m telescope at Palomar Observatory and on 2018-01-11.92 with SPRAT mounted on the 2m Liverpool Telescope.

VizieR Online Data Catalog: Photometry of the transient event iPTF16fnl (Blagorodnova+, 2017)

NASA Astrophysics Data System (ADS)

Blagorodnova, N.; Gezari, S.; Hung, T.; Kulkarni, S. R.; Cenko, S. B.; Pasham, D. R.; Yan, L.; Arcavi, I.; Ben-Ami, S.; Bue, B. D.; Cantwell, T.; Cao, Y.; Castro-Tirado, A. J.; Fender, R.; Fremling, C.; Gal-Yam, A.; Ho, A. Y. Q.; Horesh, A.; Hosseinzadeh, G.; Kasliwal, M. M.; Kong, A. K. H.; Laher, R. R.; Leloudas, G.; Lunnan, R.; Masci, F. J.; Mooley, K.; Neill, J. D.; Nugent, P.; Powell, M.; Valeev, A. F.; Vreeswijk, P. M.; Walters, R.; Wozniak, P.

2018-03-01

On the night after discovery (2016 August 29th), we observed the source with the FLOYDS spectrograph on the Las Cumbres Observatory (LCO) 2m telescope and the Spectral Energy Distribution Machine (SEDM) on the Palomar 60 inch (P60) telescope. The SEDM is a ultra-low resolution (R~100) integral-field-unit (IFU) spectrograph. Following spectroscopic identification of iPTF16fnl as a tidal disruption event (TDE) candidate, the source was monitored at Palomar and by the Ultraviolet and Optical Telescope (UVOT) on board the Swift observatory. The UVOT observations were taken in UVW2, UVM2, UVW1, U, B, and V. At Palomar, photometry in the g and Mould-R bands were obtained with the iPTF mosaic wide-field camera on the Palomar 48-inch telescope (P48). Table 3 reports the measured Swift aperture photometry magnitudes and the difference-imaging photometry for the Palomar data spanning 2016 Aug to 2016 Dec. Radio follow-up observations of iPTF16fnl were taken with the Jansky Very Large Array (VLA; PI A. Horesh), the Arcminute Microkelvin Imager (AMI; PI K. Mooley) and the James Clerk Maxwell Telescope and the Submillimetre Common-User Bolometer Array 2 (JCMT/SCUBA-2; PI A. K. H. Kong). We also observed the location of iPTF16fnl with the X-Ray Telescope (XRT) on board the Swift satellite beginning at 19:32 UT on 30 August 2016. Regular monitoring of the field in photon counting mode continued over the course of the next four months (PIs T. Holoien and B. Cenko). (1 data file).

First VLTI/MIDI observations of a Be star: Alpha Arae

NASA Astrophysics Data System (ADS)

Chesneau, O.; Meilland, A.; Rivinius, T.; Stee, Ph.; Jankov, S.; Domiciano de Souza, A.; Graser, U.; Herbst, T.; Janot-Pacheco, E.; Koehler, R.; Leinert, C.; Morel, S.; Paresce, F.; Richichi, A.; Robbe-Dubois, S.

2005-05-01

We present the first VLTI/MIDI observations of the Be star alpha Ara (HD 158 427), showing a nearly unresolved circumstellar disk in the N band. The interferometric measurements made use of the UT1 and UT3 telescopes. The projected baselines were 102 and 74 meters with position angles of 7 ° and 55°, respectively. These measurements put an upper limit on the envelope size in the N band under the uniform disk approximation of φmax= 4±1.5 mas, corresponding to 14 R*, assuming R*=4.8 R⊙ and the Hipparcos distance of 74 pc. On the other hand the disk density must be large enough to produce the observed strong Balmer line emission. In order to estimate the possible circumstellar and stellar parameters we have used the SIMECA code developed by Stee et al. (1995, A&A, 300, 219) and Stee & Bittar (2001, A&A, 367, 532). Optical spectra taken with the échelle instrument Heros and the ESO-50 cm telescope, as well as infrared ones from the 1.6m Brazilian telescope were used together with the MIDI spectra and visibilities. These observations place complementary constraints on the density and geometry of the alpha Ara circumstellar disk. We discuss the potential truncation of the disk by a companion and we present spectroscopic indications of a periodic perturbation of some Balmer lines.

The UT 7/8 February 2013 Sila-Nunam Mutual Event and Future Predictions

NASA Technical Reports Server (NTRS)

Benecchi, S. D.; Noll, K. S.; Thirouin, A.; Ryan, E.; Grundy, W. M.; Verbiscer, A.; Doressoundiram, A.; Hestroffer, D.; Beaton, R.; Rabinowitz, D.;

Fast Optical Photometry of V404 Cyg at the MDM Observatory

NASA Astrophysics Data System (ADS)

Terndrup, D.; Wagner, R. M.; Starrfield, S.

2015-06-01

We obtained continuous fast differential optical photometry of V404 Cyg with the 1.3 m McGraw-Hill Telescope of the MDM Observatory on Kitt Peak on the nights of 2015 June 19.220-19.474, 20.194-20.472, 21.199-21.460, and 22.188-22.421 UT.

Discovery of DLT18i/AT 2018yu with PROMPT and the DLT40 Survey

NASA Astrophysics Data System (ADS)

Sand, D.; Valenti, S.; Wyatt, S.; Bostroem, K. A.; Reichart, D. E.; Haislip, J. B.; Kouprianov, V.

2018-03-01

We report the discovery of DLT18i/AT 2018yu, which was found on 2018 March 1.0 (UT) at r 17.6 mag during the ongoing D < 40 Mpc (DLT40) supernova search, using data from the PROMPT5 0.41m telescope located at CTIO.

Follow-up spectroscopy and photometry of Dwarf Nova V392 Per

NASA Astrophysics Data System (ADS)

Mugrauer, M.; Gilbert, H.; Hoffmann, S.

2018-05-01

On 2018 May 1th 20 UT (JD=2458240.333) we took spectroscopic data of the dwarf nova V392 Per (ATel #11588; ATel #11601; ATel #11605) with the echelle spectrograph FLECHAS (Mugrauer et al. 2014, AN 335, 417) at the 90cm telescope of the University Observatory Jena.

Confirmation of AT 2017eaw, a Probable Supernova in NGC 6946

NASA Astrophysics Data System (ADS)

Dong, Subo; Stanek, K. Z.

2017-05-01

Supernova candidate AT 2017eaw was discovered by Patrick Wiggins at 12.8 mag on 2017-05-14 05:42:43. We confirmed AT 2017eaw with images taken by Las Cumbres Observatory (LCO)'s 1m telescope at McDonald observatory on UT 2017-05-14 10:30:31.

Discovery and Spectroscopic Classification of DLT18q/AT2018aoz as a young type Ia Supernova

NASA Astrophysics Data System (ADS)

Sand, D.; Valenti, S.; Wyatt, S.; Bostroem, K. A.; Reichart, D. E.; Haislip, J. B.; Kouprianov, V.

2018-04-01

We report the discovery and classification of DLT18q/AT 2018aoz. The supernova was found on 2018 April 02.1 (UT) at r 15.1 mag during the ongoing D < 40 Mpc (DLT40) supernova search, using data from the PROMPT5 0.41m telescope located at CTIO.

VST: VLT Survey Telescope.

NASA Astrophysics Data System (ADS)

Arnaboldi, M.; Capaccioli, M.; Mancini, D.; Rafanelli, P.; Scaramella, R.; Sedmak, G.; Vettolani, G. P.

1998-09-01

The VLT era is rapidly approaching: the first instruments, ISAAC and FORS at UT1, will be available by the year 1999. Indeed, the beginning of the new millennium will witness fierce competition among quite a few 8-m telescopes, operated by different groups. As a consequence, there is a strong need to prepare, in a timely manner, suitable targetlists for the VLT, in order for it to play the leading role in ground-based optical and IR astronomy in the next decade. Preparation is one of the keys to success for the VLT observations.

VizieR Online Data Catalog: UV and optical photometric data for SN 2013by (Valenti+, 2015)

NASA Astrophysics Data System (ADS)

Valenti, S.; Sand, D.; Stritzinger, M.; Howell, D. A.; Arcavi, I.; McCully, C.; Childress, M. J.; Hsiao, E. Y.; Contreras, C.; Morrell, N.; Phillips, M. M.; Gromadzki, M.; Kirshner, R. P.; Marion, G. H.

2017-11-01

Photometric monitoring in BVgri of SN 2013by with the LCOGT 1 m telescope network began on 2013 April 24 (UT), and continued every two to three nights (52 epochs of data were collected) for more than 150 d, well after the light curve settled on to the 56Co decay tail. Additional imaging was obtained from Swift and the CSP. The CSP obtained 17 epochs of science images using the SITe3 CCD camera along with a set of ugriBV filters attached to the Swope 1 m telescope located at Las Campanas Observatory (LCO). (1 data file).

Liverpool Telescope classification of ATLAS16bdg as a Type Ia supernova near maximum light

NASA Astrophysics Data System (ADS)

Mundell, C. G.; Smith, R. J.; Childress, M. J.

2016-06-01

On 2016 June 15 at approximately 21:03 UT, we performed multicolour optical imaging, spectroscopy and polarimetry with the 2-m robotic Liverpool Telescope IO:O camera of galaxy NGC4708 in which a bright optical transient was reported by Tonry et al. ATel #9151 (ATLAS16bdg).

ATCA radio detection of the new X-ray transient MAXI J1813-095 as a candidate radio-quiet black hole X-ray binary

NASA Astrophysics Data System (ADS)

Russell, T. D.; Miller-Jones, J. C. A.; Sivakoff, G. R.; Tetarenko, A. J.; JACPOT XRB Collaboration

2018-02-01

We observed the new X-ray transient MAXI J1813-095 (ATels #11323, #11326, #11332) with the Australia Telescope Compact Array (ATCA) between 2018-02-22 20:52 UT and 2018-02-23 02:59 UT. Our observations were taken simultaneously at 5.5 and 9 GHz, with a bandwidth of 2 GHz at each frequency.

Spectroscopic confirmation and photometry of the Fe II nova M31N 2018-01a (AT2018gw)

NASA Astrophysics Data System (ADS)

Fabrika, S.; Sholukhova, O.; Vinokurov, A.; Valeev, A. F.; Solovyeva, Yu.; Hornoch, K.; Henze, M.; Shafter, A. W.; Williams, S. C.; Darnley, M. J.

2018-01-01

We report optical spectroscopic confirmation of the recent M31 nova candidate M31N 2018-01a (AT2018gw) (= PNV J00444425+4142449) (= ATLAS18eat) discovered by Emmanuel Conseil on 2018 Jan. 10.860 UT. The spectral data were obtained on 2018 Jan. 17.746 UT using the Russian BTA telescope equipped with the SCORPIO spectrograph.

Ten years maintaining MACAO-VLTI units in operation in the Very Large Telescope at Paranal Observatory

NASA Astrophysics Data System (ADS)

Salgado, F.; Hudepohl, G.

2016-07-01

More than 10 years have already passed since the first Multiple Application Curvature Adaptive Optics (MACAO) facilities got the first light in UT2 the 18th of April, 2003, in the Very Large Telescope (VLT) at Paranal Observatory. The achievable image sharpness of a ground-based telescope is normally limited by the effect of atmospheric turbulence. However, with Adaptive Optics (AO) techniques, this major drawback can be overcome so that the telescope produces images that are as sharp as theoretically possible, i.e., as if they were taken from space. [1] The intention of this document is summarize in few pages some highlights related with the activities needed to keep MACAO units in operation. Some statistics of problems based in Action Remedy tool is included, showing how through these years the number of problems has been reduced, even when there are still some unsolved ones. Some lessons have been learned and there are others one to learn. Corrective and predictive maintenance performed are shown too like the current measurements, transfer functions measurements, thermography pictures, health checks measuring interaction matrix and flat vectors to detect dead APDs or short circuits in the DM, etc. Some forced interventions are included as well like the removal of the cabinets from Coude rooms to avoid that acoustic noise and vibrations perturb the operations, the deformable mirrors reached by cooling leaks and a mirror that got rusty are shown too. Well knowledge of the system, good interaction between different disciplines groups to perform corrective and preventive maintenance seems to be key aspects of keeping it under control and operative during all these years leading to this good result.

VizieR Online Data Catalog: Interferometry and spectroscopy of sigma Orionis (Schaefer+, 2016)

NASA Astrophysics Data System (ADS)

Schaefer, G. H.; Hummel, C. A.; Gies, D. R.; Zavala, R. T.; Monnier, J. D.; Walter, F. M.; Turner, N. H.; Baron, F.; Ten Brummelaar, T.; Che, X.; Farrington, C. D.; Kraus, S.; Sturmann, J.; Sturmann, L.

2017-03-01

Interferometric data on the σ Orionis triple system were collected between 2010 and 2013 at the CHARA Array located on Mount Wilson, California. The array has six 1m telescopes arranged in a Y configuration with baselines ranging from 34 to 331m. here are two telescopes in each arm, labeled as E (East), W (West), and S (South). We used the Michigan Infrared Combiner (MIRC) to combine the light from three to six telescopes simultaneously. All data were collected after the photometric channels were installed in MIRC; the photometric channels measure the amount of light received from each telescope during the observations to improve the calibration. We used the low spectral resolution prism (R~42) to disperse the fringes across eight spectral channels in the H band (λ=1.5-1.8μm). Navy Prototype Optical Interferometer (NPOI) observations of σ Orionis were collected over a period from 2000 to 2013. Initially, the observations were obtained with the 3-beam combiner, and then, starting in 2002, with the 6-beam hybrid combiner. The NPOI beam combiners disperse the light and record the visibility spectra from 550 to 850 nm in 16 spectral channels. In total, some 59 nights of observations were executed, of which 26 nights were of good quality. The calibrators were selected from a list of single stars maintained at NPOI with diameters estimated from V and (V-K) using the surface brightness relation published by Mozurkewich et al. 2003AJ....126.2502M and van Belle et al. 2009MNRAS.394.1925V. The information for all of the calibrators is given in Table5. We obtained new spectroscopic radial velocity measurements of σ Orionis Aa,Ab using the 1.5m telescope at Cerro Tololo Inter-American Observatory (CTIO). We obtained 40 observations on 29 nights using the Fiber Echelle (FE) Spectrograph (http://www.ctio.noao.edu/~atokovin/echelle/FECH-overview.html) (R=25000, λ=4800-7000Å) between UT 2008 September 23 and 2009 February 21. Additional observations were obtained using the Chiron fiber-fed echelle spectrometer equipped with an image slicer (R=78000, λ=4550-8800Å) on 10 nights between UT 2012 November 4 and 2013 February 2 and 11 nights between UT 2016 January 21 and March 27. The Chiron observations were concentrated near the periastron passage of the close pair. The median radial velocities of σ Ori Aa and Ab, measured from the selected spectral lines, are presented in Table8. (5 data files).

Texas-style Fundraising and Public Relations for the International Year of Astronomy

NASA Astrophysics Data System (ADS)

Preston, Sandra; Barna, J. W.; Geiger, S.; Johnson, R.; Rimm, N.; Griffin, J.; Watson, K.

2008-05-01

McDonald Observatory can be a leader in Texas for the International Year of Astronomy (IYA09) celebration. Our strategy builds on the IYA09 program, tailoring it for the Texas audience, while also nationally promoting McDonald Observatory, UT Astronomy, the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) and our partnership in the Giant Magellan Telescope (GMT). We will also use this opportunity to make a concentrated outreach effort toward the Hispanic and Spanish-speaking communities in Texas and the nation, aligning with the IYA09 objective for improving relations with underrepresented and minority populations. Fundraising is a key ingredient to our success in 2009 and the future. With NASA Office of Space Science funding for education and public outreach being rethought, we will be focusing on new sources for fundraising, including private donations and corporate sponsorship, augmented by planned giving. We will take advantage of the timing to raise funds for special IYA09 programs, as well as for our large telescope projects HETDEX and GMT, along with our endowment and planned giving programs for education, outreach, and research. We will work with the UT McCombs School of Business on corporate sponsorship. During this time we will also go through a branding experience that will visually unify McDonald Observatory, UT Astronomy, and the education and public outreach programs. A consistent brand that can be used on the website and other media is our goal to build a stronger public presence that will aid us in our fundraising efforts. A Public Relations Internship Project produced a report to help launch this process. We are working with the UT College of Communications Advertising Department and with Hill Strategic Brand Solutions in Houston, Texas. We hope that our efforts will produce Texas-sized results!

SALT Spectroscopic classification of ASASSN-18lw as a dwarf nova

NASA Astrophysics Data System (ADS)

Buckley, D. A. H.; Gromadzki, M.; Dong, Subo; Stanek, K. Z.

2018-06-01

ASASSN-18lw (AT 2018cgo; RA: 19:28:50.74 Dec: -19:32:54.02) was discovered by the All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014) on 2018 June 5.92 UT. It was observed with the Southern African Large Telescope (SALT) using the Robert Stobie Spectrograph on 2018 June 10.92 UT (HJD 2458280.4297) employing the PG300 lines/mm grating.

ESPRESSO: the ultimate rocky exoplanets hunter for the VLT

NASA Astrophysics Data System (ADS)

Mégevand, Denis; Zerbi, Filippo M.; Cabral, Alexandre; Di Marcantonio, Paolo; Amate, Manuel; Pepe, Francesco; Cristiani, Stefano; Rebolo, Rafael; Santos, Nuno C.; Dekker, Hans; Abreu, Manuel; Affolter, Michael; Avila, Gerardo; Baldini, Veronica; Bristow, Paul; Broeg, Christopher; Carvas, Pedro; Cirami, Roberto; Coelho, João.; Comari, Maurizio; Conconi, Paolo; Coretti, Igor; Cupani, Guido; D'Odorico, Valentina; De Caprio, Vincenzo; Delabre, Bernard; Figueira, Pedro; Fleury, Michel; Fragoso, Ana; Genolet, Ludovic; Gomes, Ricardo; Gonzalez Hernandez, Jonay; Hughes, Ian; Iwert, Olaf; Kerber, Florian; Landoni, Marco; Lima, Jorge; Lizon, Jean-Louis; Lovis, Christophe; Maire, Charles; Mannetta, Marco; Martins, Carlos; Moitinho, André; Molaro, Paolo; Monteiro, Manuel; Rasilla, José Luis; Riva, Marco; Santana Tschudi, Samuel; Santin, Paolo; Sosnowska, Danuta; Sousa, Sergio; Spanò, Paolo; Tenegi, Fabio; Toso, Giorgio; Vanzella, Eros; Viel, Matteo; Zapatero Osorio, Maria Rosa

2012-09-01

ESPRESSO, the VLT rocky exoplanets hunter, will combine the efficiency of modern echelle spectrograph with extreme radial-velocity precision. It will be installed at Paranal on ESO's VLT in order to achieve a gain of two magnitudes with respect to its predecessor HARPS, and the instrumental radial-velocity precision will be improved to reach 10 cm/s level. We have constituted a Consortium of astronomical research institutes to fund, design and build ESPRESSO on behalf of and in collaboration with ESO, the European Southern Observatory. The project has passed the preliminary design review in November 2011. The spectrograph will be installed at the so-called "Combined Coudé Laboratory" of the VLT, it will be linked to the four 8.2 meters Unit Telescopes (UT) through four optical "Coudé trains" and will be operated either with a single telescope or with up to four UTs. In exchange of the major financial and human effort the building Consortium will be awarded with guaranteed observing time (GTO), which will be invested in a common scientific program. Thanks to its characteristics and the ability of combining incoherently the light of 4 large telescopes, ESPRESSO will offer new possibilities in many fields of astronomy. Our main scientific objectives are, however, the search and characterization of rocky exoplanets in the habitable zone of quiet, near-by G to M-dwarfs, and the analysis of the variability of fundamental physical constants. In this paper, we present the ambitious scientific objectives, the capabilities of ESPRESSO, the technical solutions for the system and its subsystems, enlightening the main differences between ESPRESSO and its predecessors. The project aspects of this facility are also described, from the consortium and partnership structure to the planning phases and milestones.

Debris search around (486958) 2014 MU69: Results from SOFIA and ground-based occultation campaigns

NASA Astrophysics Data System (ADS)

Young, Eliot F.; Buie, Marc W.; Porter, Simon Bernard; Zangari, Amanda Marie; Stern, S. Alan; Ennico, Kimberly; Reach, William T.; Pfueller, Enrico; Wiedemann, Manuel; Fraser, Wesley Cristopher; Camargo, Julio; Young, Leslie; Wasserman, Lawrence H.; New Horizons MU69 Occultation Team

2017-10-01

The New Horizons spacecraft is scheduled to fly by the cold classical KBO 2014 MU69 on 1-Jan-2019. The spacecraft speed relative to the MU69 will be in excess of 14 km/s. At these encounter velocities, impact with debris could be fatal to the spacecraft. We report on searches for debris in the neighborhood of MU69 conducted from SOFIA and ground-based sites. SOFIA observed the star field around MU69 on 10-Jul-2017 (UT) with their Focal Plane Imager (FPI+), operating at 20 Hz from 7:25 to 8:10 UT, spanning the time of the predicted occultation. Several large fixed telescopes observed the 3-Jun-2017, 10-Jul-2017 and/or the 17-Jul-2017 occultation events, including the 4-meter SOAR telescope, the 8-meter Gemini South telescope, and many 16-inch portable telescopes that were arranged in picket fences in South Africa and Argentina. We report on the light curves from these observing platforms and constraints on the optical depth due to debris or rings within the approximate Hill sphere (about 60,000 km across) of MU69. This work was supported by the New Horizons mission and NASA, with astrometric support from the Gaia mission and logistical support from Argentina and the US embassies in Buenos Aires and CapeTown. At SOAR, data acquisition has been done with a Raptor camera (visitor instrument) funded by the Observatorio Nacional/MCTIC.

AMBER/VLTI and MIDI/VLTI spectro-interferometric observations of the B[e] supergiant CPD-57°2874. Size and geometry of the circumstellar envelope in the near- and mid-IR

NASA Astrophysics Data System (ADS)

Domiciano de Souza, A.; Driebe, T.; Chesneau, O.; Hofmann, K.-H.; Kraus, S.; Miroshnichenko, A. S.; Ohnaka, K.; Petrov, R. G.; Preisbisch, T.; Stee, P.; Weigelt, G.; Lisi, F.; Malbet, F.; Richichi, A.

2007-03-01

We present the first high spatial and spectral resolution observations of the circumstellar envelope (CSE) of a B[e] supergiant (CPD-57°2874), performed with the Very Large Telescope Interferometer (VLTI). Spectra, visibilities and closure phase were obtained using the beam-combiner instruments AMBER (near-IR interferometry with three 8.3 m Unit Telescopes or UTs) and MIDI (mid-IR interferometry with two UTs). The interferometric observations of the CSE are well fitted by an elliptical Gaussian model with FWHM diameters varying linearly with wavelength. Typical diameters measured are ≃1.8×3.4 mas or ≃4.5×8.5 AU (adopting a distance of 2.5 kpc) at 2.2 μm, and ≃12×15 mas or ≃30×38 AU at 12 μm. The size of the region emitting the Brγ flux is ≃2.8×5.2 mas or ≃7.0×13.0 AU. The major-axis position angle of the elongated CSE in the mid-IR (≃144°) agrees well with previous polarimetric data, hinting that the hot-dust emission originates in a disk-like structure. In addition to the interferometric observations we also present new optical (UBVR_cI_c) and near-IR (JHKL) broadband photometric observations of CPD-57°2874. Our spectro-interferometric VLTI observations and data analysis support the non-spherical CSE paradigm for B[e] supergiants. Based on observations collected at the European Southern Observatory, Paranal, Chile, within the AMBER science demonstration time programme 074.A-9026 and the MIDI open time programme 074.D-0101.

The optical re-brightening of nova M31N 2017-11a

NASA Astrophysics Data System (ADS)

Xu, Zhijian; Gao, Xing; Li, Yanxi; Zhao, Jingyuan; Zhang, Mi

2017-12-01

We report the initial discovery of the optical re-brightening of the Fe II class nova M31N 2017-11a (AT2017hvi = PTSS-17zap) which was first reported by PMO-Tsinghua Supernova Survey (PTSS, http://www.cneost.org/ptss/ ), (2017, TNS Discovery Report https://wis-tns.weizmann.ac.il/object/2017hvi) at r-Sloan magnitude 18.5 on 2017-11-04 16:41:02 UT. Spectroscopy by Williams & Darnley using the 2-m Liverpool telescope (ATel #10990) on 2017 Nov 20.11 UT, and by Fabrika et al., (ATel #10998) taken two days later at the Russian BTA telescope, showed Balmer emission lines together with numerous strong Fe II lines, confirming its classification as a classical Fe II class nova.

EVN detection of Aql X-1 in outburst

NASA Astrophysics Data System (ADS)

Tudose, V.; Paragi, Z.; Miller-Jones, J.; Garrett, M.; Fender, R.; Rushton, A.; Spencer, R.

2009-11-01

The X-ray binary Aql X-1 has been in outburst in the last few weeks (ATEL #2288, #2296, #2299, #2302, #2303). We observed the system on 2009 November 19 between 14:30-19:00 UT at 5 GHz with the European VLBI Network (EVN) using the e-VLBI technique. The participating radio telescopes were Effelsberg (1 Gbps), Medicina (896 Mbps), Onsala 25m (1 Gbps), Torun (1 Gbps), Westerbork (1 Gbps), Yebes (896 Mbps), and Cambridge (128 Mbps).

The Perfect Science Machine

NASA Astrophysics Data System (ADS)

2008-05-01

ESO celebrates 10 years since First Light of the VLT Today marks the 10th anniversary since First Light with ESO's Very Large Telescope (VLT), the most advanced optical telescope in the world. Since then, the VLT has evolved into a unique suite of four 8.2-m Unit Telescopes (UTs) equipped with no fewer than 13 state-of-the-art instruments, and four 1.8-m moveable Auxiliary Telescopes (ATs). The telescopes can work individually, and they can also be linked together in groups of two or three to form a giant 'interferometer' (VLTI), allowing astronomers to see details corresponding to those from a much larger telescope. Green Flash at Paranal ESO PR Photo 16a/08 The VLT 10th anniversary poster "The Very Large Telescope array is a flagship facility for astronomy, a perfect science machine of which Europe can be very proud," says Tim de Zeeuw, ESO's Director General. "We have built the most advanced ground-based optical observatory in the world, thanks to the combination of a long-term adequately-funded instrument and technology development plan with an approach where most of the instruments were built in collaboration with institutions in the member states, with in-kind contributions in labour compensated by guaranteed observing time." Sitting atop the 2600m high Paranal Mountain in the Chilean Atacama Desert, the VLT's design, suite of instruments, and operating principles set the standard for ground-based astronomy. It provides the European scientific community with a telescope array with collecting power significantly greater than any other facilities available at present, offering imaging and spectroscopy capabilities at visible and infrared wavelengths. Blue Flash at Paranal ESO PR Photo 16b/08 A Universe of Discoveries The first scientifically useful images, marking the official 'First Light' of the VLT, were obtained on the night of 25 to 26 May 1998, with a test camera attached to "Antu", Unit Telescope number 1. They were officially presented to the press on the 27 May, exactly ten years ago. Since then, all four Unit Telescopes and four Auxiliary Telescopes went into routine operations and the number of instruments has continued to grow, to fill all the possible positions in the telescopes where instruments can be attached. In 2007, about 500 peer-reviewed papers using data collected with VLT and VLTI instruments at Paranal were published in scientific journals. Since the start of science operations, in April 1999, the VLT has led to the publication of more than 2200 refereed papers, an average of about one paper published every single working day. "The combination of high operational efficiency, system reliability and uptime for scientific observations results in very high scientific productivity," says Andreas Kaufer, director of the La Silla Paranal Observatory. The VLT and VLTI have contributed to all areas of astronomy, including the nature of dark matter and dark energy; the extreme physics of gamma-ray bursts and supernovae; the formation, structure and evolution of galaxies; the properties of exoplanets, Solar System objects, star clusters and stellar populations, the interstellar and intergalactic medium, and of super-massive black holes in galactic nuclei, in particular the one in the Galactic Centre; and the formation of stars and planets. The stunning scientific success of the VLT has attracted new member states to ESO. In the past decade Portugal joined (in 2001, after a ten-year associate status), followed by the United Kingdom (2002), Finland (2004), Spain (2006) and the Czech Republic (2007). Austria also announced its intent to join later this year. Another measure of success is the number of observing proposals made every year for the use of the VLT, which is now above the 1900 mark. On average, the amount of time requested to use the VLT is 6 times higher than what is available. The VLT will continue to increase in power over the next decade. The first of the second-generation VLT instruments, X-Shooter, will come online this year, with KMOS, SPHERE and MUSE to follow, together with multiple laser guide stars, an adaptive secondary mirror on Yepun (UT4), and one or more third-generation instruments, including an ultra-stable high-resolution spectrograph at the combined focus. The VLTI will also be equipped with second-generation instruments. Clearly, the VLT's story has only begun. More Information The VLT was designed from the start as an integrated system of four 8.2m telescopes, including the possibility to combine the light from individual telescopes for optical interferometry, enabling stupendous spatial resolution. First light on Antu occurred in May 1998, with Kueyen, Melipal and Yepun following soon after. Most of the VLT and VLTI instruments were built in close collaboration with institutes in the member states. The first-generation instrument suite was completed in 2007 with the commissioning of CRIRES. The Paranal arsenal includes turnkey adaptive optics systems and a rapid-response mode to react to fast transient events. Recently, the near-infrared imager HAWK-I was added as a 'generation-1.5' instrument.

Discovery of DLT18h/AT 2018xx with PROMPT and the DLT40 Survey

NASA Astrophysics Data System (ADS)

Sand, D.; Valenti, S.; Wyatt, S.; Bostroem, K. A.; Reichart, D. E.; Haislip, J. B.; Kouprianov, V.

2018-02-01

We report the discovery of DLT18h/AT 2018xx, which was first imaged on 2018 Feb 21.1 (UT) at R 17.2 mag during the ongoing D < 40 Mpc (DLT40) one day cadence supernova search, which uses data from the PROMPT5 0.41m telescope located at CTIO.

Giant Metrewave Radio Telescope Monitoring of the Black Hole X-Ray Binary, V404 Cygni during Its 2015 June Outburst

DOE Office of Scientific and Technical Information (OSTI.GOV)

Chandra, Poonam; Kanekar, Nissim

We report results from a Giant Metrewave Radio Telescope (GMRT) monitoring campaign of the black hole X-ray binary V404 Cygni during its 2015 June outburst. The GMRT observations were carried out at observing frequencies of 1280, 610, 325, and 235 MHz, and extended from June 26.89 UT (a day after the strongest radio/X-ray outburst) to July 12.93 UT. We find the low-frequency radio emission of V404 Cygni to be extremely bright and fast-decaying in the outburst phase, with an inverted spectrum below 1.5 GHz and an intermediate X-ray state. The radio emission settles to a weak, quiescent state ≈11 daysmore » after the outburst, with a flat radio spectrum and a soft X-ray state. Combining the GMRT measurements with flux density estimates from the literature, we identify a spectral turnover in the radio spectrum at ≈1.5 GHz on ≈ June 26.9 UT, indicating the presence of a synchrotron self-absorbed emitting region. We use the measured flux density at the turnover frequency with the assumption of equipartition of energy between the particles and the magnetic field to infer the jet radius (≈4.0 × 10{sup 13} cm), magnetic field (≈0.5 G), minimum total energy (≈7 × 10{sup 39} erg), and transient jet power (≈8 × 10{sup 34} erg s{sup −1}). The relatively low value of the jet power, despite V404 Cygni’s high black hole spin parameter, suggests that the radio jet power does not correlate with the spin parameter.« less

Spectroscopic Confirmation of TCP J07134590-2112330 as a Galactic Classical Nova in Canis Major

NASA Astrophysics Data System (ADS)

Strader, Jay; Chomiuk, Laura; Bahramian, Arash; Swihart, Sam

2018-03-01

TCP J07134590-2112330 was discovered by Yuji Nakamura on 2018 March 24.5 UT as a 12 mag optical transient. We obtained spectroscopic observations of TCP J07134590-2112330 with the Goodman spectrograph on the 4-m SOAR telescope on 2018 Mar 25.1 UT, with a low-resolution spectrum (R 1200) covering 3850-7850 A. The spectrum indicates that TCP J07134590-2112330 is a young classical nova, with strong hydrogen Balmer emission lines and additional strong lines of [O I] and Fe II. The Balmer lines show P Cygni profiles; the FWHM of the H alpha emission component is 1250 km/s, and the absorption trough extends to -2000 km/s.

Fermi Spots a Record Flare from Blazar

NASA Image and Video Library

2015-07-10

Blazar 3C 279's historic gamma-ray flare can be seen in this image from the Large Area Telescope (LAT) on NASA's Fermi satellite. Gamma rays with energies from 100 million to 100 billion electron volts (eV) are shown; for comparison, visible light has energies between 2 and 3 eV. The image spans 150 degrees, is shown in a stereographic projection, and represents an exposure from June 11 at 00:28 UT to June 17 at 08:17 UT. Credit: NASA/DOE/Fermi LAT Collaboration

Spectroscopic classification of Gaia17apq and Gaia17apv with Double Spectrograph on Palomar 200-inch telescope

NASA Astrophysics Data System (ADS)

Blagorodnova, N.; Adams, S.

2017-03-01

We report the classification of Gaia17apq and Gaia17apv (SN2017cao and SN2017cat), discovered by the Gaia ESA survey. The observations were performed on UT 2017-03-16 with the Double Spectrograph (DBSP; range 350-1000nm, spectral resolution R 4000) on Palomar 200-inch (P200) telescope.

Mid-Infrared Long-Baseline Interferometry of the Symbiotic Mira Star RX Pup with the VLTI/MIDI Instrument

NASA Astrophysics Data System (ADS)

Driebe, T.; Hofmann, K.-H.; Ohnaka, K.; Schertl, D.; Weigelt, G.

2007-11-01

We present mid-infrared long-baseline interferometric observations of the symbiotic Mira star RX Pup obtained with the VLTI/MIDI instrument within the framework of the Science Demonstration Time (SDT) program in February 2004. Four visibility measurements have been carried out using the unit telescopes UT2 and UT3, with projected baseline lengths ranging from 34.7 to 46.5 m. All visibility measurements show a distinct wavelength dependence: a rather steep decrease between 8 and 10 μm, and a shallower monotonic increase longward of 10 μm. For the corresponding uniform disk diameter, this visibility shape translates into a diameter increase by a factor of 2 from 25 to 50 mas between 8 and 10 μm and an almost wavelength-independent diameter between 10 and 13 μm. As we show by means of radiative transfer modeling with the code dusty, this wavelength dependence measured with VLTI/MIDI can be interpreted as the mid-infrared signature of a circumstellar dust shell which is dominated by silicate dust.

VizieR Online Data Catalog: BVI photometry of LMC bar variables (Di Fabrizio+, 2005)

NASA Astrophysics Data System (ADS)

di Fabrizio, L.; Clementini, G.; Maio, M.; Bragaglia, A.; Carretta, E.; Gratton, R.; Montegriffo, P.; Zoccali, M.

2005-01-01

We present the Johnson-Cousins B,V and I time series data obtained for 162 variable stars (135 RR Lyrae, 4 candidate Anomalous Cepheids, 11 Classical Cepheids, 11 eclipsing binaries and 1 delta Scuti star) in two 13x13 square arcmin areas close to the bar of the Large Magellanic Cloud. The photometric observations presented in this paper were carried out at the 1.54m Danish telescope located in La Silla, Chile, on the nights 4-7 January 1999, UT, and 23-24 January 2001, UT, respectively. In the paper we give coordinates, finding charts, periods, epochs, amplitudes, and mean quantities (intensity- and magnitude-averaged luminosities) of the variables with full coverage of the light variations, along with a discussion of the pulsation properties of the RR Lyrae stars in the sample. (8 data files).

Onsala Space Observatory: IVS Network Station

NASA Technical Reports Server (NTRS)

Haas, Ruediger; Elgered, Gunnar; Loefgren, Johan; Ning, Tong; Scherneck, Hans-Georg

2013-01-01

During 2012 we participated in 40 IVS sessions. As in the previous four years, we used the majority of the sessions that involved both Onsala and Tsukuba to do ultra-rapid dUT1 observations together with our colleagues in Tsukuba. We observed one four-station ultra-rapid EOP session together with Tsukuba, Hobart, and HartRAO. We also observed the RadioAstron satellite and several GLONASS satellites using the Onsala 25-m telescope. The highlight in 2012 was that our proposal to the Knut and Alice Wallenberg Foundation to establish a twin-telescope system at Onsala in accordance with the VLBI2010 recommendations was accepted.

Spectroscopic classification of PS17chm with Double Spectrograph on Palomar 200-inch telescope

NASA Astrophysics Data System (ADS)

Blagorodnova, N.; Kupfer, T.; Burdge, K.; Kasliwal, M.; Adams, S.

2017-04-01

We report the classification of PS17chm, discovered by the by the Pan-STARRS Survey for Transients (see Chambers et al. 2016, arXiv:1612.05560, and http://pswww.ifa.hawaii.edu ). The observations were performed on UT 2017-04-19 with the Double Spectrograph (DBSP; range 350-1000nm, spectral resolution R 4000) on Palomar 200-inch (P200) telescope.

Flares and Their Underlying Magnetic Complexity

NASA Astrophysics Data System (ADS)

Engell, Alexander J.; Siarkowski, Marek; Gryciuk, Magda; Sylwester, Janusz; Sylwester, Barbara; Golub, Leon; Korreck, Kelly; Cirtain, Jonathan

2011-01-01

SphinX (Solar PHotometer IN X-rays), a full-disk-integrated spectrometer, observed 137 flare-like/transient events with active region (AR) 11024 being the only AR on disk. The Hinode X-Ray Telescope (XRT) and Solar Optical Telescope observe 67 of these events and identified their location from 12:00 UT on July 3 through 24:00 UT 2009 July 7. We find that the predominant mechanisms for flares observed by XRT are (1) flux cancellation and (2) the shearing of underlying magnetic elements. Point- and cusp-like flare morphologies seen by XRT all occur in a magnetic environment where one polarity is impeded by the opposite polarity and vice versa, forcing the flux cancellation process. The shearing is either caused by flux emergence at the center of the AR and separation of polarities along a neutral line or by individual magnetic elements having a rotational motion. Both mechanisms are observed to contribute to single- and multiple-loop flares. We observe that most loop flares occur along a large portion of a polarity inversion line. Point- and cusp-like flares become more infrequent as the AR becomes organized with separation of the positive and negative polarities. SphinX, which allows us to identify when these flares occur, provides us with a statistically significant temperature and emission scaling law for A and B class flares: EM = 6.1 × 1033 T 1.9±0.1.

Columbus State University Global Observation and Outreach for the 2012 Transit of Venus

NASA Astrophysics Data System (ADS)

Perry, Matthew; McCarty, C.; Bartow, M.; Hood, J. C.; Lodder, K.; Johnson, M.; Cruzen, S. T.; Williams, R. N.

2013-01-01

Faculty, staff and students from Columbus State University’s (CSU’s) Coca-Cola Space Science Center presented a webcast of the 2012 Transit of Venus from three continents to a global audience of 1.4 million unique viewers. Team members imaged the transit with telescopes using white-light, hydrogen-alpha, and calcium filters, from Alice Springs, Australia; the Gobi Desert, Mongolia; Bryce Canyon, UT; and Columbus, GA. Images were webcast live during the transit in partnership with NASA’s Sun-Earth Day program, and Science Center staff members were featured on NASA TV. Local members of the public were brought in for a series of outreach initiatives, in both Georgia and Australia, before and during the transit. The data recorded from the various locations have been archived for use in demonstrating principles such as the historical measurement of the astronomical unit.

New Occultation Systems and the 2005 July 11 Charon Occultation

NASA Astrophysics Data System (ADS)

Young, L. A.; French, R. G.; Gregory, B.; Olkin, C. B.; Ruhland, C.; Shoemaker, K.; Young, E. F.

2005-08-01

Charon's density is an important input to models of its formation and internal structure. Estimates range from 1.59 to 1.83 g/cm3 (Olkin et al. 2003. Icarus 164, 254), with Charon's radius as the main source of uncertainty. Reported values of Charon's radius from mutual events range from 593±13 (Buie et al. 1992, Icarus 97, 211) to 621±21 km (Young & Binzel 1994, Icarus 108), while an occultation observed from a single site gives a lower limit on the radius of 601.5 km (Walker 1980 MNRAS 192, 47; Elliot & Young 1991, Icarus 89, 244). On 2005 July 11 UT (following this abstract submission date), Charon is predicted to occult the star C313.2. If successful, this event will be the first Charon occultation observed since 1980, and the first giving multiple chords across Charon's disk. This event is expected to measure Charon's radius to 1 km. Our team is observing from three telescopes in Chile, the 4.0-m Blanco and the 0.9-m telescopes at Cerro Tololo and the 4.2-m SOAR telescope at Cerro Pachon. At SOAR, we will be using the camera from our new PHOT systems (Portable High-speed Occultation Telescopes). The PHOT camera is a Princeton Instrument MicroMAX:512BFT from Roper Scientific, a 512×512 frame-transfer CCD with a readnoise of only 3 electrons at the 100 kHz digitization rate. The camera's exposures are triggered by a custom built, compact, stand-alone GPS-based pulse-train generator. A PHOT camera and pulse-train generator were used to observe the occultation of 2MASS 1275723153 by Pluto on 2005 June 15 UT from Sommers-Bausch Observatory in Boulder Colorado; preliminary analysis shows this was at best a grazing occultation from this site and a successful engineering run for the July 11 Charon occultation. The work was supported, in part, by NSF AST-0321338 (EFY) and NASA NNG-05GF05G (LAY).

Spectroscopic classification of SN 2018brz as a type Ia supernova before maximum

NASA Astrophysics Data System (ADS)

Galbany, Lluis; Lopez-Sanchez, Angel R.; Ascasibar, Yago; Fiegert, Kristin

2018-05-01

We report the spectroscopic classification of SN 2018brz (RA=08:33:22.27, DEC=-76:37:39.8) in an anonymous host galaxy. The candidate was discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN: Shappee et al. 2014) on UT 2018-05-15 at 16.5 mag. Observations were performed on the 4m Anglo-Australian Telescope at Siding Spring Observatory on 2018 May 19 9:15 UT, using Koala+AAOmega and Grisms 580V+1000R (3500-6000A and 6300-7300A).

ASASSN-18ca: Discovery of A Probable Nova in M31

NASA Astrophysics Data System (ADS)

Brimacombe, J.; Vallely, P.; Stanek, K. Z.; Kochanek, C. S.; Brown, J. S.; Shields, J.; Thompson, T. A.; Shappee, B. J.; Holoien, T. W.-S.; Prieto, J. L.; Bersier, D.; Dong, Subo; Bose, S.; Chen, Ping; Stritzinger, M.; Holmbo, S.

2018-02-01

During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin"), using data from the quadruple 14-cm "Leavitt" telescope in Fort Davis, Texas, we discovered a new transient source, most likely a nova, in the nearby galaxy M31. ASASSN-18ca (AT 2018pp) was discovered in images obtained on UT 2018-02-08.07 at g 16.5 mag. We do not detect (g > 18.6) the object in images taken on UT 2018-02-06.12 and before.

Optical Spectroscopy of TCP J04432130+4721280 (V392 Per) Confirms a Nova Eruption

NASA Astrophysics Data System (ADS)

Wagner, R. M.; Terndrup, D.; Darnley, M. J.; Starrfield, S.; Woodward, C. E.; Henze, M.

2018-04-01

Following reports of a new transient of magnitude 6.2 in Perseus on 2018 April 29.4740 UT discovered by Y. Nakamura designated TCP J04432130+4721280 (http://www.cbat.eps.harvard.edu/unconf/followups/J04432130+4721280.html) and positionally coincident with the previously known U Gem type dwarf nova V392 Per, we obtained an optical spectrum on 2018 April 30.116 UT (range: 396-687 nm; resolution 0.3 nm) with the 2.4 m Hiltner telescope (+OSMOS) of the MDM Observatory on Kitt Peak.

Spectroscopic Classification of PS16ccj with Mayall/KOSMOS

NASA Astrophysics Data System (ADS)

Pan, Y.-C.; Foley, R. J.; Jha, S. W.; Rest, A.; Scolnic, D.

2016-05-01

We report the classification of PS16ccj from spectroscopic observation with KOSMOS on the Mayall telescope. The observation was made on 2016 May 05 UT. We classify PS16ccj as a SN Ia near maximum light.

Discovery of an Apparent Nova in M81

NASA Astrophysics Data System (ADS)

Hornoch, K.; Kucakova, H.; Williams, S. C.; Henze, M.; Sala, G.; Jose, J.; Figueira, J.; Sin, P.; Meusinger, H.; Darnley, M. J.; Kaur, A.; Hartmann, D. H.; Shafter, A. W.

2017-12-01

The M81 nova monitoring collaboration reports the discovery of an apparent nova in M81 on a co-added 3150-s unfiltered CCD frame taken on 2017 Dec. 2.127 UT with the 0.65-m telescope at Ondrejov (OND).

Discovery of a Probable Nova in M81

NASA Astrophysics Data System (ADS)

Hornoch, K.; Kucakova, H.; Williams, S. C.; Henze, M.; Sala, G.; Jose, J.; Meusinger, H.; Darnley, M. J.; Kaur, A.; Hartmann, D. H.; Shafter, A. W.

2018-01-01

The M81 nova monitoring collaboration reports the discovery of a probable nova in M81 on a co-added 3150-s unfiltered CCD frame taken on 2018 Jan. 30.776 UT with the 0.65-m telescope at Ondrejov (OND).

Discovery of two Probable Novae in M81

NASA Astrophysics Data System (ADS)

Hornoch, K.; Kucakova, H.; Henze, M.; Sala, G.; Jose, J.; Figueira, J.; Sin, P.; Hernanz, M.; Williams, S. C.; Meusinger, H.; Darnley, M. J.; Kaur, A.; Hartmann, D. H.; Shafter, A. W.

2017-09-01

The M81 nova monitoring collaboration reports the discovery of two probable novae in M81 on a co-added 2700-s unfiltered CCD frame taken on 2017 Sep. 18.129 UT with the 0.65-m telescope at Ondrejov (OND).

Discovery of a Probable Nova in M81

NASA Astrophysics Data System (ADS)

Hornoch, K.; Kucakova, H.; Williams, S. C.; Henze, M.; Sala, G.; Jose, J.; Figueira, J.; Sin, P.; Meusinger, H.; Darnley, M. J.; Kaur, A.; Hartmann, D. H.; Shafter, A. W.

2017-12-01

The M81 nova monitoring collaboration reports the discovery of a probable nova in M81 on a co-added 2610-s unfiltered CCD frame taken on 2017 Dec. 26.016 UT with the 0.65-m telescope at Ondrejov (OND).

Spectroscopic Classification of SN 2018gv with Keck I/LRIS

NASA Astrophysics Data System (ADS)

Siebert, M. R.; Dimitriadis, G.; Foley, R. J.

2018-01-01

We obtained spectroscopic observations of SN 2018gv with the LRIS spectrograph on the 10-m Keck I telescope on 2018 Jan 16 UT. The spectrum indicates that SN 2018gv is a very young, normal Type Ia supernova.

WATER IN COMETS 71P/CLARK AND C/2004 B1 (LINEAR) WITH SPITZER

DOE Office of Scientific and Technical Information (OSTI.GOV)

Bockelee-Morvan, Dominique; Woodward, Charles E.; Kelley, Michael S.

2009-05-10

We present 5.5-7.6 {mu}m spectra of comets 71P/Clark (2006 May 27.56 UT, r{sub h} = 1.57 AU pre-perihelion) and C/2004 B1 (LINEAR) (2005 October 15.22 UT, r{sub h} = 2.21 AU pre-perihelion and 2006 May 16.22 UT, r{sub h} = 2.06 AU post-perihelion) obtained with the Spitzer Space Telescope. The {nu}{sub 2} vibrational band of water is detected with a signal-to-noise ratio of 11-50. Fitting the spectra using a fluorescence model of water emission yields a water rotational temperature of < 18 K for 71P/Clark and {approx_equal}14 {+-} 2 K (pre-perihelion) and 23 {+-} 4 K (post-perihelion) for C/2004 B1more » (LINEAR). The water ortho-to-para ratio in C/2004 B1 (LINEAR) is measured to be 2.31 {+-} 0.18, which corresponds to a spin temperature of 26{sup +3} {sub -2} K. Water production rates are derived. The agreement between the water model and the measurements is good, as previously found for Spitzer spectra of C/2003 K4 (LINEAR). The Spitzer spectra of these three comets do not show any evidence for emission from polycyclic aromatic hydrocarbons and carbonate minerals, in contrast to results reported for comets 9P/Tempel 1 and C/1995 O1 (Hale-Bopp)« less

And Then There Were Three...!

NASA Astrophysics Data System (ADS)

2000-01-01

VLT MELIPAL Achieves Successful "First Light" in Record Time This was a night to remember at the ESO Paranal Observatory! For the first time, three 8.2-m VLT telescopes were observing in parallel, with a combined mirror surface of nearly 160 m 2. In the evening of January 26, the third 8.2-m Unit Telescope, MELIPAL ("The Southern Cross" in the Mapuche language), was pointed to the sky for the first time and successfully achieved "First Light". During this night, a number of astronomical exposures were made that served to evaluate provisionally the performance of the new telescope. The ESO staff expressed great satisfaction with MELIPAL and there were broad smiles all over the mountain. The first images ESO PR Photo 04a/00 ESO PR Photo 04a/00 [Preview - JPEG: 400 x 352 pix - 95k] [Normal - JPEG: 800 x 688 pix - 110k] Caption : ESO PR Photo 04a/00 shows the "very first light" image for MELIPAL . It is that of a relatively bright star, as recorded by the Guide Probe at about 21:50 hrs local time on January 26, 2000. It is a 0.1 sec exposure, obtained after preliminary adjustment of the optics during a few iterations with the computer controlled "active optics" system. The image quality is measured as 0.46 arcsec FWHM (Full-Width at Half Maximum). ESO PR Photo 04b/00 ESO PR Photo 04b/00 [Preview - JPEG: 400 x 429 pix - 39k] [Normal - JPEG: 885 x 949 pix - 766k] Caption : ESO PR Photo 04b/00 shows the central region of the Crab Nebula, the famous supernova remnant in the constellation Taurus (The Bull). It was obtained early in the night of "First Light" with the third 8.2-m VLT Unit Telescope, MELIPAL . It is a composite of several 30-sec exposures with the VLT Test Camera in three broad-band filters, B (here rendered as blue; most synchrotron emission), V (green) and R (red; mostly emission from hydrogen atoms). The Crab Pulsar is visible to the left; it is the lower of the two brightest stars near each other. The image quality is about 0.9 arcsec, and is completely determined by the external seeing caused by the atmospheric turbulence above the telescope at the time of the observation. The coloured, vertical lines to the left are artifacts of a "bad column" of the CCD. The field measures about 1.3 x 1.3 arcmin 2. This image may be compared with that of the same area that was recently obtained with the FORS2 instrument at KUEYEN ( PR Photo 40g/99 ). Following two days of preliminary adjustments after the installation of the secondary mirror, cf. ESO PR Photos 03a-n/00 , MELIPAL was pointed to the sky above Paranal for the first time, soon after sunset in the evening of January 26. The light of a bright star was directed towards the Guide Probe camera, and the VLT Commissioning Team, headed by Dr. Jason Spyromilio , initiated the active optics procedure . This adjusts the 150 computer-controlled supports under the main 8.2-m Zerodur mirror as well as the position of the secondary 1.1-m Beryllium mirror. After just a few iterations, the optical quality of the recorded stellar image was measured as 0.46 arcsec ( PR Photo 04a/00 ), a truly excellent value, especially at this stage! Immediately thereafter, at 22:16 hrs local time (i.e., at 01:16 hrs UT on January 27), the shutter of the VLT Test Camera at the Cassegrain focus was opened. A 1-min exposure was made through a R(ed) optical filter of a distant star cluster in the constellation Eridanus (The River). The light from its faint stars was recorded by the CCD at the focal plane and the resulting frame was read into the computer. Despite the comparatively short exposure time, myriads of stars were seen when this "first frame" was displayed on the computer screen. Moreover, the sizes of these images were found to be virtually identical to the 0.6 arcsec seeing measured simultaneously with a monitor telescope, outside the telescope enclosure. This confirmed that MELIPAL was in very good shape. Nevertheless, these very first images were still slightly elongated and further optical adjustments and tests were therefore made to eliminate this unwanted effect. It is a tribute to the extensive experience and fine skills of the ESO staff that within only 1 hour, a 30 sec exposure of the central region of the Crab Nebula in Taurus with round images was obtained, cf. PR Photo 04b/00 . The ESO Director General, Dr. Catherine Cesarsky , who assumed her function in September 1999, was present in the Control Room during these operations. She expressed great satisfaction with the excellent result and warmly congratulated the ESO staff to this achievement. She was particularly impressed with the apparent ease with which a completely new telescope of this size could be adjusted in such a short time. A part of her statement on this occasion was recorded on ESO PR Video Clip 02/00 that accompanies this Press Release. Three telescopes now in operation at Paranal At 02:30 UT on January 27, 2000, three VLT Unit Telescopes were observing in parallel, with measured seeing values of 0.6 arcsec ( ANTU - "The Sun"), 0.7 arcsec ( KUEYEN -"The Moon") and 0.7 arcsec ( MELIPAL ). MELIPAL has now joined ANTU and KUEYEN that had "First Light" in May 1998 and March 1999, respectively. The fourth VLT Unit Telescope, YEPUN ("Sirius") will become operational later this year. While normal scientific observations continue with ANTU , the UVES and FORS2 astronomical instruments are now being commissioned at KUEYEN , before this telescope will be handed over to the astronomers on April 1, 2000. The telescope commissioning period will now start for MELIPAL , after which its first instrument, VIMOS will be installed later this year. Impressions from the MELIPAL "First Light" event First Light for MELIPAL ESO PR Video Clip 02/00 "First Light for MELIPAL" (3350 frames/2:14 min) [MPEG Video+Audio; 160x120 pix; 3.1Mb] [MPEG Video+Audio; 320x240 pix; 9.4 Mb] [RealMedia; streaming; 34kps] [RealMedia; streaming; 200kps] ESO Video Clip 02/00 shows sequences from the Control Room at the Paranal Observatory, recorded with a fixed TV-camera on January 27 at 03:00 UT, soon after the moment of "First Light" with the third 8.2-m VLT Unit Telescope ( MELIPAL ). The video sequences were transmitted via ESO's dedicated satellite communication link to the Headquarters in Garching for production of the Clip. It begins with a statement by the Manager of the VLT Project, Dr. Massimo Tarenghi , as exposures of the Crab Nebula are obtained with the telescope and the raw frames are successively displayed on the monitor screen. In a following sequence, ESO's Director General, Dr. Catherine Cesarsky , briefly relates the moment of "First Light" for MELIPAL , as she experienced it at the telescope controls. ESO Press Photo 04c/00 ESO Press Photo 04c/00 [Preview; JPEG: 400 x 300; 44k] [Full size; JPEG: 1600 x 1200; 241k] The computer screen with the image of a bright star, as recorded by the Guide Probe in the early evening of January 26; see also PR Photo 04a/00. This image was used for the initial adjustments by means of the active optics system. (Digital Photo). ESO Press Photo 04d/00 ESO Press Photo 04d/00 [Preview; JPEG: 400 x 314; 49k] [Full size; JPEG: 1528 x 1200; 189k] ESO staff at the moment of "First Light" for MELIPAL in the evening of January 26. The photo was made in the wooden hut on the telescope observing floor from where the telescope was controlled during the first hours. (Digital Photo). ESO PR Photos may be reproduced, if credit is given to the European Southern Observatory. The ESO PR Video Clips service to visitors to the ESO website provides "animated" illustrations of the ongoing work and events at the European Southern Observatory. The most recent clip was: ESO PR Video Clip 01/00 with aerial sequences from Paranal (12 January 2000). Information is also available on the web about other ESO videos.

VizieR Online Data Catalog: Observed red supergiants in the inner Galaxy (Messineo+, 2016)

NASA Astrophysics Data System (ADS)

Messineo, M.; Zhu, Q.; Menten, K. M.; Ivanov, V. D.; Figer, D. F.; Kudritzki, R.-P.; Rosie, Chen C.-H.

2018-02-01

Spectroscopic observations were carried out with the Son of ISAAC (SofI; Moorwood et al. 1998Msngr..91....9M) Spectrograph on the ESO/New Technology Telescope (NTT) 3.58 m telescope of the La Silla Observatory, on the three nights from UT 2015 June 16 to 19-program ID 095.D-0252(A). Spectra with the low-resolution red grism, and the 0.6" wide slit, delivering resolution R~980 over the wavelength range λ=1.53-2.52 μm were obtained for 94 targets. For each target a minimum number of four exposures, nodded along the slit, were taken in an ABBA sequence. Typical integration times per frame ranged from 2 to 100 s (DITsxNDITs). (1 data file).

Independent Discovery of a Probable Nova in M81

NASA Astrophysics Data System (ADS)

Kucakova, H.; Hornoch, K.; Williams, S. C.; Henze, M.; Sala, G.; Jose, J.; Meusinger, H.; Darnley, M. J.; Kaur, A.; Hartmann, D. H.; Shafter, A. W.

2018-03-01

The M81 nova monitoring collaboration reports the independent discovery of a probable nova in M81 on a co-added 1350-s unfiltered CCD frame taken on 2018 Mar. 21.952 UT with the 0.65-m telescope at Ondrejov.

Independent Discovery of a Probable Nova in M81

NASA Astrophysics Data System (ADS)

Hornoch, K.; Kucakova, H.; Williams, S. C.; Henze, M.; Sala, G.; Jose, J.; Meusinger, H.; Darnley, M. J.; Kaur, A.; Hartmann, D. H.; Shafter, A. W.

2018-04-01

The M81 nova monitoring collaboration reports the independent discovery of a probable nova in M81 on a co-added 2700-s unfiltered CCD frame taken on 2018 Apr. 2.815 UT with the 0.65-m telescope at Ondrejov.

Independent Discovery of an Apparent Nova in M81

NASA Astrophysics Data System (ADS)

Hornoch, K.; Kucakova, H.; Williams, S. C.; Henze, M.; Sala, G.; Jose, J.; Meusinger, H.; Darnley, M. J.; Kaur, A.; Hartmann, D. H.; Shafter, A. W.

2018-02-01

The M81 nova monitoring collaboration reports the independent discovery of an apparent nova in M81 on a co-added 2700-s unfiltered CCD frame taken on 2018 Feb. 19.039 UT with the 0.65-m telescope at Ondrejov (OND).

Swift detection of MAXI J1820+070

NASA Astrophysics Data System (ADS)

Kennea, J. A.; Marshall, F. E.; Page, K. L.; Palmer, D. M.; Siegel, M. H.; Neil Gehrels Swift Observatory Team

2018-03-01

This is reposted from GCN #22471 as it is of interest to the transient community. At 00:11:39 UT, the Swift Burst Alert Telescope (BAT) triggered and located MAXI J1820+070 (Kawamuro et al, 2018; ATel #11399) (trigger=813771, retriggering as trigger=813772).

Classification of ASASSN-15ph as a Normal Type Ia Supernova

NASA Astrophysics Data System (ADS)

Zinn, J.; Porter, A.; Wagner, R. M.

2015-09-01

We obtained an optical spectrum (range: 398-686 nm; resolution 0.3 nm) of ASASSN-15ph (ATEL #8028) on 2015 September 12.346 UT with the Hiltner 2.4 m telescope (+OSMOS) of the MDM Observatory on Kitt Peak, Arizona.

Independent Discovery of a Probable Luminous Nova in M81

NASA Astrophysics Data System (ADS)

Hornoch, K.; Kucakova, H.; Williams, S. C.; Henze, M.; Sala, G.; Jose, J.; Meusinger, H.; Darnley, M. J.; Kaur, A.; Hartmann, D. H.; Shafter, A. W.

2018-04-01

The M81 nova monitoring collaboration reports the independent discovery of a probable luminous nova in M81 on a co-added 4410-s unfiltered CCD frame taken on 2018 Apr. 9.044 UT with the 0.65-m telescope at Ondrejov.

FLOYDS Classification of DLT17u/AT 2017cbv as a Very Young Type Ia Supernova

NASA Astrophysics Data System (ADS)

Hosseinzadeh, G.; Howell, D. A.; Sand, D.; Valenti, S.; Tartaglia, L.; McCully, C.; Bostroem, K. A.; Wyatt, S.; Arcavi, I.

2017-03-01

We obtained a spectrum of DLT17u/AT 2017cbv on 2017 March 10.7 UT (ATel #10158) with the robotic FLOYDS instrument mounted on the Las Cumbres Observatory 2-meter telescope in Siding Spring, Australia.

Spectroscopic Classifications of PSN J20372558+6607115 with Lick 3-m Reflector

NASA Astrophysics Data System (ADS)

Foley, R. J.; Zheng, W.; Filippenko, A. V.; van Dyk, S. D.

2015-03-01

We report the classifications of PSN J20372558+6607115 (discovered by K. Shima and announced on the CBAT TOCP) from a spectrum obtained with the Kast dual-beam spectrograph on the Lick 3-m Shane telescope on 2015 March 26 UT.

Planetary radar targets 1999 AP10, 2000 TO64, 2000 UJ1, and 2000 XK44: Four S-complex near-Earth asteroids.

NASA Astrophysics Data System (ADS)

Hicks, M.; Lawrence, K.

2009-12-01

We report taxonomic classifications of four near-Earth asteroids (1999 AP10, 2000 TO64, 2000 UJ1, and 2000 XK44) scheduled for radar observation by the JPL radar group at the Arecibo facility in Oct-Nov 2009, using long-slit CCD spectroscopy acquired at the Palomar 5-m telescope on 2009 Nov 09 UT. Table 1 lists the observation circumstances. Normalized reflectance spectra are shown in Figures 1-4 [1]VizieR Online Data Catalog: White dwarf candidates in DECam first field (Belardi+, 2016)

NASA Astrophysics Data System (ADS)

Belardi, C.; Kilic, M.; Munn, J. A.; Gianninas, A.; Barber, S. D.; Dey, A.; Stetson, P. B.

2018-02-01

We used DECam mounted on the Blanco 4m Telescope on UT 2014 Feb 2-9 to obtain g-band exposures of a three square degree field (corresponding to a single DECam pointing) centred at Right Ascension RA=09:03:02 and Declination DE=-04:35:00. Our observations were performed under the NOAO program 2014A-0073. This field was previously observed by the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS1) between 2003 and 2008, and is part of the CFHTLS Wide 2 field, which is a 25 square degree field with MegaCam ugriz photometry available. The earlier MegaCam data provide the first epoch for our proper motion measurements. (4 data files).

High angular resolution N-band observation of the silicate carbon star IRAS08002-3803 with the VLTI/MIDI instrument . Dusty environment spatially resolved

NASA Astrophysics Data System (ADS)

Ohnaka, K.; Driebe, T.; Hofmann, K.-H.; Leinert, Ch.; Morel, S.; Paresce, F.; Preibisch, Th.; Richichi, A.; Schertl, D.; Schöller, M.; Waters, L. B. F. M.; Weigelt, G.; Wittkowski, M.

2006-01-01

We present the results of N-band spectro-interferometric observations of the silicate carbon star IRAS08002-3803 with the MID-infrared Interferometric instrument (MIDI) at the Very Large Telescope Interferometer (VLTI) of the European Southern Observatory (ESO). The observations were carried out using two unit telescopes (UT2 and UT3) with projected baseline lengths ranging from 39 to 47 m. Our observations of IRAS08002-3803 have spatially resolved the dusty environment of a silicate carbon star for the first time and revealed an unexpected wavelength dependence of the angular size in the N band: the uniform-disk diameter is found to be constant and 36 mas (72 Rstar) between 8 and 10 μm, while it steeply increases longward of 10 μm to reach 53 mas (106 Rstar) at 13 μm. Model calculations with our Monte Carlo radiative transfer code show that neither spherical shell models nor axisymmetric disk models consisting of silicate grains alone can simultaneously explain the observed wavelength dependence of the visibility and the spectral energy distribution (SED). We propose that the circumstellar environment of IRAS08002-3803 may consist of two grain species coexisting in the disk: silicate and a second grain species, for which we consider amorphous carbon, large silicate grains, and metallic iron grains. Comparison of the observed visibilities and SED with our models shows that such disk models can fairly - though not entirely satisfactorily - reproduce the observed SED and N-band visibilities. Our MIDI observations and the radiative transfer calculations lend support to the picture where oxygen-rich material around IRAS08002-3803 is stored in a circumbinary disk surrounding the carbon-rich primary star and its putative low-luminosity companion.

Spectroscopic classification of SN 2018kv as a type Ia supernova

NASA Astrophysics Data System (ADS)

Zhang, Jujia; Lu, Kaixing; Wang, Xiaofeng; Xu, Zhijian; Li, Wenxiong; Zhang, Tianmeng; Tan, Hanjie; Li, Zhitong; Song, Hao; University, Jun Mo (Tsinghua

2018-01-01

We obtained an optical spectrum (range 350-900 nm) of SN 2018kv, discovered by the Tsinghua-NAOC Transient Survey, on UT 2018 Jan. 26.9 with the Li-Jiang 2.4 m telescope (LJT+YFOSC) at Li-Jiang Observatory of Yunnan Observatories.

Spectroscopic Classification of SN 2017ixe as a Type Ia Supernova

NASA Astrophysics Data System (ADS)

Zhang, Jujia; Yu, Xiaoguang; Wang, Xiaofeng

2017-12-01

We obtained an optical spectrum (range 340-900 nm) of SN 2017ixe (PSP17G), discovered by XOSS, on UT Dec. 15.7 2017 with the Li-Jiang 2.4 m telescope (LJT + YFOSC) at Li-Jiang Observatory of Yunnan Observatories (YNAO).

Spectroscopic classification of SN 2018iq as a Type Ia Supernova

NASA Astrophysics Data System (ADS)

Zhang, Jujia; Lu, Kaixing; Wang, Xiaofeng

2018-01-01

We obtained an optical spectrum (range 350-900 nm) of SN 2018iq (=AT2017jzx), discovered by Koichi Itagaki, on UT 2018 Jan. 20.7 with the Li-Jiang 2.4 m telescope (LJT+YFOSC) at Li-Jiang Observatory of Yunnan Observatories.

Superhump Period of MASTER OT

NASA Astrophysics Data System (ADS)

Garnavich, Peter; McClelland, Colin

2013-02-01

We observed the optical transient MASTER OT J065608.28+744455.2 (ATEL #4783) with the Vatican Advanced Technology Telescope (VATT) and VATT4K CCD camera. V-band imaging began at 2013 Feb. 5.15 (UT) and continued for 3.3 hours with a time resolution of 22 seconds.

Further spectroscopy of the 2017 outburst of PT And

NASA Astrophysics Data System (ADS)

Williams, S. C.; Darnley, M. J.

2017-09-01

We obtained our first spectrum of the 2017 outburst of PT And (AT 2017gay) on 2017 Aug 17.05 UT and reported the results in ATel #10647. Another spectrum, taken 2017 Aug 24.16 with the Nordic Optical Telescope was reported by ATel #10672.

Transgenic Restoration of Urea Transporter A1 Confers Maximal Urinary Concentration in the Absence of Urea Transporter A3.

PubMed

Klein, Janet D; Wang, Yanhua; Mistry, Abinash; LaRocque, Lauren M; Molina, Patrick A; Rogers, Richard T; Blount, Mitsi A; Sands, Jeff M

2016-05-01

Urea has a critical role in urinary concentration. Mice lacking the inner medullary collecting duct (IMCD) urea transporter A1 (UT-A1) and urea transporter A3 (UT-A3) have very low levels of urea permeability and are unable to concentrate urine. To investigate the role of UT-A1 in the concentration of urine, we transgenically expressed UT-A1 in knockout mice lacking UT-A1 and UT-A3 using a construct with a UT-A1 gene that cannot be spliced to produce UT-A3. This construct was inserted behind the original UT-A promoter to yield a mouse expressing only UT-A1 (UT-A1(+/+)/UT-A3(-/-)). Western blot analysis demonstrated UT-A1 in the inner medulla of UT-A1(+/+)/UT-A3(-/-) and wild-type mice, but not in UT-A1/UT-A3 knockout mice, and an absence of UT-A3 in UT-A1(+/+)/UT-A3(-/-) and UT-A1/UT-A3 knockout mice. Immunohistochemistry in UT-A1(+/+)/UT-A3(-/-) mice also showed negative UT-A3 staining in kidney and other tissues and positive UT-A1 staining only in the IMCD. Urea permeability in isolated perfused IMCDs showed basal permeability in the UT-A1(+/+)/UT-A3(-/-) mice was similar to levels in wild-type mice, but vasopressin stimulation of urea permeability in wild-type mice was significantly greater (100% increase) than in UT-A1(+/+)/UT-A3(-/-) mice (8% increase). Notably, basal urine osmolalities in both wild-type and UT-A1(+/+)/UT-A3(-/-) mice increased upon overnight water restriction. We conclude that transgenic expression of UT-A1 restores basal urea permeability to the level in wild-type mice but does not restore vasopressin-stimulated levels of urea permeability. This information suggests that transgenic expression of UT-A1 alone in mice lacking UT-A1 and UT-A3 is sufficient to restore urine-concentrating ability. Copyright © 2016 by the American Society of Nephrology.

Transgenic Restoration of Urea Transporter A1 Confers Maximal Urinary Concentration in the Absence of Urea Transporter A3

PubMed Central

Wang, Yanhua; Mistry, Abinash; LaRocque, Lauren M.; Molina, Patrick A.; Rogers, Richard T.; Blount, Mitsi A.; Sands, Jeff M.

2016-01-01

Urea has a critical role in urinary concentration. Mice lacking the inner medullary collecting duct (IMCD) urea transporter A1 (UT-A1) and urea transporter A3 (UT-A3) have very low levels of urea permeability and are unable to concentrate urine. To investigate the role of UT-A1 in the concentration of urine, we transgenically expressed UT-A1 in knockout mice lacking UT-A1 and UT-A3 using a construct with a UT-A1 gene that cannot be spliced to produce UT-A3. This construct was inserted behind the original UT-A promoter to yield a mouse expressing only UT-A1 (UT-A1+/+/UT-A3−/−). Western blot analysis demonstrated UT-A1 in the inner medulla of UT-A1+/+/UT-A3−/− and wild-type mice, but not in UT-A1/UT-A3 knockout mice, and an absence of UT-A3 in UT-A1+/+/UT-A3−/− and UT-A1/UT-A3 knockout mice. Immunohistochemistry in UT-A1+/+/UT-A3−/− mice also showed negative UT-A3 staining in kidney and other tissues and positive UT-A1 staining only in the IMCD. Urea permeability in isolated perfused IMCDs showed basal permeability in the UT-A1+/+/UT-A3−/− mice was similar to levels in wild-type mice, but vasopressin stimulation of urea permeability in wild-type mice was significantly greater (100% increase) than in UT-A1+/+/UT-A3−/− mice (8% increase). Notably, basal urine osmolalities in both wild-type and UT-A1+/+/UT-A3−/− mice increased upon overnight water restriction. We conclude that transgenic expression of UT-A1 restores basal urea permeability to the level in wild-type mice but does not restore vasopressin-stimulated levels of urea permeability. This information suggests that transgenic expression of UT-A1 alone in mice lacking UT-A1 and UT-A3 is sufficient to restore urine-concentrating ability. PMID:26407594

Fermi Spots a Record Flare from Blazar

NASA Image and Video Library

2015-07-10

Blazar 3C 279's historic gamma-ray flare can be seen in this image from the Large Area Telescope (LAT) on NASA's Fermi satellite. Gamma rays with energies from 100 million to 100 billion electron volts (eV) are shown; for comparison, visible light has energies between 2 and 3 eV. The image spans 150 degrees, is shown in a stereographic projection, and represents an exposure from June 11 at 00:28 UT to June 17 at 08:17 UT. Read more: go.nasa.gov/1TqBAdJ Credit: NASA/DOE/Fermi LAT Collaboration NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Bipolar gas outflow from the nova V458 Vul

NASA Astrophysics Data System (ADS)

Goranskij, V. P.; Barsukova, E. A.; Fatkhullin, T. A.

2010-06-01

Classical nova V458 Vul (N Vul 2007 No.1) was detected as a supersoft X-ray source by the Swift XRT (ATel#1246, #1603). This star is interesting with its spectral class change: features of Fe II class nova completely changed by features of He/N class in the SSS phase (T.N. Tarasova, IBVS No.5807). We performed spectral observations of V458 Vul with the Russian 6-m telescope BTA and spectral camera SCORPIO on 2010 June 9.84 UT.

VizieR Online Data Catalog: GMOS spectroscopic obs. of SNR candidates in M83 (Winkler+, 2017)

NASA Astrophysics Data System (ADS)

Winkler, P. F.; Blair, W. P.; Long, K. S.

2017-11-01

We used the GMOS on the 8.2m Gemini-South telescope to obtain all the spectra reported here. Most were obtained in a classically scheduled observing run on 2011 April 7-9 (UT); masks 1-7. We later obtained spectra for two additional masks (which we refer to as masks 8 and 9 for simplicity) in a queue-scheduled program (GS-2015A-Q-90) during the 2015A semester. (6 data files).

Magnetic fields in central stars of planetary nebulae?

NASA Astrophysics Data System (ADS)

Jordan, S.; Bagnulo, S.; Werner, K.; O'Toole, S. J.

2012-06-01

Context. Most planetary nebulae have bipolar or other non-spherically symmetric shapes. Magnetic fields in the central star may be responsible for this lack of symmetry, but observational studies published to date have reported contradictory results. Aims: We search for correlations between a magnetic field and departures from the spherical geometry of the envelopes of planetary nebulae. Methods: We determine the magnetic fields from spectropolarimetric observations of ten central stars of planetary nebulae. The results of the analysis of the observations of four stars were previously presented and discussed in the literature, while the observations of six stars, plus additional measurements of a star previously observed, are presented here for the first time. Results: All our determinations of magnetic field in the central planetary nebulae are consistent with null results. Our field measurements have a typical error bar of 150-300 G. Previous spurious field detections using data acquired with FORS1 (FOcal Reducer and low dispersion Spectrograph) of the Unit Telescope 1 (UT1) of the Very Large Telescope (VLT) were probably due to the use of different wavelength calibration solutions for frames obtained at different position angles of the retarder waveplate. Conclusions: There is currently no observational evidence of magnetic fields with a strength of the order of hundreds Gauss or higher in the central stars of planetary nebulae. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, under programme ID 072.D-0089 (PI = Jordan) and 075.D-0289 (PI = Jordan).

Spectroscopic classification of SN 2018bsn as a type Ia supernova before the maximum

NASA Astrophysics Data System (ADS)

Zhang, Jujia; Ye, Kai; Xu, Zhijian; Li, Wenxiong; Wang, Xiaofeng; Mo, Jun; Tan, Hanjie; Zhang, Tianmeng

2018-05-01

We obtained an optical spectrum (range 350-890 nm) of SN 2018bsn, discovered by the Tsinghua-NAOC Transient Survey (TNTS), on UT May 17.7 2018 with the 2.4 m telescope (LJT + YFOSC) at Lijiang Observatory of Yunnan Observatories (YNAO).

Spectroscopic Classification of SN 2018bgc (=ATLAS18nvs) as a Type Ia Supernova

NASA Astrophysics Data System (ADS)

Lin, Han; Wang, Xiaofeng; Xiang, Danfeng; Rui, Liming; Hu, Lei; Hu, Maokai; Zhang, Xinhan; Li, Xue; Zhang, Tianmeng; Zhang, Jujia

2018-05-01

We obtained an optical spectrum (range 385-855 nm) of SN 2018bgc(=ATLAS18nvs), discovered by ATLAS, on UT May 08.60 2018 with the 2.16-m telescope (+BFOSC) at Xinglong Station of National Astronomical Observatories of China (NAOC).

PNV J00424253+4115139 - A Luminous Fe II-class Nova in M31

NASA Astrophysics Data System (ADS)

Neric, M.; Wilber, A.; Wagner, R. M.; Starrfield, S.; Woodward, C. E.

2015-06-01

We obtained a spectrum (range: 398-686 nm; resolution 0.3 nm) of PNV J00424253+4115139 (ATEL #7584, #7586, and #7597) on 2015 June 7.435 UT with the 2.4 m Hiltner Telescope (+OSMOS) of the MDM Observatory on Kitt Peak, Arizona.

Spectroscopic Classifications of Optical Transients with Keck I/LRIS

NASA Astrophysics Data System (ADS)

Foley, R. J.; Rojas-Bravo, C.

2018-05-01

We report the following classifications of optical transients from spectroscopic observations with LRIS on the Keck I 10-m telescope. Targets were supplied by the ASAS-SN and PSH. All observations were made on 2018 May 10 UT. Classifications were performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024).

Spectroscopic Classifications of AT2017fqf as SN Ia and AT2017fqk as SN II

NASA Astrophysics Data System (ADS)

Tartaglia, Leonardo; Valenti, Stefano; Bostroem, K. Azalee; Yang, Sheng; Hosseinzadeh, G.

2017-07-01

We report the following classifications of optical transients from spectroscopic observations with the Kast spectrograph on the Shane telescope. All observations were made on 2017 July 27 UT. Classifications were performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024).

VizieR Online Data Catalog: Deep NIR spectrum of the Orion Bar PDR (Kaplan+, 2017)

NASA Astrophysics Data System (ADS)

Kaplan, K. F.; Dinerstein, H. L.; Oh, H.; Mace, G. N.; Kim, H.; Sokal, K. R.; Pavel, M. D.; Lee, S.; Pak, S.; Park, C.; Oh, J. S.; Jaffe, D. T.

2017-11-01

The data were taken with the IGRINS on the 2.7m Harlan J. Smith Telescope at the McDonald Observatory on the night of 2014 October 24 UT; R~45000 or 7.5km/s in two separate H- and K-band channels (1.45-2.45μm). Figure 1 shows the finder chart and the IGRINS slit position and angle superposed on the Orion Bar. The center of the slit was positioned at 05:35:19.73,-05:25:26.7 (J2000). (1 data file).

Chromospheric and Coronal Structure of Polar Plumes. 1; Magnetic Structure and Radiative Energy Balance

NASA Technical Reports Server (NTRS)

Allen, Maxwell J.; Oluseyi, Hakeem M.; Walker, Arthur B. C.; Hoover, Richard B.; Barbee, Troy W., Jr.

1997-01-01

The Multi-Spectral Solar Telescope Array (MSSTA), a rocket-borne solar observatory, was successfully launched from White Sands Missile Range, New Mexico, on May 13, 1991 at 19:05 UT. The telescope systems onboard the MSSTA obtained several full disk solar images in narrow bandpasses centered around strong soft X-ray, EUV, and FUV emission lines. Each telescope was designed to be sensitive to the coronal plasmas at a particular temperature, for seven temperatures ranging from 20,000 K to 4,000,000 K. We report here on the images obtained during the initial flight of the MSSTA, and on the chromospheric and coronal structure of polar plumes observed over both poles of the Sun. We have also co-aligned the MSSTA images with Kitt Peak magnetograms taken on the same day. We are able to positively identify the magnetic structures underlying the polar plumes we analyze as unipolar. We discuss the plume observations and present a radiative energy balance model derived from them.

Spectroscopic classification of SN 2018bxs as a type Ia supernova a few days before maximum

NASA Astrophysics Data System (ADS)

Wyatt, Samuel; Andrews, Jennifer; Sand, David; Smith, Nathan

2018-06-01

On UT 2018 May 25.3 we obtained an optical spectrum (range 370-800 nm) of AT2018bxs (=ATLAS18ppz), discovered by ATLAS (Tonry et al. 2011, PASP, 123, 58) with the 2.3m Bok telescope (+ Boller & Chivens spectrograph) on Kitt Peak, Arizona.

Spectroscopic classification of AT2018aes as a supernova impostor

NASA Astrophysics Data System (ADS)

Andrews, Jennifer; Smith, Nathan; Van Dyk, Schuyler D.

2018-03-01

A visual-wavelength optical spectrum of AT2018aes obtained on UT 2018 Mar 13 (JD 2458190.84) with the Magellan Clay telescope (+ LDSS3 spectrograph, VPH-all grism) reveals a narrow H-alpha emission line with a velocity of 525 km/s, with wings extending to roughly +/-1000 km/s.

The discovery of DLT17cd/AT 2017fzw with PROMPT

NASA Astrophysics Data System (ADS)

Tartaglia, L.; Sand, D.; Wyatt, S.; Valenti, S.; Bostroem, K. A.; Reichart, D. E.; Haislip, J. B.; Kouprianov, V.

2017-08-01

We report the discovery of DLT17cd/AT 2017fzw. The object was discovered on 2017 08 09.36 UT at R 17.17 mag, during the ongoing D < 40 Mpc (DLT40) one day cadence supernova search, using data from the PROMPT 5 0.41m telescope located at CTIO.

Spectroscopic Classification of SN 2018bq (=ASASSN-18ac) as a Type Ia Supernova

NASA Astrophysics Data System (ADS)

Lin, Han; Xiang, Danfeng; Rui, Liming; Wang, Xiaofeng; Xiao, Feng; Ren, Juanjuan; Zhang, Tianmeng; Zhang, Jujia

2018-01-01

We obtained an optical spectrum (range 510-860 nm) of SN 2018bq(=ASASSN-18ac), discovered by All Sky Automated Survey for Supernova(ASAS-SN), on UT 09.81 2018 with the 2.16-m telescope (+BFOSC) at Xinglong Station of National Astronomical Observatories of China (NAOC).

Optical Photometry of the Nova Outburst TCP J04432130+4721280 (V392 Per)

NASA Astrophysics Data System (ADS)

Konyves-Toth, R.; Csak, B.; Pal, A.; Vinko, J.

2018-05-01

We obtained new photometric observations of TCP J04432130+4721280 (V392 Per, ATel #11588, #11590), R.A = 04:43:21.38, Dec = +47:21:25.9, on 2018-04-30.80 UT. The data were taken with the 60/90 cm Schmidt telescope at Konkoly Observatory, Piszkesteto, Hungary.

Medium Resolution Spectroscopy of Boyajian's Star (KIC 8462852)

NASA Astrophysics Data System (ADS)

Steele, I. A.; Lamb, G. P.; Copperwheat, C. M.; Jermak, H. E.

2017-05-01

ATel #10405 reports that a several percent dip in the brightness of KIC 8462852 is underway. We report medium resolution spectroscopy (R=2500) taken with the FRODOSpec fibre fed integral field spectrograph of the 2.0 meter Liverpool Telescope, La Palma obtained on 20th May 2017 starting at 01:20UT.

Optical Timing of X-Ray Transient MAXI J1727-203 with ULTRACAM/NTT

NASA Astrophysics Data System (ADS)

Paice, J. A.; Gandhi, P.; Dhillon, V. S.; Marsh, T. R.; Buckley, D. A. H.; Kotze, M. M.; Altamirano, D.; Charles, P. A.

2018-06-01

MAXI J1727-203 is a new X-ray transient discovered on 5th June 2018 14:29 UT by MAXI (ATel #11683), with an optical counterpart detected by GROND (Atel #11690) and confirmed by the Hiltner telescope (ATel #11691), MASTER (ATel #11692) and Swift/UVOT (ATel #11697).

A Great Moment for Astronomy

NASA Astrophysics Data System (ADS)

1998-05-01

VLT First Light Successfully Achieved The European Southern Observatory announces that First Light has been achieved with the first VLT 8.2-m Unit Telescope at the Paranal Observatory. Scientifically useful images have been obtained as scheduled, on May 25 - 26, 1998. A first analysis of these images convincingly demonstrates the exceptional potential of the ESO Very Large Telescope. Just one month after the installation and provisional adjustment of the optics, the performance of this giant telescope meets or surpasses the design goals, in particular as concerns the achievable image quality. Exposures lasting up to 10 minutes confirm that the tracking, crucial for following the diurnal rotation of the sky, is very accurate and stable. It appears that the concept developed by ESO for the construction of the VLT, namely an actively controlled, single thin mirror, yields a very superior performance. In fact, the angular resolution achieved even at this early stage is unequalled by any large ground-based telescope . The combination of large area and fine angular resolution will ultimately result in a sensitivity for point sources (e.g. stars), which is superior to any yet achieved by existing telescopes on Earth. The present series of images demonstrate these qualities and include some impressive first views with Europe's new giant telescope. After further optimization of the optical, mechanical and electronic systems, and with increasing operational streamlining, this telescope will be able to deliver unique astronomical data of the highest quality. The commissioning and science verification phases of the complex facility including instruments will last until April 1, 1999, at which time the first visiting astronomers will be received. The full significance of this achievement for astronomy will take time to assess. For Europe, this is a triumph of the collaboration between nations, institutions and industries. For the first time in almost a century, European astronomers will have at their disposal the best optical/infrared telescope in the world. We can now look forward with great expectations to the realization of many exciting research projects. The First Light Images Images of various celestial objects were obtained with the VLT CCD Test Camera, some of which are included in a new series, First Astronomical Images from the VLT UT1. None have been subjected to image processing beyond flat-fielding (to remove variations of the digital detector sensitivity over the field) and cosmetic cleaning. They all display the recorded image structure, pixel by pixel. A detailed evaluation with accompanying explanations is presented in the figure captions. 1. Omega Centauri Tracking Tests This 10-minute image demonstrates that the telescope is able to track continuously with a very high precision and thus is able to take full advantage of the frequent, very good atmospheric conditions at Paranal. The images of the stars in this southern globular cluster are very sharp (0.43 arcsec) and are perfectly round, everywhere in the field. 2. The Quadruple Clover Leaf Quasar This 2-minute exposure of the well-known Clover Leaf quasar, a quadruple gravitational lens in which the largest distance between two components is only 1.3 arcsec, was obtained during a period of excellent seeing (0.32 arcsec) measured with a seeing monitor at the top of Paranal. The recorded angular resolution of just 0.38 arcsec demonstrates near-perfect optical quality of the telescope . 3. The Central Area of Globular Cluster M4 This is a colour composite of a field near the centre of the nearest globular cluster. At a seeing of 0.53 arcsec, the blue exposure reaches magnitude B = 24 in only 2 minutes (at signal-to-noise ratio = 5) in a bright sky. A simple extrapolation shows that B ~ 28 would be reached in a 1-hour exposure in a dark sky. The large mirror surface of the VLT UT1 and its ability to produce very sharp images, ensures that faint objects may be observed extremely efficiently. 4. Fine Structure of the Butterfly Nebula This beautiful colour picture is a composite of three exposures through broad-band blue, green and red filters, lasting a total of 25 minutes. It shows the great complexity of this planetary nebula. It also demonstrates the exceptional efficiency with which features of faint surface brightness can be recorded with the VLT . Strong radiation from a dying star in a binary system at the centre impacts on the surrounding material that has been thrown out earlier from the system. 5) High-velocity Ejecta in Eta Carinae This fine picture was obtained during an exposure lasting only 10 seconds. It shows fine structures around this very active object in a detail never before achieved with any ground-based telescope . In the lower insert, a short exposure of the central Homunculus Nebula (seeing 0.38 arcsec) provides a clear view of the three-dimensional structure of this bipolar object. 6. The Dust Band in Centaurus A An amazing amount of faint details is shown in this high-resolution exposure (0.49 arcsec) of the central dust band in the nearby, southern galaxy Centaurus A, obtained through a broad-band red filter and lasting only 10 seconds. The VLT Unit Telescopes will be able to image many other galaxies in similar detail. 7. The Energetic Jet in Messier 87 The First Light took place during the night of May 25 - 26, 1998. Following a short interval of reasonable observing conditions, less optimal atmospheric conditions were encountered. The present photo, a three-colour composite (ultraviolet, blue, green) of the central region of the giant elliptical galaxy Messier 87 in the Virgo Cluster, was obtained during this night. 8. Total Optical Control The 8.2-m main and the 1.1-m secondary mirrors of the VLT Unit Telescopes are completely computer-controlled by means of an Active Optics system. In this way, the shape of the mirror can be optimized very quickly for a given observational purpose. This sequence of 9 images illustrates how the appearance of a stellar image at the focal plane is fully controllable. Fast and thorough optical adjustment ensures the best possible optical quality at all times . 9. Image Quality of the VLT This diagram demonstrates that First Light specifications have been fully met and, more impressively, that the actual VLT performance is sometimes already within the more stringent specifications that were expected to be fulfilled only three years from now. The final steps before "First Light" The final, critical testing phase commenced with the installation of the 8.2-m primary (at that time still uncoated) Zerodur mirror and 1.1-m secondary Beryllium mirror during the second half of April. The optics were then gradually brought into position during carefully planned, successive adjustments. Due to the full integration of an advanced, active control system into the VLT concept, this delicate process went amazingly fast, especially when compared to other ground-based telescopes. It included a number of short test exposures in early May, first with the Guide Camera that is used to steer the telescope. Later, some exposures were made with the Test Camera mounted just below the main mirror at the Cassegrain Focus, in a central space inside the mirror cell. It will continue to be used during the upcoming Commissioning Phase, until the first major instruments (FORS and ISAAC) are attached to the UT1, later in 1998. The 8.2-m mirror was successfully aluminized at the Paranal Mirror Coating facility on May 20 and was reattached to the telescope tube the day thereafter, cf. ESO PR Photos 13a-e/98 and ESO PR Photos 14a-i/98. Further test exposures were then made to check the proper functioning of the telescope mechanics, optics and electronics. This has lead up to the moment of First Light , i.e. the time when the telescope is considered able to produce the first, astronomically useful images. Despite an intervening spell of bad atmospheric conditions, this important event took place during the night of May 25 - 26, 1998, right on the established schedule. How to obtain ESO Press Information ESO Press Information is made available on the World-Wide Web (URL: http://www.eso.org ). ESO Press Photos may be reproduced, if credit is given to the European Southern Observatory.

EVN observations of the radio galaxy M87 following a TeV flare

NASA Astrophysics Data System (ADS)

Giroletti, M.; Giovannini, G.; Beilicke, M.; Cesarini, A.; Krawczynski, H.

2010-02-01

We report on EVN observations of the radio galaxy M87, taken at 5 GHz on 2010 Feb 10. Data were acquired by 7 radio telescopes from 21:40 UT on Feb 10 to 8:30 UT on Feb 11, directly streamed to the central data processor at JIVE, and correlated in real-time (eVLBI). This permits us to promptly report on the status of the radio jet of the source, following the increase in gamma ray emission above 100GeV reported by MAGIC (ATel #2431) The observations have an angular resolution of about 7 mas x 3 mas and rms noise of 0.12 mJy/beam.

Optical identification of IGR J18308-1232 as a Cataclysmic Variable

NASA Astrophysics Data System (ADS)

Parisi, P.; Masetti, N.; Jimenez, E.; Chavushyan, V.; Bassani, L.; Bazzano, A.; Bird, A. J.

2008-09-01

We report on a spectroscopic analysis of optical sources inside the error circle of the XMM-Newton slew source XMMLS1 J183049.6-123218 (see Ibarra et al., ATel #1527), associated with the unidentified INTEGRAL source IGR J18308-1232 (Bird et al. 2007, ApJS, 170, 175). The observations were performed on 2008 June 28, starting at 06:37 UT, with the Boller & Chivens spectrograph mounted on the 2.1m telescope of the Observatorio Astronomico Nacional (San Pedro Martir, Baja California, Mexico), for a total exposure time of 7200 s.

The Origin of the Double Main Belt Asteroid (90) Antiope by Component-Resolved Spectroscopy

NASA Astrophysics Data System (ADS)

Marchis, Franck; Enriquez, J. E.; Emery, J. P.; Berthier, J.; Descamps, P.

2009-09-01

The origin of (90) Antiope double binary asteroid remains an unsolved puzzle, despite an intensive campaign of observations conducted mostly using the VLT-UT4 telescope equipped with an adaptive Optics system (NACO) in 2007 (Descamps et al., Icarus 2007) and lightcurve data analysis by Descamps et al (Icarus, in press, 2009). These studies suggested that the two rubble pile (density ˜1.3 g/cc porosity˜50%) ellipsoidal (D˜86 km) components have similar surface characteristics and that a 68-km bowl-shaped impact crater is located on one of the components. This giant crater could be the aftermath of a tremendous collision of a 100-km sized proto-Antiope with another Themis family member. This violent shock could have produced the break-up of proto-Antiope into two equisized bodies. To test if the components come from the same parent body, we recorded individual spectra of the components using SPIFFI, a near-infrared (1.1 - 2.45 μm) integral field spectrograph fed by SINFONI, an adaptive optics module available on VLT-UT4. Using our orbital model we requested telescope time when the separation of the components of 90 Antiope was larger than 0.087” during the Feb. 2009 opposition to minimize the contamination between components. Their spectra, in J band (R-2000, S/N=70) and H+K band (R=1500, S/N=230) were recorded in Feb 01.25, Feb 03.30 and Feb 21.20 UT. The data reduction is still in progress. We could extract the H+K spectra on two epochs (Feb 01 and 21). The spectra of each component do not display any significant absorption features and their slope is in aggrement with typical C-type near-infrared spectra from De Meo et al (Icarus, 2009). They are quite similar, with typical variations by less than 5%, and imply that both bodies were formed at the same time from the same material. We acknowledge the support from NSF grant AAG-0807468.

Skylab ATM/S-056 X-ray event analyzer: Instrument description, parameter determination, and analysis example (15 June 1973 1B/M3 flare)

NASA Technical Reports Server (NTRS)

Wilson, R. M.

1976-01-01

The Skylab ATM/S-056 X-Ray Event Analyzer, part of an X-ray telescope experiment, is described. The techniques employed in the analysis of its data to determine electron temperatures and emission measures are reviewed. The analysis of a sample event - the 15 June 1973 1B/M3 flare - is performed. Comparison of the X-Ray Event Analyzer data with that of the SolRad 9 observations indicates that the X-Ray Event Analyzer accurately monitored the sun's 2.5 to 7.25 A X-ray emission and to a lesser extent the 6.1 to 20 A emission. A mean average peak temperature of 15 million K at 1,412 UT and a mean average peak electron density (assuming a flare volume of 10 to the 13 power cu km) of 27 million/cu mm at 1,416 to 1,417 UT are deduced for the event. The X-Ray Event Analyzer data, having a 2.5 s time resolution, should be invaluable in comparisons with other high-time resolution data (e.g., radio bursts).

Observations of Comet 2P/Encke During the Fall 2013 Apparition

NASA Technical Reports Server (NTRS)

Abell, Paul; Woodney, L.; Fernandez, Yanga R.; Mueller, Beatrice E.; Samarasinha, Nalin H.; Chi, Brian; Farr, Cynthia; Redinger, Haley; Schlueter, Lindsey

2013-01-01

We will present preliminary results from our observational campaign of Comet 2P/Encke during its 2013 perihelion passage. At optical wavelengths Encke is an extremely dust poor comet that has in past perihelion passages emitted a gas jet in the form a sunward fan. We expect to characterize both the morphology and lightcurve of the comet. The low optical dust means that even near perihelion the nuclear signature can be obtained in lightcurve data taken with narrowband continuum filters which cut out the gas emission. The campaign will consist of both narrowband and broadband imaging as well as infrared spectroscopy. Imaging will be obtained from 8 nights on the KPNO 2.1m between Sept. 7 and 14 UT. Additionally, the Murillo Family Observatory, a 0.5m telescope on the CSUSB campus which is equipped with both broadband filters and a narrowband Hale-Bopp set of filters will be used to observe the comet every clear night the moon allows between late August and early October to obtain extensive lightcurve data. These data will overlap both the Kitt Peak observations and the infrared spectroscopy which will be obtained with the SpeX instrument at the IRTF on four nights between September 26 UT and October 2 UT.

Supernova 2011at = PSN J09285756-1448206 in MCG -02-24-27

NASA Astrophysics Data System (ADS)

Waagen, Elizabeth O.

2011-03-01

Announces the discovery of SN 2011at = PSN J09285756-1448206 in MCG -02-24-27 by Lou Cox, Jack Newton, and Tim Puckett (Ellijay, GA, in the course of the Puckett Observatory Supernova Search) on 2011 March 10.214 UT at unfiltered CCD magnitude 14.5. Spectra obtained March 11.81 UT with the Swift satellite (+UVOT) by F. Bufano (Istituto Nazionale di Astrofisica (INAF), Osservatorio Astronomico di Catania), S. Benetti (INAF, Osservatorio Astronomico di Padova), and A. Pastorello (Queen's University, Belfast, et al.); and on March 12 UT with the F. L. Whipple Observatory 1.5-m telescope (+FAST) by M. Calkins (reported by G. H. Marion, Harvard-Smithsonian Center for Astrophysics (CfA), on behalf of the CfA Supernova Group) show SN 2011at to be a type-Ia supernova a few days before/around maximum. The object was designated PSN J09285756-1448206 when posted on the Central Bureau's Transient Objects Confirmation Page (TOCP) webpage. Initially announced in CBET 2676 (Daniel W. ! E. Green, ed.). Finder charts with sequence may be created using the AAVSO Variable Star Plotter (http://www.aavso.org/vsp). Observations should be submitted to the AAVSO International Database. See full Alert Notice for more details.

ESO-NTT Large Program spectroscopic classification of SNhunt 121

NASA Astrophysics Data System (ADS)

Benitez-Herrera, S.; Taubenberger, S.; Valenti, S.; Benetti, S.; Pastorello, A.

2012-04-01

We report, on behalf of a larger collaboration, that a spectrogram of SNhunt121 (PSN J06424255-2726498), obtained on Apr. 14.02 UT with the European Southern Observatory's New Technology Telescope (+ EFOSC2; range 365-930 nm; resolution 1.8 nm), shows it to be a peculiar type-Ic supernova. The best matches to this spectrum found by GELATO (Harutyunyan et al. 2008, A.Ap. 488, 383; available at https://gelato.tng.iac.es/login.cgi) suggest that SNhunt121 is a few weeks after maximum light.

Tests of stellar model atmospheres by optical interferometry. VLTI/VINCI limb-darkening measurements of the M4 giant ψ Phe

NASA Astrophysics Data System (ADS)

Wittkowski, M.; Aufdenberg, J. P.; Kervella, P.

2004-01-01

We present K-band interferometric measurements of the limb-darkened (LD) intensity profile of the M 4 giant star ψ Phoenicis obtained with the Very Large Telescope Interferometer (VLTI) and its commissioning instrument VINCI. High-precision squared visibility amplitudes in the second lobe of the visibility function were obtained employing two 8.2 m Unit Telescopes (UTs). This took place one month after light from UTs was first combined for interferometric fringes. In addition, we sampled the visibility function at small spatial frequencies using the 40 cm test siderostats. Our measurement constrains the diameter of the star as well as its center-to-limb intensity variation (CLV). We construct a spherical hydrostatic PHOENIX model atmosphere based on spectrophotometric data from the literature and compare its CLV prediction with our interferometric measurement. We compare as well CLV predictions by plane-parallel hydrostatic PHOENIX, ATLAS 9, and ATLAS 12 models. We find that the Rosseland angular diameter as predicted by comparison of the spherical PHOENIX model with spectrophotometry is in good agreement with our interferometric diameter measurement. The shape of our measured visibility function in the second lobe is consistent with all considered PHOENIX and ATLAS model predictions, and is significantly different to uniform disk (UD) and fully darkened disk (FDD) models. We derive high-precision fundamental parameters for ψ Phe, namely a Rosseland angular diameter of 8.13 ± 0.2 mas, with the Hipparcos parallax corresponding to a Rosseland linear radius R of 86 ± 3 R⊙, and an effective temperature of 3550 ± 50 K, with R corresponding to a luminosity of \\log L/L⊙=3.02 ± 0.06. Together with evolutionary models, these values are consistent with a mass of 1.3 ± 0.2 M⊙, and a surface gravity of \\log g = 0.68 ± 0.11. Based on public data released from the European Southern Observatory VLTI obtained from the ESO/ST-ECF Science Archive Facility. The VLTI was operated with the commissioning instrument VINCI and the MONA beam combiner.

Very Long Baseline Interferometry: Dependencies on Frequency Stability

NASA Astrophysics Data System (ADS)

Nothnagel, Axel; Nilsson, Tobias; Schuh, Harald

2018-04-01

Very Long Baseline Interferometry (VLBI) is a differential technique observing radiation of compact extra-galactic radio sources with pairs of radio telescopes. For these observations, the frequency standards at the telescopes need to have very high stability. In this article we discuss why this is, and we investigate exactly how precise the frequency standards need to be. Four areas where good clock performance is needed are considered: coherence, geodetic parameter estimation, correlator synchronization, and UT1 determination. We show that in order to ensure the highest accuracy of VLBI, stability similar to that of a hydrogen maser is needed for time-scales up to a few hours. In the article, we are considering both traditional VLBI where extra-galactic radio sources are observed, as well as observation of man-made artificial radio sources emitted by satellites or spacecrafts.

Evaluation of performance of the MACAO systems at the VLTI

NASA Astrophysics Data System (ADS)

Rengaswamy, Sridharan; Haguenauer, Pierre; Brillant, Stephane; Cortes, Angela; Girard, Julien H.; Guisard, Stephane; Paufique, Jérôme; Pino, Andres

2010-07-01

Multiple Application Curvature Adaptive Optics (MACAO) systems are used at the coudé focus of the unit telescopes (UTs) at the La-Silla Paranal Observatory, Paranal, to correct for the wave-front aberrations induced by the atmosphere. These systems are in operation since 2005 and are designed to provide beams with 10 mas residual rms tip-tilt error to the VLTI laboratory. We have initiated several technical studies such as measuring the Strehl ratio of the images recorded at the guiding camera of the VLTI, establishing the optimum setup of the MACAO to get collimated and focused beam down to the VLTI laboratory and to the instruments, and ascertaining the data generated by the real time computer, all aimed at characterizing and improving the overall performance of these systems. In this paper we report the current status of these studies.

1. OVERALL VIEW OF KIDNEY LAKE, LOOKING SOUTHWEST High ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

1. OVERALL VIEW OF KIDNEY LAKE, LOOKING SOUTHWEST - High Mountain Dams in Upalco Unit, Kidney Lake Dam, Ashley National Forest, 4.7 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

1. OVERALL VIEW OF MILK LAKE, LOOKING NORTHEAST High ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

1. OVERALL VIEW OF MILK LAKE, LOOKING NORTHEAST - High Mountain Dams in Upalco Unit, Milk Lake Dam, Ashley National Forest, 9.4 miles Northwest of Swift Creek Campground, Mountain Home, Duchesne County, UT

VizieR Online Data Catalog: WINERED CN-red band emission in comet C/2013 R1 (Shinnaka+, 2017)

NASA Astrophysics Data System (ADS)

Shinnaka, Y.; Kawakita, H.; Kondo, S.; Ikeda, Y.; Kobayashi, N.; Hamano, S.; Sameshima, H.; Fukue, K.; Matsunaga, N.; Yasui, C.; Izumi, N.; Mizumoto, M.; Otsubo, S.; Takenaka, K.; Watase, A.; Kawanishi, T.; Nakanishi, K.; Nakaoka, T.

2018-05-01

High-resolution spectroscopic observations of comet C/2013 R1 (Lovejoy; hereafter, comet Lovejoy) in the near-infrared wavelength region were performed using the WINERED spectrograph (Ikeda et al. 2016SPIE.9908E..5ZI) mounted on the Nasmyth focus of the 1.3 m Araki telescope (F/10) at Koyama Astronomical Observatory, Japan (Yoshikawa et al. 2012SPIE.8444E..6GY). We used a slit of length 47" and width 1.5". This slit width corresponds to a spectral resolving power of R=28000 (two pixels). The observations of comet Lovejoy were performed on 2013 November 30, from 19:08 UT to 21:04 UT; the total integration time was 6000 s on source. The heliocentric and geocentric distances were 0.91 au and 0.49 au, respectively, and the relative velocities of the comet to the Sun and observer were -14.5 km/s and 25.8 km/s, respectively, at the observations. We put the comet at the center of the slit during the exposures. Other calibration data (darks, flats, and comparison-lamp frames) were also acquired. (1 data file).

Spectroscopic Classification of SN 2017ixg as a young Type Ia Supernova with detached HVF of Si II 6355

NASA Astrophysics Data System (ADS)

Zhang, Jujia; Yu, Xiaoguang; Wang, Xiaofeng

2017-12-01

We obtained an optical spectrum (range 340-900 nm) of SN 2017ixg (ATLAS17nrq), discovered by ATLAS and TNTS, on UT Dec. 15.6 2017 with the Li-Jiang 2.4 m telescope (LJT + YFOSC) at Li-Jiang Observatory of Yunnan Observatories (YNAO).

Spectroscopic Classification of ASASSN-15cz and ASASSN-15da as Type Ia Supernovae

NASA Astrophysics Data System (ADS)

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

2015-02-01

We obtained optical spectroscopy (range 398-685 nm; resolution 0.3 nm) of ASASSN-15cz (ATEL #7058) and ASASSN-15da (ATEL #7061) on 2015 February 13.18 and 13.35 UT respectively using the Hiltner 2.4 m telescope (+OSMOS) of the MDM Observatory on Kitt Peak, Arizona.

Classification of ASASSN-15js and ASASSN-15kk as Normal Type Ia Supernovae

NASA Astrophysics Data System (ADS)

Porter, A.; Wilber, A.; Neric, M.; Wagner, R. M.; Starrfield, S.; Woodward, C. E.

2015-06-01

We obtained optical spectra (range: 398-686 nm; resolution 0.3 nm) of ASASSN-15js (ATEL #7548) and ASASSN-15kk (ATEL #7593) on 2015 June 7.159 and 8.206 UT respectively with the Hiltner 2.4 m Telescope (+OSMOS) of the MDM Observatory on Kitt Peak, Arizona.

Spectroscopic Classification of DLT18w/AT2018bko with SOAR

NASA Astrophysics Data System (ADS)

Pan, Y.-C.; Foley, R. J.

2018-05-01

< p > We report the classification of DLT18w/AT2018bko (ATel #11638) from spectroscopic observation performed on 2018 May 13 UT with the Goodman spectrograph on the Southern Astrophysical Research (SOAR) telescope. The spectrum appears to be blue and shows Balmer absorption lines at z=0, indicating that the transient is Galactic.

Discovery of DLT18v/AT2018beg with PROMPT and the DLT40 Survey

NASA Astrophysics Data System (ADS)

Sand, D.; Valenti, S.; Wyatt, S.; Yang, S.; Reichart, D. E.; Haislip, J. B.; Kouprianov, V.

2018-05-01

We report the discovery of DLT18v/AT 2018beg, which was first imaged by the PROMPT5 0.41m telescope located at CTIO on 2018 May 03.35 (UT) at r 17.9 mag during the ongoing D < 40 Mpc (DLT40) sub-day cadence supernova search.

Discovery of a Probable Nova in M31

NASA Astrophysics Data System (ADS)

Hornoch, K.; Kucakova, H.; Vrastil, J.

2018-04-01

We report the discovery of a probable nova in M31 on a co-added 720-s R-band CCD frame taken on 2018 Apr. 3.788 UT with the 0.65-m telescope at Ondrejov. The object designated PNV J00425509+4119009 is located at R.A. = 0h42m55s.09, Decl.

Proceedings: ecology and management of pinyon-juniper communities within the Interior West; 1997 September 15-18; Provo, UT

Treesearch

Stephen B. Monsen; Richard Stevens

1999-01-01

A symposium held September 15-18,1997, in Provo, UT, and Sanpete County, UT, provided information on the ecology, management, resource values, and restoration of pinyon-juniper communities in the Interior Western United States. The conference was hosted by the USDA Forest Service, Rocky Mountain Research Station and the Utah Division of Wildlife Resources in...

A Statistical Study of Multiply Imaged Systems in the Lensing Cluster Abell 68

NASA Astrophysics Data System (ADS)

Richard, Johan; Kneib, Jean-Paul; Jullo, Eric; Covone, Giovanni; Limousin, Marceau; Ellis, Richard; Stark, Daniel; Bundy, Kevin; Czoske, Oliver; Ebeling, Harald; Soucail, Geneviève

2007-06-01

We have carried out an extensive spectroscopic survey with the Keck and VLT telescopes, targeting lensed galaxies in the background of the massive cluster Abell 68. Spectroscopic measurements are obtained for 26 lensed images, including a distant galaxy at z=5.4. Redshifts have been determined for 5 out of 7 multiple-image systems. Through a careful modeling of the mass distribution in the strongly lensed regime, we derive a mass estimate of 5.3×1014 Msolar within 500 kpc. Our mass model is then used to constrain the redshift distribution of the remaining multiply imaged and singly imaged sources. This enables us to examine the physical properties for a subsample of 7 Lyα emitters at 1.7<~z<~5.5, whose unlensed luminosities of ~=1041 ergs s-1 are fainter than similar objects found in blank fields. Of particular interest is an extended Lyα emission region surrounding a highly magnified source at z=2.6, detected in VIMOS integral field spectroscopy data. The physical scale of the most distant lensed source at z=5.4 is very small (<300 pc), similar to the lensed z~5.6 emitter reported by Ellis et al. in Abell 2218. New photometric data available for Abell 2218 allow for a direct comparison between these two unique objects. Our survey illustrates the practicality of using lensing clusters to probe the faint end of the z~2-5 Lyα luminosity function in a manner that is complementary to blank-field narrowband surveys. Data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Also based on observations collected at the Very Large Telescope (Antu/UT1 and Melipal/UT3), European Southern Observatory, Paranal, Chile (ESO programs 070.A-0643 and 073.A-0774), the NASA/ESA Hubble Space Telescope (program 8249) obtained at the Space Telescope Science Institute, which is operated by AURA under NASA contract NAS5-26555, and the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii.

1. OVERALL VIEW OF BROWN DUCK LAKE, LOOKING SOUTHWEST ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

1. OVERALL VIEW OF BROWN DUCK LAKE, LOOKING SOUTHWEST - High Mountain Dams in Upalco Unit, Brown Duck Lake Dam, Ashley National Forest, 4.4 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

Optimized scheduling of VLBI UT1 intensive sessions for twin telescopes employing impact factor analysis

NASA Astrophysics Data System (ADS)

Leek, Judith; Artz, Thomas; Nothnagel, Axel

2015-09-01

Daily Very Long Baseline Interferometry (VLBI) intensive measurements make an important contribution to the regular monitoring of Earth rotation variations. Since these variations are quite rapid, their knowledge is important for navigation with global navigation satellite system and for investigations in Earth sciences. Unfortunately, the precision of VLBI intensive observations is 2-3 times worse than the precision of regular 24h-VLBI measurements with networks of 5-10 radio telescopes. The major advancement of research in this paper is the improvement of VLBI intensive results by (a) using twin telescopes instead of single telescopes and (b) applying an entirely new scheduling concept for the individual observations. Preparatory investigations of standardintensive sessions suggest that the impact factors of the observations are well suited for the identification of the most influential observations which are needed for the determination of certain parameters within the entire design of a VLBI session. Based on this experience, the scheduling method is designed for optimizing the observations' geometry for a given network of radio telescopes and a predefined set of parameters to be estimated. The configuration of at least two twin telescopes, or one twin and two single telescopes, offers the possibility of building pairwise sub-nets that observe two different sources simultaneously. In addition to an optimized observing plan, a special parametrization for twin telescopes leads to an improved determination of Earth rotation variations, as it is shown by simulated observations. In general, an improvement of about 50 % in the formal errors can be realized using twin radio telescopes. This result is only due to geometric improvements as higher slew rates of the twin telescopes are not taken into account.

Ultrasonic Phased Array Assessment of the Interference Fit and Leak Path of the North Anna Unit 2 Control Rod Drive Mechanism Nozzle 63 with Destructive Validation

DOE Office of Scientific and Technical Information (OSTI.GOV)

Crawford, Susan L.; Cinson, Anthony D.; MacFarlan, Paul J.

2012-08-01

The objective of this investigation was to evaluate the efficacy of ultrasonic testing (UT) for primary water leak path assessments of reactor pressure vessel (RPV) upper head penetrations. Operating reactors have experienced leakage when stress corrosion cracking of nickel-based alloy penetrations allowed primary water into the annulus of the interference fit between the penetration and the low-alloy steel RPV head. In this investigation, UT leak path data were acquired for an Alloy 600 control rod drive mechanism nozzle penetration, referred to as Nozzle 63, which was removed from the North Anna Unit 2 reactor when the RPV head was replacedmore » in 2002. In-service inspection prior to the head replacement indicated that Nozzle 63 had a probable leakage path through the interference fit region. Nozzle 63 was examined using a phased-array UT probe with a 5.0-MHz, eight-element annular array. Immersion data were acquired from the nozzle inner diameter surface. The UT data were interpreted by comparing to responses measured on a mockup penetration with known features. Following acquisition of the UT data, Nozzle 63 was destructively examined to determine if the features identified in the UT examination, including leakage paths and crystalline boric acid deposits, could be visually confirmed. Additional measurements of boric acid deposit thickness and low-alloy steel wastage were made to assess how these factors affect the UT response. The implications of these findings for interpreting UT leak path data are described.« less

Kinematic optimization of upgrade to the Hobby-Eberly Telescope through novel use of commercially available three-dimensional CAD package

NASA Astrophysics Data System (ADS)

Wedeking, Gregory A.; Zierer, Joseph J.; Jackson, John R.

2010-07-01

The University of Texas, Center for Electromechanics (UT-CEM) is making a major upgrade to the robotic tracking system on the Hobby Eberly Telescope (HET) as part of theWide Field Upgrade (WFU). The upgrade focuses on a seven-fold increase in payload and necessitated a complete redesign of all tracker supporting structure and motion control systems, including the tracker bridge, ten drive systems, carriage frames, a hexapod, and many other subsystems. The cost and sensitivity of the scientific payload, coupled with the tracker system mass increase, necessitated major upgrades to personnel and hardware safety systems. To optimize kinematic design of the entire tracker, UT-CEM developed novel uses of constraints and drivers to interface with a commercially available CAD package (SolidWorks). For example, to optimize volume usage and minimize obscuration, the CAD software was exercised to accurately determine tracker/hexapod operational space needed to meet science requirements. To verify hexapod controller models, actuator travel requirements were graphically measured and compared to well defined equations of motion for Stewart platforms. To ensure critical hardware safety during various failure modes, UT-CEM engineers developed Visual Basic drivers to interface with the CAD software and quickly tabulate distance measurements between critical pieces of optical hardware and adjacent components for thousands of possible hexapod configurations. These advances and techniques, applicable to any challenging robotic system design, are documented and describe new ways to use commercially available software tools to more clearly define hardware requirements and help insure safe operation.

Forskolin stimulation promotes urea transporter UT-A1 ubiquitination, endocytosis, and degradation in MDCK cells

PubMed Central

Su, Hua; Carter, Conner B.; Laur, Oskar; Sands, Jeff M.

2012-01-01

The adenylyl cyclase stimulator forskolin (FSK) stimulates UT-A1 phosphorylation, membrane trafficking, and urea transport activity. Here, we found that FSK stimulation induces UT-A1 ubiquitination in UT-A1 Madin-Darby canine kidney (MDCK) cells. This suggests that phosphorylation by FSK also triggers the protein degradation machinery for UT-A1. UT-A1-MDCK cells were treated with 100 μg/ml cycloheximide to inhibit protein synthesis, with or without 10 μM FSK. Total UT-A1 protein abundance was significantly reduced after FSK treatment, concomitantly ubiquitinated UT-A1 was increased. We then specifically investigated the effect of FSK on UT-A1 expressed on the cell plasma membrane. FSK treatment accelerated UT-A1 removal from the cell plasma membrane by increasing UT-A1 endocytosis as judged by biotinylation/MesNa treatment and confocal microscopy. We further found that inhibition of the clathrin-mediated endocytic pathway, but not the caveolin-mediated endocytic pathway, significantly blocks FSK-stimulated UT-A1 endocytosis. The PKA inhibitor H89 and the proteasome inhibitors MG132 and lactacystin reduced FSK-induced membrane UT-A1 reduction. Our study shows that FSK activates the UT-A1 urea transporter and the activation/phosphorylation subsequently triggers the downregulation of UT-A1, which represents an important mechanism for the cell to return to the basal conditions after vasopressin stimulation. PMID:22914781

Genes and proteins of urea transporters.

PubMed

Sands, Jeff M; Blount, Mitsi A

2014-01-01

A urea transporter protein in the kidney was first proposed in 1987. The first urea transporter cDNA was cloned in 1993. The SLC14a urea transporter family contains two major subgroups: SLC14a1, the UT-B urea transporter originally isolated from erythrocytes; and SLC14a2, the UT-A group originally isolated from kidney inner medulla. Slc14a1, the human UT-B gene, arises from a single locus located on chromosome 18q12.1-q21.1, which is located close to Slc14a2. Slc14a1 includes 11 exons, with the coding region extending from exon 4 to exon 11, and is approximately 30 kb in length. The Slc14a2 gene is a very large gene with 24 exons, is approximately 300 kb in length, and encodes 6 different isoforms. Slc14a2 contains two promoter elements: promoter I is located in the typical position, upstream of exon 1, and drives the transcription of UT-A1, UT-A1b, UT-A3, UT-A3b, and UT-A4; while promoter II is located within intron 12 and drives the transcription of UT-A2 and UT-A2b. UT-A1 and UT-A3 are located in the inner medullary collecting duct, UT-A2 in the thin descending limb and liver, UT-A5 in testis, UT-A6 in colon, UT-B1 primarily in descending vasa recta and erythrocytes, and UT-B2 in rumen.

Earth Glint Observations Conducted During the Deep Impact Spacecraft Flyby

NASA Technical Reports Server (NTRS)

Barry, R. K.; Deming, L. D.; Robinson, T.; Hewagama, T.

2010-01-01

We describe observations of Earth conducted using the High Resolution Instrument (HRI) - a 0.3 m f/35 telescope - on the Deep Impact (DI) spacecraft during its recent flybys. Earth was observed on five occasions: 2008-Mar-18 18:18 UT, 2008-May-28 20:05 UT, 2008-Jun-4 16:57 UT, 2009-Mar-27 16:19 and 2009-Oct-4 09:37 UT. Each set of observations was conducted over a full 24-hour rotation of Earth and a total of thirteen NIR spectra were taken on two-hour intervals during each observing period. Photometry in the 450, SSO, 650 and 8S0 nm filters was taken every fifteen minutes and every hour for the 350, 750 and 950 nm filters. The spacecraft was located over the equator for the three sets of observations in 2008, while the 2009- Mar and 2009-Oct were taken over the north and south Polar Regions, respectively. Observations of calibrator stars Canopus and Achernar were conducted on multiple occasions through all filters. The observations detected a strong specular glint not necessarily associated with a body of water. We describe spectroscopic characterization of the glint and evidence for the possibility of detection of reflection from high cirrus clouds. We describe implications for observations of extrasolar planets.

The Mysterious Transient ROTSE3 J115649.1+542726 is an Extremely Luminous Type II SN at z = 0.21

NASA Astrophysics Data System (ADS)

Chornock, R.; Miller, A. A.; Perley, D. A.; Bloom, J. S.

2008-08-01

We report on further spectroscopic observations of the transient ROTSE3 J115649.1+542726 discovered by Yuan et al. (ATEL #1515) and followed up by several groups (ATEL #1524, ATEL #1576, ATEL #1578, and ATEL #1593). We observed the object for 840 s using the Low-Resolution Imaging Spectrometer (LRIS; Oke et al. 1995) on the Keck I 10-m telescope on 2008 Aug 3.25 UT. Our initial observations of this object (ATEL #1576) showed a blue and largely featureless spectrum, but at later epochs several unidentified weak spectral features appeared (ATEL #1576 and ATEL #1593).

Spectroscopic classification of AT 2017ixr as a nova in M31

NASA Astrophysics Data System (ADS)

Williams, S. C.; Darnley, M. J.; Carey, G.

2018-01-01

We obtained spectra of the transient AT 2017ixr (see TNS) with the SPRAT spectrograph (resolution R 350; Piascik et al. 2014) on the 2-m Liverpool Telescope (LT; Steele et al. 2004) on 2017 Dec 27.90 and 2018 Jan 12.83 UT. The first spectrum (2017 Dec 27) shows narrow H & alpha; emission on a blue continuum.

Spectroscopic classification of TCP J00333837+4836022 as a nova in NGC 147

NASA Astrophysics Data System (ADS)

Williams, S. C.; Darnley, M. J.

2017-12-01

We obtained a spectrum of the transient TCP J00333837+4836022 (see CBAT TOCP) with the SPRAT spectrograph (resolution R 350; Piascik et al. 2014) on the 2-m Liverpool Telescope (Steele et al. 2004) on 2017 Dec 24.82 UT. The only emission clearly present is H & alpha;, which displays a P-Cygni profile.

Spectroscopic classification of PTSS-18fdb (AT 2018cni) as a peculiar type Ia supernova before maximum

NASA Astrophysics Data System (ADS)

Zhang, Jujia; Tan, Hanjie; Li, Wenxiong; Li, Bin; Li, Zhitong; Wang, Xiaofeng; Xu, Zhijian; Zhao, Haibin; Wang, Lifan

2018-06-01

We obtained an optical spectrum (range 350-890 nm) of PTSS-18fdb (AT 2018cni), discovered by the PMO-Tsinghua Supernova Survey (PTSS, http://www.cneost.org/ptss/), on UT 2018 June 17.7 with the Li-Jiang 2.4 m telescope (LJT+YFOSC) at Li-Jiang Observatory of Yunnan Observatories.

Spectroscopic classification of PTSS-18ecg (SN 2018bhb) as a type Ia supernova around maximum

NASA Astrophysics Data System (ADS)

Zhang, Jujia; Ding, Xu; Wang, Xiaofeng; Li, Wenxiong; Li, Bin; Xu, Zhijian; Tan, Hanjie; Zhao, Haibin; Wang, Lifan; Li, Zhitong

2018-05-01

We obtained an optical spectrum (range 350-890 nm) of PTSS-18ecg (SN 2018bhb), discovered by the PMO-Tsinghua Supernova Survey (PTSS, http://www.cneost.org/ptss/), on UT 2018 May 10.7 with the Li-Jiang 2.4 m telescope (LJT+YFOSC) at Li-Jiang Observatory of Yunnan Observatories.

Urea Transport and Clinical Potential of Urearetics

PubMed Central

Klein, Janet D.; Sands, Jeff M.

2016-01-01

Purpose of review Urea is transported by urea transporter proteins in kidney, erythrocytes, and other tissues. Mice in which different urea transporters have been knocked-out have urine concentrating defects, which has led to the development and testing of UT-A and UT-B inhibitors as urearetics. This review summarizes the knowledge gained during the past year on urea transporter regulation and investigations into the clinical potential of urearetics. Recent findings UT-A1 undergoes several post-translational modifications that increase its function by increasing UT-A1 accumulation in the apical plasma membrane. UT-A1 is phosphorylated by PKA, Epac, PKCα, and AMPK, all at different serine residues. UT-A1 is also regulated by 14-3-3, which contributes to UT-A1 removal from the membrane. UT-A1 is glycosylated with various glycan moieties in animal models of diabetes mellitus. Transgenic expression of UT-A1 into UT-A1/UT-A3 knock-out mice restores urine concentrating ability. UT-B is present in descending vasa recta and urinary bladder, and is linked to bladder cancer. Inhibitors of UT-A and UT-B have been developed that result in diuresis with fewer abnormalities in serum electrolytes than conventional diuretics. Summary Urea transporters play critical roles in the urine concentrating mechanism. Urea transport inhibitors are a promising new class of diuretic agents. PMID:27367911

3. OVERALL VIEW OF TWIN POTS RESERVOIR, LOOKING SOUTHEAST ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

3. OVERALL VIEW OF TWIN POTS RESERVOIR, LOOKING SOUTHEAST - High Mountain Dams in Upalco Unit, Twin Pots Dam, Ashley National Forest, 10.1 miles North of Mountain Home, Mountain Home, Duchesne County, UT

Urea transport and clinical potential of urearetics.

PubMed

Klein, Janet D; Sands, Jeff M

2016-09-01

Urea is transported by urea transporter proteins in kidney, erythrocytes, and other tissues. Mice in which different urea transporters have been knocked out have urine-concentrating defects, which has led to the development and testing of urea transporters Slc14A2 (UT-A) and Slc14A1 (UT-B) inhibitors as urearetics. This review summarizes the knowledge gained during the past year on urea transporter regulation and investigations into the clinical potential of urearetics. UT-A1 undergoes several posttranslational modifications that increase its function by increasing UT-A1 accumulation in the apical plasma membrane. UT-A1 is phosphorylated by protein kinase A, exchange protein activated by cyclic AMP, protein kinase Cα, and AMP-activated protein kinase, all at different serine residues. UT-A1 is also regulated by 14-3-3, which contributes to UT-A1 removal from the membrane. UT-A1 is glycosylated with various glycan moieties in animal models of diabetes mellitus. Transgenic expression of UT-A1 into UT-A1/UT-A3 knockout mice restores urine-concentrating ability. UT-B is present in descending vasa recta and urinary bladder, and is linked to bladder cancer. Inhibitors of UT-A and UT-B have been developed that result in diuresis with fewer abnormalities in serum electrolytes than conventional diuretics. Urea transporters play critical roles in the urine-concentrating mechanism. Urea transport inhibitors are a promising new class of diuretic agent.

Rocket FUV Observations of the Io Plasma Torus During the Shoemaker-Levy/9 Impacts

NASA Technical Reports Server (NTRS)

Stern, S. A.; Slater, D.; Cash, W.; Wilkinson, E.; Green, J.; Gladstone, R.

1995-01-01

We observed the Io torus from 820-1140 A on universal time (UT) 20.25 July 1994 from a sounding rocket telescope/spectrograph. These observations serve as only the fourth published spectrum of the torus in this wavelength range, and the only far ultraviolet (FUV) data documenting the state of the torus during the Shoemaker Levy 9 Impacts.

MASTER Optical Flare Detection from the Fastes Accretor in Our Galaxy - IGR J00291+5934.

NASA Astrophysics Data System (ADS)

Lipunov, V.; Rebolo, R.; Serra-Ricart, M.; Lodieu, N.; Israelian, G.; Lipunov, V.; Gorbovskoy, E.; Kornilov, V.; Balanutsa, P.; Tiurina, N.; Kuznetsov, A.; Chazov, V.; Vlasenko, D.; Gorbunov, I.; Buckley, D.; Potter, S.; Kotze, M.; Gress, O.; Budnev, N. M.; Ivanov, K.; Tlatov, A.; Dormidontov, D.; Senik, V.; Parhomenko, A. V.; Krushinski, V.; Zalozhnykh, I.; Sergienko, Yu.; Gabovich, A.; Yurkov, V.

2015-07-01

MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru, Lipunov et al., Advances in Astronomy, MASTER Global Robotic Net, 2010) located in IAC was pointed to the Swift IGR J00291+5934 (Cummings et al., GCN 18051) 24 sec after notice time and 1103 sec after trigger time at 2015-07-24 05:42:03 UT.

Elevated utero/placental GR/NR3C1 is not required for the induction of parturition in the dog.

PubMed

Gram, Aykut; Trachsel, Alexandra; Boos, Alois; Kowalewski, Mariusz P

2016-10-01

The endocrine mechanisms that lead to initiation of parturition in dogs are still not fully understood. The prepartum luteolysis is associated with increased prostaglandin (PG) F2α secretion; however, there is no pregnancy- or parturition-related increase in estrogens. Moreover, unlike in other mammalian species, in the dog, increased peripartum levels of cortisol measured sporadically in maternal peripheral blood are not mandatory for normal parturition. Nevertheless, auto/paracrine effects of cortisol at the placental feto-maternal level cannot be excluded. Therefore, the aim of this study was to investigate the expression and localization of glucocorticoid receptor (GR/NR3C1) in canine utero/placental (Ut/Pl) units and uterine interplacental sites at selected time points during pregnancy (pre-implantation, post-implantation and mid-gestation), and at normal and antigestagen-induced parturition. The Ut/Pl expression of GR/NR3C1 did not change significantly from pre-implantation until mid-gestation; however, it was strongly induced during the prepartum luteolysis. Within the interplacental samples, expression of GR/NR3C1-mRNA was greater post-implantation than pre-implantation and did not change afterward, i.e. toward mid-gestation. Compartmentalization studies within the Ut/Pl units, involving placenta, endometrium and myometrium separately, performed at the prepartum luteolysis revealed the highest GR/NR3C1-mRNA levels in placenta compared with endometrium and myometrium. Interestingly, in antigestagen-treated mid-pregnancy dogs, Ut/Pl and interplacental GR/NR3C1-mRNA expression remained unaffected. At the cellular level, placental GR/NR3C1 was clearly detectable in placenta fetalis, i.e. in trophoblast cells. In conclusion, increased expression of GR/NR3C1 during normal parturition, but not following antigestagen-treatment, suggest that it is not required for initiating the signaling cascade of PG synthesis leading to the induction of parturition in the dog. © 2016 Society for Reproduction and Fertility.

6. VIEW OF OUTLET GATE WHEEL AND STEM, LOOKING NORTHWEST ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

6. VIEW OF OUTLET GATE WHEEL AND STEM, LOOKING NORTHWEST - High Mountain Dams in Upalco Unit, Twin Pots Dam, Ashley National Forest, 10.1 miles North of Mountain Home, Mountain Home, Duchesne County, UT

9. VIEW OF LATERAL GATE ON CANAL NEAR DAM, LOOKING ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

9. VIEW OF LATERAL GATE ON CANAL NEAR DAM, LOOKING SOUTHEAST - High Mountain Dams in Upalco Unit, Twin Pots Dam, Ashley National Forest, 10.1 miles North of Mountain Home, Mountain Home, Duchesne County, UT

The 26 December 2001 Solar Event Responsible for GLE63. I. Observations of a Major Long-Duration Flare with the Siberian Solar Radio Telescope

NASA Astrophysics Data System (ADS)

Grechnev, V. V.; Kochanov, A. A.

2016-12-01

Ground level enhancements (GLEs) of cosmic-ray intensity occur, on average, once a year. Because they are rare, studying the solar sources of GLEs is especially important to approach understanding their origin. The SOL2001-12-26 eruptive-flare event responsible for GLE63 seems to be challenging in some aspects. Deficient observations limited our understanding of it. Analysis of additional observations found for this event provided new results that shed light on the flare configuration and evolution. This article addresses the observations of this flare with the Siberian Solar Radio Telescope (SSRT). Taking advantage of its instrumental characteristics, we analyze the detailed SSRT observations of a major long-duration flare at 5.7 GHz without cleaning the images. The analysis confirms that the source of GLE63 was associated with an event in active region 9742 that comprised two flares. The first flare (04:30 - 05:03 UT) reached a GOES importance of about M1.6. Two microwave sources were observed, whose brightness temperatures at 5.7 GHz exceeded 10 MK. The main flare, up to an importance of M7.1, started at 05:04 UT and occurred in strong magnetic fields. The observed microwave sources reached a brightness temperature of about 250 MK. They were not static. After appearing on the weaker-field periphery of the active region, the microwave sources moved toward each other nearly along the magnetic neutral line, approaching the stronger-field core of the active region, and then moved away from the neutral line like expanding ribbons. These motions rule out an association of the non-thermal microwave sources with a single flaring loop.

Analysis of Mount St. Helens ash from optical photoelectric photometry

NASA Technical Reports Server (NTRS)

Cardelli, J. A.; Ackerman, T. P.

1983-01-01

The optical properties of suspended dust particles from the eruption of Mt. St. Helens on July 23, 1980 are investigated using photoelectric observations of standard stars obtained on the 0.76-m telescope at the University of Washington 48 hours after the eruption. Measurements were made with five broad-band filters centered at 3910, 5085, 5480, 6330, and 8050 A on stars of varying color and over a wide range of air masses. Anomalous extinction effects due to the volcanic ash were detected, and a significant change in the wavelength-dependent extinction parameter during the course of the observations was established by statistical analysis. Mean particle size (a) and column density (N) are estimated using the Mie theory, assuming a log-normal particle-size distribution: a = 0.18 micron throughout; N = 1.02 x 10 to the 9th/sq cm before 7:00 UT and 2.33 x 10 to the 9th/sq cm after 8:30 UT on July 25, 1980. The extinction is attributed to low-level, slowly migrating ash, possibly combined with products of gas-to-particle conversion and coagulation.

VizieR Online Data Catalog: WASP-31b:HST/Spitzer transmission spectral survey (Sing+, 2015)

NASA Astrophysics Data System (ADS)

Sing, D. K.; Wakeford, H. R.; Showman, A. P.; Nikolov, N.; Fortney, J. J.; Burrows, A. S.; Ballester, G. E.; Deming, D.; Aigrain, S.; Desert, J.-M.; Gibson, N. P.; Henry, G. W.; Knutson, H.; Lecavelier Des Etangs, A.; Pont, F.; Vidal-Madjar, A.; Williamson, M. W.; Wilson, P. A.

2017-11-01

We observed two transits of WASP-31b with the HST STIS G430L grating during 2012 June 13 and 26, as well as one transit with the STIS G750L during 2012 July 10. In addition to the STIS data, observations of WASP-31b were also conducted in the infrared with WFC3 on the HST. Observations began on 2012 May 13 at 12:53 using the IR G141 grism in forward spatial scan mode over five HST orbits. We analyse two transit observations obtained using the Infrared Array Camera (IRAC) instrument (Programme 90092 with P.I. Desert) on the Spitzer space telescope in the 3.6 μm and 4.5 μm channels in subarray mode (32x32 pixel, or 39 centred on the planets host). The 3.6 μm observation was performed on UT 2013 March 9 (between 06:59 and 11:37) and the 4.5 observation was performed on UT 2013 March 19 (between 12:19 and 16:58). (1 data file).

Fourth Light at Paranal!

NASA Astrophysics Data System (ADS)

2000-09-01

VLT YEPUN Joins ANTU, KUEYEN and MELIPAL It was a historical moment last night (September 3 - 4, 2000) in the VLT Control Room at the Paranal Observatory , after nearly 15 years of hard work. Finally, four teams of astronomers and engineers were sitting at the terminals - and each team with access to an 8.2-m telescope! From now on, the powerful "Paranal Quartet" will be observing night after night, with a combined mirror surface of more than 210 m 2. And beginning next year, some of them will be linked to form part of the unique VLT Interferometer with unparalleled sensitivity and image sharpness. YEPUN "First Light" Early in the evening, the fourth 8.2-m Unit Telescope, YEPUN , was pointed to the sky for the first time and successfully achieved "First Light". Following a few technical exposures, a series of "first light" photos was made of several astronomical objects with the VLT Test Camera. This instrument was also used for the three previous "First Light" events for ANTU ( May 1998 ), KUEYEN ( March 1999 ) and MELIPAL ( January 2000 ). These images served to evaluate provisionally the performance of the new telescope, mainly in terms of mechanical and optical quality. The ESO staff were very pleased with the results and pronounced YEPUN fit for the subsequent commissioning phase. When the name YEPUN was first given to the fourth VLT Unit Telescope, it was supposed to mean "Sirius" in the Mapuche language. However, doubts have since arisen about this translation and a detailed investigation now indicates that the correct meaning is "Venus" (as the Evening Star). For a detailed explanation, please consult the essay On the Meaning of "YEPUN" , now available at the ESO website. The first images At 21:39 hrs local time (01:39 UT), YEPUN was turned to point in the direction of a dense Milky Way field, near the border between the constellations Sagitta (The Arrow) and Aquila (The Eagle). A guide star was acquired and the active optics system quickly optimized the mirror system. At 21:44 hrs (01:44 UT), the Test Camera at the Cassegrain focus within the M1 mirror cell was opened for 30 seconds, with the planetary nebula Hen 2-428 in the field. The resulting "First Light" image was immediately read out and appeared on the computer screen at 21:45:53 hrs (01:45:53 UT). "Not bad! - "Very nice!" were the first, "business-as-usual"-like comments in the room. The zenith distance during this observation was 44° and the image quality was measured as 0.9 arcsec, exactly the same as that registered by the Seeing Monitoring Telescope outside the telescope building. There was some wind. ESO PR Photo 22a/00 ESO PR Photo 22a/00 [Preview - JPEG: 374 x 400 pix - 128k] [Normal - JPEG: 978 x 1046 pix - 728k] Caption : ESO PR Photo 22a/00 shows a colour composite of some of the first astronomical exposures obtained by YEPUN . The object is the planetary nebula Hen 2-428 that is located at a distance of 6,000-8,000 light-years and seen in a dense sky field, only 2° from the main plane of the Milky Way. As other planetary nebulae, it is caused by a dying star (the bluish object at the centre) that shreds its outer layers. The image is based on exposures through three optical filtres: B(lue) (10 min exposure, seeing 0.9 arcsec; here rendered as blue), V(isual) (5 min; 0.9 arcsec; green) and R(ed) (3 min; 0.9 arcsec; red). The field measures 88 x 78 arcsec 2 (1 pixel = 0.09 arcsec). North is to the lower right and East is to the lower left. The 5-day old Moon was about 90° away in the sky that was accordingly bright. The zenith angle was 44°. The ESO staff then proceeded to take a series of three photos with longer exposures through three different optical filtres. They have been combined to produce the image shown in ESO PR Photo 22a/00 . More astronomical images were obtained in sequence, first of the dwarf galaxy NGC 6822 in the Local Group (see PR Photo 22f/00 below) and then of the spiral galaxy NGC 7793 . All 8.2-m telescopes now in operation at Paranal The ESO Director General, Catherine Cesarsky , who was present on Paranal during this event, congratulated the ESO staff to the great achievement, herewith bringing a major phase of the VLT project to a successful end. She was particularly impressed by the excellent optical quality that was achieved at this early moment of the commissioning tests. A measurement showed that already now, 80% of the light is concentrated within 0.22 arcsec. The manager of the VLT project, Massimo Tarenghi , was very happy to reach this crucial project milestone, after nearly fifteen years of hard work. He also remarked that with the M2 mirror already now "in the active optics loop", the telescope was correctly compensating for the somewhat mediocre atmospheric conditions on this night. The next major step will be the "first light" for the VLT Interferometer (VLTI) , when the light from two Unit Telescopes is combined. This event is expected in the middle of next year. Impressions from the YEPUN "First Light" event First Light for YEPUN - ESO PR VC 06/00 ESO PR Video Clip 06/00 "First Light for YEPUN" (5650 frames/3:46 min) [MPEG Video+Audio; 160x120 pix; 7.7Mb] [MPEG Video+Audio; 320x240 pix; 25.7 Mb] [RealMedia; streaming; 34kps] [RealMedia; streaming; 200kps] ESO Video Clip 06/00 shows sequences from the Control Room at the Paranal Observatory, recorded with a fixed TV-camera in the evening of September 3 at about 23:00 hrs local time (03:00 UT), i.e., soon after the moment of "First Light" for YEPUN . The video sequences were transmitted via ESO's dedicated satellite communication link to the Headquarters in Garching for production of the clip. It begins at the moment a guide star is acquired to perform an automatic "active optics" correction of the mirrors; the associated explanation is given by Massimo Tarenghi (VLT Project Manager). The first astronomical observation is performed and the first image of the planetary nebula Hen 2-428 is discussed by the ESO Director General, Catherine Cesarsky . The next image, of the nearby dwarf galaxy NGC 6822 , arrives and is shown and commented on by the ESO Director General. Finally, Massimo Tarenghi talks about the next major step of the VLT Project. The combination of the lightbeams from two 8.2-m Unit Telescopes, planned for the summer of 2001, will mark the beginning of the VLT Interferometer. ESO Press Photo 22b/00 ESO Press Photo 22b/00 [Preview; JPEG: 400 x 300; 88k] [Full size; JPEG: 1600 x 1200; 408k] The enclosure for the fourth VLT 8.2-m Unit Telescope, YEPUN , photographed at sunset on September 3, 2000, immediately before "First Light" was successfully achieved. The upper part of the mostly subterranean Interferometric Laboratory for the VLTI is seen in front. (Digital Photo). ESO Press Photo 22c/00 ESO Press Photo 22c/00 [Preview; JPEG: 400 x 300; 112k] [Full size; JPEG: 1280 x 960; 184k] The initial tuning of the YEPUN optical system took place in the early evening of September 3, 2000, from the "observing hut" on the floor of the telescope enclosure. From left to right: Krister Wirenstrand who is responsible for the VLT Control Software, Jason Spyromilio - Head of the Commissioning Team, and Massimo Tarenghi , VLT Manager. (Digital Photo). ESO Press Photo 22d/00 ESO Press Photo 22d/00 [Preview; JPEG: 400 x 300; 112k] [Full size; JPEG: 1280 x 960; 184k] "Mission Accomplished" - The ESO Director General, Catherine Cesarsky , and the Paranal Director, Roberto Gilmozzi , face the VLT Manager, Massimo Tarenghi at the YEPUN Control Station, right after successful "First Light" for this telescope. (Digital Photo). An aerial image of YEPUN in its enclosure is available as ESO PR Photo 43a/99. The mechanical structure of YEPUN was first pre-assembled at the Ansaldo factory in Milan (Italy) where it served for tests while the other telescopes were erected at Paranal. An early photo ( ESO PR Photo 37/95 ) is available that was obtained during the visit of the ESO Council to Milan in December 1995, cf. ESO PR 18/95. Paranal at sunset ESO Press Photo 22e/00 ESO Press Photo 22e/00 [Preview; JPEG: 400 x 200; 14kb] [Normal; JPEG: 800 x 400; 84kb] [High-Res; JPEG: 4000 x 2000; 4.0Mb] Wide-angle view of the Paranal Observatory at sunset. The last rays of the sun illuminate the telescope enclosures at the top of the mountain and some of the buildings at the Base Camp. The new "residencia" that will provide living space for the Paranal staff and visitors from next year is being constructed to the left. The "First Light" observations with YEPUN began soon after sunset. This photo was obtained in March 2000. Additional photos (September 6, 2000) ESO PR Photo 22f/00 ESO PR Photo 22f/00 [Preview - JPEG: 400 x 487 pix - 224k] [Normal - JPEG: 992 x 1208 pix - 1.3Mb] Caption : ESO PR Photo 22f/00 shows a colour composite of three exposures of a field in the dwarf galaxy NGC 6822 , a member of the Local Group of Galaxies at a distance of about 2 million light-years. They were obtained by YEPUN and the VLT Test Camera at about 23:00 hrs local time on September 3 (03:00 UT on September 4), 2000. The image is based on exposures through three optical filtres: B(lue) (10 min exposure; here rendered as blue), V(isual) (5 min; green) and R(ed) (5 min; red); the seeing was 0.9 - 1.0 arcsec. Individual stars of many different colours (temperatures) are seen. The field measures about 1.5 x 1.5 arcmin 2. Another image of this galaxy was obtained earlier with ANTU and FORS1 , cf. PR Photo 10b/99. ESO Press Photo 22g/00 ESO Press Photo 22g/00 [Preview; JPEG: 400 x 300; 136k] [Full size; JPEG: 1280 x 960; 224k] Most of the crew that put together YEPUN is here photographed after the installation of the M1 mirror cell at the bottom of the mechanical structure (on July 30, 2000). Back row (left to right): Erich Bugueno (Mechanical Supervisor), Erito Flores (Maintenance Technician); front row (left to right) Peter Gray (Mechanical Engineer), German Ehrenfeld (Mechanical Engineer), Mario Tapia (Mechanical Engineer), Christian Juica (kneeling - Mechanical Technician), Nelson Montano (Maintenance Engineer), Hansel Sepulveda (Mechanical Technican) and Roberto Tamai (Mechanical Engineer). (Digital Photo). ESO PR Photos may be reproduced, if credit is given to the European Southern Observatory. The ESO PR Video Clips service to visitors to the ESO website provides "animated" illustrations of the ongoing work and events at the European Southern Observatory. The most recent clip was: ESO PR Video Clip 05/00 ("Portugal to Accede to ESO (27 June 2000). Information is also available on the web about other ESO videos.

Regulation of Urea Transporters by Tonicity-responsive Enhancer Binding Protein

PubMed Central

Kwon, H. Moo; Kim, Jim

2007-01-01

Urea accumulation in the renal inner medulla plays a key role in the maintenance of maximal urinary concentrating ability. Urea transport in the kidney is mediated by transporter proteins that include renal urea transporter (UT-A) and erythrocyte urea transporter (UT-B). UT-A1 and UT-A2 are produced from the same gene. There is an active tonicity-responsive enhancer (TonE) in the promoter of UT-A1, and the UT-A1 promoter is stimulated by hypertonicity via tonicity-responsive enhancer binding protein (TonEBP). The downregulation of UT-A2 raises the possibility that TonEBP also regulates its promoter. There is some evidence that TonEBP regulates expression of UT-A in vivo; (1) during the renal development of the urinary concentrating ability, expression of TonEBP precedes that of UT-A1; (2) in transgenic mice expressing a dominant negative form of TonEBP, expression of UT-A1 and UT-A2 is severely impaired; (3) in treatment with cyclosporine A, TonEBP was significantly downregulated after 28 days. This downregulation involves mRNA levels of UT-A2; (4) in hypokalemic animals, downregulation of TonEBP contributed to the down regulation of UT-A in the inner medulla. These data support that TonEBP directly contributes to the urinary concentration and renal urea recycling by the regulation of urea transporters. PMID:24459497

8. VIEW OF DOWNSTREAM OUTLET CULVERT AND WING RETAINING WALLS, ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

8. VIEW OF DOWNSTREAM OUTLET CULVERT AND WING RETAINING WALLS, LOOKING NORTHWEST - High Mountain Dams in Upalco Unit, Twin Pots Dam, Ashley National Forest, 10.1 miles North of Mountain Home, Mountain Home, Duchesne County, UT

A DECAMETER STATIONARY TYPE IV BURST IN IMAGING OBSERVATIONS ON 2014 SEPTEMBER 6

DOE Office of Scientific and Technical Information (OSTI.GOV)

Koval, Artem; Chen, Yao; Feng, Shiwei

2016-08-01

First-of-its-kind radio imaging of a decameter solar stationary type IV radio burst has been presented in this paper. On 2014 September 6 the observations of type IV burst radio emission were carried out with the two-dimensional heliograph based on the Ukrainian T-shaped radio telescope (UTR-2), together with other telescope arrays. Starting at ∼09:55 UT and for ∼3 hr, the radio emission was kept within the observational session of UTR-2. The interesting observation covered the full evolution of this burst, “from birth to death.” During the event lifetime, two C-class solar X-ray flares with peak times 11:29 UT and 12:24 UTmore » took place. The time profile of this burst in radio has a double-humped shape that can be explained by injection of energetic electrons, accelerated by the two flares, into the burst source. According to the heliographic observations, we suggest that the burst source was confined within a high coronal loop, which was part of a relatively slow coronal mass ejection. The latter has been developed for several hours before the onset of the event. Through analysis of about 1.5 × 10{sup 6} heliograms (3700 temporal frames with 4096 images in each frame that correspond to the number of frequency channels), the radio burst source imaging shows a fascinating dynamical evolution. Both space-based ( GOES , SDO , SOHO , STEREO ) data and various ground-based instrumentation (ORFEES, NDA, RSTO, NRH) records have been used for this study.« less

FORS2 observes a multi-epoch transmission spectrum of the hot Saturn-mass exoplanet WASP-49b

NASA Astrophysics Data System (ADS)

Lendl, M.; Delrez, L.; Gillon, M.; Madhusudhan, N.; Jehin, E.; Queloz, D.; Anderson, D. R.; Demory, B.-O.; Hellier, C.

2016-03-01

Context. Transmission spectroscopy has proven to be a useful tool for the study of exoplanet atmospheres, because the absorption and scattering signatures of the atmosphere manifest themselves as variations in the planetary transit depth. Several planets have been studied with this technique, leading to the detection of a small number of elements and molecules (Na, K, H2O), but also revealing that many planets show flat transmission spectra consistent with the presence of opaque high-altitude clouds. Aims: We apply this technique to the MP = 0.40MJ, Rp = 1.20RJ, P = 2.78 d planet WASP-49b, aiming to characterize its transmission spectrum between 0.73 and 1 ¯m and search for the features of K and H2O. Owing to its density and temperature, the planet is predicted to possess an extended atmosphere and is thus a good target for transmission spectroscopy. Methods: Three transits of WASP-49b have been observed with the FORS2 instrument installed at the VLT/UT1 telescope at the ESO Paranal site. We used FORS2 in MXU mode with grism GRIS_600z, producing simultaneous multiwavelength transit light curves throughout the I' and z' bands. We combined these data with independent broadband photometry from the Euler and TRAPPIST telescopes to obtain a good measurement of the transit shape. Strong correlated noise structures are present in the FORS2 light curves, which are due to rotating flat-field structures that are introduced by inhomogeneities of the linear atmospheric dispersion corrector's transparency. We accounted for these structures by constructing common noise models from the residuals of light curves bearing the same noise structures and used them together with simple parametric models to infer the transmission spectrum. Results: We present three independent transmission spectra of WASP-49b between 0.73 and 1.02 ¯m, as well as a transmission spectrum between 0.65 and 1.02 ¯m from the combined analysis of FORS2 and broadband data. The results obtained from the three individual epochs agree well. The transmission spectrum of WASP-49b is best fit by atmospheric models containing a cloud deck at pressure levels of 1 mbar or lower. Based on photometric observations made with FORS2 on the ESO VLT/UT1 (Prog. ID 090.C-0758), EulerCam on the Euler-Swiss telescope and the Belgian TRAPPIST telescope.The photometric time series data in this work are only available in electronic form 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/587/A67

Swift observation of Nova Ophiuchi 2018 No.2 = PNV J17140261-2849237 = TCP J17140253-2849233

NASA Astrophysics Data System (ADS)

Sokolovsky, K.

2018-03-01

The nova candidate PNV J17140261-2849237 = TCP J17140253-2849233 was discovered by H. Nishimura, T. Kojima, K. Nishiyama and F. Kabashima. A. Takao reports the transient (9.5mag) visible at unfiltered images obtained on 2018-03-10.753 UT. Spectroscopic observations with the 2m Liverpool Telescope confirmed the transient to be a Fe II type nova (ATel #11398).

Spectroscopy of PSN J19583553+0236163

NASA Astrophysics Data System (ADS)

Leonard, D. C.; Moustakas, J.; Swift, B. J.; McCarthy, D.; Bailey, V.; Carrico, E.; Carter, A.; Chui, E.; Douglas, E.; Eggeman, E.; Goldberg, R.; Grant, R.; Hartman, K.; Hellerstein, J.; Hooper, E.; Horlick-Cruz, C.; Hunter, L.; Jiles, T.; Johnson, E. D.; Kumar, K.; Lappe, L.; Lee, J.; Lee, W.; Marsh, F.; Mehta, G.; Miller, P.; Rampalli, R.; Reed, J.; Rice, K.; Saldivar, H.; Salgado-Flores, M.; Schlingman, A.; Schlingman, W. F.; Schlingman, W. M.; Scibelli, S.; Sinclair, K.; Steincamp, I.; Stock, N.; Todd, N.; Vargas, L. L. Aizpuru; Yamanaka, S.; Zachary, E.

2011-06-01

As part of the 2011 Advanced Teen Astronomy Camp (http://www.astronomycamp.org), we obtained a low dispersion optical spectrum (range 370-690 nm) of PSN J19583553+0236163 in UGC 11501 with the 2.3m Bok telescope (+ Boller & Chivens spectrograph) at Steward Observatory, on 2011 June 23 UT. Cross-correlation with a library of supernova spectra using the Supernova Identification code (SNID; Blondin and Tonry 2007, Ap.J.

Spectroscopic Classification of ASASSN-16cu as a Type Ia SN

NASA Astrophysics Data System (ADS)

Strader, Jay; Chomiuk, Laura; Shishkovsky, Laura

2016-03-01

We obtained an optical spectrum of ASASSN-16cu (ATel #8796) on UT March 29.37 with the Goodman Spectrograph on the SOAR telescope. Classification with SNID (Blondin and Tonry 2007, ApJ, 666, 1024) indicates ASASSN-16cu is a normal Type Ia SN observed at about 70 days after peak. The redshift is consistent with proposed host galaxy IC 4723 (z=0.011128, via NED).

Multiband Optical Follow-up Observations of GRB 020813 at the Kiso and Bisei Observatories

NASA Astrophysics Data System (ADS)

Urata, Y.; Nishiura, S.; Miyata, T.; Mito, H.; Kawabata, T.; Nakada, Y.; Aoki, T.; Soyano, T.; Tarusawa, K.; Yoshida, A.; Tamagawa, T.; Makishima, K.

2003-09-01

Observations were made of the optical afterglow of GRB 020813 (Fox, Blake, & Price) with the Kiso observatory 1.05 m Schmidt telescope and the Bisei astronomical observatory 1.01 m telescope. Four-band (B, V, R, and I) photometric data points were obtained on 2002 August 13 (10:52-16:46 UT), or 0.346-0.516 days after the burst. In order to investigate the early-time (<1 day) evolution of the afterglow, four-band light curves were produced by analyzing the data taken at these two astronomical observatories as well as the publicly released data taken using the Magellan Baade telescope (Gladders & Hall). The light curves can be approximated by a broken power law, of which the indices are approximately 0.46 and 1.33 before and after a break at ~0.2 days, respectively. The optical spectral index stayed approximately constant at ~0.9 over 0.17-4.07 days after the burst. Since the temporal decay index after the break and the spectral index measured at that time are both consistent with those predicted by a spherical expansion model, the early break is unlikely to be a jet break but is likely to represent the end of an early bump in the light curve, as was observed in the optical afterglow of GRB 021004.

CFBDSIR 2149-0403: young isolated planetary-mass object or high-metallicity low-mass brown dwarf?

NASA Astrophysics Data System (ADS)

Delorme, P.; Dupuy, T.; Gagné, J.; Reylé, C.; Forveille, T.; Liu, M. C.; Artigau, E.; Albert, L.; Delfosse, X.; Allard, F.; Homeier, D.; Malo, L.; Morley, C.; Naud, M. E.; Bonnefoy, M.

2017-06-01

Aims: We conducted a multi-wavelength, multi-instrument observational characterisation of the candidate free-floating planet CFBDSIR J214947.2-040308.9, a late T-dwarf with possible low-gravity features, in order to constrain its physical properties. Methods: We analysed nine hours of X-shooter spectroscopy with signal detectable from 0.8 to 2.3 μm, as well as additional photometry in the mid-infrared using the Spitzer Space Telescope. Combined with a VLT/HAWK-I astrometric parallax, this enabled a full characterisation of the absolute flux from the visible to 5 μm, encompassing more than 90% of the expected energy emitted by such a cool late T-type object. Our analysis of the spectrum also provided the radial velocity and therefore the determination of its full 3D kinematics. Results: While our new spectrum confirms the low gravity and/or high metallicity of CFBDSIR 2149, the parallax and kinematics safely rule out membership to any known young moving group, including AB Doradus. We use the equivalent width of the K I doublet at 1.25 μm as a promising tool to discriminate the effects of low-gravity from the effects of high-metallicity on the emission spectra of cool atmospheres. In the case of CFBDSIR 2149, the observed K I doublet clearly favours the low-gravity solution. Conclusions: CFBDSIR 2149 is therefore a peculiar late-T dwarf that is probably a young, planetary-mass object (2-13 MJup, <500 Myr) possibly similar to the exoplanet 51 Eri b, or perhaps a 2-40 MJup brown dwarf with super-solar metallicity. Based on observations obtained with X-shooter on VLT-UT2 at ESO-Paranal (run 091.D-0723). Based on observations obtained with HAWKI on VLT-UT4 (run 089.C-0952, 090.C-0483, 091.C-0543,092.C-0548,293.C-5019(A) and run 086.C-0655(A)). Based on observations obtained with ISAAC on VLT-UT3 at ESO-Paranal (run 290.C-5083). Based on observation obtained with WIRCam at CFHT (program 2012BF12). Based on Spitzer Space telescope DDT observation (program 10166).

Optical Counterpart to MAXI J1647-227

NASA Astrophysics Data System (ADS)

Garnavich, P.; Magno, K.; Applegate, A.

2012-06-01

We observed the field of the X-ray transient MAXI J1647-227 (Negoro et al., ATEL#4175) with the Vatican Advance Technology Telescope (VATT) and VATT4K CCD imager beginning June 16.244 UT. R-band images reveal an optical source near the position of the Swift localization (Kennea et al., ATEL#4178) that is not visible on the Digitized Sky Survey. Based on USNO-B1.0 catalog stars in the field, we find the optical transient has a position of 16:48:12.32 -23:00:53.56 (error of 0.2 arcsec) which is within 2 arcsec of the Swift X-ray position.

Detection of a long-duration solar gamma-ray flare on Jun. 11, 1991 with EGRET on Compton-GRO

NASA Technical Reports Server (NTRS)

Kanbach, G.; Bertsch, D. L.; Fitchel, C. E.; Hartman, R. C.; Hunter, S. D.; Kniffen, D. A.; Kwok, P. W.; Lin, Y. C.; Mattox, J. R.; Mayer-Hasslewander, H. A.

1992-01-01

On 11 Jun. 1991, the Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory (Comption-GRO) observed high energy gamma radiation above 30 MeV from the Sun following an intense flare around 2:00 Universal Time (UT). After the decay of most of the x ray flare, which caused nearly complete deadtime losses in EGRET, high energy emission was registered during the interval from about 3:30 UT to at least 10:30 UT. Gamma rays were detected up to energies above 1 GeV. The solar origin of the emission is assured by the time profile of the gamma ray count rate and by time resolved sky maps, which show a clear maximum at the position of the sun. The gamma ray lightcurve of the flare can be described with two components: a fast decaying emission with an e-folding time constant of about 25 minutes and a slow decay with about 255 minutes. There are indications for a spectral evolution with time, such that the emission below 100 MeV fades away earlier than the 100 to 300 MeV radiation, roughly in the time scale of the fast component. The spectrum of the flare can be fitted with a composite of a proton generated pion neutral spectrum and an electron bremsstrahlung component. The latter can be identified with the fast decaying component of the lightcurve.

Gamma rays of 0.3 to 30 MeV from PSR 0531+21

NASA Technical Reports Server (NTRS)

White, R. S.; Sweeney, W.; Tuemer, T.; Zych, A. D.

1985-01-01

Pulsed gamma rays from the Crab Pulsar PSR 0531+21 are reported for energies of 0.3 to 30 MeV. The observations were carried out with the UCR gamma ray double Compton scatter telescope launched on a balloon from Palestine, Texas at 4.5 GV, at 2200 LT, September 29, 1978. Two 8 hr observations of the pulsar were made, the first starting at 0700 UT (0200 LT) September 30 just after reaching float altitude of 4.5 g/sq cm. Analysis of the total gamma ray flux from the Crab Nebula plus pulsar using telescope vertical cell pairs was published previously. The results presented supersede the preliminary ones. The double scatter mode of the UCR telescope measures the energy of each incident gamma ray from 1 to 30 MeV and its incident angle to a ring on the sky. The time of arrival is measured to 0.05 ms. The direction of the source is obtained from overlapping rings on the sky. The count rate of the first scatter above a threshold of 0.3 MeV is recorded every 5.12 ms. The Crab Pulsar parameters were determined from six topocentric arrival times of optical pulses.

Ultra-Rapid dUT1 Measurements on Japan-Fennoscandian Baselines - Application to 24-hour Sessions

NASA Technical Reports Server (NTRS)

Matsuzaka, Shigeru; Kurihara, Shinobu; Sekido, Mamoru; Hobiger, Thomas; Haas, Rudiger; Ritakari, Jouko; Wagner, Jan

2010-01-01

GSI, NICT, OSO, and MRO have been engaged in Ultra-rapid dUT1 experiments since 2007 aiming at the technological possibility of real-time dUT1 results using the e-VLBI technique. We have already successfully determined dUT1 in less than four minutes after the end of an experimental Intensive session in 2008, and at present we routinely get the results within 30 minutes for regular Intensives. In 2009 we applied the technique to 24-hour sessions and continuously obtained dUT1 values by processing and analyzing Tsukuba Onsala data in near real-time. It showed a detailed behavior of UT1 variations, which could be very valuable for scientific study as well as for precise prediction of UT1-UTC.

Middle and long-term prediction of UT1-UTC based on combination of Gray Model and Autoregressive Integrated Moving Average

NASA Astrophysics Data System (ADS)

Jia, Song; Xu, Tian-he; Sun, Zhang-zhen; Li, Jia-jing

2017-02-01

UT1-UTC is an important part of the Earth Orientation Parameters (EOP). The high-precision predictions of UT1-UTC play a key role in practical applications of deep space exploration, spacecraft tracking and satellite navigation and positioning. In this paper, a new prediction method with combination of Gray Model (GM(1, 1)) and Autoregressive Integrated Moving Average (ARIMA) is developed. The main idea is as following. Firstly, the UT1-UTC data are preprocessed by removing the leap second and Earth's zonal harmonic tidal to get UT1R-TAI data. Periodic terms are estimated and removed by the least square to get UT2R-TAI. Then the linear terms of UT2R-TAI data are modeled by the GM(1, 1), and the residual terms are modeled by the ARIMA. Finally, the UT2R-TAI prediction can be performed based on the combined model of GM(1, 1) and ARIMA, and the UT1-UTC predictions are obtained by adding the corresponding periodic terms, leap second correction and the Earth's zonal harmonic tidal correction. The results show that the proposed model can be used to predict UT1-UTC effectively with higher middle and long-term (from 32 to 360 days) accuracy than those of LS + AR, LS + MAR and WLS + MAR.

Direct Measurements of the Convective Recycling of the Upper Troposphere

NASA Technical Reports Server (NTRS)

Bertram, Timothy H.; Perring, Anne E.; Wooldridge, Paul J.; Crounse, John D.; Kwan, Alan J.; Wennberg, Paul O.; Scheuer, Eric; Dibb, Jack; Avery, Melody; Sachse, Glen;

An Overview of the Mid-Infrared Spectro-Interferometer MATISSE: Science, Concept, and Current Status

NASA Technical Reports Server (NTRS)

Matter, A.; Lopez, B.; Antonelli, P.; Lehmitz, M.; Bettonvil, F.; Beckmann, U.; Lagarde, S.; Jaffe, W.; Petrov, R. G.; Berio, P.;

Bi-static Optical Observations of GEO Objects

NASA Technical Reports Server (NTRS)

Seitzer, Patrick; Barker, Edwin S.; Cowardin, Heather; Lederer, Susan M.; Buckalew, Brent

2014-01-01

A bi-static study of objects at Geosynchronous Earth Orbit (GEO) was conducted using two ground-based wide-field optical telescopes. The University of Michigan's 0.6-m MODEST (Michigan Orbital Debris Survey Telescope) located at the Cerro Tololo Inter- American Observatory in Chile was employed in a series of coordinated observations with the U.S. Naval Observatory's (USNO) 1.3-m telescope at the USNO Flagstaff Station near Flagstaff, Arizona, USA. The goals of this project are twofold: (1) Obtain optical distances to known and unknown objects at GEO from the difference in the observed topocentric position of objects measured with respect to a reference star frame. The distance can be derived directly from these measurements, and is independent of any orbital solution. The wide geographical separation of these two telescopes means that the parallax difference is larger than ten degrees, and (2) Compare optical photometry in similar filters of GEO objects taken during the same time period from the two sites. The object's illuminated surfaces presented different angles of reflected sunlight to the two telescopes.During a four hour period on the night.of 22 February 2014 (UT), coordinated observations were obtained for eight different GEO positions. Each coordinated observation sequence was started on the hour or half-hour, and was selected to ensure the same cataloged GEO object was available in the field of view of both telescopes during the thirty minute observing sequence. GEO objects were chosen to be both controlled and uncontrolled at a range of orbital inclinations, and the objects were not tracked. Instead both telescopes were operated with all drives off in GEO survey mode to discover un-cataloged objects at GEO. The initial results from this proof-of-concept observing run will be presented, with the intent of laying the foundation for future large-scale bi-static observing campaigns of the GEO regime.

VizieR Online Data Catalog: HST and Magellan observations of Haumea system (Hastings+, 2016)

NASA Astrophysics Data System (ADS)

Hastings, D. M.; Ragozzine, D.; Fabrycky, D. C.; Burkhart, L. D.; Fuentes, C.; Margot, J.-L.; Brown, M. E.; Holman, M.

2017-01-01

The Hubble Space Telescope (HST) observations of the Haumea system comprised five HST orbits' worth of 100s exposures of the Wide Field Planetary Camera 2 from 2009 February 4 (Program 11971) and 10 HST orbits' worth of 44s exposures of the Wide Field Camera 3 from 2010 June 28 (Program 12243). This system was also observed on the night of UT 2009 June 2 with the Magellan Baade telescope at Las Campanas Observatory in Chile. We used the Raymond and Beverly Sackler Magellan Instant Camera (MagIC). Observations were taken from the beginning of the night until it was unobservable, for a total of ~5hr. We centered the system on one of the four quadrants defined by the instrument's four amplifiers. The seeing was constant during the observations and consistently close to 0.5'', smaller than Hi'iaka's separation of 1.4''. The SITe CCD detector has a pixel scale of 0.069''/pixel. We set the exposure times at 120s to avoid saturation and optimize readout time. The filter selected was Johnson-Cousins R. Standard calibrations were taken at the beginning and end of the night. The telescope guiding system ensured that the pointing was constant to within an FWHM over the course of the observations. Table1 presents the relative normalized photometry inferred from our observations. (1 data file).

Rotation-stimulated structures in the CN and C3 comae of comet 103P/Hartley 2 close to the EPOXI encounter

NASA Astrophysics Data System (ADS)

Waniak, W.; Borisov, G.; Drahus, M.; Bonev, T.

2012-07-01

Context. In late 2010, a Jupiter family comet 103P/Hartley 2 was the subject of an intensive world-wide investigation. On UT October 20.7, the comet approached the Earth within only 0.12 AU, and on UT November 4.6 it was visited by the NASA EPOXI spacecraft. Aims: We joined this international effort and organized a ground-based observing campaign with three key goals to: (1) measure the parameters of the nucleus rotation in a time series of CN; (2) investigate the compositional structure of the coma by comparing the CN images with nightly snapshots of C3; and (3) investigate the photochemical relation of CN to HCN, using the HCN data collected nearly simultaneously with our images. Methods: The images were obtained through narrowband filters using the two-meter telescope of the Rozhen National Astronomical Observatory. They were taken over four nights about the moment of the EPOXI encounter. Image processing methods and periodicity analysis techniques were used to identify transient coma structures and investigate their repeatability and kinematics. Results: We observe shells, arc-, jet- and spiral-like patterns that are very similar for the CN and C3 comae. The CN features expanded outwards with the sky-plane projected velocities of between 0.1 to 0.3 km s-1. A corkscrew structure, observed on November 6, evolved with a much higher velocity of 0.66 km s-1. The photometry of the inner coma of CN shows variability with a period of 18.32 ± 0.30 h (valid for the middle moment of our run, UT 2010 Nov 5.0835), which we attribute to the nucleus rotation. This result is fully consistent with independent determinations around the same time by other teams. The pattern of repeatability is, however, imperfect, which is understendable given the suggested excitation of the rotation state, and the variability detected in CN correlates well with the cyclic changes in HCN, but only in the active phases. The identified coma structures, along with the snapshot of the nucleus orientation obtained by EPOXI, enable us to estimate the spin axis orientation. We obtain RA = 122°, Dec = +16° (epoch J2000.0), neglecting at this point the rotational excitation. Based on data collected with two-meter RCC telescope at Rozhen National Astronomical Observatory.Appendix A and movies are available in electronic form at http://www.aanda.org

NIR observations of ASAS SN2018gq

NASA Astrophysics Data System (ADS)

Beamin, Juan C.; Gromadzki, Mariusz

2018-04-01

We report Near IR follow up for the transient ASAS SN2018gq (Atels #11500, #11501,#11509 #11518). We obtained a NIR spectrum from 0.85-2.4 microns with the Arcoriris instrument at the 4m Blanco Telescope in cerro Tololo, Chile, on the night 2018-04-04 at 08:59:21 UT. The total integration was 20 minutes, and the telluric correction was performed with HD119430 A0V star.

Radio constraints on the mass-loss rate of the Type Ia SN 2018gv

NASA Astrophysics Data System (ADS)

Ryder, S. D.; Lundqvist, P.; Perez-Torres, M. A.; Kundu, E.; Kool, E. C.; Bjornsson, C.-I.; Fransson, C.

2018-01-01

The young Type Ia SN 2018gv (ATel #11175, #11177) in the galaxy NGC 2525 has been observed with the Australia Telescope Compact Array (ATCA) at 5.5 and 9.0 GHz on 2018 Jan 18.6 UT. No radio emission was detected at the reported location, to a 3-sigma upper limit of 120 microJy/beam (5.5 GHz) and 30 microJy/beam (9.0 GHz).

Spectroscopic Classification of SN 2018nt as a Reddened Type Ia Supernova

NASA Astrophysics Data System (ADS)

Vinko, J.; Szeged, U.; Wheeler, J. C.

2018-02-01

An optical spectrum (range 360-700 nm) of SN 2018nt (K2 C16-0043), was obtained with the "Low Resolution Spectrograph-2" (LRS2) on the 10m Hobby-Eberly Telescope at McDonald Observatory by S. Odewahn on 2018 Feb 05.20 UT. The spectrum is consistent with that of a heavily reddened Type Ia supernova (with Av > 2 mag) about 3 weeks after maximum light.

Spectroscopic classification of AT 2017cfd as a young Type Ia supernova

NASA Astrophysics Data System (ADS)

Vinko, J.; Wheeler, J. C.

2017-03-01

We report the spectroscopic observation of AT 2017cfd, a transient discovered by the Lick Observatory Supernova Search (LOSS) on 2017-03-16. A spectrum (range 3700-9300 Angstroms), taken with the new "Low Resolution Spectrograph-2" (LRS2) on the 10m Hobby-Eberly Telescope at McDonald Observatory by Steve Odewahn on 2017-03-18.16 UT, is similar to that of a Type Ia supernova before maximum light.

Radio Observations of Nova Muscae 2018 and Nova Carinae 2018 (ASASSN-18fv)

NASA Astrophysics Data System (ADS)

Ryder, S. D.; Kool, E. C.; Chomiuk, L.

2018-04-01

The two optically-bright Galactic novae in Musca (CBET #4473, ATel #11183, #11201, #11212, #11296) and in Carina (ATel #11454, #11456, #11457, #11460, #11468) were observed at radio wavelengths using the Australia Telescope Compact Array (ATCA) on 2018 Apr 3.3 UT. Nova Muscae 2018 has faded by a factor of 3 at 9.0 and 5.5 GHz since peaking at > 30 mJy/bm in mid-March.

VLT deformable secondary mirror: integration and electromechanical tests results

NASA Astrophysics Data System (ADS)

Biasi, R.; Andrighettoni, M.; Angerer, G.; Mair, C.; Pescoller, D.; Lazzarini, P.; Anaclerio, E.; Mantegazza, M.; Gallieni, D.; Vernet, E.; Arsenault, R.; Madec, P.-Y.; Duhoux, P.; Riccardi, A.; Xompero, M.; Briguglio, R.; Manetti, M.; Morandini, M.

2012-07-01

The VLT Deformable secondary is planned to be installed on the VLT UT#4 as part of the telescope conversion into the Adaptive Optics test Facility (AOF). The adaptive unit is based on the well proven contactless, voice coil motor technology that has been already successfully implemented in the MMT, LBT and Magellan adaptive secondaries, and is considered a promising technical choice for the forthcoming ELT-generation adaptive correctors, like the E-ELT M4 and the GMT ASM. The VLT adaptive unit has been recently assembled after the completion of the manufacturing and modular test phases. In this paper, we present the most relevant aspects of the system integration and report the preliminary results of the electromechanical tests performed on the unit. This test campaign is a typical major step foreseen in all similar systems built so far: thanks to the metrology embedded in the system, that allows generating time-dependent stimuli and recording in real time the position of the controlled mirror on all actuators, typical dynamic response quality parameters like modal settling time, overshoot and following error can be acquired without employing optical measurements. In this way the system dynamic and some aspect of its thermal and long term stability can be fully characterized before starting the optical tests and calibrations.

Renal Phenotype of UT-A Urea Transporter Knockout Mice

PubMed Central

Fenton, Robert A.; Flynn, Anneliese; Shodeinde, Adetola; Smith, Craig P.; Schnermann, Jurgen; Knepper, Mark A.

2006-01-01

The urea transporters UT-A1 and UT-A3 mediate rapid transepithelial urea transport across the inner medullary collecting duct (IMCD). In a previous study, using a new mouse model in which both UT-A1 and UT-A3 were genetically deleted from the IMCD (UT-A1/3−/− mice), we investigated the role of these transporters in the function of the renal inner medulla. Here we report a series of studies investigating more generally the renal phenotype of UT-A1/3−/− mice. Pathological screening revealed abnormalities in both the testis (increased size) and kidney (decreased size and vascular congestion) of UT-A1/3−/− mice. Total urinary nitrate and nitrite excretion rates in UT-A1/3−/− mice were more than double those in wildtype mice. Total renal blood flow was not different between UT-A1/3−/− and wildtype mice, but underwent a greater percentage decrease in response to NG-Nitro-L-arginine Methyl Ester Hydrochloride (L-NAME) infusion. Whole kidney glomerular filtration rate was not different in UT-A1/3−/− mice compared to controls and underwent a similar increase in response to a greater dietary protein intake. Fractional urea excretion was markedly elevated in UT-A1/3−/− mice on a 40% protein diet, reaching 102.4 ± 8.8% of the filtered load, suggesting that there may be active urea secretion along the renal tubule. Although there was a marked urinary concentrating defect in UT-A1/3−/− mice, there was no decrease in aquaporin-2 or -3 expression. Furthermore, although urea accumulation in the inner medulla was markedly attenuated, there was no decrease in NaCl concentration in tissue from outer medulla or 2 levels of the inner medulla. PMID:15829709

VizieR Online Data Catalog: IMF in 3 low-redshift strong lenses from SNELLS (Newman+, 2017)

NASA Astrophysics Data System (ADS)

Newman, A. B.; Smith, R. J.; Conroy, C.; Villaume, A.; van Dokkum, P.

2018-04-01

The SINFONI Nearby Elliptical Lens Locator Survey (SNELLS) lenses (Smith+ 2015MNRAS.449.3441S) were observed using the IMACS spectrograph at the 6.5m Magellan Baade telescope during 2015 April 9-10 and 2015 September 25. Spectroscopic observations cover the wavelength range 3565-9415Å continuously with a uniform resolution of 2.8Å. Total exposure times ranged from 60 minutes to 100 minutes per grating. See section 2.1. All SNELLS lenses were also observed using FIRE, a near-infrared echellete spectrograph at the Magellan Baade telescope, during the nights of 2015 April 8, May 3, and September 25. The FIRE spectra cover 0.82-2.51um, but in this paper we use only the region around the Wing-Ford band of FeH near 9916Å for SNL-0 and SNL-1. On-target exposure times for SNL-0 and SNL-1 were 32 minutes and 54 minutes, respectively. The 1" wide slit provided a resolution of R~4000. See section 2.2. We acquired optical and near-infrared spectra for all the SNELLS lenses with X-shooter at the 8.2m UT2 of the ESO Very Large Telescope (VLT). See section 2.3. We obtained r-band images of SNL-1 and SNL-2 using the LDSS-3 imaging spectrograph at the Magellan 2 telescope. Photometric calibration was tied to the SDSS DR9. For SNL-0, we used Hubble Heritage observations taken with the Advanced Camera for Surveys and the F625W filter (Proposal 10710). When constructing our dynamical model of SNL-2, we also use an R-band image obtained in excellent seeing with FORS2 at the VLT. See section 2.4. (2 data files).

Serotyping reanalysis of unserotypable Actinobacillus pleuropneumoniae isolates by agar gel diffusion test.

PubMed

Morioka, Ayako; Shimazaki, Yoko; Uchiyama, Mariko; Suzuki, Shoko

2016-05-03

We observed increasing unserotypable (UT) Actinobacillus pleuropneumoniae isolates using agar gel diffusion (AGD) test. To reanalyze their serovar, we performed rapid slide agglutination (RSA) test and multiplex PCR for 47 UT isolates. Of these, 25 were serovar 1 (UT-serovar 1), 20 were serovar 2 (UT-serovar 2) and 2 were serovar 15 (UT-serovar 15). We examined serotyping antigen extraction temperature to determine heat influence. UT-serovar 1 and 15 were influenced by heat, because their precipitation lines were observed in the case of low antigen extraction temperature. To investigate the relationship between antigenicity and genotype, we performed pulsed-field gel electrophoresis (PFGE) analysis using UT-serovar 2 and 15. The predominant PFGE pattern of UT-serovar 2 was identical to that of serovar 2.

Serotyping reanalysis of unserotypable Actinobacillus pleuropneumoniae isolates by agar gel diffusion test

PubMed Central

MORIOKA, Ayako; SHIMAZAKI, Yoko; UCHIYAMA, Mariko; SUZUKI, Shoko

2016-01-01

We observed increasing unserotypable (UT) Actinobacillus pleuropneumoniae isolates using agar gel diffusion (AGD) test. To reanalyze their serovar, we performed rapid slide agglutination (RSA) test and multiplex PCR for 47 UT isolates. Of these, 25 were serovar 1 (UT-serovar 1), 20 were serovar 2 (UT-serovar 2) and 2 were serovar 15 (UT-serovar 15). We examined serotyping antigen extraction temperature to determine heat influence. UT-serovar 1 and 15 were influenced by heat, because their precipitation lines were observed in the case of low antigen extraction temperature. To investigate the relationship between antigenicity and genotype, we performed pulsed-field gel electrophoresis (PFGE) analysis using UT-serovar 2 and 15. The predominant PFGE pattern of UT-serovar 2 was identical to that of serovar 2. PMID:26726101

7. VIEW SHOWING DOWNSTREAM FACE AND TOE OF DAM, WITH ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

7. VIEW SHOWING DOWNSTREAM FACE AND TOE OF DAM, WITH OUTLET CULVERT AND WING RETAINING WALLS, LOOKING NORTH - High Mountain Dams in Upalco Unit, Twin Pots Dam, Ashley National Forest, 10.1 miles North of Mountain Home, Mountain Home, Duchesne County, UT

Biochemical properties of urea transporters.

PubMed

Chen, Guangping

2014-01-01

Urea and urea transporters (UT) are critical to the production of concentrated urine and hence in maintaining body fluid balance. The UT-A1 urea transporter is the major and most important UT isoform in the kidney. Native UT-A1, expressed in the terminal inner medullary collecting duct (IMCD) epithelial cells, is a glycosylated protein with two glycoforms of 117 and 97 kDa. Vasopressin is the major hormone in vivo that rapidly increases urea permeability in the IMCD through increases in phosphorylation and apical plasma-membrane accumulation of UT-A1. The cell signaling pathway for vasopressin-mediated UT-A1 phosphorylation and activity involves two cAMP-dependent signaling pathways: protein kinase A (PKA) and exchange protein activated by cAMP (Epac). In this chapter, we will discuss UT-A1 regulation by phosphorylation, ubiquitination, and glycosylation.

DOE Office of Scientific and Technical Information (OSTI.GOV)

Zou, P.; Fang, C.; Chen, P. F.

It is important to study the fine structures of solar filaments with high-resolution observations, since it can help us understand the magnetic and thermal structures of the filaments and their dynamics. In this paper, we study a newly formed filament located inside the active region NOAA 11762, which was observed by the 1.6 m New Solar Telescope at Big Bear Solar Observatory from 16:40:19 UT to 17:07:58 UT on 2013 June 5. As revealed by the H α filtergrams, cool material is seen to be injected into the filament spine with a speed of 5–10 km s{sup -1}. At themore » source of the injection, brightenings are identified in the chromosphere, which are accompanied by magnetic cancellation in the photosphere, implying the importance of magnetic reconnection in replenishing the filament with plasmas from the lower atmosphere. Counter-streamings are detected near one endpoint of the filament, with the plane-of-the-sky speed being 7–9 km s{sup -1} in the H α red-wing filtergrams and 9–25 km s{sup -1} in the blue-wing filtergrams. The observations are indicative that this active region filament is supported by a sheared arcade without magnetic dips, and the counter-streamings are due to unidirectional flows with alternative directions, rather than due to the longitudinal oscillations of filament threads as in many other filaments.« less

Material Supply and Magnetic Configuration of an Active Region Filament

NASA Astrophysics Data System (ADS)

Zou, P.; Fang, C.; Chen, P. F.; Yang, K.; Hao, Q.; Cao, Wenda

2016-11-01

It is important to study the fine structures of solar filaments with high-resolution observations, since it can help us understand the magnetic and thermal structures of the filaments and their dynamics. In this paper, we study a newly formed filament located inside the active region NOAA 11762, which was observed by the 1.6 m New Solar Telescope at Big Bear Solar Observatory from 16:40:19 UT to 17:07:58 UT on 2013 June 5. As revealed by the Hα filtergrams, cool material is seen to be injected into the filament spine with a speed of 5-10 km s-1. At the source of the injection, brightenings are identified in the chromosphere, which are accompanied by magnetic cancellation in the photosphere, implying the importance of magnetic reconnection in replenishing the filament with plasmas from the lower atmosphere. Counter-streamings are detected near one endpoint of the filament, with the plane-of-the-sky speed being 7-9 km s-1 in the Hα red-wing filtergrams and 9-25 km s-1 in the blue-wing filtergrams. The observations are indicative that this active region filament is supported by a sheared arcade without magnetic dips, and the counter-streamings are due to unidirectional flows with alternative directions, rather than due to the longitudinal oscillations of filament threads as in many other filaments.

Spectroscopic classification AT 2017jdm as a nova, and likely recurrent eruption of M31N 2007-10b

NASA Astrophysics Data System (ADS)

Williams, S. C.; Darnley, M. J.

2017-12-01

We obtained a spectrum of the transient AT 2017jdm (discovered by F. Castellani, R. Belligoli, C. Marangoni and F. Marziali; see TNS) with the SPRAT spectrograph (resolution R 350; Piascik et al. 2014) on the 2-m Liverpool Telescope (Steele et al. 2004) on 2017 Dec 24.86 UT. The spectrum shows extremely broad Balmer emission, with FWHM of H & alpha; measured at 10,000 km/s.

Spectrum of Transient ASASSN-13at

NASA Astrophysics Data System (ADS)

Garnavich, Peter; Deal, Shanel

2013-06-01

We observed the transient ASASSN-13at (ATEL 5168) on June 28.3 (UT) with the Vatican Advanced Technology Telescope (VATT) and VATTSPEC instrument. The resulting spectrum covers the wavelength range between 365 nm and 750 nm with a resolution of 1100. The spectrum of ASASSN-13at shows a blue continuum with strong Balmer absorption lines. Helium absorption at 447 nm and 588 nm is also seen. Blue-shifted emission lines are visible within the Halpha and Hbeta absorption features.

Medicina-Noto VLBI observation of SN2013ej

NASA Astrophysics Data System (ADS)

Sokolovsky, K.; Giroletti, M.; Stagni, M.; Nanni, M.; Mahabal, A.

2013-08-01

We used the 32m radio telescopes of Istituto di Radioastronomia (INAF-IRA) in Medicina and Noto as a two-element very long baseline interferometer to search for a possible radio counterpart of SN2013ej, a type IIP supernova (CBET #3606, ATel #5228, #5229, #5230, #5237, #5243) in M74. The observations were conducted at 6.7 GHz on 2013 July 31.3 UT, 6 days after the first optical detection reported in CBET #3609.

DOE Office of Scientific and Technical Information (OSTI.GOV)

Dittmann, J. A.; Close, L. M.; Scuderi, L. J.

We present here observations of the transit of WASP-10b on 2009 October 14 UT taken from the University of Arizona's 1.55 m Kuiper telescope on Mount Bigelow. Conditions were photometric and accuracies of 2.0 mmag rms were obtained throughout the transit. We have found that the ratio of the planet to host star radii is in agreement with the measurements of Christian et al. instead of the refinements of Johnson et al., suggesting that WASP-10b is indeed inflated beyond what is expected from theoretical modeling. We find no evidence for large (>20 s) transit timing variations in WASP-10b's orbit frommore » the ephemeris of Christian et al. and Johnson et al.« less

DAO Spectroscopic classification of SN 2017iuu = ATLAS17nnf

NASA Astrophysics Data System (ADS)

Balam, D. D.; Observatory, Dominion Astrophysical; Canada, National Research Council of; Thanjavur, K.; Hsiao, E.; Graham, M. L.

2017-12-01

D. D. Balam, Dominion Astrophysical Observatory, National Research Council of Canada, K. Thanjavur (University of Victoria), E. Hsiao, Florida State University and M. L. Graham (University of Washington) report that a spectrogram (range 390-710 nm, resolution 0.3 nm) of 2017iuu = ATLAS17nnf (J. Tonry, B. Stalder, L. Denneau, A. Heinze, H. Weiland (IfA, University of Hawaii), A. Rest (STScI), K.W. Smith, S. J. Smartt, M. Fulton, O. McBrien (Queen's University Belfast), obtained on Dec. 11.33 UT with the 1.82-m Plaskett Telescope of the National Research Council of Canada, shows it to be a normal type Ia supernova near maximum light.

VizieR Online Data Catalog: GOODS-S CANDELS multiwavelength catalog (Guo+, 2013)

NASA Astrophysics Data System (ADS)

Guo, Y.; Ferguson, H. C.; Giavalisco, M.; Barro, G.; Willner, S. P.; Ashby, M. L. N.; Dahlen, T.; Donley, J. L.; Faber, S. M.; Fontana, A.; Galametz, A.; Grazian, A.; Huang, K.-H.; Kocevski, D. D.; Koekemoer, A. M.; Koo, D. C.; McGrath, E. J.; Peth, M.; Salvato, M.; Wuyts, S.; Castellano, M.; Cooray, A. R.; Dickinson, M. E.; Dunlop, J. S.; Fazio, G. G.; Gardner, J. P.; Gawiser, E.; Grogin, N. A.; Hathi, N. P.; Hsu, L.-T.; Lee, K.-S.; Lucas, R. A.; Mobasher, B.; Nandra, K.; Newman, J. A.; van der Wel, A.

2014-04-01

The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS; Grogin et al. 2011ApJS..197...35G; Koekemoer et al. 2011ApJS..197...36K) is designed to document galaxy formation and evolution over the redshift range of z=1.5-8. The core of CANDELS is to use the revolutionary near-infrared HST/WFC3 camera, installed on HST in 2009 May, to obtain deep imaging of faint and faraway objects. The GOODS-S field, centered at RAJ2000=03:32:30 and DEJ2000=-27:48:20 and located within the Chandra Deep Field South (CDFS; Giacconi et al. 2002, Cat. J/ApJS/139/369), is a sky region of about 170arcmin2 which has been targeted for some of the deepest observations ever taken by NASA's Great Observatories, HST, Spitzer, and Chandra as well as by other world-class telescopes. The field has been (among others) imaged in the optical wavelength with HST/ACS in F435W, F606W, F775W, and F850LP bands as part of the HST Treasury Program: the Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261); in the mid-IR (3.6-24um) wavelength with Spitzer as part of the GOODS Spitzer Legacy Program (PI: M. Dickinson). The CDF-S/GOODS field was observed by the MOSAIC II imager on the CTIO 4m Blanco telescope to obtain deep U-band observations in 2001 September. Another U-band survey in GOODS-S was carried out using the VIMOS instrument mounted at the Melipal Unit Telescope of the VLT at ESO's Cerro Paranal Observatory, Chile. This large program of ESO (168.A-0485; PI: C. Cesarsky) was obtained in service mode observations in UT3 between 2004 August and fall 2006. In the ground-based NIR, imaging observations of the CDFS were carried out in J, H, Ks bands using the ISAAC instrument mounted at the Antu Unit Telescope of the VLT. Data were obtained as part of the ESO Large Programme 168.A-0485 (PI: C. Cesarsky) as well as ESO Programmes 64.O-0643, 66.A-0572, and 68.A-0544 (PI: E. Giallongo) with a total allocation time of ~500 hr from 1999 October to 2007 January. The CANDELS/GOODS-S field was also observed in the NIR as part of the ongoing HAWK-I UDS and GOODS-S survey (HUGS; VLT large program ID 186.A-0898; PI: A. Fontana; A. Fontana et al., in preparation) using the High Acuity Wide field K-band Imager (HAWK-I) on VLT. (1 data file).

Alternative channels for urea in the inner medulla of the rat kidney.

PubMed

Nawata, C Michele; Dantzler, William H; Pannabecker, Thomas L

2015-12-01

The ascending thin limbs (ATLs) and lower descending thin limbs (DTLs) of Henle's loop in the inner medulla of the rat are highly permeable to urea, and yet no urea transporters have been identified in these sections. We hypothesized that novel, yet-unidentified transporters in these tubule segments could explain the high urea permeability. cDNAs encoding for Na(+)-glucose transporter 1a (SGLT1a), Na(+)-glucose transporter 1 (NaGLT1), urea transporter (UT)-A2c, and UT-A2d were isolated and cloned from the Munich-Wistar rat inner medulla. SGLT1a is a novel NH2-terminal truncated variant of SGLT1. NaGLT1 is a Na(+)-dependent glucose transporter primarily located in the proximal tubules and not previously described in the thin limbs. UT-A2c and UT-A2d are novel variants of UT-A2. UT-A2c is truncated at the COOH terminus, and UT-A2d has one exon skipped. When rats underwent water restriction for 72 h, mRNA levels of SGLT1a increased in ATLs, NaGLT1 levels increased in both ATLs and DTLs, and UT-A2c increased in ATLs. [(14)C]urea uptake assays performed on Xenopus oocytes heterologously expressing these proteins revealed that despite having structural differences from their full-length versions, SGLT1a, UT-A2c, and UT-A2d enhanced urea uptake. NaGLT1 also facilitated urea uptake. Uptakes were Na(+) independent and inhibitable by phloretin and/or phloridzin. Our data indicate that there are several alternative channels for urea in the rat inner medulla that could potentially contribute to the high urea permeabilities in thin limb segments. Copyright © 2015 the American Physiological Society.

Alternative channels for urea in the inner medulla of the rat kidney

PubMed Central

Dantzler, William H.; Pannabecker, Thomas L.

2015-01-01

The ascending thin limbs (ATLs) and lower descending thin limbs (DTLs) of Henle's loop in the inner medulla of the rat are highly permeable to urea, and yet no urea transporters have been identified in these sections. We hypothesized that novel, yet-unidentified transporters in these tubule segments could explain the high urea permeability. cDNAs encoding for Na+-glucose transporter 1a (SGLT1a), Na+-glucose transporter 1 (NaGLT1), urea transporter (UT)-A2c, and UT-A2d were isolated and cloned from the Munich-Wistar rat inner medulla. SGLT1a is a novel NH2-terminal truncated variant of SGLT1. NaGLT1 is a Na+-dependent glucose transporter primarily located in the proximal tubules and not previously described in the thin limbs. UT-A2c and UT-A2d are novel variants of UT-A2. UT-A2c is truncated at the COOH terminus, and UT-A2d has one exon skipped. When rats underwent water restriction for 72 h, mRNA levels of SGLT1a increased in ATLs, NaGLT1 levels increased in both ATLs and DTLs, and UT-A2c increased in ATLs. [14C]urea uptake assays performed on Xenopus oocytes heterologously expressing these proteins revealed that despite having structural differences from their full-length versions, SGLT1a, UT-A2c, and UT-A2d enhanced urea uptake. NaGLT1 also facilitated urea uptake. Uptakes were Na+ independent and inhibitable by phloretin and/or phloridzin. Our data indicate that there are several alternative channels for urea in the rat inner medulla that could potentially contribute to the high urea permeabilities in thin limb segments. PMID:26423860

Results from the 2010 Feb 14 and July 4 Pluto Occultations

NASA Astrophysics Data System (ADS)

Young, Leslie; Sicardy, B.; Widemann, T.; Brucker, M. J.; Buie, M. W.; Fraser, B.; Van Heerden, H.; Howell, R. R.; Lonergan, K.; Olkin, C. B.; Reitsema, H. J.; Richter, A.; Sepersky, T.; Wasserman, L. H.; Young, E. F.

2010-10-01

The Portable High-speed Occultation Telescope (PHOT) group observed two occultations by Pluto in 2010. The first, of a I=9.3 magnitudue star on 2010 Feb 14, was organized by the Meudon occultation group, with the PHOT group as collaborators. For this bright but low-elevation event, we deployed to three sites in Europe: Obs. Haute Provence, France (0.8-m; L. Young, H. Reitsema), Leopold Figl, Austria (1.5-m; E. Young), and Apline Astrovillage, Lu, Switzerland (0.36-m; C. Olkin, L. Wasserman). We obtained a lightcurve at Lu under clear conditions, which will be combined with two other lightcurves from the Meudon group, from Sisteron and Pic du Midi, France. We observed the second Pluto occultation, of a I=13.2 star on 2010 July 4 UT, from four sites in South Africa: with our portable telescope near Upington (0.36-m; M. Buie, L. Wasserman), the Boyden telescope in Bloemfontein (1.5-m; L. Young, M. Brucker), the Innes telescope in Johannesburg (0.67-m; T. Sepersky, B. Fraser), and the telescope at Aloe Ridge north of Johannesburg (0.62-m; R. Howell, K. Lonergan, A. Richter). Upington was cloudy, Boyden had heavy scattered clouds, and Innes suffered from haze and telescope mechanical problems. A lightcurve was obtained from Aloe Ridge under clear conditions. Data was also obtained by Karl-Ludwig Bath & Thomas Sauer at Hakos, Namibia and by Berto Monard of ASSA near Pretoria, South Africa. The length of the Aloe Ridge chord suggests it is nearly central. These observations give us four contiguous years in which we observed one or more Pluto occultations, providing constraints on the seasonal evolution of Pluto's atmosphere. Thanks are due to Marcelo Assafin and Jim Elliot for sharing predictions prior to the July event. This work was supported, in part, by NASA PAST NNX08A062G.

Ground-based multiwavelength observations of comet 103P/Hartley 2

DOE Office of Scientific and Technical Information (OSTI.GOV)

Gicquel, A.; Villanueva, G. L.; Cordiner, M. A.

2014-10-10

The Jupiter-family comet 103P/Hartley 2 (103P) was the target of the NASA EPOXI mission. In support of this mission, we conducted observations from radio to submillimeter wavelengths of comet 103P in the three weeks preceding the spacecraft rendezvous on UT 2010 November 4.58. This time period included the passage at perihelion and the closest approach of the comet to the Earth. Here, we report detections of HCN, H{sub 2}CO, CS, and OH and upper limits for HNC and DCN toward 103P using the Arizona Radio Observatory Kitt Peak 12 m telescope (ARO 12 m) and submillimeter telescope (SMT), the Jamesmore » Clerk Maxwell Telescope (JCMT), and the Green Bank Telescope (GBT). The water production rate, Q{sub H{sub 2O}} = (0.67-1.07) × 10{sup 28} s{sup –1}, was determined from the GBT OH data. From the average abundance ratios of HCN and H{sub 2}CO relative to water (0.13 ± 0.03% and 0.14 ± 0.03%, respectively), we conclude that H{sub 2}CO is depleted and HCN is normal with respect to typically observed cometary mixing ratios. However, the abundance ratio of HCN with water shows a large diversity with time. Using the JCMT data, we measured an upper limit for the DCN/HCN ratio <0.01. Consecutive observations of ortho-H{sub 2}CO and para-H{sub 2}CO on November 2 (from data obtained at the JCMT) allowed us to derive an ortho:para ratio (OPR) of ≈2.12 ± 0.59 (1σ), corresponding to T {sub spin} > 8 K (2σ).« less

On the morphology of the compact dust shell in the symbiotic system HM Sagittae

NASA Astrophysics Data System (ADS)

Sacuto, S.; Chesneau, O.

2009-01-01

Context: The symbiotic system HM Sagittae consists of a Mira star and a secondary White Dwarf component. The dust content of the system was severely affected by the nova outburst in 1975, which is still ongoing. The capabilities of optical interferometry operating in the mid-IR allow us to investigate the current geometry of the dust envelope. Aims: We test our previous spectro-interferometric study of this system with new interferometric configurations, increasing the uv coverage and allowing us to ascertain the appearance of the source between 8 and 13 μm. Methods: We used the MIDI instrument of the VLTI with the unit telescopes (UTs) and auxiliary telescopes (ATs) providing baselines oriented from PA = 42° to 127°. The data are interpreted by means of an elliptical Gaussian model and the spherical radiative transfer code DUSTY. Results: We demonstrate that the data can be reproduced well by an optically thick dust shell of amorphous silicate, typical of those encountered around Mira stars, whose measured dimension increases from 8 to 13 μm. We confirm that the envelope is more extended in a direction perpendicular to the binary axis. The level of elongation increases with wavelength in contrast to our claim in a previous study. Conclusions: The wider uv coverage allows us to deepen our previous investigations of the close circumstellar structure of this object. Based on observations made with the Very Large Telescope Interferometer at Paranal Observatory under programs 075.D-0484, 077.D-0216, and 079.D-0213. Reduced visibilities and differential phases are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/493/1043

VizieR Online Data Catalog: Detailed abundances of KOI stars with planets. I. (Schuler+, 2015)

NASA Astrophysics Data System (ADS)

Schuler, S. C.; Vaz, Z. A.; Katime Santrich, O. J.; Cunha, K.; Smith, V. V.; King, J. R.; Teske, J. K.; Ghezzi, L.; Howell, S. B.; Isaacson, H.

2016-03-01

We have analyzed high-resolution, high-signal-to-noise ratio (S/N) spectra of seven stars, each of which has at least one confirmed small planet discovered by Kepler. The spectra of these stars were obtained as part of the Kepler Follow-up Observing Program (KFOP). The 10m Keck I telescope and High Resolution Echelle Spectrometer (HIRES) are being utilized for precise RV measurements of high-priority KOIs. The KFOP spectra are characterized by a spectral resolution of R=50000 and span 3650-7950Å with incomplete coverage in the reddest orders. Additional observations of Kepler-21 were made independently with Keck/HIRES and the 4m Mayall telescope and echelle spectrograph at Kitt Peak National Observatory (KPNO) in UT 2011. (4 data files).

Two VLT 8.2-m Unit Telescopes in Action

NASA Astrophysics Data System (ADS)

1999-04-01

Visitors at ANTU - Astronomical Images from KUEYEN The VLT Control Room at the Paranal Observatory is becoming a busy place indeed. From here, two specialist teams of ESO astronomers and engineers now operate two VLT 8.2-m Unit Telescopes in parallel, ANTU and KUEYEN (formerly UT1 and UT2, for more information about the naming and the pronunciation, see ESO Press Release 06/99 ). Regular science observations have just started with the first of these giant telescopes, while impressive astronomical images are being obtained with the second. The work is hard, but the mood in the control room is good. Insiders claim that there have even been occasions on which the groups have had a friendly "competition" about which telescope makes the "best" images! The ANTU-team has worked with the FORS multi-mode instrument , their colleagues at KUEYEN use the VLT Test Camera for the ongoing tests of this new telescope. While the first is a highly developed astronomical instrument with a large-field CCD imager (6.8 x 6.8 arcmin 2 in the normal mode; 3.4 x 3.4 arcmin 2 in the high-resolution mode), the other is a less complex CCD camera with a smaller field (1.5 x 1.5 arcmin 2 ), suited to verify the optical performance of the telescope. As these images demonstrate, the performance of the second VLT Unit Telescope is steadily improving and it may not be too long before its optical quality will approach that of the first. First KUEYEN photos of stars and galaxies We present here some of the first astronomical images, taken with the second telescope, KUEYEN, in late March and early April 1999. They reflect the current status of the optical, electronic and mechanical systems, still in the process of being tuned. As expected, the experience gained from ANTU last year has turned out to be invaluable and has allowed good progress during this extremely delicate process. ESO PR Photo 19a/99 ESO PR Photo 19a/99 [Preview - JPEG: 400 x 433 pix - 160k] [Normal - JPEG: 800 x 866 pix - 457k] [High-Res - JPEG: 1985 x 2148 pix - 2.0M] ESO PR Photo 19b/99 ESO PR Photo 19b/99 [Preview - JPEG: 400 x 478 pix - 165k] [Normal - JPEG: 800 x 956 pix - 594k] [High-Res - JPEG: 3000 x 3583 pix - 7.1M] Caption to PR Photo 19a/99 : This photo was obtained with VLT KUEYEN on April 4, 1999. It is reproduced from an excellent 60-second R(ed)-band exposure of the innermost region of a globular cluster, Messier 68 (NGC 4590) , in the southern constellation Hydra (The Water-Snake). The distance to this 8-mag cluster is about 35,000 light years, and the diameter is about 140 light-years. The excellent image quality is 0.38 arcsec , demonstrating a good optical and mechanical state of the telescope, already at this early stage of the commissioning phase. The field measures about 90 x 90 arcsec 2. The original scale is 0.0455 pix/arcsec and there are 2048x2048 pixels in one frame. North is up and East is left. Caption to PR Photo 19b/99 : This photo shows the central region of spiral galaxy ESO 269-57 , located in the southern constellation Centaurus at a distance of about 150 million light-years. Many galaxies are seen in this direction at about the same distance, forming a loose cluster; there are also some fainter, more distant ones in the background. The designation refers to the ESO/Uppsala Survey of the Southern Sky in the 1970's during which over 15,000 southern galaxies were catalogued. ESO 269-57 is a tightly bound object of type Sar , the "r" referring to the "ring" that surrounds the bright centre, that is overexposed here. The photo is a composite, based on three exposures (Blue - 600 sec; Yellow-Green - 300 sec; Red - 300 sec) obtained with KUEYEN on March 28, 1999. The image quality is 0.7 arcsec and the field is 90 x 90 arcsec 2. North is up and East is left. ESO PR Photo 19c/99 ESO PR Photo 19c/99 [Preview - JPEG: 400 x 478 pix - 132k] [Normal - JPEG: 800 x 956 pix - 446k] [High-Res - JPEG: 3000 x 3583 pix - 4.6M] ESO PR Photo 19d/99 ESO PR Photo 19d/99 [Preview - JPEG: 400 x 454 pix - 86k] [Normal - JPEG: 800 x 907 pix - 301k] [High-Res - JPEG: 978 x 1109 pix - 282k] Caption to PR Photo 19c/99 : Somewhat further out in space, and right on the border between the southern constellations Hydra and Centaurus lies this knotty spiral galaxy, IC 4248 ; the distance is about 210 million light-years. It was imaged with KUEYEN on March 28, 1999, with the same filters and exposure times as used for Photo 19b/99. The image quality is 0.75 arcsec and the field is 90 x 90 arcsec 2. North is up and East is left. Caption to PR Photo 19d/99 : This is a close-up view of the double galaxy NGC 5090 (right) and NGC 5091 (left), in the southern constellation Centaurus. The first is a typical S0 galaxy with a bright diffuse centre, surrounded by a fainter envelope of stars (not resolved in this picture). However, some of the starlike objects seen in this region may be globular clusters (or dwarf galaxies) in orbit around NGC 5090. The other galaxy is of type Sa (the spiral structure is more developed) and is seen at a steep angle. The three-colour composite is based on frames obtained with KUEYEN on March 29, 1999, with the same filters and exposure times as used for Photo 19b/99. The image quality is 0.7 arcsec and the field is 90 x 90 arcsec 2. North is up and East is left. ( Note inserted on April 26: The original caption text identified the second galaxy as NGC 5090B - this error has now been corrected. ESO PR Photo 19e/99 ESO PR Photo 19e/99 [Preview - JPEG: 400 x 441 pix - 282k] [Normal - JPEG: 800 x 882 pix - 966k] [High-Res - JPEG: 3000 x 3307 pix - 6,4M] Caption to PR Photo 19e/99 : Wide-angle photo of the second 8.2-m VLT Unit Telescope, KUEYEN , obtained on March 10, 1999, with the main mirror and its cell in place at the bottom of the telescope structure. The Test Camera with which the astronomical images above were made, is positioned at the Cassegrain focus, inside this mirror cell. The Paranal Inauguration on March 5, 1999, took place under this telescope that was tilted towards the horizon to accommodate nearly 300 persons on the observing floor. Astronomical observations with ANTU have started On April 1, 1999, the first 8.2-m VLT Unit Telescope, ANTU , was "handed over" to the astronomers. Last year, about 270 observing proposals competed about the first, precious observing time at Europe's largest optical telescope and more than 100 of these were accommodated within the six-month period until the end of September 1999. The complete observing schedule is available on the web. These observations will be carried out in two different modes. During the Visitor Mode , the astronomers will be present at the telescope, while in the Service Mode , ESO observers perform the observations. The latter procedure allows a greater degree of flexibility and the possibility to assign periods of particularly good observing conditions to programmes whose success is critically dependent on this. The first ten nights at ANTU were allocated to service mode observations. After some initial technical problems with the instruments, these have now started. Already in the first night, programmes at ISAAC requiring 0.4 arcsec conditions could be satisfied, and some images better than 0.3 arcsec were obtained in the near-infrared . The first astronomers to use the telescope in visitors mode will be Professors Immo Appenzeller (Heidelberg, Germany; "Photo-polarimetry of pulsars") and George Miley (Leiden, The Netherlands; "Distant radio galaxies") with their respective team colleagues. How to obtain ESO Press Information ESO Press Information is made available on the World-Wide Web (URL: http://www.eso.org../ ). ESO Press Photos may be reproduced, if credit is given to the European Southern Observatory. Note also the dedicated webarea with VLT Information.

Optical spectroscopy of SN2014J

NASA Astrophysics Data System (ADS)

Kotak, R.

2014-01-01

Authors: J. Polshaw, R. Kotak, J. R. Maund, S. J. Smartt (QUB), M. Fraser, N. Walton (IoA), J. M. Abreu (IAC), M. Balcells, C. Benn, J. Mendez, A. Oscoz, O. Zamora, C. Zurita (ING) A spectrum of the supernova SN 2014J in the nearby galaxy M82 was obtained on Jan. 23.2 2014 (UT) at the 2.54m Isaac Newton Telescope (INT) with IDS and the grating R1200R (approximate wavelength range 5600 - 7500A, at 2A resolution).

Pre discovery R band limits for SN 2017aew

NASA Astrophysics Data System (ADS)

Steele, I. A.; Newsam, A. M.

2017-05-01

A 90 second R band image of the galaxy NGC6948 was obtained on 2017 May 06 at 04:13UT using the 2.0m Liverpool Telescope, La Palma. The image was obtained by the National Schools Observatory on behalf of St Anne's Catholic School, Southampton, UK. Inspection of the image shows no source visible at the co-ordinates of SN 2017aew (ATel #10381) down to a limit of R=21.2 (photometry calibrated with respect to the nearby USNO object 1501-0283085).

Spectroscopic Classification of SN 2017ghm as a Type Ia Supernova

NASA Astrophysics Data System (ADS)

Vinko, J.; Wheeler, J. C.; Wang, X.; Li, W.; Li, Z.; Xiang, D.; Rui, L.; Lin, H.; Xu, Z.; Li, B.; Zhao, H.; Wang, L.; Tan, H.; Zhang, J.

2017-09-01

An optical spectrum (range 360-680 nm) of SN 2017ghm (=PTSS-17uyml), discovered by the PMO-Tsinghua Supernova Survey (PTSS, http://www.cneost.org/ptss/), was obtained with the new "Low Resolution Spectrograph-2" (LRS2) on the 10m Hobby-Eberly Telescope at McDonald Observatory by S. Rostopchin on 2017 Aug 31.17 UT. The spectrum is consistent with that of a heavily reddened Type Ia supernova (with Av > 2.3 mag) around maximum light.

Spectroscopic classification of AT 2018adg as a Type Ic supernova

NASA Astrophysics Data System (ADS)

Williams, S. C.; Nordin, J.; Hook, I. M.

2018-03-01

We obtained a spectrum of the transient AT 2018adg (see TNS) with the SPRAT spectrograph (resolution R 350; Piascik et al. 2014) on the 2-m Liverpool Telescope (LT; Steele et al. 2004) on 2018 Mar 11.13 UT. The spectrum is consistent with AT 2018adg being a Type Ic supernova around peak brightness, at a redshift of z 0.02 to 0.03, in agreement with the host galaxy redshift of z = 0.022 (da Costa et al. 1998).

Molecular Mechanisms of Urea Transport in Health and Disease

PubMed Central

Klein, Janet D.; Blount, Mitsi A.; Sands, Jeff M.

2012-01-01

In the late 1980s, urea permeability measurements produced values that could not be explained by paracellular transport or lipid phase diffusion. The existence of urea transport proteins were thus proposed and less than a decade later, the first urea transporter was cloned. The SLC14A family of urea transporters has two major subgroups, designated SLC14A1 (or UT-B) and Slc14A2 (or UT-A). UT-B and UT-A gene products are glycoproteins located in various extra-renal tissues however, a majority of the resulting isoforms are found in the kidney. The UT-B (Slc14A1) urea transporter was originally isolated from erythrocytes and two isoforms have been reported. In kidney, UT-B is located primarily in the descending vasa recta. The UT-A (Slc14A2) urea transporter yields 6 distinct isoforms, of which 3 are found chiefly in the kidney medulla. UT-A1 and UT-A3 are found in the inner medullary collecting duct (IMCD), while UT-A2 is located in the thin descending limb. These transporters are crucial to the kidney’s ability to concentrate urine. The regulation of urea transporter activity in the IMCD involves acute modification through phosphorylation and subsequent movement to the plasma membrane. UT-A1 and UT-A3 accumulate in the plasma membrane in response to stimulation by vasopressin or hypertonicity. Long term regulation of the urea transporters in the IMCD involves altering protein abundance in response to changes in hydration status, low protein diets, or adrenal steroids. Urea transporters have been studied using animal models of disease including diabetes mellitus, lithium intoxication, hypertension, and nephrotoxic drug responses. Exciting new genetically engineered mouse models are being developed to study these transporters. PMID:23007461

Molecular mechanisms of urea transport in health and disease.

PubMed

Klein, Janet D; Blount, Mitsi A; Sands, Jeff M

2012-12-01

In the late 1980s, urea permeability measurements produced values that could not be explained by paracellular transport or lipid phase diffusion. The existence of urea transport proteins were thus proposed and less than a decade later, the first urea transporter was cloned. The family of urea transporters has two major subgroups, designated SLC14A1 (or UT-B) and Slc14A2 (or UT-A). UT-B and UT-A gene products are glycoproteins located in various extra-renal tissues however, a majority of the resulting isoforms are found in the kidney. The UT-B (Slc14A1) urea transporter was originally isolated from erythrocytes and two isoforms have been reported. In kidney, UT-B is located primarily in the descending vasa recta. The UT-A (Slc14A2) urea transporter yields six distinct isoforms, of which three are found chiefly in the kidney medulla. UT-A1 and UT-A3 are found in the inner medullary collecting duct (IMCD), while UT-A2 is located in the thin descending limb. These transporters are crucial to the kidney's ability to concentrate urine. The regulation of urea transporter activity in the IMCD involves acute modification through phosphorylation and subsequent movement to the plasma membrane. UT-A1 and UT-A3 accumulate in the plasma membrane in response to stimulation by vasopressin or hypertonicity. Long-term regulation of the urea transporters in the IMCD involves altering protein abundance in response to changes in hydration status, low protein diets, or adrenal steroids. Urea transporters have been studied using animal models of disease including diabetes mellitus, lithium intoxication, hypertension, and nephrotoxic drug responses. Exciting new genetically engineered mouse models are being developed to study these transporters.

Effects of the 2011 Tohoku Earthquake on VLBI Geode- tic Measurements

NASA Astrophysics Data System (ADS)

MacMillan, D.; Behrend, D.; Kurihara, S.

2012-12-01

The VLBI antenna TSUKUB32 at Tsukuba, Japan observes in 24-hour observing sessions once per week with the R1 operational network and on additional days with other networks on a more irregular basis. Further, the antenna is an endpoint of the single-baseline, 1-hr Intensive Int2 sessions observed on the weekends for the determination of UT1. TSUKUB32 returned to normal operational observing one month after the earthquake. The antenna is 160 km west and 240 km south of the epicenter of the Tohoku earthquake. We looked at the transient behavior of the TSUKUB32 position time series following the earthquake and found that significant deformation is continuing. The eastward rate relative to the long-term rate prior to the earthquake was about 20 cm/yr four months after the earthquake and 9 cm/yr after one year. The VLBI series agrees closely with the corresponding JPL (Jet Propulsion Laboratory) GPS series measured by the co-located GPS antenna TSUK. The co-seismic UEN displacement at Tsukuba as determined by VLBI was (-90 mm, 640 mm, 44 mm). We examined the effect of the variation of the TSUKUB32 position on EOP estimates and then used the GPS data to correct its position for the estimation of UT1 in the Tsukuba-Wettzell Int2 Intensive experiments. For this purpose and to provide operational UT1, the IVS scheduled a series of weekend Intensive sessions observing on the Kokee-Wettzell baseline immediately before each of the two Tsukuba-Wettzell Intensive sessions. Comparisons between the UT1 estimates from these weekend sessions and the USNO (United States Naval Observatory) combination series were used to validate the GPS correction to the TSUKUB32 position.

Modulation of kidney urea transporter UT-A3 activity by alpha2,6-sialylation

PubMed Central

Qian, Xiaoqian; Sands, Jeff M.; Song, Xiang; Chen, Guangping

2016-01-01

Two urea transporters, UT-A1 and UT-A3, are expressed in the kidney terminal inner medullary collecting duct (IMCD) and are important for the production of concentrated urine. UT-A1, as the largest isoform of all UT-A urea transporters, has gained much attention and been extensively studied; however the role and the regulation of UT-A3 are less explored. In this study, we investigated UT-A3 regulation by glycosylation modification. A site-directed mutagenesis verified a single glycosylation site in UT-A3 at Asn279. Loss of the glycosylation reduced forskolin-stimulated UT-A3 cell membrane expression and urea transport activity. UT-A3 has two glycosylation forms, 45 kDa and 65 kDa. Using sugar specific-binding lectins, the UT-A3 glycosylation profile was examined. The 45 kDa form was pulled down by lectin Con A and GNL, indicating an immature glycan with a high amount of mannose (Man); whereas the 65 kDa form is a mature glycan composed of acetylglucosamine (GlcNAc), poly-N-acetyllactosame (poly-LacNAc) that was pulled down by WGA and tomato lectin, respectively. Interestingly, the mature form of UT-A3 glycan contains significant amounts of sialic acid. We explored the enzymes responsible for directing UT-A3 sialylation. Sialyltransferase ST6GalI, but not ST3GalIV, catabolizes UT-A3 α2, 6-sialylation. Activation of PKC by PDB treatment promoted UT-A3 glycan sialylation and membrane surface expression. PKC inhibitor chelerythrine blocks ST6GalI-induced UT-A3 sialylation. Increased sialylation by ST6GalI increased UT-A3 protein stability and urea transport activity. Collectively, our study reveals a novel mechanism of UT-A3 regulation by ST6GalI-mediated sialylation modification that may play an important in kidney urea reabsorption and the urinary concentrating mechanism. PMID:26972907

Urea transporter proteins as targets for small-molecule diuretics.

PubMed

Esteva-Font, Cristina; Anderson, Marc O; Verkman, Alan S

2015-02-01

Conventional diuretics such as furosemide and thiazides target salt transporters in kidney tubules, but urea transporters (UTs) have emerged as alternative targets. UTs are a family of transmembrane channels expressed in a variety of mammalian tissues, in particular the kidney. UT knockout mice and humans with UT mutations exhibit reduced maximal urinary osmolality, demonstrating that UTs are necessary for the concentration of urine. Small-molecule screening has identified potent and selective inhibitors of UT-A, the UT protein expressed in renal tubule epithelial cells, and UT-B, the UT protein expressed in vasa recta endothelial cells. Data from UT knockout mice and from rodents administered UT inhibitors support the diuretic action of UT inhibition. The kidney-specific expression of UT-A1, together with high selectivity of the small-molecule inhibitors, means that off-target effects of such small-molecule drugs should be minimal. This Review summarizes the structure, expression and function of UTs, and looks at the evidence supporting the validity of UTs as targets for the development of salt-sparing diuretics with a unique mechanism of action. UT-targeted inhibitors may be useful alone or in combination with conventional diuretics for therapy of various oedemas and hyponatraemias, potentially including those refractory to treatment with current diuretics.

Disappearance of Comet C/2010 X1 (Elenin): Gone With a Whimper, Not a Bang

NASA Astrophysics Data System (ADS)

Li, Jing; Jewitt, David

2015-04-01

We examine the rise and sudden demise of comet C/2010 X1 (Elenin) on its approach to perihelion. Discovered inbound at 4.2 AU, this long-period comet was predicted to become very bright when near perihelion, at 0.48 AU on 2011 September 10. Observations starting 2011 February (heliocentric distance ˜3.5 AU) indeed show the comet to brighten by about 11 mag, with most of the increase occurring inside 1 AU from the Sun. The peak brightness reached mR = 6 on UT 2011 August 12.95 ± 0.50, when at ˜0.83 AU from the Sun. Thereafter, the comet faded even as the heliocentric distance continued to decrease. We find that most of the surge in brightness in mid-August resulted from dust-particle forward scattering, not from a sudden increase in the activity. A much smaller (˜3 mag) brightening began on UT 2011 August 18 ± 1 (heliocentric distance 0.74 AU), reached a maximum on UT 2011 August 30 ± 1 (at 0.56 AU), and reflects the true breakup of the nucleus. This second peak was matched by a change in the morphology from centrally condensed to diffuse. The estimated cross section of the nucleus when at 1 AU inbound was ˜1 km2, corresponding to an equal-area circle of radius 0.6 km. Observations were taken after the second peak using the Canada-France-Hawaii 3.6 m telescope to search for surviving fragments of the nucleus. None were found to a limiting red magnitude r‧ = 24.4, corresponding to radii ≲40 m (red geometric albedo = 0.04 assumed). The brightening, the progressive elongation of the debris cloud, and the absence of a central condensation in data taken after UT 2011 August 30 are consistent with disintegration of the nucleus into a power law size distribution of fragments with index q = 3.3 ± 0.2 combined with the action of radiation pressure. In such a distribution, the largest particles contain most of the mass while the smallest particles dominate the scattering cross section and apparent brightness. We speculate about physical processes that might cause nucleus disruption in a comet when still 0.7 AU from the Sun. Tidal stresses and devolatilization of the nucleus by sublimation are both negligible at this distance. However, the torque caused by mass loss, even at the very low rates measured in comet Elenin, is potentially large enough to be responsible by driving the nucleus to rotational instability.

IVS: Current Status and Future Plans

NASA Astrophysics Data System (ADS)

Behrend, D.; Nothnagel, A.; Petrachenko, W. T.; Tuccari, G.

2016-12-01

The International VLBI Service for Geodesy and Astrometry (IVS) is a globally operating service that coordinates and performs Very Long Baseline Interferometry (VLBI) activities through its constituent components. The VLBI activities are associated with the creation, provision, dissemination, and archiving of relevant VLBI data and products. The products mostly pertain to the determination of the celestial and terrestrial reference frames, the Earth orientation parameters (EOP), atmospheric parameters as well as other ancillary parameters. The IVS observational network currently consists of about 40 radio telescopes worldwide. Subsets of these telescopes (8-12 stations) participate in 24-hour observing sessions that are run several times per week and in 1-hour intensive sessions for UT1 determination every day. The current VLBI network was developed mainly in the 1970s and 1980s. A number of factors, including aging infrastructure and demanding new scientific requirements, started to challenge its future sustainability and relevance. In response, the IVS and other groups developed and started implementing the next generation VLBI system, called VGOS (VLBI Global Observing System), at existing and new sites. The VGOS network is expected to reach maturity in the early 2020s. We describe the current status, progress, and anticipated prospects of geodetic/astrometric VLBI and the IVS.

VizieR Online Data Catalog: Robo-AO observed cool subdwarf companions (Ziegler+, 2015)

NASA Astrophysics Data System (ADS)

Ziegler, C.; Law, N. M.; Baranec, C.; Riddle, R. L.; Fuchs, J. T.

2017-09-01

We selected targets from the 564 spectral type F- through M-subdwarf candidates studied by Marshall (2007, J/AJ/134/778). These targets were selected from the New Luyten Two-Tenths catalog (NLTT; Luyten, 1979nlcs.book.....L; Luyten & Hughes 1980, Proper-Motion Survey with the Forty-Eight Inch Schmidt Telescope LV First Supplement to the NLTT Catalogue (Minneapolis, MN: Univ. Minnesota Press)) of high proper motion stars (>0.18 arcsec/yr) using a reduced proper motion diagram (RPM). Of the 552 subdwarfs confirmed by Marshall, a randomly selected sample of 348 G-, K-, and M-subdwarfs were observed by Robo-AO when available between other high priority surveys. We obtained high-angular-resolution images of the 348 subdwarfs during 32 separate nights of observations between 2012 September 3 and 2013 August 21 (UT). The observations were performed using the Robo-AO laser adaptive optics system (Riddle et al. 2012SPIE.8447E..2OR; Baranec et al. 2013, J. Visualized Exp. 72 e50021; 2014ApJ...790L...8B) mounted on the Palomar 60 inch telescope. (1 data file).

Glycogen Synthase Kinase-3 Modulates Hyperosmotic-Induced Urea Transporter A1 Relocation in the Inner Medullary Collecting Duct Cells.

PubMed

Li, Yong-Xia; Huang, Yun; Liu, Song; Mao, Yan; Yuan, Cheng-Yan; Yang, Xiao; Yao, Li-Jun

2016-01-01

Glycogen synthase kinase 3 (GSK3) regulates urine concentration by mediating the vasopressin-induced aquaporin 2 expression and water permeability, although it is unknown whether GSK3 also mediates the accumulation of the urea transporter A1 (UT-A1). The aim of this study is to investigate the effect of GSK3 on UT-A1 distribution. Mouse inner medullary collecting duct 3 cells were transfected with UT-A1-GFP construct. The stable transfected cells were cultured under hypertonic conditions, treated with GSK3 inhibitor lithium chloride, GSK3 activator, lysosome or proteasome inhibitor. The expression levels of UT-A1, GSK3, and phospho-GSK3 were analyzed using western blot. The interaction between UT-A1 and the Golgi apparatus was examined using confocal immunofluorescence microscope. The UT-A1 trafficking was examined using the biotinylation of surface membranes. UT-A1 dissociated away from the Golgi apparatus and translocated to the plasma membrane under hypertonic-NaCl and NaCl plus urea stimulation. This movement was accompanied by the increased phosphorylation of GSK3 and its localization on the cellular membrane. Moreover, these results were duplicated by treating the cells with the GSK3 inhibitor, and by contrast, were partially reversed by the GSK3 activator. Treating cells with a lysosome or proteasome inhibitor failed to attenuate the effects of hypertonic stimulus, indicating that the loss of UT-A1 from the Golgi was not due to degradation. Our results suggest that GSK3 may in part modulate the hypertonic-induced intracellular UT-A1 redistribution and its accumulation on the plasma membrane, which may constitute another mechanism by which GSK3 modulates urine concentration. © 2016 S. Karger AG, Basel.

Evidence that one is more likely to see the aurora near Moscow than near Ann Arbor

NASA Astrophysics Data System (ADS)

Liemohn, Michael; Immel, Thomas; Katus, Roxanne

We present a superposed epoch analysis of solar wind drivers and geomagnetic index responses during magnetic storms, categorized as a function of universal time (UT) of the storm peak, to investigate the dependency of storm intensity on UT. Storms with Dst minimum less than - 100 nT were identified in the 1970 - 2012 era (totaling 310 events), covering four solar cycles. The storms were classified into 6 groups based on the UT of the minimum Dst (36 to 82 events per bin), then each grouping was superposed on a timeline that aligns the time of the minimum Dst. Fifteen different quantities were considered, seven solar wind parameters and eight activity indices derived from ground-based magnetometers. Statistical analyses of the superposed means against each other (between the different UT groupings) were conducted to determine the mathematical significance of similarities and differences in the time series plots. It was found that most of the solar wind parameters have essentially no significant difference between the UT groupings, as expected. The exception is solar wind velocity, which appears to be bifurcated into two levels with three of the UT groupings systematically faster than the other three (although, interestingly, not three consecutive UT bins). The geomagnetic activity indices, however, all show statistically significant differences with UT during the main phase and/or early recovery phase. Specifically, the 16, 20, and 00 UT groupings are stronger storms than those in the other UT bins. That is, storms are stronger when the Asian sector is on the nightside (American sector on the dayside) during the main phase. An inference from these findings, therefore, is that one is more likely to see the aurora near Moscow in Russia than near Ann Arbor, Michigan in the United States, even though these two cities have very similar magnetic latitudes (52 degrees).

VizieR Online Data Catalog: MILO. I. HD 7449 radial velocities (Rodigas+, 2016)

NASA Astrophysics Data System (ADS)

Rodigas, T. J.; Arriagada, P.; Faherty, J.; Anglada-Escude, G.; Kaib, N.; Butler, R. P.; Shectman, S.; Weinberger, A.; Males, J. R.; Morzinski, K. M.; Close, L. M.; Hinz, P. M.; Crane, J. D.; Thompson, I.; Teske, J.; Diaz, M.; Minniti, D.; Lopez-Morales, M.; Adams, F. C.; Boss, A. P.

2016-04-01

We observed HD 7449 using the Magellan Clay Telescope at the Las Campanas Observatory in Chile on the nights of UT 2014 November 5 and 22. We observed the star with VisAO at Ys (0.99um) and with Clio-2 at H (1.65um) and Ks (2.15um) on the first night and with VisAO at r' (0.63um), i' (0.77um), z' (0.91um), and with Clio-2 at J (1.1um) on the second night. RV data on HD 7449 were first acquired as part of the Magellan Planet Search Program, which originally made use of the MIKE echelle spectrometer (R~70000 in the blue and ~50000 in the red; wavelength coverage ranges from 3900 to 6200Å) on the Magellan Clay telescope until 2009 September. HD 7449 was subsequently observed using the Carnegie Magellan/PFS (3880-6680Å with R~80000 in the iodine region). We also included in our analysis RVs measured with HARPS and CORALIE. These RVs were originally reported in Dumusque et al. (2011, J/A+A/535/A55). HARPS data on HD 7449 has been supplemented by the ESO archive. See section 2.2 for further explanations. (1 data file).

Science alliance: A vital ORNL-UT partnership

DOE Office of Scientific and Technical Information (OSTI.GOV)

Richmond, C.R.; Riedinger, L.; Garritano, T.

1991-01-01

Partnerships between Department of Energy national laboratories and universities have long been keys to advancing scientific research and education in the United States. Perhaps the most enduring and closely knit of these relationships is the one between Oak Ridge National Laboratory and the University of Tennessee at Knoxville. Since its birth in the 1940's, ORNL has had a very special relationship with UT, and today the two institutions have closer ties than virtually any other university and national laboratory. Seven years ago, ORNL and UT began a new era of cooperation by creating the Science Alliance, a Center of Excellencemore » at UT sponsored by the Tennessee Higher Education Commission. As the oldest and largest of these centers, the Science Alliance is the primary vehicle through which Tennessee promotes research and educational collaboration between UT and ORNL. By letting the two institutions pool their intellectual and financial resources, the alliance creates a more fertile scientific environment than either could achieve on its own. Part of the UT College of Liberal Arts, the Science Alliance is composed of four divisions (Biological Sciences, Chemical Sciences, Physical Sciences, and Mathematics and Computer Science) that team 100 of the university's top faculty with their outstanding colleagues from ORNL.« less

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 new interesting scientific results on the basis of data from ESO telescopes, including several results from the unmatched interferometer mode of the VLT, the VLTI, some of which were highlighted in ESO Press Releases. Certainly worth noting is the possible first ever bona-fide image of an exoplanet and the discovery of the lightest known exoplanet . At the beginning of the year, Paranal welcomed the first Auxiliary Telescope, while on the instrument side as well, 2004 was a good year: we saw the arrival of SINFONI on the VLT, of AMBER on the VLTI, and the installation at the NACO Adaptive Optics instrument of the " Simultaneous Differential Imager (SDI)" to detect exoplanets. And the first prototype of the Astrophysical Virtual Observatory was able to provide unprecedented results on the existence of Type-2 quasars by discovering an entire population of obscured, powerful supermassive black holes. Many of these developments are described in ESO's Press Releases, most with Press Photos, cf. the 2004 PR Index. Some of last year's ESO PR highlights may be accessed directly via the clickable image above.

8. August, 1971. SECOND FLOOR LOOKING NW. EVAPORATOR UNITS USED ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

8. August, 1971. SECOND FLOOR LOOKING NW. EVAPORATOR UNITS USED IN SEQUENCE TO REDUCE OR CONCENTRATE BEET JUICE. - Utah Sugar Company, Garland Beet Sugar Refinery, Factory Street, Garland, Box Elder County, UT

Transient Weakening of Earth's Magnetic Shield Probed by a Cosmic Ray Burst.

PubMed

Mohanty, P K; Arunbabu, K P; Aziz, T; Dugad, S R; Gupta, S K; Hariharan, B; Jagadeesan, P; Jain, A; Morris, S D; Rao, B S; Hayashi, Y; Kawakami, S; Oshima, A; Shibata, S; Raha, S; Subramanian, P; Kojima, H

2016-10-21

The GRAPES-3 tracking muon telescope in Ooty, India measures muon intensity at high cutoff rigidities (15-24 GV) along nine independent directions covering 2.3 sr. The arrival of a coronal mass ejection on 22 June 2015 18:40 UT had triggered a severe G4-class geomagnetic storm (storm). Starting 19:00 UT, the GRAPES-3 muon telescope recorded a 2 h high-energy (∼20  GeV) burst of galactic cosmic rays (GCRs) that was strongly correlated with a 40 nT surge in the interplanetary magnetic field (IMF). Simulations have shown that a large (17×) compression of the IMF to 680 nT, followed by reconnection with the geomagnetic field (GMF) leading to lower cutoff rigidities could generate this burst. Here, 680 nT represents a short-term change in GMF around Earth, averaged over 7 times its volume. The GCRs, due to lowering of cutoff rigidities, were deflected from Earth's day side by ∼210° in longitude, offering a natural explanation of its night-time detection by the GRAPES-3. The simultaneous occurrence of the burst in all nine directions suggests its origin close to Earth. It also indicates a transient weakening of Earth's magnetic shield, and may hold clues for a better understanding of future superstorms that could cripple modern technological infrastructure on Earth, and endanger the lives of the astronauts in space.

High-frequency torsional Alfvén waves as an energy source for coronal heating

PubMed Central

Srivastava, Abhishek Kumar; Shetye, Juie; Murawski, Krzysztof; Doyle, John Gerard; Stangalini, Marco; Scullion, Eamon; Ray, Tom; Wójcik, Dariusz Patryk; Dwivedi, Bhola N.

2017-01-01

The existence of the Sun’s hot atmosphere and the solar wind acceleration continues to be an outstanding problem in solar-astrophysics. Although magnetohydrodynamic (MHD) modes and dissipation of magnetic energy contribute to heating and the mass cycle of the solar atmosphere, yet direct evidence of such processes often generates debate. Ground-based 1-m Swedish Solar Telescope (SST)/CRISP, Hα 6562.8 Å observations reveal, for the first time, the ubiquitous presence of high frequency (~12–42 mHz) torsional motions in thin spicular-type structures in the chromosphere. We detect numerous oscillating flux tubes on 10 June 2014 between 07:17 UT to 08:08 UT in a quiet-Sun field-of-view of 60” × 60” (1” = 725 km). Stringent numerical model shows that these observations resemble torsional Alfvén waves associated with high frequency drivers which contain a huge amount of energy (~105 W m−2) in the chromosphere. Even after partial reflection from the transition region, a significant amount of energy (~103 W m−2) is transferred onto the overlying corona. We find that oscillating tubes serve as substantial sources of Alfvén wave generation that provide sufficient Poynting flux not only to heat the corona but also to originate the supersonic solar wind. PMID:28256538

Design, motivation, and on-sky tests of an efficient fiber coupling unit for 1-meter class telescopes

NASA Astrophysics Data System (ADS)

Bottom, Michael; Muirhead, Philip S.; Swift, Jonathan J.; Zhao, Ming; Gardner, Paul; Plavchan, Peter P.; Riddle, Reed L.; Herzig, Erich; Johnson, John A.; Wright, Jason T.; McCrady, Nate; Wittenmyer, Robert A.

2014-08-01

We present the science motivation, design, and on-sky test data of a high-throughput fiber coupling unit suitable for automated 1-meter class telescopes. The optical and mechanical design of the fiber coupling is detailed and we describe a flexible controller software designed specifically for this unit. The system performance is characterized with a set of numerical simulations, and we present on-sky results that validate the performance of the controller and the expected throughput of the fiber coupling. This unit was designed specifically for the MINERVA array, a robotic observatory consisting of multiple 0.7 m telescopes linked to a single high-resolution stabilized spectrograph for the purpose of exoplanet discovery using high-cadence radial velocimetry. However, this unit could easily be used for general astronomical purposes requiring fiber coupling or precise guiding.

CPO Prediction: Accuracy Assessment and Impact on UT1 Intensive Results

NASA Technical Reports Server (NTRS)

Malkin, Zinovy

2010-01-01

The UT1 Intensive results heavily depend on the celestial pole offset (CPO) model used during data processing. Since accurate CPO values are available with a delay of two to four weeks, CPO predictions are necessarily applied to the UT1 Intensive data analysis, and errors in the predictions can influence the operational UT1 accuracy. In this paper we assess the real accuracy of CPO prediction using the actual IERS and PUL predictions made in 2007-2009. Also, results of operational processing were analyzed to investigate the actual impact of EOP prediction errors on the rapid UT1 results. It was found that the impact of CPO prediction errors is at a level of several microseconds, whereas the impact of the inaccuracy in the polar motion prediction may be about one order of magnitude larger for ultra-rapid UT1 results. The situation can be amended if the IERS Rapid solution will be updated more frequently.

Modulation of kidney urea transporter UT-A3 activity by alpha2,6-sialylation.

PubMed

Qian, Xiaoqian; Sands, Jeff M; Song, Xiang; Chen, Guangping

2016-07-01

Two urea transporters, UT-A1 and UT-A3, are expressed in the kidney terminal inner medullary collecting duct (IMCD) and are important for the production of concentrated urine. UT-A1, as the largest isoform of all UT-A urea transporters, has gained much attention and been extensively studied; however, the role and the regulation of UT-A3 are less explored. In this study, we investigated UT-A3 regulation by glycosylation modification. A site-directed mutagenesis verified a single glycosylation site in UT-A3 at Asn279. Loss of the glycosylation reduced forskolin-stimulated UT-A3 cell membrane expression and urea transport activity. UT-A3 has two glycosylation forms, 45 and 65 kDa. Using sugar-specific binding lectins, the UT-A3 glycosylation profile was examined. The 45-kDa form was pulled down by lectin concanavalin A (Con A) and Galant husnivalis lectin (GNL), indicating an immature glycan with a high amount of mannose (Man), whereas the 65-kDa form is a mature glycan composed of acetylglucosamine (GlcNAc) and poly-N-acetyllactosame (poly-LacNAc) that was pulled down by wheat germ agglutinin (WGA) and tomato lectin, respectively. Interestingly, the mature form of UT-A3 glycan contains significant amounts of sialic acid. We explored the enzymes responsible for directing UT-A3 sialylation. Sialyltransferase ST6GalI, but not ST3GalIV, catabolizes UT-A3 α2,6-sialylation. Activation of protein kinase C (PKC) by PDB treatment promoted UT-A3 glycan sialylation and membrane surface expression. The PKC inhibitor chelerythrine blocks ST6GalI-induced UT-A3 sialylation. Increased sialylation by ST6GalI increased UT-A3 protein stability and urea transport activity. Collectively, our study reveals a novel mechanism of UT-A3 regulation by ST6GalI-mediated sialylation modification that may play an important role in kidney urea reabsorption and the urinary concentrating mechanism.

Data and Tools | Research Site Name | NREL

Science.gov Websites

aliqua. Ut enim ad minim veniam, quis nostrud exercitation ullamco laboris nisi ut aliquip ex ea commodo laboris nisi ut aliquip ex ea commodo consequat. Research Topic 1 Lorem Ipsum Tool 1 Lorem Ipsum Facility

Fifteen Years of Web Based Data Management at Tooele Army Depot

DTIC Science & Technology

2012-03-28

Redding, CA CLTP – Clayton Environmental Consultants, Inc., Pleasanton, CA CTB – Curtis &  Tompkins , Berkeley, CA DCHM – Data Chem, Salt Lake City, UT...Operable Unit 2 - 2005 331 £ David Barker ) Operable Unit 2 - 2006 85 - 18 19 20 21 22 ) Operable Unit 2 - 2007 41 ~ Evin McKinne~ 25 26 27 28 29 1,719...Geophysical Data 42 18 19 20 21 22 23 ) Electronic Data 3,018 £ Angelika Lugo 25~ 27 28 29 30 ) System Management 935 £ David Hill 1 2 3 4 5 6

Polythelia: still a marker of urinary tract anomalies in children?

PubMed

Ferrara, Pietro; Giorgio, Valentina; Vitelli, Ottavio; Gatto, Antonio; Romano, Valerio; Del Bufalo, Francesca; Nicoletti, Alessandro

2009-01-01

Supernumerary nipples (SNN), or polythelia, are the most common form of the accessory mammary tissue malformation. The frequency of this condition ranges from 0.2% to 5.6% depending on various factors. This condition is associated with several anomalies, although this association is often controversial. The aim of this study was to evaluate the association between SNN and kidney/urinary tract (K/UT) anomalies, where anomalies is taken to mean functional disorders, malformations and diseases. A case-control study was performed. The study evaluated 166 children (case group) referred to the Pediatric Nephrology Unit of the Department of Pediatrics of the Catholic University of Rome and 182 children (control group) admitted to the Department of Pediatrics because of pathologies not involving the urinary tract. There were 11 children with SNN in the case group, and only two patients in the control group (6.62% vs 1.09%, p<0.05). The results show a high incidence of K/UT anomalies in children with SNN, and therefore K/UT should be investigated in this specific population.

Orientation and size dependence of the elastic properties of zinc oxide nanobelts

NASA Astrophysics Data System (ADS)

Kulkarni, A. J.; Zhou, M.; Ke, F. J.

2005-12-01

Molecular dynamics simulations are performed to characterize the response of zinc oxide (ZnO) nanobelts to tensile loading. The ultimate tensile strength (UTS) and Young's modulus are obtained as functions of size and growth orientation. Nanobelts in three growth orientations are generated by assembling the unit wurtzite cell along the [0001], [01\\bar {1} 0] , and [2\\bar {1} \\bar {1}0] crystalline axes. Following the geometric construction, dynamic relaxation is carried out to yield free-standing nanobelts at 300 K. Two distinct configurations are observed in the [0001] and [01\\bar {1} 0] orientations. When the lateral dimensions are above 10 Å, nanobelts with rectangular cross-sections are seen. Below this critical size, tubular structures involving two concentric shells similar to double-walled carbon nanotubes are obtained. Quasi-static deformations of belts with [2\\bar {1} \\bar {1} 0] and [01\\bar {1} 0] orientations consist of three stages, including initial elastic stretching, wurtzite-ZnO to graphitic-ZnO structural transformation, and cleavage fracture. On the other hand, [0001] belts do not undergo any structural transformation and fail through cleavage along (0001) planes. Calculations show that the UTS and Young's modulus of the belts are size dependent and are higher than the corresponding values for bulk ZnO. Specifically, as the lateral dimensions increase from 10 to 40 Å, decreases between 38-76% and 24-63% are observed for the UTS and Young's modulus, respectively. This effect is attributed to the size-dependent compressive stress induced by tensile surface stress in the nanobelts. [01\\bar {1} 0] and [2\\bar {1} \\bar {1} 0] nanobelts with multi-walled tubular structures are seen to have higher values of elastic moduli (~340 GPa) and UTS (~36 GPa) compared to their wurtzite counterparts, echoing a similar trend in multi-walled carbon nanotubes.

Detection of optical and X-ray QPOs at similar frequencies in MAXI J1820+070

NASA Astrophysics Data System (ADS)

Yu, Wenfei; Zhang, Jujia; Yan, Zhen; Wang, Xiaofeng; Bai, Jinming

2018-04-01

We report the V-band photometric observation of MAXI J1820+070 (also named ASASSN-18ey, see ATELs #11399, #11400, #11403, #11404, #11406, #11418, #11420, #11421, #11423, #11424, #11425, #11426, #11432, #11437, #11439, #11440, #11445, #11451, #11478, #11481) with the Lijiang 2.4m telescope (+YFOSC) at Lijiang Gaomeigu Station of Yunnan observatories, in comparison with the Swift/XRT observation of MAXI J1820+070 on the same day. Optical photometry observations of the source were performed on March 30th, April 1st, and April 4th. The optical observation from UT 19:53:35 to 20:19:45 on April 1st 2018 is the only observation among three with enough exposure and short frame time to investigate variability on time scales of seconds or longer.

"First Light" Approaches for VLT MELIPAL

NASA Astrophysics Data System (ADS)

2000-01-01

The year 1999 was a very busy one at ESO's Paranal Observatory , the site of the Very Large Telescope (VLT). Soon after the official Inauguration on March 5, 1999, regular observations started with the first 8.2-m VLT Unit Telescope ANTU . During the first nine months of operation (April - December 1999), about 79,000 exposures were made with the FORS1 and ISAAC astronomical instruments at this telescope. Altogether, more than 68 Gigabytes of unique data were gathered during this period for about 200 individual research programmes and stored in the VLT Data Archive. "First Light" was successfully achieved early in the year for the second 8.2-m VLT Unit telescope, KUEYEN . It has since been equipped with two powerful instruments, UVES and FORS2. Science observations with this telescope will start on April 1, 2000. Already in early December 1999, ahead of the schedule, the third 8.2-m Zerodur mirror in its cell was attached to the third 8.2-m VLT Unit Telescope, MELIPAL , cf. ESO PR Photos 42a-ad/99. The moment of "First Light" is approaching for this telescope. Originally planned for mid-February 2000, this significant event is now expected to take place about two weeks ahead of schedule, in late January 2000. From then on, the VLT will possess nearly 160 square metres of extremely accurate, highly reflecting mirror surface. While the observations for "First Light" and the subsequent commissioning period will be carried out with the VLT Test Camera, MELIPAL will receive its first special astronomical instrument, the VIsible MultiObject Spectrograph (VIMOS) towards the middle of the year. It is optimized for large field imaging and spectroscopic surveys and will become a real workhorse of the VLT for this type of research projects, together with the Near InfraRed MultiObject Spectrograph (NIRMOS) , to be installed later at the fourth 8.2-m Unit Telescope, YEPUN . YEPUN will have "First Light" later this year and the work on this telescope also progresses well. The "M1 Dummy" that was mounted on the telescope frame for balance during the mechanical assembly was removed on January 4. The next day, it was transported down to the Base Camp storage area where it was lifted off the Carriage using a combination of two cranes. The empty M1 Carriage was then moved to the Mirror Maintenance Building (MMB) where the fourth M1 Cell with a dummy concrete mirror was loaded. Later that day it was transported up to YEPUN and the next morning (January 6), the Mirror Cell was moved inside the enclosure. Over the next weeks, it will be fitted to the back of the telescope structure. In parallel, the "M2 Unit" on which the 1.1-m secondary mirror of beryllium will later be mounted, is now being assembled in the Integration Laboratory in the MMB. The following digital photos were obtained during the past days and illustrate the recent work.

The Astronomical Almanac Online - Glossary

Science.gov Websites

Astronomical Almanac. Δ A B C D E F G H I J K L M N O P Q R S T U V W X Y Z $\\boldmath{\\Delta {\\rm T}}$: the difference between Terrestrial Time (TT) and Universal Time (UT): $\\Delta {\\rm T} = {\\rm TT} - {\\rm UT}1 $. $\\boldmath{\\Delta {\\rm UT1}}$ (or $\\boldmath{\\Delta {\\rm UT}}$): the value of the difference between

HUBBLE VIEWS DISTANT GALAXIES THROUGH A COSMIC LENS

NASA Technical Reports Server (NTRS)

2002-01-01

Near-infrared image of Jupiter taken in a 2.22 micron filter from the Apache Point Observatory 3.5-meter telescope at 05:35 UT July 19. The G and D impact sites appear in this spectral region of strong methane absorption as image as a single white cloud over 14,000 km in diameter. At higher contrast, the impact regions can be resolved into an intensely bright core about 4,000 km diameter embedded within the larger cloud. Mark Marley and Nancy Chanover, Department of Astronomy, New Mexico State University

Spectroscopic identification of SNe 2004ds and SN 2004dt

NASA Astrophysics Data System (ADS)

Gal-Yam, Avishay

2004-08-01

A. Gal-Yam, D. Fox and S. Kulkarni, California Institute of Technology, report on red spectra (range 550-780 nm) obtained by Kulkarni and Fox on Aug. 13.5 UT at the 10-m Keck I telescope (+ LRIS). The spectrum of of SN 2004ds (IAUC #8386), shows a broad, well-developed P-Cyg H_alpha line and suggests that this is a type II supernova. The spectrum of SN 2004dt (IAUC #8386), shows the distinctive Si II 6100 absorption trough around 6100 Angstrom, indicating this is a young SN Ia.

New disk nova candidate in M 31

NASA Astrophysics Data System (ADS)

Henze, M.; Pietsch, W.; Burwitz, V.; Rodriguez, J.; Bochinski, J.; Busuttil, R.; Haswell, C. A.; Holmes, S.; Kolb, U.

2012-02-01

We report the discovery of a possible nova in the south-western disk of M 31 on a 5x120s dithered stacked CCD image obtained with the Open University PIRATE Planewave CDK17 0.43m Dall-Kirkham f/6.7 telescope at the Observatorio Astronomico de Mallorca (Costitx, Spain), using an SBIG STX 16803 CCD Camera (with a Kodak 4k x 4k chip with 9 microns sq. pixels) and Baader clear filter, on 2012 Feb 15.803 UT with a R magnitude of 17.5 (accuracy of 0.2 mag).

Disappearance of the Supergiant Progenitor of SN 2011dh in M51

NASA Astrophysics Data System (ADS)

Van Dyk, Schuyler D.; Filippenko, Alexei V.; Fox, Ori; Kelly, Patrick; Smith, Nathan

2013-03-01

We report that in Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) observations at F555W and F814W with the UVIS channel, conducted on 2013 March 2 UT as part of our Cycle 20 Snapshot program GO-13029 (PI: A. Filippenko), we have discovered that the yellow supergiant star, identified by Van Dyk et al. (2011, ApJ, 741, L28) and Maund et al. (2011, MNRAS, 739, L37) at the position of the Type IIb SN 2011dh in M51, has vanished.

Fermi/LAT search for counterpart to the IceCube event 67093193 (run 127853)

NASA Astrophysics Data System (ADS)

Vianello, G.; Magill, J. D.; Omodei, N.; Kocevski, D.; Ajello, M.; Buson, S.; Krauss, F.; Chiang, J.

2016-04-01

on behalf of the Fermi-LAT team: We have searched the Fermi Large Area Telescope data for a high-energy gamma-ray counterpart for the IceCube High Energy Starting Event (HESE) 67093193, detected in run 127853 on 2016-04-27 05:52:32.00 UT (AMON GCN notice rev. 2, http://gcn.gsfc.nasa.gov/notices_amon/67093193_127853.amon . See http://gcn.gsfc.nasa.gov/doc/Public_Doc_AMON_IceCube_GCN_Alerts_v2.pdf for a description of HESE events and related GCN notices).

Salt-sparing diuretic action of a water-soluble urea analog inhibitor of urea transporters UT-A and UT-B in rats

PubMed Central

Cil, Onur; Esteva-Font, Cristina; Tas, Sadik Taskin; Su, Tao; Lee, Sujin; Anderson, Marc O.; Ertunc, Mert; Verkman, A. S.

2015-01-01

Inhibitors of kidney urea transporter (UT) proteins have potential use as salt-sparing diuretics (‘urearetics’) with a different mechanism of action than diuretics that target salt transporters. To study UT inhibition in rats, we screened about 10,000 drugs, natural products and urea analogs for inhibition of rat UT-A1. Drug and natural product screening found nicotine, sanguinarine and an indolcarbonylchromenone with IC50 of 10–20 μM. Urea analog screening found methylacetamide and dimethylthiourea (DMTU). DMTU fully and reversibly inhibited rat UT-A1 and UT-B by a noncompetitive mechanism with IC50 of 2–3 mM. Homology modeling and docking computations suggested DMTU binding sites on rat UT-A1. Following a single intraperitoneal injection of 500 mg/kg DMTU, peak plasma concentration was 9 mM with t1/2 of about 10 hours, and a urine concentration of 20–40 mM. Rats chronically treated with DMTU had a sustained, reversible reduction in urine osmolality from 1800 to 600 mOsm, a 3-fold increase in urine output, and mild hypokalemia. DMTU did not impair urinary concentrating function in rats on a low protein diet. Compared to furosemide-treated rats, the DMTU-treated rats had greater diuresis and reduced urinary salt loss. In a model of Syndrome of Inappropriate Antidiuretic Hormone secretion, DMTU treatment prevented hyponatremia and water retention produced by water-loading in dDAVP-treated rats. Thus, our results establish a rat model of UT inhibition and demonstrate the diuretic efficacy of UT inhibition. PMID:25993324

Salt-sparing diuretic action of a water-soluble urea analog inhibitor of urea transporters UT-A and UT-B in rats.

PubMed

Cil, Onur; Esteva-Font, Cristina; Tas, Sadik Taskin; Su, Tao; Lee, Sujin; Anderson, Marc O; Ertunc, Mert; Verkman, Alan S

2015-08-01

Inhibitors of kidney urea transporter (UT) proteins have potential use as salt-sparing diuretics ('urearetics') with a different mechanism of action than diuretics that target salt transporters. To study UT inhibition in rats, we screened about 10,000 drugs, natural products and urea analogs for inhibition of rat UT-A1. Drug and natural product screening found nicotine, sanguinarine and an indolcarbonylchromenone with IC50 of 10-20 μM. Urea analog screening found methylacetamide and dimethylthiourea (DMTU). DMTU fully and reversibly inhibited rat UT-A1 and UT-B by a noncompetitive mechanism with IC50 of 2-3 mM. Homology modeling and docking computations suggested DMTU binding sites on rat UT-A1. Following a single intraperitoneal injection of 500 mg/kg DMTU, peak plasma concentration was 9 mM with t1/2 of about 10 h, and a urine concentration of 20-40 mM. Rats chronically treated with DMTU had a sustained, reversible reduction in urine osmolality from 1800 to 600 mOsm, a 3-fold increase in urine output, and mild hypokalemia. DMTU did not impair urinary concentrating function in rats on a low protein diet. Compared to furosemide-treated rats, the DMTU-treated rats had greater diuresis and reduced urinary salt loss. In a model of syndrome of inappropriate antidiuretic hormone secretion, DMTU treatment prevented hyponatremia and water retention produced by water-loading in dDAVP-treated rats. Thus, our results establish a rat model of UT inhibition and demonstrate the diuretic efficacy of UT inhibition.

Urinary concentrating defect in mice with selective deletion of phloretin-sensitive urea transporters in the renal collecting duct

PubMed Central

Fenton, Robert A.; Chou, Chung-Lin; Stewart, Gavin S.; Smith, Craig P.; Knepper, Mark A.

2004-01-01

To investigate the role of inner medullary collecting duct (IMCD) urea transporters in the renal concentrating mechanism, we deleted 3 kb of the UT-A urea transporter gene containing a single 140-bp exon (exon 10). Deletion of this segment selectively disrupted expression of the two known IMCD isoforms of UT-A, namely UT-A1 and UT-A3, producing UT-A1/3-/- mice. In isolated perfused IMCDs from UT-A1/3-/- mice, there was a complete absence of phloretin-sensitive or vasopressin-stimulated urea transport. On a normal protein intake (20% protein diet), UT-A1/3-/- mice had significantly greater fluid consumption and urine flow and a reduced maximal urinary osmolality relative to wild-type controls. These differences in urinary concentrating capacity were nearly eliminated when urea excretion was decreased by dietary protein restriction (4% by weight), consistent with the 1958 Berliner hypothesis stating that the chief role of IMCD urea transport in the concentrating mechanism is the prevention of urea-induced osmotic diuresis. Analysis of inner medullary tissue after water restriction revealed marked depletion of urea in UT-A1/3-/- mice, confirming the concept that phloretin-sensitive IMCD urea transporters play a central role in medullary urea accumulation. However, there were no significant differences in mean inner medullary Na+ or Cl- concentrations between UT-A1/3-/- mice and wild-type controls, indicating that the processes that concentrate NaCl were intact. Thus, these results do not corroborate the predictions of passive medullary concentrating models stating that NaCl accumulation in the inner medulla depends on rapid vasopressin-regulated urea transport across the IMCD epithelium. PMID:15123796

A stellar occultation by (486958) 2014 MU69: results from the 2017 July 17 portable telescope campaign

NASA Astrophysics Data System (ADS)

Zangari, Amanda Marie; Buie, Marc W.; Stern, S. Alan; Terrell, Dirk; Porter, Simon Bernard; Verbiscer, Anne J.; Soto, Alejandro; Tamblyn, Peter; Benecchi, Susan; Parker, Alex; Wasserman, Lawrence H.; Young, Eliot F.; Skrutskie, Michael F.; New Horizons MU69 Occultation Observing Team

2017-10-01

On 2017 July 17, (486958) 2014 MU69 passed in front of a star as seen from the area north of Comodoro Rivadavia, in Chubut Province, Argentina. Despite challenging wind conditions, twenty two portable telescopes recorded data of the g'= 12.60 mag star in a 45-minute block centered on the predicted midtime of roughly 03:50 UT. Each telescope was spaced approximately 4 km apart in a “picket fence” pattern to target an object as small as 10 km. The picket fence spanned roughly 100 km. Five telescopes observed a solid body occultation.Occultation data provide a unique one-dimensional probe of the 2014 MU69 system that is impossible to achieve from direct imaging. These data will allow for fits of the size and shape of 2014 MU69, and from its derived size, the albedo . The occultation data will also aid in navigation of NASA’s New Horizons spacecraft toward its January 1, 2019 encounter with 2014 MU69.We will detail the July 17 occultation campaign and present analyses of the light curves from each portable station, including occultation timing and constraints on dust and and other objects in the system derived from the occultation baseline data.This work would not have been possible without the financial support of the New Horizons mission and NASA, astrometric support of the Gaia mission and HST, and logistical support from Argentina, CONAE and specifically Comodoro Rivadavia as well as assistance from the US Embassy in Buenos Aires.

Outbursting comet P/2010 V1 (Ikeya-Murakami): A miniature comet Holmes

DOE Office of Scientific and Technical Information (OSTI.GOV)

Ishiguro, Masateru; Jewitt, David; Hanayama, Hidekazu

2014-05-20

The short-period comet P/2010 V1 (Ikeya-Murakami, hereafter {sup V}1{sup )} was discovered visually by two amateur astronomers. The appearance of the comet was peculiar, consisting of an envelope, a spherical coma near the nucleus and a tail extending in the anti-solar direction. We investigated the brightness and the morphological development of the comet by taking optical images with ground-based telescopes. Our observations show that V1 experienced a large-scale explosion between UT 2010 October 31 and November 3. The color of the comet was consistent with the Sun (g' – R {sub C} = 0.61 ± 0.20, R {sub C} –more » I {sub C} = 0.20 ± 0.20, and B – R {sub C} = 0.93 ± 0.25), suggesting that dust particles were responsible for the brightening. We used a dynamical model to understand the peculiar morphology, and found that the envelope consisted of small grains (0.3-1 μm) expanding at a maximum speed of 500 ± 40 m s{sup –1}, while the tail and coma were composed of a wider range of dust particle sizes (0.4-570 μm) and expansion speeds 7-390 m s{sup –1}. The total mass of ejecta is ∼5 × 10{sup 8} kg and kinetic energy ∼5 × 10{sup 12} J. These values are much smaller than in the historic outburst of 17P/Holmes in 2007, but the energy per unit mass (1 × 10{sup 4} J kg{sup –1}) is comparable. The energy per unit mass is about 10% of the energy released during the crystallization of amorphous water ice suggesting that crystallization of buried amorphous ice can supply the mass and energy of the outburst ejecta.« less

The Use of Daily Geodetic UT1 and LOD Data in the Optimal Estimation of UT1 and LOD With the JPL Kalman Earth Orientation Filter

NASA Technical Reports Server (NTRS)

Freedman, A. P.; Steppe, J. A.

1995-01-01

The Jet Propulsion Laboratory Kalman Earth Orientation Filter (KEOF) uses several of the Earth rotation data sets available to generate optimally interpolated UT1 and LOD series to support spacecraft navigation. This paper compares use of various data sets within KEOF.

Emergence of late-onset placental dysfunction: relationship to the change in uterine artery blood flow resistance between the first and third trimesters.

PubMed

Llurba, Elisa; Turan, Ozhan; Kasdaglis, Tania; Harman, Chris R; Baschat, Ahmet A

2013-06-01

To test if emergence of third-trimester (T3) placental dysfunction is related to the impedance change in uterine artery blood flow resistance between the first trimester (T1) and T3. Mean T1 and T3 uterine artery (mUtA) pulsatility index (PI) was measured in 1098 singletons. Each patient's individual mUtA-PI change was calculated ([(T3 PI - T1 PI/interval in days)] × 100; ΔmUtA-PI). This parameter and T1 and T3 mUtA-PI z-scores were related to placenta-related disease (PRD) and to constitutionally small neonates (CS). Forty-seven (5%) women had PRD and 83 (8.7%) delivered a CS neonate. T1 and T3 mUtA-PI z-scores were higher with PRD (0.418 versus -0.097 and 1.06 versus -0.13, p < 0.001 for all). Change in mUtA-PI (ΔmUtA PI) was similar for patients with PRD. However, the prevalence of PRD doubled with rising ΔmUtA-PI (11.1% versus 5.2%, p = 0.041). T3 uterine artery Doppler performs significantly better in detecting patients at risk for late-onset PRD than T1 or the gestational age change in uterine artery Doppler resistance This suggests that a proportion of late emerging PRD is not amenable to early screening by uterine artery Doppler. Further research is essential to identify the optimal screening strategy for late-onset placental dysfunction. Thieme Medical Publishers 333 Seventh Avenue, New York, NY 10001, USA.

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 Year of Astronomy 2009. 100HA is on track to be the largest single science public outreach event ever, with more than 1500 events registered in over 130 countries. 100HA will take place over four days and nights, from 2-5 April 2009. It is a worldwide celebration composed of a broad range of activities aimed at involving the public. During this period, people from around the globe will share the experience and wonder of observing the sky. For many, it will be their first glimpse of the marvels of the heavens through a telescope. For others, it is the perfect opportunity to impart their knowledge and excitement, helping unveil the cosmos to fresh and eager eyes. Astronomers at ESO are also organising local public events near their headquarters in Garching, near Munich. In the Munich city centre, ESO astronomers, together with colleagues from the Excellence Cluster Universe, will share their views of the cosmos with members of the public. ESO in Chile is also participating in a series of events to celebrate the 100 Hours of Astronomy. In Antofagasta, an exhibition by international and local astrophotographers will be unveiled at the main mall in the city. Star parties will be organised for the public in the desert outside Antofagasta, in coordination with the local university UCN. In Santiago, ESO is offering, along with other international observatories and the Chilean astronomical community, a complete set of programmes, including public talks, night observations and interactive exhibitions. In San Pedro de Atacama, the ALMA project will install an inflatable planetarium for the local community, and astronomy workshops and star parties will be offered to the public. More information ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe. It is supported by 14 countries: Austria, Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO plays also a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in the Atacama Desert region of Chile: La Silla, Paranal and Chajnantor. The vision of the IYA2009 is to help the citizens of the world rediscover their place in the Universe through the day and night-time skies the impact of astronomy and basic sciences on our daily lives, and understand better how scientific knowledge can contribute to a more equitable and peaceful society. Ustream.TV is the live interactive video broadcast platform that enables anyone with a camera and an internet connection to quickly and easily broadcast to a global audience of unlimited size. In less than two minutes, anyone can become a broadcaster by creating their own channel on Ustream or by broadcasting through their own site, empowering them to engage with their audience and further build their brand.

Transition-Region/Coronal Signatures of Penumbral Microjets: Hi-C, SDO/AIA and Hinode (SOT/FG) Observations

NASA Technical Reports Server (NTRS)

Tiwari, Sanjiv K.; Alpert, Shane E.; Moore, Ronald L.; Winebarger, Amy R.

2014-01-01

Penumbral microjets are bright, transient features seen in the chromosphere of sunspot penumbrae. Katsuaka et al. (2007) noted their ubiquity and characterized them using the Ca II H-line filter on Hinode's Solar Optical Telescope (SOT). The jets are 1000{4000 km in length, 300{400 km in width, and last less than one minute. It was proposed that these penumbral microjets could contribute to the transition-region and coronal heating above sunspots. We examine whether these microjets appear in the transition-region (TR) and/or corona or are related{ temporally and spatially{ to similar brightenings in the TR and/or corona. First, we identify penumbral microjets with the SOT's Ca II H-line filter. The chosen sunspot is observed on July 11, 2012 from 18:50:00 UT to 20:00:00 UT at approx. 14 inches, -30 inches. We then examine the sunspot in the same field of view and at the same time in other wavelengths. We use the High Resolution Coronal Imager Telescope (Hi-C) at 193A and the 1600A, 304A, 171A, 193A, and 94A passbands of the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamic Observatory. We include examples of these jets and where they should appear in the other passbands, but find no signifcant association, except for a few jets with longer lifetimes and bigger sizes seen at locations in the penumbra with repeated stronger brightenings. We conclude that the normal microjets are not heated to transition-region/coronal temperatures, but the larger jets are.

DISAPPEARANCE OF COMET C/2010 X1 (ELENIN): GONE WITH A WHIMPER, NOT A BANG

DOE Office of Scientific and Technical Information (OSTI.GOV)

Li, Jing; Jewitt, David, E-mail: jli@igpp.ucla.edu

We examine the rise and sudden demise of comet C/2010 X1 (Elenin) on its approach to perihelion. Discovered inbound at 4.2 AU, this long-period comet was predicted to become very bright when near perihelion, at 0.48 AU on 2011 September 10. Observations starting 2011 February (heliocentric distance ∼3.5 AU) indeed show the comet to brighten by about 11 mag, with most of the increase occurring inside 1 AU from the Sun. The peak brightness reached m{sub R} = 6 on UT 2011 August 12.95 ± 0.50, when at ∼0.83 AU from the Sun. Thereafter, the comet faded even as themore » heliocentric distance continued to decrease. We find that most of the surge in brightness in mid-August resulted from dust-particle forward scattering, not from a sudden increase in the activity. A much smaller (∼3 mag) brightening began on UT 2011 August 18 ± 1 (heliocentric distance 0.74 AU), reached a maximum on UT 2011 August 30 ± 1 (at 0.56 AU), and reflects the true breakup of the nucleus. This second peak was matched by a change in the morphology from centrally condensed to diffuse. The estimated cross section of the nucleus when at 1 AU inbound was ∼1 km{sup 2}, corresponding to an equal-area circle of radius 0.6 km. Observations were taken after the second peak using the Canada–France–Hawaii 3.6 m telescope to search for surviving fragments of the nucleus. None were found to a limiting red magnitude r′ = 24.4, corresponding to radii ≲40 m (red geometric albedo = 0.04 assumed). The brightening, the progressive elongation of the debris cloud, and the absence of a central condensation in data taken after UT 2011 August 30 are consistent with disintegration of the nucleus into a power law size distribution of fragments with index q = 3.3 ± 0.2 combined with the action of radiation pressure. In such a distribution, the largest particles contain most of the mass while the smallest particles dominate the scattering cross section and apparent brightness. We speculate about physical processes that might cause nucleus disruption in a comet when still 0.7 AU from the Sun. Tidal stresses and devolatilization of the nucleus by sublimation are both negligible at this distance. However, the torque caused by mass loss, even at the very low rates measured in comet Elenin, is potentially large enough to be responsible by driving the nucleus to rotational instability.« less

The Hale-Bopp comet - an unexpected guest

NASA Astrophysics Data System (ADS)

Gorodetchi, Dumitru

A number of 3 photographs are given of the comewt Hale-Bopp made at UT 1997 March 18.0937 (refractor RT-80(80 cm., 1:10); Fomapan T-800 (DT=10 min). 2) UT 1997 March 18.010; Cassegrain-reflector AT -400 (630, 1:16); film 100 ASA (DT=1 min) 3)UT 1997 April 5.8097; telobiectiv Tair -11 (13,5 cm, 1:2.8); Fomapan T-800 (DT =2 min)

Diuresis and reduced urinary osmolality in rats produced by small-molecule UT-A-selective urea transport inhibitors.

PubMed

Esteva-Font, Cristina; Cil, Onur; Phuan, Puay-Wah; Su, Tao; Lee, Sujin; Anderson, Marc O; Verkman, A S

2014-09-01

Urea transport (UT) proteins of the UT-A class are expressed in epithelial cells in kidney tubules, where they are required for the formation of a concentrated urine by countercurrent multiplication. Here, using a recently developed high-throughput assay to identify UT-A inhibitors, a screen of 50,000 synthetic small molecules identified UT-A inhibitors of aryl-thiazole, γ-sultambenzosulfonamide, aminocarbonitrile butene, and 4-isoxazolamide chemical classes. Structure-activity analysis identified compounds that inhibited UT-A selectively by a noncompetitive mechanism with IC50 down to ∼1 μM. Molecular modeling identified putative inhibitor binding sites on rat UT-A. To test compound efficacy in rats, formulations and administration procedures were established to give therapeutic inhibitor concentrations in blood and urine. We found that intravenous administration of an indole thiazole or a γ-sultambenzosulfonamide at 20 mg/kg increased urine output by 3-5-fold and reduced urine osmolality by ∼2-fold compared to vehicle control rats, even under conditions of maximum antidiuresis produced by 1-deamino-8-D-arginine vasopressin (DDAVP). The diuresis was reversible and showed urea > salt excretion. The results provide proof of concept for the diuretic action of UT-A-selective inhibitors. UT-A inhibitors are first in their class salt-sparing diuretics with potential clinical indications in volume-overload edemas and high-vasopressin-associated hyponatremias. © FASEB.

Hypoxia-Inducible Factor Pathway Inhibition Resolves Tumor Hypoxia and Improves Local Tumor Control After Single-Dose Irradiation

DOE Office of Scientific and Technical Information (OSTI.GOV)

Helbig, Linda; Department of Radiation Oncology, University Hospital Carl Gustav Carus, Technische Universität Dresden, Dresden; Koi, Lydia

2014-01-01

Purpose: To study the effects of BAY-84-7296, a novel orally bioavailable inhibitor of mitochondrial complex I and hypoxia-inducible factor 1 (HIF-1) activity, on hypoxia, microenvironment, and radiation response of tumors. Methods and Materials: UT-SCC-5 and UT-SCC-14 human squamous cell carcinomas were transplanted subcutaneously in nude mice. When tumors reached 4 mm in diameter BAY-84-7296 (Bayer Pharma AG) or carrier was daily administered to the animals. At 7 mm tumors were either excised for Western blot and immunohistologic investigations or were irradiated with single doses. After irradiation animals were randomized to receive BAY-84-7296 maintenance or carrier. Local tumor control was evaluatedmore » 150 days after irradiation, and the dose to control 50% of tumors (TCD{sub 50}) was calculated. Results: BAY-84-7296 decreased nuclear HIF-1α expression. Daily administration of inhibitor for approximately 2 weeks resulted in a marked decrease of pimonidazole hypoxic fraction in UT-SCC-5 (0.5% vs 21%, P<.0001) and in UT-SCC-14 (0.3% vs 19%, P<.0001). This decrease was accompanied by a significant increase in fraction of perfused vessels in UT-SCC-14 but not in UT-SCC-5. Bromodeoxyuridine and Ki67 labeling indices were significantly reduced only in UT-SCC-5. No significant changes were observed in vascular area or necrosis. BAY-84-7296 before single-dose irradiation significantly decreased TCD{sub 50}, with an enhancement ratio of 1.37 (95% confidence interval [CI] 1.13-1.72) in UT-SCC-5 and of 1.55 (95% CI 1.26-1.94) in UT-SCC-14. BAY-84-7296 maintenance after irradiation did not further decrease TCD{sub 50}. Conclusions: BAY-84-7296 resulted in a marked decrease in tumor hypoxia and substantially reduced radioresistance of tumor cells with the capacity to cause a local recurrence after irradiation. The data suggest that reduction of cellular hypoxia tolerance by BAY-84-7296 may represent the primary biological mechanism underlying the observed enhancement of radiation response. Whether this mechanism contributes to the improved outcome of fractionated chemoradiation therapy warrants further investigation.« less

IM Nor monitoring requested for HST COS observations

NASA Astrophysics Data System (ADS)

Waagen, Elizabeth O.

2017-02-01

Dr. Ed Sion (Villanova University) and colleagues have requested AAVSO observers' assistance in monitoring the symbiotic-type recurrent nova IM Nor in support of observations with the Hubble Space Telescope Cosmic Origins Spectrograph scheduled for 2017 February 13 - 17 UT. These observations are part of a study on short orbital period recurrent novae as Supernovae Type Ia progenitors. It is essential to know 24 hours prior to the HST COS observations that IM Nor is not in outburst, in order to protect the instrumentation. Also, photometry is needed throughout the HST window to insure knowledge of the brightness of the system. Observers are asked to monitor IM Nor with nightly snapshot images (V preferred) from now through February 20, and to report their observations promptly. It will be especially important to know the brightness of IM Nor each night through February 17 UT. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Observations should be submitted to the AAVSO International Database. See full Alert Notice for more details.

Rejuvenation of a ten-year old AO curvature sensor: combining obsolescence correction and performance upgrade of MACAO

NASA Astrophysics Data System (ADS)

Haguenauer, P.; Fedrigo, E.; Pettazzi, L.; Reinero, C.; Gonte, F.; Pallanca, L.; Frahm, R.; Woillez, J.; Lilley, P.

2016-07-01

The MACAO curvature wavefront sensors have been designed as a generic adaptive optics sensor for the Very Large Telescope. Six systems have been manufactured and implemented on sky: four installed in the UTs Coudé train as an AO facility for the VLTI, and two in UT's instruments, SINFONI and CRIRES. The MACAO-VLTI have now been in use for scientific operation for more than a decade and are planned to be operated for at least ten more years. As second generation instruments for the VLTI were planned to start implementation in end of 2015, accompanied with a major upgrade of the VLTI infrastructure, we saw it as a good time for a rejuvenation project of these systems, correcting the obsolete components. This obsolescence correction also gave us the opportunity to implement improved capabilities: the correction frequency was pushed from 420 Hz to 1050 Hz, and an automatic vibrations compensation algorithm was added. The implementation on the first MACAO was done in October 2014 and the first phase of obsolescence correction was completed in all four MACAO-VLTI systems in October 2015 with the systems delivered back to operation. The resuming of the scientific operation of the VLTI on the UTs in November 2015 allowed to gather statistics in order to evaluate the improvement of the performances through this upgrade. A second phase of obsolescence correction has now been started, together with a global reflection on possible further improvements to secure observations with the VLTI.

Optical low-dispersion spectroscopic observations of Comet 103P/Hartley 2 at Koyama Astronomical Observatory during the EPOXI flyby

NASA Astrophysics Data System (ADS)

Shinnaka, Yoshiharu; Kawakita, Hideyo; Kobayashi, Hitomi; Naka, Chiharu; Arai, Akira; Arasaki, Takayuki; Kitao, Eiji; Taguchi, Gaku; Ikeda, Yuji

2013-02-01

We performed low-dispersion spectroscopic observations of Comet 103P/Hartley 2 in optical wavelengths using the LOSA/F2 mounted on the 1.3 m-Araki telescope at Koyama Astronomical Observatory on UT 2010 November 4 during the close approach of the Deep Impact spacecraft to the nucleus of Comet 103P/Hartley 2 in the EPOXI mission flyby. Our observations have revealed the chemistry of the coma at optical wavelengths; including CN, C3, C2 and NH2 along with H2O from [OI] emission at 6300 Å. Resultant mixing ratios of these radicals put the comet into the normal group in chemical composition. The mixing ratios with respect to H2O obtained in our observations are basically consistent with the previous optical spectro-photometric observations of Comet 103P/Hartley 2 in 1991 by A'Hearn et al. (A'Hearn, M.F., Millis, R.L., Schleicher, D.G., Osip, D.J., Birch, P.V. [1995]. Icarus 118, 223-270), the optical spectroscopic observations in 1998 by Fink (Fink, U. [2009]. Icarus 201, 311-334) and also consistent with the observations on UT 2010 October 27 and 29 by Lara et al. (Lara, L.M., Lin, Z.-Y., Meech, K. [2011]. Astron. Astrophys. 532, A87) (but only for the ratio relative to CN).

New Observatory at the University of Tennessee at Martin

NASA Astrophysics Data System (ADS)

Crews, Lionel J.; Chrysler, R.; Turner, K.

2010-01-01

A new observatory has been completed at the University of Tennessee at Martin and is now open for student research, local teacher training, and public outreach. The telescope is a 16" Meade RCT on a Software Bisque Paramount ME mount, 10' HomeDome, and SBIG CCD camera. The project endured many delays from a necessary change in housing from roll-top roof to dome, to the shutter blowing off in a heavy windstorm. This project was funded primarily by a Tennessee Math-Science Partnership grant (PI: Dr. Michael Gibson, UT Martin) directed at secondary teacher training in sciences.

EVN e-VLBI detections of MAXI J1659-152

NASA Astrophysics Data System (ADS)

Paragi, Z.; van der Horst, A. J.; Granot, J.; Taylor, G. B.; Kouveliotou, C.; Garrett, M. A.; Wijers, R. A. M. J.; Ramirez-Ruiz, E.; Kuulkers, E.; Gehrels, N.; Woods, P. M.

2010-10-01

We observed MAXI J1659-152 (Negoro et al. 2010, ATel #2873; Mangano et al. 2010, GCN #11296) following its sub-millimeter and centimeter radio detections (de Ugarte Postigo et al. 2010, GCN #11304; van der Horst et al. 2010, ATel #2874) with the European VLBI Network (EVN) in real-time e-VLBI mode on 30 September 2010, from 13:30 to 18:30 UT at 4.9 GHz. The participating telescopes were Cambridge, Effelsberg, Jodrell Bank (MkII), Hartebeesthoek, Medicina, Onsala, Torun and Westerbork sending data at a rate of ~1024 Mbps to the EVN Data Processor at JIVE.

Urea transporter UT-B deletion induces DNA damage and apoptosis in mouse bladder urothelium.

PubMed

Dong, Zixun; Ran, Jianhua; Zhou, Hong; Chen, Jihui; Lei, Tianluo; Wang, Weiling; Sun, Yi; Lin, Guiting; Bankir, Lise; Yang, Baoxue

2013-01-01

Previous studies found that urea transporter UT-B is abundantly expressed in bladder urothelium. However, the dynamic role of UT-B in bladder urothelial cells remains unclear. The objective of this study is to evaluate the physiological roles of UT-B in bladder urothelium using UT-B knockout mouse model and T24 cell line. Urea and NO measurement, mRNA expression micro-array analysis, light and transmission electron microscopy, apoptosis assays, DNA damage and repair determination, and intracellular signaling examination were performed in UT-B null bladders vs wild-type bladders and in vitro T24 epithelial cells. UT-B was highly expressed in mouse bladder urothelium. The genes, Dcaf11, MCM2-4, Uch-L1, Bnip3 and 45 S pre rRNA, related to DNA damage and apoptosis were significantly regulated in UT-B null urothelium. DNA damage and apoptosis highly occurred in UT-B null urothelium. Urea and NO levels were significantly higher in UT-B null urothelium than that in wild-type, which may affect L-arginine metabolism and the intracellular signals related to DNA damage and apoptosis. These findings were consistent with the in vitro study in T24 cells that, after urea loading, exhibited cell cycle delay and apoptosis. UT-B may play an important role in protecting bladder urothelium by balancing intracellular urea concentration. Disruption of UT-B function induces DNA damage and apoptosis in bladder, which can result in bladder disorders.

Urea Transporter UT-B Deletion Induces DNA Damage and Apoptosis in Mouse Bladder Urothelium

PubMed Central

Zhou, Hong; Chen, Jihui; Lei, Tianluo; Wang, Weiling; Sun, Yi; Lin, Guiting; Bankir, Lise; Yang, Baoxue

2013-01-01

Background Previous studies found that urea transporter UT-B is abundantly expressed in bladder urothelium. However, the dynamic role of UT-B in bladder urothelial cells remains unclear. The objective of this study is to evaluate the physiological roles of UT-B in bladder urothelium using UT-B knockout mouse model and T24 cell line. Methodology/Principal Findings Urea and NO measurement, mRNA expression micro-array analysis, light and transmission electron microscopy, apoptosis assays, DNA damage and repair determination, and intracellular signaling examination were performed in UT-B null bladders vs wild-type bladders and in vitro T24 epithelial cells. UT-B was highly expressed in mouse bladder urothelium. The genes, Dcaf11, MCM2-4, Uch-L1, Bnip3 and 45 S pre rRNA, related to DNA damage and apoptosis were significantly regulated in UT-B null urothelium. DNA damage and apoptosis highly occurred in UT-B null urothelium. Urea and NO levels were significantly higher in UT-B null urothelium than that in wild-type, which may affect L-arginine metabolism and the intracellular signals related to DNA damage and apoptosis. These findings were consistent with the in vitro study in T24 cells that, after urea loading, exhibited cell cycle delay and apoptosis. Conclusions/Significance UT-B may play an important role in protecting bladder urothelium by balancing intracellular urea concentration. Disruption of UT-B function induces DNA damage and apoptosis in bladder, which can result in bladder disorders. PMID:24204711

Space Shuttle Projects

NASA Image and Video Library

1989-11-27

The primary payload for Space Shuttle Mission STS-35, launched December 2, 1990, was the ASTRO-1 Observatory. Designed for round the clock observation of the celestial sphere in ultraviolet and X-ray astronomy, ASTRO-1 featured a collection of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo- Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-ray Telescope (BBXRT). Ultraviolet telescopes mounted on Spacelab elements in cargo bay were to be operated in shifts by flight crew. Loss of both data display units (used for pointing telescopes and operating experiments) during mission impacted crew-aiming procedures and forced ground teams at Marshall Space Flight Center to aim ultraviolet telescopes with fine-tuning by flight crew. BBXRT, also mounted in cargo bay, was directed from outset by ground-based operators at Goddard Space Flight Center. This is the logo or emblem that was designed to represent the ASTRO-1 payload.

Understanding U.S. Strategy: A Reader,

DTIC Science & Technology

1983-01-01

Originally intended asa means of prevntlng Sp nihandPr tuguee 1 :1 In the Western Hemisphre after de ~t of bap~’ Frac, the Monroe Doctrine evtually...goals ntm de isel broso sasatttnololes ss ut Ivet ay lmso keh undes1rabl rases at th npatioa evel6_ heae t o nffigswltthepIOwllO o - neorA - w att leg...surreptitiously (which could easily go undiscov- ered by the United States), and abrogated the treaty in de facto fashion by using its space weaponry at the

Performance of the Finnish Diabetes Risk Score and a Simplified Finnish Diabetes Risk Score in a Community-Based, Cross-Sectional Programme for Screening of Undiagnosed Type 2 Diabetes Mellitus and Dysglycaemia in Madrid, Spain: The SPREDIA-2 Study.

PubMed

Salinero-Fort, M A; Burgos-Lunar, C; Lahoz, C; Mostaza, J M; Abánades-Herranz, J C; Laguna-Cuesta, F; Estirado-de Cabo, E; García-Iglesias, F; González-Alegre, T; Fernández-Puntero, B; Montesano-Sánchez, L; Vicent-López, D; Cornejo-Del Río, V; Fernández-García, P J; Sánchez-Arroyo, V; Sabín-Rodríguez, C; López-López, S; Patrón-Barandio, P; Gómez-Campelo, P

2016-01-01

To evaluate the performance of the Finnish Diabetes Risk Score (FINDRISC) and a simplified FINDRISC score (MADRISC) in screening for undiagnosed type 2 diabetes mellitus (UT2DM) and dysglycaemia. A population-based, cross-sectional, descriptive study was carried out with participants with UT2DM, ranged between 45-74 years and lived in two districts in the north of metropolitan Madrid (Spain). The FINDRISC and MADRISC scores were evaluated using the area under the receiver operating characteristic curve method (ROC-AUC). Four different gold standards were used for UT2DM and any dysglycaemia, as follows: fasting plasma glucose (FPG), oral glucose tolerance test (OGTT), HbA1c, and OGTT or HbA1c. Dysglycaemia and UT2DM were defined according to American Diabetes Association criteria. The study population comprised 1,426 participants (832 females and 594 males) with a mean age of 62 years (SD = 6.1). When HbA1c or OGTT criteria were used, the prevalence of UT2DM was 7.4% (10.4% in men and 5.2% in women; p<0.01) and the FINDRISC ROC-AUC for UT2DM was 0.72 (95% CI, 0.69-0.74). The optimal cut-off point was ≥13 (sensitivity = 63.8%, specificity = 65.1%). The ROC-AUC of MADRISC was 0.76 (95% CI, 0.72-0.81) with ≥13 as the optimal cut-off point (sensitivity = 84.8%, specificity = 54.6%). FINDRISC score ≥12 for detecting any dysglycaemia offered the best cut-off point when HbA1c alone or OGTT and HbA1c were the criteria used. FINDRISC proved to be a useful instrument in screening for dysglycaemia and UT2DM. In the screening of UT2DM, the simplified MADRISC performed as well as FINDRISC.

Generation and phenotypic analysis of mice lacking all urea transporters.

PubMed

Jiang, Tao; Li, Yingjie; Layton, Anita T; Wang, Weiling; Sun, Yi; Li, Min; Zhou, Hong; Yang, Baoxue

2017-02-01

Urea transporters (UT) are a family of transmembrane urea-selective channel proteins expressed in multiple tissues and play an important role in the urine concentrating mechanism of the mammalian kidney. UT inhibitors have diuretic activity and could be developed as novel diuretics. To determine if functional deficiency of all UTs in all tissues causes physiological abnormality, we established a novel mouse model in which all UTs were knocked out by deleting an 87 kb of DNA fragment containing most parts of Slc14a1 and Slc14a2 genes. Western blot analysis and immunofluorescence confirmed that there is no expression of urea transporter in these all-UT-knockout mice. Daily urine output was nearly 3.5-fold higher, with significantly lower urine osmolality in all-UT-knockout mice than that in wild-type mice. All-UT-knockout mice were not able to increase urinary urea concentration and osmolality after water deprivation, acute urea loading, or high protein intake. A computational model that simulated UT-knockout mouse models identified the individual contribution of each UT in urine concentrating mechanism. Knocking out all UTs also decreased the blood pressure and promoted the maturation of the male reproductive system. Thus, functional deficiency of all UTs caused a urea-selective urine-concentrating defect with little physiological abnormality in extrarenal organs. Copyright © 2016 International Society of Nephrology. Published by Elsevier Inc. All rights reserved.

Generation and phenotypic analysis of mice lacking all urea transporters

PubMed Central

Jiang, Tao; Li, Yingjie; Layton, Anita T.; Wang, Weiling; Sun, Yi; Li, Min; Zhou, Hong; Yang, Baoxue

2017-01-01

Urea transporters (UT) are a family of transmembrane urea-selective channel proteins expressed in multiple tissues and play an important role in the urine concentrating mechanism of the mammalian kidney. UT inhibitors have been identified to have diuretic activity and might be developed as novel diuretics. To determine if functional deficiency of all UTs in all tissues causes physiological abnormality, we established a novel mouse model in which all UTs were knocked out by deleting an 87 kb of DNA fragment containing most parts of Slc14a1 and Slc14a2 genes. Western blot analysis and immunofluorescence confirmed that there is no expression of urea transporter in all-UT-knockout mice. Daily urine output was nearly 3.5-fold higher, with significantly lower urine osmolality, in all-UT-knockout-mice than that in wild-type mice, and urine osmolality was significantly lower. All-UT-knockout mice were not able to increase urinary urea concentration and osmolality after water deprivation, acute urea loading or high protein intake. A computational model that simulated UT knockout mouse models identified the individual contribution of each UT in urine concentrating mechanism. Knocking out all UTs also decreased the blood pressure and promoted the maturation of the male reproductive system. These results revealed that functional deficiency of all UTs caused urea selective urine concentrating defect with little physiological abnormality in extrarenal organs. PMID:27914708

A photometric study of the hot exoplanet WASP-19b

NASA Astrophysics Data System (ADS)

Lendl, M.; Gillon, M.; Queloz, D.; Alonso, R.; Fumel, A.; Jehin, E.; Naef, D.

2013-04-01

Context. The sample of hot Jupiters that have been studied in great detail is still growing. In particular, when the planet transits its host star, it is possible to measure the planetary radius and the planet mass (with radial velocity data). For the study of planetary atmospheres, it is essential to obtain transit and occultation measurements at multiple wavelengths. Aims: We aim to characterize the transiting hot Jupiter WASP-19b by deriving accurate and precise planetary parameters from a dedicated observing campaign of transits and occultations. Methods: We have obtained a total of 14 transit lightcurves in the r'-Gunn, I-Cousins, z'-Gunn, and I + z' filters and 10 occultation lightcurves in z'-Gunn using EulerCam on the Euler-Swiss telescope and TRAPPIST. We also obtained one lightcurve through the narrow-band NB1190 filter of HAWK-I on the VLT measuring an occultation at 1.19 μm. We performed a global MCMC analysis of all new data, together with some archive data in order to refine the planetary parameters and to measure the occultation depths in z'-band and at 1.19 μm. Results: We measure a planetary radius of Rp = 1.376 ± 0.046 RJ, a planetary mass of Mp = 1.165 ± 0.068 MJ, and find a very low eccentricity of e = 0.0077-0.0032+0.0068, compatible with a circular orbit. We have detected the z'-band occultation at 3σ significance and measure it to be δFocc,z' = 352 ± 116 ppm, more than a factor of 2 smaller than previously published. The occultation at 1.19 μm is only marginally constrained at δFocc,NB1190 = 1711-726+745 ppm. Conclusions: We show that the detection of occultations in the visible range is within reach, even for 1 m class telescopes if a considerable number of individual events are observed. Our results suggest an oxygen-dominated atmosphere of WASP-19b, making the planet an interesting test case for oxygen-rich planets without temperature inversion. Based on photometric observations made with HAWK-I on the ESO VLT/UT4 (Prog. ID 084.C-0532), EulerCam on the Euler-Swiss telescope and the Belgian TRAPPIST telescope, as well as archive data from the Faulkes South Telescope, CORALIE on the Euler-Swiss telescope, HARPS on the ESO 3.6 m telescope (Prog. ID 084-C-0185), and HAWK-I (Prog. ID 083.C-0377(A)).The photometric time series data in this work are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/552/A2

Studying the evolution of a type III radio from the Sun up to 1 AU

NASA Astrophysics Data System (ADS)

Mann, Gottfried; Breitling, Frank; Vocks, Christian; Fallows, Richard; Melnik, Valentin; Konovalenko, Alexander

2017-04-01

On March 16, 2016, a type III burst was observed with the ground-based radio telescopes LOFAR and URAN-2 as well as with the radiospectrometer aboard the spacecraft WIND.It started at 80 MHz at 06:37 UT and reached 50 kHz after 23 minutes. A type III burst are considered as the radio signature of an electron beam travelling from the corona into the interplanetary space. The energetic electrons carrying the beam excites Langmuir waves, which convert into radio waves by wave-particle interaction. The relationship between the drift rate and the frequency as derived from the dynamic radio spectra reveals that the velocity of the electrons generating the radio waves of the type III burst is increasing with increasing distance from the center of the Sun.

ESPRESSO: projecting a rocky exoplanet hunter for the VLT

NASA Astrophysics Data System (ADS)

Mégevand, Denis; Herreros, José-Miguel; Zerbi, Filippo; Cabral, Alexandre; Di Marcantonio, Paolo; Lovis, Christophe; Pepe, Francesco; Cristiani, Stefano; Rebolo, Rafael; Santos, Nuno C.

2010-07-01

ESPRESSO is a high-resolution, highly stable spectrograph for the VLT. It will inherit and enhance most capabilities from HARPS and UVES, combining both stability and efficiency. The main science driver will be the detection and characterization of Earth-like planets, but many additional science cases will benefit from its highly stable spectroscopic observations. The facility will be installed at the combined Coudé focus of the VLT and may be linked with any of the four UT telescopes, enabling thus a great flexibility for the efficient use of telescope time. This particularity makes the interface with the VLT more complex than for an instrument fed by a single telescope. It impacts on the complexity of the relationship between the consortium providing the instrument and ESO, the customer. The targeted high RV accuracy requires very high performances in stability and resolution, which in turn require adequate technical solutions at several levels. This paper describes the instrument system and subsystems, enlightening the most valuable differences between ESPRESSO and it's predecessors, the details of the project, entering now the design phases, the ESPRESSO consortium, composed of Italian, Portuguese, Spanish and Swiss institutes, and the relationship between the consortium and ESO.

A Weak Solar Burst Submillimeter Only Spectral Component During a GOES M Class Flare: Implications for its Emission Mechanisms

NASA Astrophysics Data System (ADS)

Cristiani, G. D.; Giménez de Castro, C. G.; Mandrini, C. H.; et al.

2008-09-01

Since the installation of the Submillimeter Solar Radio Telescope, a new spectral burst component was discovered at frequencies above 100 GHz, creating the THz bursts category. In all the reported cases, the events were X class flares and the THz component was increasing with frequency. We report for the first time an M class flare which shows a submillimeter radio spectral component different from the one in microwave classical bursts. Two successive flares of 2 minute duration occurred in active region NOAA 10226 with 2 minutes delay. They started at around 13:15 UT and had an M 6.8 maximum intensity in soft X-rays. The submillimeter flux density from the Solar Submillimeter Telescope (SST) is used in addition to microwave total Sun patrol telescope observations. Images with H filters from the H-alpha Solar Telescope for Argentina (HASTA) and in the extreme UV from the Extreme-ultraviolet Imaging Telescope (EIT) are used to characterize the flaring region. An extensive analysis of the magnetic topology evolution is derived from Michelson Doppler Imager (MDI) magnetograms and used to constrain the space of solutions for the possible emission mechanisms. The submillimeter component is observed at 212 GHz only. We have upper limits for the emission at 89.4and 405 GHz which are smaller than the observed flux density at 212 GHz. The analysis of the magnetic topology reveals a very compact and complex system of arches that reconnects at a low height, while from the soft X-ray observations we deduce that the flaring area is compact and dense (n=1e12 cm-3). The finding of a submillimeter only burst component in a medium size flare indicates that the phenomenon is more universal than shown until now. The multiwavelength analysis reveals that neither positron synchrotron nor free-free emission could produce the submillimeter component, which is explained here by synchrotron of accelerated electrons in a rather complex and compact magnetic configuration.

A university system's approach to enhancing the educational mission of health science schools and institutions: the University of Texas Academy of Health Science Education

PubMed Central

Buja, L. Maximilian; Cox, Susan M.; Lieberman, Steven A.; MacClements, Jonathan; Williams, Janet F.; Esterl, Robert M.; Shine, Kenneth I.

2013-01-01

Background The academy movement developed in the United States as an important approach to enhance the educational mission and facilitate the recognition and work of educators at medical schools and health science institutions. Objectives Academies initially formed at individual medical schools. Educators and leaders in The University of Texas System (the UT System, UTS) recognized the academy movement as a means both to address special challenges and pursue opportunities for advancing the educational mission of academic health sciences institutions. Methods The UTS academy process was started by the appointment of a Chancellor's Health Fellow for Education in 2004. Subsequently, the University of Texas Academy of Health Science Education (UTAHSE) was formed by bringing together esteemed faculty educators from the six UTS health science institutions. Results Currently, the UTAHSE has 132 voting members who were selected through a rigorous, system-wide peer review and who represent multiple professional backgrounds and all six campuses. With support from the UTS, the UTAHSE has developed and sustained an annual Innovations in Health Science Education conference, a small grants program and an Innovations in Health Science Education Award, among other UTS health science educational activities. The UTAHSE represents one university system's innovative approach to enhancing its educational mission through multi- and interdisciplinary as well as inter-institutional collaboration. Conclusions The UTAHSE is presented as a model for the development of other consortia-type academies that could involve several components of a university system or coalitions of several institutions. PMID:23490406

Stinging Nettle (Urtica dioica L.) Attenuates FFA Induced Ceramide Accumulation in 3T3-L1 Adipocytes in an Adiponectin Dependent Manner.

PubMed

Obanda, Diana N; Zhao, Peng; Richard, Allison J; Ribnicky, David; Cefalu, William T; Stephens, Jacqueline M

2016-01-01

Excess dietary lipids result in the accumulation of lipid metabolites including ceramides that can attenuate insulin signaling. There is evidence that a botanical extract of Urtica dioica L. (stinging nettle) improves insulin action, yet the precise mechanism(s) are not known. Hence, we examined the effects of Urtica dioica L. (UT) on adipocytes. We investigated the effects of an ethanolic extract of UT on free fatty acid (palmitic acid) induced inhibition of insulin-stimulated Akt serine phosphorylation and modulation of ceramidase expression in 3T3-L1 adipocytes. Adipocytes were exposed to excess FFAs in the presence or absence of UT. Effects on adiponectin expression, ceramidase expression, ceramidase activity, ceramide accumulation and insulin signaling were determined. As expected, FFAs reduced adiponectin expression and increased the expression of ceramidase enzymes but not their activity. FFA also induced the accumulation of ceramides and reduced insulin-stimulated phosphorylation of Akt in adipocytes. The effects of FFA were partially reversed by UT. UT enhanced adiponectin expression and ceramidase activity in the presence of excess FFAs. UT abated ceramide accumulation and increased insulin sensitivity via enhanced Akt phosphorylation. A siRNA knockdown of adiponectin expression prevented UT from exerting positive effects on ceramidase activity but not Akt phosphorylation. In adipocytes, the ability of UT to antagonize the negative effects of FFA by modulating ceramidase activity and ceramide accumulation is dependent on the presence of adiponectin. However, the ability of UT to enhance Akt phosphorylation is independent of adiponectin expression. These studies demonstrate direct effects of UT on adipocytes and suggest this botanical extract is metabolically beneficial.

Stinging Nettle (Urtica dioica L.) Attenuates FFA Induced Ceramide Accumulation in 3T3-L1 Adipocytes in an Adiponectin Dependent Manner

PubMed Central

Obanda, Diana N.; Zhao, Peng; Richard, Allison J.; Ribnicky, David; Cefalu, William T.; Stephens, Jacqueline M.

2016-01-01

Objective Excess dietary lipids result in the accumulation of lipid metabolites including ceramides that can attenuate insulin signaling. There is evidence that a botanical extract of Urtica dioica L. (stinging nettle) improves insulin action, yet the precise mechanism(s) are not known. Hence, we examined the effects of Urtica dioica L. (UT) on adipocytes. Research Design We investigated the effects of an ethanolic extract of UT on free fatty acid (palmitic acid) induced inhibition of insulin-stimulated Akt serine phosphorylation and modulation of ceramidase expression in 3T3-L1 adipocytes. Adipocytes were exposed to excess FFAs in the presence or absence of UT. Effects on adiponectin expression, ceramidase expression, ceramidase activity, ceramide accumulation and insulin signaling were determined. Results As expected, FFAs reduced adiponectin expression and increased the expression of ceramidase enzymes but not their activity. FFA also induced the accumulation of ceramides and reduced insulin-stimulated phosphorylation of Akt in adipocytes. The effects of FFA were partially reversed by UT. UT enhanced adiponectin expression and ceramidase activity in the presence of excess FFAs. UT abated ceramide accumulation and increased insulin sensitivity via enhanced Akt phosphorylation. A siRNA knockdown of adiponectin expression prevented UT from exerting positive effects on ceramidase activity but not Akt phosphorylation. Conclusions In adipocytes, the ability of UT to antagonize the negative effects of FFA by modulating ceramidase activity and ceramide accumulation is dependent on the presence of adiponectin. However, the ability of UT to enhance Akt phosphorylation is independent of adiponectin expression. These studies demonstrate direct effects of UT on adipocytes and suggest this botanical extract is metabolically beneficial. PMID:26939068

The UT-A Urea Transporter Promoter, UT-Aα, Targets Principal Cells of the Renal Inner Medullary Collecting Duct

PubMed Central

Fenton, Robert A.; Shodeinde, Adetola; Knepper, Mark A.

2006-01-01

The urea transporters, UT-A1 and UT-A3, two members of the UT-A gene family, are localized to the terminal portion of the inner medullary collecting duct (IMCD). In this manuscript, we demonstrate that 4.2-kb of the 5′-flanking region of the UT-A gene (UT-Aα promoter) is sufficient to drive the IMCD-specific expression of a heterologous reporter gene, β-galactosidase (β-Gal), in transgenic mice. RT-PCR, immunoblotting and immunohistochemistry demonstrate that within the kidney, transgene expression is confined to the terminal portion of the IMCD. Co-localization studies with aquaporin 2 show that expression is localized to the principal cells of the IMCD2 and IMCD3 regions. Utilizing β-Gal activity assays, we further show that within the kidney, the β-Gal transgene can be regulated by both water restriction and glucocorticoids, similar to the regulation of the endogenous UT-A gene. These results demonstrate that 4.2-kb of the UT-Aα promoter is sufficient to drive expression of a heterologous reporter gene in a tissue-specific and cell-specific fashion in transgenic mice PMID:16091580

A Comprehensive Study on the Internet of Underwater Things: Applications, Challenges, and Channel Models †

PubMed Central

Wu, Geng-De; Huang, Chun-Ju

2017-01-01

The Internet of Underwater Things (IoUT) is a novel class of Internet of Things (IoT), and is defined as the network of smart interconnected underwater objects. IoUT is expected to enable various practical applications, such as environmental monitoring, underwater exploration, and disaster prevention. With these applications, IoUT is regarded as one of the potential technologies toward developing smart cities. To support the concept of IoUT, Underwater Wireless Sensor Networks (UWSNs) have emerged as a promising network system. UWSNs are different from the traditional Territorial Wireless Sensor Networks (TWSNs), and have several unique properties, such as long propagation delay, narrow bandwidth, and low reliability. These unique properties would be great challenges for IoUT. In this paper, we provide a comprehensive study of IoUT, and the main contributions of this paper are threefold: (1) we introduce and classify the practical underwater applications that can highlight the importance of IoUT; (2) we point out the differences between UWSNs and traditional TWSNs, and these differences are the main challenges for IoUT; and (3) we investigate and evaluate the channel models, which are the technical core for designing reliable communication protocols on IoUT. PMID:28640220

A Comprehensive Study on the Internet of Underwater Things: Applications, Challenges, and Channel Models.

PubMed

Kao, Chien-Chi; Lin, Yi-Shan; Wu, Geng-De; Huang, Chun-Ju

2017-06-22

The Internet of Underwater Things (IoUT) is a novel class of Internet of Things (IoT), and is defined as the network of smart interconnected underwater objects. IoUT is expected to enable various practical applications, such as environmental monitoring, underwater exploration, and disaster prevention. With these applications, IoUT is regarded as one of the potential technologies toward developing smart cities. To support the concept of IoUT, Underwater Wireless Sensor Networks (UWSNs) have emerged as a promising network system. UWSNs are different from the traditional Territorial Wireless Sensor Networks (TWSNs), and have several unique properties, such as long propagation delay, narrow bandwidth, and low reliability. These unique properties would be great challenges for IoUT. In this paper, we provide a comprehensive study of IoUT, and the main contributions of this paper are threefold: (1) we introduce and classify the practical underwater applications that can highlight the importance of IoUT; (2) we point out the differences between UWSNs and traditional TWSNs, and these differences are the main challenges for IoUT; and (3) we investigate and evaluate the channel models, which are the technical core for designing reliable communication protocols on IoUT.

Erythropoietin Receptor Signaling Is Membrane Raft Dependent

PubMed Central

McGraw, Kathy L.; Fuhler, Gwenny M.; Johnson, Joseph O.; Clark, Justine A.; Caceres, Gisela C.; Sokol, Lubomir; List, Alan F.

2012-01-01

Upon erythropoietin (Epo) engagement, Epo-receptor (R) homodimerizes to activate JAK2 and Lyn, which phosphorylate STAT5. Although recent investigations have identified key negative regulators of Epo-R signaling, little is known about the role of membrane localization in controlling receptor signal fidelity. Here we show a critical role for membrane raft (MR) microdomains in creation of discrete signaling platforms essential for Epo-R signaling. Treatment of UT7 cells with Epo induced MR assembly and coalescence. Confocal microscopy showed that raft aggregates significantly increased after Epo stimulation (mean, 4.3±1.4(SE) vs. 25.6±3.2 aggregates/cell; p≤0.001), accompanied by a >3-fold increase in cluster size (p≤0.001). Raft fraction immunoblotting showed Epo-R translocation to MR after Epo stimulation and was confirmed by fluorescence microscopy in Epo stimulated UT7 cells and primary erythroid bursts. Receptor recruitment into MR was accompanied by incorporation of JAK2, Lyn, and STAT5 and their activated forms. Raft disruption by cholesterol depletion extinguished Epo induced Jak2, STAT5, Akt and MAPK phosphorylation in UT7 cells and erythroid progenitors. Furthermore, inhibition of the Rho GTPases Rac1 or RhoA blocked receptor recruitment into raft fractions, indicating a role for these GTPases in receptor trafficking. These data establish a critical role for MR in recruitment and assembly of Epo-R and signal intermediates into discrete membrane signaling units. PMID:22509308

KIC 8462852 optical dipping event

NASA Astrophysics Data System (ADS)

Waagen, Elizabeth O.

2017-05-01

T. Boyajian (Louisiana State University) et al. reported in ATel #10405 that an optical dip is underway in KIC 8462852 (Boyajian's Star, Tabby's Star) beginning on 2017 May 18 UT. Tentative signs of small dips had been seen beginning April 24, and enhanced monitoring had begun at once at Fairborn Observatory (Tennessee State University). Photometry and spectroscopy from there on May 18 and 19 UT showed a dip underway. Cousins V photometry showed a drop of 0.02 magnitude, the largest dip (and the first clear one) seen in more than a year of monitoring. AAVSO observer Bruce Gary (GBL, Hereford, AZ) carried out V photometry which showed a fading from 11.906 V ± 0.004 to 11.9244 V ± 0.0033 between UT 2017 May 14 and May 19, a drop of 1.7%. Swift/UVOT observations obtained May 18 15:19 did not show a statistically significant drop in v, but Gary's photometry is given more weight. r'-band observations from Las Cumbres Observatory obtained 2017 May 17 to May 19 showed a 2% dip. Spectra by I. Steele (Liverpool JMU) et al. taken on 2017 May 20 with the 2.0 meter Liverpool Telescope, La Palma, showed no differences in the source compared to a reference spectrum taken 2016 July 4 when the system was not undergoing a dip (ATel #10406).Dips typically last for a few days, and larger dips can last over a week. It is not clear that this dip is over. Precision time-series V photometry is urgently requested from AAVSO observers, although all photometry is welcome. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). See full Alert Notice for more details. KIC 8462852 was the subject of AAVSO Alert Notices 532 and 542. See also Boyajian et al. 2016, also available as a preprint (http://arxiv.org/abs/1509.03622). General information about KIC 8462852 may be found at http://www.wherestheflux.com/.

VizieR Online Data Catalog: Imaging and spectroscopy in Lynx W (Jorgensen+, 2014)

NASA Astrophysics Data System (ADS)

Jorgensen, I.; Chiboucas, K.; Toft, S.; Bergmann, M.; Zirm, A.; Schiavon, R. P.; Grutzbauch, R.

2017-01-01

Ground-based imaging of RX J0848.6+4453 was obtained primarily to show the performance gain provided by replacing the original E2V charge-coupled devices (E2V CCDs) in Gemini Multi-Object Spectrograph on Gemini North (GMOS-N) with E2V Deep Depletion CCDs (E2V DD CCDs). This replacement was done in 2011 October. Imaging of RX J0848.6+4453 was obtained with the original E2V CCDs in 2011 October (UT 2011 Oct 1 to 2011 Oct 2; Program ID: GN-2011B-DD-3) and repeated with the E2V DD CCDs in 2011 November. The imaging was done in the z' filter. For the observations with the original E2V CCDs the total exposure time was 60 minutes (obtained as 12 five-minute exposures) and the co-added image had an image quality of FWHM=0.52'' measured from point sources in the field. For the E2V DD CCDs a total exposure time of 55 minutes was obtained and the resulting image quality was FWHM=0.51''. Imaging of RX J0848.6+4453 was also obtained with Hubble Space Telescope /Advanced Camera for Surveys (HST/ACS using the filters F775W and F850LP) under the program ID 9919. The spectroscopic observations were obtained in multi-object spectroscopic (MOS) mode with GMOS-N (UT 2011 Nov 24 to 2012 Jan 4, Program ID: GN-2011B-DD-5; UT 2013 Mar 9 to 2013 May 18, Program ID: GN-2013A-Q-65). Table10 lists the photometric parameters for the spectroscopic sample as derived from the HST/ACS observations in F850LP and F775W. Tables 11 and 12 list the results from the template fitting and the derived line strengths, respectively. (3 data files).

Eradicating Organized Criminal Gangs in Jamaica: Can Lessons be Learnt From a Successful Counterinsurgency

DTIC Science & Technology

2008-01-01

34’Sa’tanrrlCl-I’o • ;S0.t..rUt 1\\1ar ,,’ FrankJ’ield" !I; E’ort Antoa"io ~*I~$~’ ’~t:.;:;: "::f;i’I’,":; . ’.. ......... [ilu’c’ 7" IOt ;.s:uc/i’ CaL"es...dissemination), Crime Management Unit, Fraud Squad, Forensic Laboratory, Bureau of Special Investigation, Canine Division, Protective Services, and the National

Interpretation of NO and OH Emission from 1976 Airborne Measurements,

DTIC Science & Technology

1979-01-01

Development. .~\\ . 0.. ’ ~1 AIR FORCE GEOPHYSICS LABORATORY AIR FORCE SYSTEMS COMMAND UNITED STATES AIR FORCE UANSCOM APE , MASSACHUSETTS 01731 79 09 17 ...INGSCHEDULE 16. DISTRIBUTION STATEMENT (of tAle R.port) Approved for public release , distribution unlimited 17 . DISTRIBUTION STATEMENT (of iS. abet,act .nt...for March 7, 1976 from 1000 to 1030 UT, and processed 2.94 pm data with the OH background removed 17 Figure 5. Measured 39l4~ , 2.94 pm , and 1.7 pm

Status and Prospects for Combined GPS LOD and VLBI UT1 Measurements

NASA Astrophysics Data System (ADS)

Senior, K.; Kouba, J.; Ray, J.

2010-01-01

A Kalman filter was developed to combine VLBI estimates of UT1-TAI with biased length of day (LOD) estimates from GPS. The VLBI results are the analyses of the NASA Goddard Space Flight Center group from 24-hr multi-station observing sessions several times per week and the nearly daily 1-hr single-baseline sessions. Daily GPS LOD estimates from the International GNSS Service (IGS) are combined with the VLBI UT1-TAI by modeling the natural excitation of LOD as the integral of a white noise process (i.e., as a random walk) and the UT1 variations as the integration of LOD, similar to the method described by Morabito et al. (1988). To account for GPS technique errors, which express themselves mostly as temporally correlated biases in the LOD measurements, a Gauss-Markov model has been added to assimilate the IGS data, together with a fortnightly sinusoidal term to capture errors in the IGS treatments of tidal effects. Evaluated against independent atmospheric and oceanic axial angular momentum (AAM + OAM) excitations and compared to other UT1/LOD combinations, ours performs best overall in terms of lowest RMS residual and highest correlation with (AAM + OAM) over sliding intervals down to 3 d. The IERS 05C04 and Bulletin A combinations show strong high-frequency smoothing and other problems. Until modified, the JPL SPACE series suffered in the high frequencies from not including any GPS-based LODs. We find, surprisingly, that further improvements are possible in the Kalman filter combination by selective rejection of some VLBI data. The best combined results are obtained by excluding all the 1-hr single-baseline UT1 data as well as those 24-hr UT1 measurements with formal errors greater than 5 μs (about 18% of the multi-baseline sessions). A rescaling of the VLBI formal errors, rather than rejection, was not an effective strategy. These results suggest that the UT1 errors of the 1-hr and weaker 24-hr VLBI sessions are non-Gaussian and more heterogeneous than expected, possibly due to the diversity of observing geometries used, other neglected systematic effects, or to the much shorter observational averaging interval of the single-baseline sessions. UT1 prediction services could benefit from better handling of VLBI inputs together with proper assimilation of IGS LOD products, including using the Ultra-rapid series that is updated four times daily with 15 hr delay.

A prospective randomized comparison of unsedated ultrathin versus standard esophagogastroduodenoscopy in routine outpatient gastroenterology practice: does it work better through the nose?

PubMed

Birkner, B; Fritz, N; Schatke, W; Hasford, J

2003-08-01

In an outpatient gastroenterological practice setting, highly effective diagnostic procedures and patient satisfaction play an important role. Ultrathin endoscopy in unsedated patients has been shown to be more cost-effective and time-efficient in comparison with standard endoscopy. A prospective randomized study was carried out in unsedated patients to compare performance, feasibility, safety, and patient tolerance between ultrathin transnasal (UT), ultrathin oral (UO), and standard (SO) esophagogastroduodenoscopy (EGD). A total of 200 of 600 eligible patients consented to participate in the study, and were randomly assigned to undergo UT, UO, or SO. Patients reported their tolerance of the procedure (anxiety, pain, gagging, and overall satisfaction; Likert scale 1-10), and the endoscopists reported the effectiveness of the procedure (handling, picture quality, and overall performance; Likert scale 1-10). Statistics were calculated using the Kruskal-Wallis test. After randomization, 65, 67, and 68 patients were allocated to the UT, UO, and SO groups, respectively. Failure to achieve complete EGD by the intended route occurred in 14 patients (22 %) in the UT group. Compared to the SO group, patients in the UT and UO groups rated anxiety before the procedure as being more intense - median score (10 % quantile estimate; 90 % quantile estimate): UT, 2.0 (1.0; 4.0); UO, 2.0 (1.0; 4.0); SO, 0.0 (0.0; 2.0); p < 0.0001), whereas SO patients experienced a higher level of anxiety during the procedure ( P < 0.0001). Pain during insertion of the endoscope was the least intense in the UO group: UT, 2.0 (1.0; 5.0); UO, 1.0 (1.0; 3.0); SO, 2.0 (1.0; 4.0); P < 0.001). Gagging during insertion was more pronounced in the UO group: UT, 2.0 (1.0; 4.0); UO, 3.0 (1.0; 7.0); SO, 2.0 (1.0; 5.0); P < 0.01). The patients' score for the overall assessment was better in the SO group ( P < 0.0001). The endoscopists' overall assessment for ultrathin EGD was poorer than for standard EGD: UT, 3.0 (2.0; 5.0); UO, 3.0 (2.0; 5.0); SO, 2.0 (1.0; 3.0); P < 0.0001). Ultrathin endoscopy through both the transnasal and oral routes has limited use in routine outpatient practice. Techniques for reducing pain and gagging may improve patient tolerance. Further technical improvements are needed to allow routine implementation.

UKIRT observer's manual

NASA Astrophysics Data System (ADS)

Davies, J. K.

1991-04-01

The United Kingdom 3.8 m Infrared Telescope (UKIRT) located at the summit of Mauna Kea on the big island of Hawaii is described. Summit sky conditions are photometric more than half the time and spectroscopic more than three quarters of the time. Photometry through all atmospheric windows in the 1 to 30 micrometer range and spectroscopy in the 1 to 5 micrometer range are possible. The telescope is equipped with a 1 to 5 micrometer infrared camera housing a 58 by 62 element detector array. Other individual instruments and aspects of operation at the telescope are described.

Improved UT1 Predictions through Low-Latency VLBI Observations

DTIC Science & Technology

2010-03-14

J Geod (2010) 84:399–402 DOI 10.1007/s00190-010-0372-8 SHORT NOTE Improved UT1 predictions through low-latency VLBI observations Brian Luzum · Axel...polar motion and nutation on UT1 determinations from VLBI Intensive obser- vations. J Geod 82(12):863. doi:10.1007/s00190-008-0212-2 Ray JR, Carter WE...Behrend D (2007) The International VLBI Service for Geodesy and Astrometry (IVS): current capabilities and future prospects. J Geod 81(6–8):479. doi

Contrast Threshold of Lunar Crescents Visibility for Ramadan and Syawal 1431 H at Bosscha Observatory

NASA Astrophysics Data System (ADS)

Arumaningtyas, E. P.; Raharto, M.

2010-12-01

In this paper we present the prediction of the first lunar crescent visibility using contrast based on Schaefer's model and best time proposed by [12] for the beginning of Ramadhan and Syawal 1431 H at observing place in Bosscha Observatory, [E 107° 36.96', S 6° 49.55', with elevation of 1310 meters above sea level]. The geocentric altitude of the Moon at the sunset time on August 10 is 1° 58.98' and illuminated fraction of crescent (FI) = 0.20%. On August 11, 2010 the altitude of the Moon at the sunset time is 15° 42.71' and FI = 2.57%. The calculated contrast on August 10, 2010 is less than zero. It means that the brightness of the moon is smaller than brightness of the sky. Based on the contrast value, it is impossible to observe the lunar crescent by the naked eye at that time, even equipped by special design telescope for the crescent observation at Bosscha Observatory. Sultan [11] proposed a predicted model it is still possible to observe the very young lunar crescent even under circumstance before the time of sunset, if the contrast of sky is perfect. On August 11, 2010 contrast has its maximum at 50 minutes after sunset. The result of observation of the lunar crescent at Bosscha Observatory, the crescent could be seen before sunset at 17.15 local time (UT+7 hours) using special design telescope with additional nose of 1 meter length [6]. The model used here is tend to predict the brightness for naked eye observation, which less contrast compare to observation with the well design telescope.

VizieR Online Data Catalog: Very metal-poor stars in the Milky Way's halo (Carollo+, 2014)

NASA Astrophysics Data System (ADS)

Carollo, D.; Freeman, K.; Beers, T. C.; Placco, V. M.; Tumlinson, J.; Martell, S. L.

2017-07-01

The Aoki et al. (2013, J/AJ/145/13) sample comprises 137 stars observed at high spectral resolution (R~30000), in the course of four observing runs between 2008 March and October, using the High Dispersion Spectrograph (Noguchi et al. 2002PASJ...54..855N) at the Subaru Telescope. We also include 190 stars from the Yong et al. (2013, J/ApJ/762/26) sample - the 38 stars from their "program sample," and 152 stars in their literature compilation. High-resolution spectra (22000

The afocal telescope of the ESA ARIEL mission: analysis of the layout

NASA Astrophysics Data System (ADS)

Da Deppo, Vania; Middleton, Kevin; Focardi, Mauro; Morgante, Gianluca; Corso, Alain Jody; Pace, Emanuele; Claudi, Riccardo; Micela, Giuseppina

2017-09-01

ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) is one of the three present candidates as an M4 ESA mission to be launched in 2026. During its foreseen 3.5 years operation, it will observe spectroscopically in the infrared a large population of known transiting planets in the neighborhood of the Solar System. The aim is to enable a deep understanding of the physics and chemistry of these exoplanets. ARIEL is based on a 1-m class telescope ahead of a suite of instruments: two spectrometer channels covering the band 1.95 to 7.8 μm and four photometric channels (two wide and two narrow band) in the range 0.5 to 1.9 μm. The ARIEL optical design is conceived as a fore-module common afocal telescope that will feed the spectrometer and photometric channels. The telescope optical design is based on an eccentric pupil two-mirror classic Cassegrain configuration coupled to a tertiary paraboloidal mirror. The temperature of the primary mirror (M1) will be monitored and finely tuned by means of an active thermal control system based on thermistors and heaters. They will be switched on and off to maintain the M1 temperature within ±1 K thanks to a proportional-integral-derivative (PID) controller implemented within the Telescope Control Unit (TCU), a Payload electronics subsystem mainly in charge of the active thermal control of the two detectors owning to the spectrometer. TCU will collect the housekeeping data of the controlled subsystems and will forward them to the spacecraft (S/C) by means of the Instrument Control Unit (ICU), the main Payload's electronic Unit linked to the S/C On Board Computer (OBC).

Antigenic and functional properties of the human red blood cell urea transporter hUT-B1.

PubMed

Lucien, Nicole; Sidoux-Walter, Frédéric; Roudier, Nathalie; Ripoche, Pierre; Huet, Martine; Trinh-Trang-Tan, Marie-Marcelle; Cartron, Jean-Pierre; Bailly, Pascal

2002-09-13

The Kidd (JK) blood group locus encodes the urea transporter hUT-B1, which is expressed on human red blood cells and other tissues. The common JK*A/JK*B blood group polymorphism is caused by a single nucleotide transition G838A changing Asp-280 to Asn-280 on the polypeptide, and transfection of erythroleukemic K562 cells with hUT-B1 cDNAs carrying either the G838 or the A838 nucleotide substitutions resulted in the isolation of stable clones that expressed the Jk(a) or Jk(b) antigens, respectively, thus providing the first direct demonstration that the hUT-B1 gene encodes the Kidd blood group antigens. In addition, immunochemical analysis of red blood cells demonstrated that hUT-B1 also exhibits ABO determinants attached to the single N-linked sugar chain at Asn-211. Moreover, immunoadsorption studies, using inside-out and right-side-out red cell membrane vesicles as competing antigen, demonstrated that the C- and N-terminal ends of hUT-B1 are oriented intracellularly. Mutagenesis and functional studies by expression in Xenopus oocytes revealed that both cysteines Cys-25 and Cys-30 (but not alone) are essential for plasma membrane addressing. Conversely, the transport function was not affected by the JK*A/JK*B polymorphism, C-terminal deletion (residues 360-389), or mutation of the extracellular N-glycosylation consensus site and remains poorly para-chloromercuribenzene sulfonate (pCMBS)-sensitive. However, transport studies by stopped flow light scattering using Jk-K562 transfectants demonstrated that the hUT-B1-mediated urea transport is pCMBS-sensitive in an erythroid context, as reported previously for the transporter of human red blood cells. Mutagenesis analysis also indicated that Cys-151 and Cys-236, at least alone, are not involved in pCMBS inhibition. Altogether, these antigenic, topologic, and functional properties might have implications into the physiology of hUT-B1 and other members of the urea transporter family.

Four Eyes Are Better

NASA Astrophysics Data System (ADS)

2002-09-01

VLT Interferometer Passes Another Technical Hurdle Summary During the nights of September 15/16 and 16/17, 2002, preliminary tests were successfully carried out during which the light beams from all four VLT 8.2-m Unit Telescopes (UTs) at the ESO Paranal Observatory were successively combined, two by two, to produce interferometric fringes . This marks a next important step towards the full implementation of the VLT Interferometer (VLTI) that will ultimately provide European astronomers with unequalled opportunities for exciting front-line research projects. It is no simple matter to ensure that the quartet of ANTU, KUEYEN, MELIPAL and YEPUN , each a massive giant with a suite of computer-controlled active mirrors, can work together by sending beams of light towards a common focal point via a complex system of compensating optics. Yet, in the span of only two nights, the four VLT telescopes were successfully "paired" to do exactly this, yielding a first tantalizing glimpse of the future possibilities with this new science machine. While there is still a long way ahead to the routine production of extremely sharp, interferometric images, the present test observations have allowed to demonstrate directly the 2D-resolution capacity of the VLTI by means of multiple measurements of a distant star. Much valuable experience was gained during those two nights and the ESO engineers and scientists are optimistic that the extensive test observations with the numerous components of the VLTI will continue to progress rapidly. Five intense, technical test periods are scheduled during the next six months; some of these with the Mid-Infrared interferometric instrument for the VLTI (MIDI) which will soon be installed at Paranal. Later in 2003, the first of the four moveable VLTI 1.8-m Auxiliary Telescopes (ATs) will be put in place on the top of the mountain; together they will permit regular interferometric observations, also without having to use the large UTs. PR Photo 22a/02 : Delay Lines in the Interferometric Tunnel. PR Photo 22b/02 : Baselines and "Interferometric PSF" from observations of the star Achernar . Combining the VLT telescopes ESO PR Photo 22a/02 ESO PR Photo 22a/02 [Preview - JPEG: 503 x 400 pix - 81k] [Normal - JPEG: 1005 x 800 pix - 488k] [Hi-Res - JPEG: 3000 x 2389 pix - 2.8M] Caption : PR Photo 22a/02 : VLT Delay Lines in the Interferometric Tunnel. Less than one year after the first combination of two 8.2-m VLT telescopes - described in detail in ESO Press Release 23/01 - successful tests have now been carried out, during which all of the four telescopes were combined pairwise in rapid succession . Of the six combinations possible (ANTU-KUEYEN, ANTU-MELIPAL, ANTU-YEPUN, KUEYEN-MELIPAL, KUEYEN-YEPUN and MELIPAL-YEPUN), only the last one could not be used, because of the current geometrical configuration of the three delay lines installed so far. The combination of the light beams from two (or more) VLT Unit Telescopes is a daunting task. It involves pointing them simultaneously towards the same celestial object, ensuring optimal optical adjustment of the computer-controlled telescope mirrors (including the shape of the 8.2-m primary mirror by "active optics"), performing extremely smooth and stable tracking of the object as the Earth turns, guiding the light beams via additional ("coudé") mirrors into the "delay lines" installed in the Interferometric Tunnel below the telescope platform, keeping the total path lengths equal to within a fraction of a micron during hours at a time and finally, to register the interferometric fringes at the focal point of the VINCI instrument [1], where the light beams encounter each other. Next year, the first adaptive optics systems for the VLTI will be inserted below the telescopes. By drastically reducing the smearing effects of the turbulent atmosphere through which the light has to pass before it enters the telescopes, this will further "stabilize" the imaging and increase the sensitivity of the VLTI by a factor of almost 100. First results with four Unit Telescopes ESO PR Photo 22b/02 ESO PR Photo 22b/02 [Preview - JPEG: 573 x 400 pix - 78k] [Normal - JPEG: 1145 x 800 pix - 232k] Caption : PR Photo 22b/02 : The left panel shows the rather incomplete set of "baselines" used during the present, short interferometric test exposures (in interferometric terminology: the "UV-plane coverage"). Each baseline is represented by two opposite, short arcs, symmetric around the origin (centre) of the diagram. The colour-coded pattern reflects the telescope pairs (ANTU-KUEYEN = magenta, ANTU-MELIPAL = red, ANTU-YEPUN = green, KUEYEN-MELIPAL = cyan, KUEYEN-YEPUN = blue), as seen from the observed object. Due to the limited time available, this distribution is far from uniform and is quite elongated in one direction. To the right is shown the reconstructed, two-dimensional interferometric point-spread function (PSF) of the star Achernar (in "negative" - with most light in the darkest areas). It is the result of subsequent computer processing of the measurements with the different baselines. On the largest scale, the image consists of an inner, round distribution of light, 0.057 arcsec wide, surrounded by an outer, much weaker, broad "ring" and with a "white" zone between these two areas. This is the "Airy disk" for a single 8.2-m telescope at this infrared wavelength (the K-band at 2.2 µm). It represents the maximum resolution (image sharpness) obtainable when observing with a single telescope. As explained in the text, the interferometric "addition" of more telescopes greatly improves that resolution. The width of the individual - slightly S-shaped - lines ("fringes") in the inclined pattern visible in the inner area, about 0.003 arcsec, represents the achieved interferometric resolution in one direction (with an angular diameter of about 0.002 arcsec, the disk of Achernar is not resolved, making it a suitable object for this resolution test). The resolution in the perpendicular direction (along the lines) is evidently less - this is due to the specific (elongated) baseline pattern during these test observations (left panel). The image provides a direct illustration of the 20-fold increase in resolution of the VLTI over a single 8.2-m telescope . At this moment, three delay lines have been installed, but for the present first test, the VLTI engineers and astronomers used the telescopes in pairs, in order to set-up the various equipment configurations properly. In this way, they could also start "teaching" the computer control software to handle this very demanding process as efficiently and user-friendly as possible in the future. With the arrival of the science instrument AMBER in mid-2003, up to three beams can be combined simultaneously. It turned out that the various predictions of mirror positions and angles were quite accurate and only a moderate amount of time was needed to "obtain fringes" in all different configurations. Measurements were then made on a number of stars, among them the brightest star in the southern constellation Eridanus (The River), known as Alpha Eridani or Achernar , that was observed several times with the different telescope pairings. This star is a hot dwarf (spectral type "B5 IV") that is located at a distance of about 145 light-years. It has also been extensively observed during earlier VLTI tests. It is a very suitable object for the present resolution tests as its angular diameter is only about 0.002 arcsec and it therefore remains unresolved at the near-infrared wavelength of the K-band used (2.2 µm). In fact, the combination of these data (including also some that were obtained in October 2001) now makes it possible to reconstruct the first interferometric "point-spread function (PSF)" of a star obtained with the VLTI , cf. PR Photo 22b/02 . This is like an "interferometric image", except that the disk of this particular star remains unresolved. The angular resolution is inversely proportional to the aperture of a telescope for single telescope observation, and to the length of the "baseline" between two telescopes for the interferometric observation. However, observing interferometrically with two telescopes will improve the resolution only in the direction parallel to this baseline, while the resolution in the perpendicular direction will remain that of a single telescope. But then the use of other telescope pairs with different baseline orientations "adds" resolution in other directions. The reconstructed PSF of Achernar shown in PR Photo 22b/02 is obviously still very incomplete, due to the technical nature of the present tests and the limited time that was spent observing the star in each configuration. However, it already presents a powerful illustration of the extreme imaging sharpness that will be achieved with the VLTI.

X-ray Pulsations from AXP 1E 1547-5407 Detected with RXTE

NASA Astrophysics Data System (ADS)

Dib, R.; Kaspi, V. M.; Gavriil, F. P.; Woods, P. M.

2008-10-01

We observed AXP 1E 1547-5407 which is currently in outburst (see ATELs #1756, #1761, #1763) with RXTE on October 4 (4 ks), and 6 (1.4 ks, 1.6 ks). The 2-20 keV pulse profile of these observations (October 04 UT 21:51:04, October 06 UT 01:46:04, and October 06 UT 23:31:04) shows a single broad pulse that is qualitatively similar to that reported in Halpern et al. (2008, ApJ, 676, 1178), though there is a possible hint of additional peaks.

Distinct sources of injections in the polar cusp observed by Cluster

NASA Astrophysics Data System (ADS)

Escoubet, C. Philippe; Reme, Henri; Dunlop, Malcolm; Daly, Patrick; Laakso, Harri; Berchem, Jean; Richard, Robert; Taylor, Matthew; Trattner, Karlheinz; Grison, Benjamin; Dandouras, Iannis; Fazakerley, Andrew; Pitout, Frederic; Masson, Arnaud

The main process that injects solar wind plasma into the polar cusp is now generally accepted to be magnetic reconnection. Depending on the IMF direction, this process takes place equatorward (for IMF southward), poleward (for IMF northward) or on the dusk or dawn sides (for IMF azimuthal) of the cusp. We report a Cluster crossing on 5 January 2002 near the exterior cusp on the southern dusk side. The IMF was mainly azimuthal (IMF-By around -5 nT), the solar wind speed lower than usual around 280 km/s and the density around 5 cm-3. The four Cluster spacecraft had an elongated configuration near the magnetopause. C4 was the first spacecraft to enter the cusp around 19:52:04 UT, followed by C2 at 19:52:35 UT, C1 at 19:54:24 UT and C3 at 20:13:15 UT. C4 and C1 observed two ion energy dispersions at 20:10 UT and 20:40 UT and C3 at 20:35 UT and 21:15 UT. Using the time of flight technique on the upgoing and downgoing ions in the dispersions, we obtain an altitude of the sources of these ions between 14 and 20 RE. Using Tsyganenko model, these sources are located on the dusk flank, past the terminator. The first injection by C3 is seen at approximately the same time as the 2nd injection on C1 but their sources at the magnetopause were separated by more than 10 RE. This would imply that two distinct sources were active at the same time on the dusk flank of the magnetosphere.

MASTER OT J015539.85+485955.6 was detected during Fermi alert inspection 3.5h after the trigger time

NASA Astrophysics Data System (ADS)

Rebolo, R.; Lipunov, V.; Gorbovskoy, E.; Serra, M.; Lodieu, N.; Israelian, G.; Suarez-Andres, L.; Shumkov, V.; Tyurina, N.; Kornilov, V.; Balanutsa, P.; Kuznetsov, A.; Vlasenko, D.; Gorbunov, I.; Vladimirov, V.; Popova, E.; Buckley, D.; Potter, S.; Kniazev, A.; Kotze, M.; Tlatov, A.; Parhomenko, A. V.; Dormidontov, D.; Senik, V.; Gress, O.; Ivanov, K.; Budnev, N. M.; Yurkov, V.; Sergienko, Yu.; Gabovich, A.; Sinyakov, E.; Krushinski, V.; Zalozhnih, I.; Shurpakov, S.

2015-11-01

MASTER-IAC, MASTER-Kislovodsk and MASTER-SAAO was pointed to the FERMI GBM GRB151107B (Stanbro, Meegan, GCN #18570 ) at 2015-11-07 20:25:52(/59s/58s) UT (R.Rebolo et al., GCN #18576 ). There were the prompt pointing observations because duration of the GRB was ~140s . After 5 minutes of the alert observations of the error-box center, MASTER telescopes in IAC and Kislovodsk started the inspect survey inside large Fermi error box (ra=00 42 28 dec=+48 48 58 r=4.533300) obtained by GCN socket.

Military versus Private Sector Construction Costs.

DTIC Science & Technology

1985-03-01

use for Government purposes, permission to quote from or reproduce por- tions of this document must be obtained from the Logistics Management ...Institute. go DTIC ELECTE LOGISTICS MANAGEMENT INSTITUTE JUN 1 11985 Bethesda, MD 20817-5886 I L- T RS-j UT- -N3T A T EM ENT A ALpprovgd tot public veaWuj...general-purpose warehouses, barracks, wheeled vehicle mainte- nance shops, and family housing units -- DoD MILCON costs are generally . equivalent to

Prediction of UT1-UTC, LOD and AAM χ3 by combination of least-squares and multivariate stochastic methods

NASA Astrophysics Data System (ADS)

Niedzielski, Tomasz; Kosek, Wiesław

2008-02-01

This article presents the application of a multivariate prediction technique for predicting universal time (UT1-UTC), length of day (LOD) and the axial component of atmospheric angular momentum (AAM χ 3). The multivariate predictions of LOD and UT1-UTC are generated by means of the combination of (1) least-squares (LS) extrapolation of models for annual, semiannual, 18.6-year, 9.3-year oscillations and for the linear trend, and (2) multivariate autoregressive (MAR) stochastic prediction of LS residuals (LS + MAR). The MAR technique enables the use of the AAM χ 3 time-series as the explanatory variable for the computation of LOD or UT1-UTC predictions. In order to evaluate the performance of this approach, two other prediction schemes are also applied: (1) LS extrapolation, (2) combination of LS extrapolation and univariate autoregressive (AR) prediction of LS residuals (LS + AR). The multivariate predictions of AAM χ 3 data, however, are computed as a combination of the extrapolation of the LS model for annual and semiannual oscillations and the LS + MAR. The AAM χ 3 predictions are also compared with LS extrapolation and LS + AR prediction. It is shown that the predictions of LOD and UT1-UTC based on LS + MAR taking into account the axial component of AAM are more accurate than the predictions of LOD and UT1-UTC based on LS extrapolation or on LS + AR. In particular, the UT1-UTC predictions based on LS + MAR during El Niño/La Niña events exhibit considerably smaller prediction errors than those calculated by means of LS or LS + AR. The AAM χ 3 time-series is predicted using LS + MAR with higher accuracy than applying LS extrapolation itself in the case of medium-term predictions (up to 100 days in the future). However, the predictions of AAM χ 3 reveal the best accuracy for LS + AR.

Australia to Build Fibre Positioner for the Very Large Telescope

NASA Astrophysics Data System (ADS)

1998-06-01

The Anglo-Australian Observatory (AAO) at Epping (New South Wales, Australia) has been awarded the contract to build a fibre positioner for the European Southern Observatory's Very Large Telescope (VLT). This new, large astronomical facility is located at the Paranal Observatory in Chile and will feature four Unit Telescopes, each with a main mirror of 8.2-m diameter. This positioner, (affectionately) known as the OzPoz , will form part of the FLAMES facility (the F ibre L arge A rea M ulti- E lement S pectrograph), to be mounted on the second Unit Telescope (UT2) of the VLT in 2001. The construction of this facility includes other institutes in Europe, e.g. Observatoire de Genève (Switzerland) and Observatoire de Meudon (France). The ESO Instrument Division will coordinate the entire project that will result in an observational capability that is unique in the world. Optical fibres at astronomical telescopes Optical fibres have come to play an increasingly important role as transmitters of information, for instance in telephone and computer networks. It may be less known that they can be used in a similar way to transmit visible and infrared light in astronomical telescopes. Over the past decade, the AAO has been refining its skills in building optical-fibre instruments for its own telescopes, the 3.9-metre Anglo-Australian Telescope and the 1.2-m UK Schmidt Telescope (a telescope dedicated to wide-field surveys). These instruments enable astronomers to study many celestial objects simultaneously, increasing the effectiveness and productivity by enormous factors. The OzPoz positioner sets up to 560 optical fibres (developed in collaboration with the Observatoire de Meudon in France) very precisely by a robotic arm to match the positions of galaxies and quasars in the telescope's focal plane. The positional accuracy is about 50 µm (0.05 mm), or 0.08 arcsec on the sky. The fibres siphon the light from these very faint and distant astronomical objects and guide it to very efficient, custom designed, spectrographs. Here the light is dispersed into its characteristic colours and analysed to determine the object's type, distance and chemical composition, etc. ESO PR Photo 18/98 ESO PR Photo 18/98 Reduced resolution 1024 x 1024 pix [JPEG, 860k] Full resolution 1500 x 1500 pix [GIF, 2.1 Mb] This image illustrates the use of the new Fibre Positioner (OzPoz). It shows an example of the 25 arcmin field-of-view of the VLT with the FLAMES facility, as recorded during the ESO Imaging Survey (EIS) with the 3.5-m New Technology Telescope (NTT) at La Silla. Within only one night, FLAMES with the OzPoz positioner will be capable of obtaining optical and infrared spectra for no less than 1/3 of the approx. 9000 objects (many of which are distant galaxies) seen in this image! They can then be used to determine their redshift, chemical composition and dynamics. This will increase enormously the observational efficiency of the VLT. In just one night, it is possible to observe and analyse thousands of objects, a task that would have taken years in the past. The contract Dr. Brian Boyle , Director of the AAO, is very pleased with the new ESO contract: "The AAO has been recognised many times in the past as being a world-leader in astronomy, but this contract marks a new era. Up until now, we have built instruments for our own telescopes to ensure we stay ahead. Now we have expanded into instrument making for other telescopes. Our engineers, computer programmers and scientists have formed a productive and innovative team which is the envy of many observatories around the world." The Director General of ESO, Professor Riccardo Giacconi , is also happy: "The Anglo-Australian Observatory has excellent credentials in instrument making, and we have no doubt about their ability to build the critical optical fibre positioner for the VLT. The spectacular success of the AAO 2dF instrument (see below) reinforced our decision." The contract will take about 3 years to build and will involve the work of at least 10 AAO engineers and technicians over this period. The AAO 2dF optical fibre positioner The 2dF (two-degree field) optical fibre positioner has taken more than seven years to perfect, and is now fully operational at the 3.9 m Anglo-Australian Telescope. With it, two very ambitious survey projects are now well underway. The 2dF Galaxy Redshift Survey and the 2dF Quasar Redshift Survey aim at analysing more than 250 000 galaxies and 3000 quasars over the next few years to give a three-dimensional picture of the Universe on a large scale. A few nights of early observations yielded spectra from 4000 galaxies and 1000 quasars; a massive data set which, through expert, dedicated software, was analysed on-line and distributed to the international science team by email within minutes of the completion of the observations. Note: [1] This Press Release is issued jointly by ESO and the Anglo-Australian Observatory (AAO). This Press Release is accompanied by ESO PR Photo 18/98 . It is available in two versions: Reduced resolution 1024 x 1024 pix [JPEG, 860k] and Full resolution 1500 x 1500 pix [GIF, 2.1 Mb]. It may be reproduced, if credit is given to the European Southern Observatory. How to obtain ESO Press Information ESO Press Information is made available on the World-Wide Web (URL: http://www.eso.org). ESO Press Photos may be reproduced, if credit is given to the European Southern Observatory.

The Accuracy of Radio Interferometric Measurements of Earth Rotation

NASA Technical Reports Server (NTRS)

Eubanks, T. M.; Steppe, J. A.; Spieth, M. A.

1985-01-01

The accuracy of very long base interferometry earth rotation (UT1) measurements is examined by intercomparing TEMPO and POLARIS data for 1982 and the first half of 1983. None of these data are simultaneous, and so a proper intercomparison requires accounting for the scatter introduced by the rapid, unpredictable, UT1 variations driven by exchanges of angular momentum with the atmosphere. A statistical model of these variations, based on meteorological estimates of the Atmospheric Angular Momentum is derived, and the optimal linear (Kalman) smoother for this model is constructed. The scatter between smoothed and independent raw data is consistent with the residual formal errors, which do not depend upon the actual scatter of the UT1 data. This represents the first time that an accurate prediction of the scatter between UT1 data sets were possible.

Crosstalk: The Journal of Defense Software Engineering. Volume 18, Number 1

DTIC Science & Technology

2005-01-01

d o t . o r g / a s k slashdot/04/04/12/1757244.shtml>. 5. Dibona , C., et al. Open Sources: Voices From the Open Source Rev- olution. 1st ed. O’Reilly...Volume 18, Number 1, January 2005 5a. CONTRACT NUMBER 5b. GRANT NUMBER 5c. PROGRAM ELEMENT NUMBER 6. AUTHOR( S ) 5d. PROJECT NUMBER 5e. TASK NUMBER...5f. WORK UNIT NUMBER 7. PERFORMING ORGANIZATION NAME( S ) AND ADDRESS(ES) OO-ALC/MASE,6022 Fir Ave,Hill AFB,UT,84056-5820 8. PERFORMING

Evidence for Atmospheric Cold-trap Processes in the Noninverted Emission Spectrum of Kepler-13Ab Using HST /WFC3

DOE Office of Scientific and Technical Information (OSTI.GOV)

Beatty, Thomas G.; Zhao, Ming; Gilliland, Ronald L.

We observed two eclipses of the Kepler-13A planetary system, on UT 2014 April 28 and UT 2014 October 13, in the near-infrared using Wide Field Camera 3 on the Hubble Space Telescope . By using the nearby binary stars Kepler-13BC as a reference, we were able to create a differential light curve for Kepler-13A that had little of the systematics typically present in HST /WFC3 spectrophotometry. We measure a broadband (1.1–1.65 μ m) eclipse depth of 734 ± 28 ppm and are able to measure the emission spectrum of the planet at R  ≈ 50 with an average precision of 70 ppm. Wemore » find that Kepler-13Ab possesses a noninverted, monotonically decreasing vertical temperature profile. We exclude an isothermal profile and an inverted profile at more than 3 σ . We also find that the dayside emission of Kepler-13Ab appears generally similar to an isolated M7 brown dwarf at a similar effective temperature. Due to the relatively high mass and surface gravity of Kepler-13Ab, we suggest that the apparent lack of an inversion is due to cold-trap processes in the planet’s atmosphere. Using a toy model for where cold traps should inhibit inversions, as well as observations of other planets in this temperature range with measured emission spectra, we argue that with more detailed modeling and more observations we may be able to place useful constraints on the size of condensates on the daysides of hot Jupiters.« less

Observation of a rapid decrease in the brightness of the coma of 2060 Chiron in 1990 January

NASA Technical Reports Server (NTRS)

Buratti, Bonnie J.; Dunbar, R. Scott

1991-01-01

Photometric observations of 2060 Chiron in the V and R filters were obtained with the 1.5-m telescope on Palomar Mountain during a 7-hr period on January 20, 1990 (UT). A general decrease of about 10 percent in integrated brightness occurred in both filters. No color dependence to the decrease was observed. A small (about 0.02 mag) rotational light curve, far smaller than the 0.09 mag (peak-to-peak) one observed by Bus et al. (1989) is superposed on the general decrease. On January 29, 1990, Luu and Jewitt (1990) observed an impulsive brightening of Chiron of approximately the same magnitude and time scale as the presently observed decrease in brightness. The combined results provide evidence that Chiron is currently exhibiting short-term fluctuations in the brightness of its coma, in addition to its well-established general decrease in brightness.

Hard X-ray imaging of the Galactic black hole candidate GX 339 - 4

NASA Technical Reports Server (NTRS)

Covault, C. E.; Grindlay, J. E.; Manandhar, R. P.

1992-01-01

Imaging and spectral observations in the energy range 25-250 keV of the black hole candidate GX 339 - 4 have been obtained with the Energetic X-ray Imaging Telescope Experiment. Observations were made during a balloon flight from Alice Springs, Australia on UT 1989 May 8-10. A single source of nearly 6-sigma significance is detected near the center of the 3.4-deg field of view with a position consistent with GX 339 - 4. This is the first imaging observation of GX 339 - 4 at hard X-ray energies. This result confirms previously reported results from nonimaging experiments showing significant hard X-ray flux up to greater than about 60 keV, with a power-law spectral fit similar to the other black hole candidates such as Cygnus X - 1. The source may have been in an outburst state similar to that recently detected with BATSE on GRO.

DOE Office of Scientific and Technical Information (OSTI.GOV)

Lipunov, Vladimir M.; Kornilov, V.; Vlasenko, D.

On 2015 June 15, the Swift space observatory discovered that the Galactic black hole candidate V404 Cyg was undergoing another active X-ray phase, after 25 years of inactivity. The 12 telescopes of the MASTER Global Robotic Net located at six sites across four continents were the first ground-based observatories to start optical monitoring of the microquasar after its gamma-ray wake up at 18{sup h} 34{sup m} 09{sup s} U.T. on 2015 June 15. In this paper, we report, for the first time, the discovery of variable optical linear polarization, changing by 4%–6% over a timescale of ∼1 hr, on twomore » different epochs. We can conclude that the additional variable polarization arises from the relativistic jet generated by the black hole in V404 Cyg. The polarization variability correlates with optical brightness changes, increasing when the flux decreases.« less

4. VIEW SHOWING UPSTREAM FACE OF DAM, LOOKING NORTHEAST ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

4. VIEW SHOWING UPSTREAM FACE OF DAM, LOOKING NORTHEAST - High Mountain Dams in Upalco Unit, Kidney Lake Dam, Ashley National Forest, 4.7 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

Alpha Monocerotids 2017

NASA Astrophysics Data System (ADS)

Roggemans, Paul; Johannink, Carl; Biets, Jean-Marie

2018-01-01

17 orbits of the annual component of the Alpha Monocerotids (246 AMO) were captured by CAMS networks between 21 and 24 November, 10 of them in the United Arab Emirates on 21 November between 21h to 24h UT.

6. VIEW SHOWING INCLINED OUTLET GATE WHEEL, STEM AND STEM ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

6. VIEW SHOWING INCLINED OUTLET GATE WHEEL, STEM AND STEM GUIDE (18' HARDESTY GATE), LOOKING SOUTHEAST - High Mountain Dams in Bonneville Unit, Long Lake Dam, Wasatch National Forest, Kamas, Summit County, UT

5. VIEW OF UPRIGHT OUTLET GATE WHEEL, STEM AND STEM ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. VIEW OF UPRIGHT OUTLET GATE WHEEL, STEM AND STEM GUIDE (HARDESTY CAST IRON RECTANGULAR SLIDE GATE), LOOKING SOUTHWEST - High Mountain Dams in Bonneville Unit, Lost Lake Dam, Kamas, Summit County, UT

On the Logical Development of Statistical Models.

DTIC Science & Technology

1983-12-01

David Steinberg, and Jean Wallis for their helpful cosments to a preliminary draft of this work. -21- REFERENCES [1] Anscombe, F. J. and Tukey, J. W ...effect of a known vector x of predictor variables. In this way we obtain an explicative-static or type 11 model and -3- W .- r󈧬 41 U) 3 0) H + N 1 0...dependency is: Yt M it + ut p(ut ) - U It P(ut M-t) - I - t (2.1) t W P01 + Vt-1(P11 - P0 1) where Yt can only have the values zero and one, p is its

Nonpeptidic urotensin-II receptor antagonists I: in vitro pharmacological characterization of SB-706375

PubMed Central

Douglas, Stephen A; Behm, David J; Aiyar, Nambi V; Naselsky, Diane; Disa, Jyoti; Brooks, David P; Ohlstein, Eliot H; Gleason, John G; Sarau, Henry M; Foley, James J; Buckley, Peter T; Schmidt, Dulcie B; Wixted, William E; Widdowson, Katherine; Riley, Graham; Jin, Jian; Gallagher, Timothy F; Schmidt, Stanley J; Ridgers, Lance; Christmann, Lisa T; Keenan, Richard M; Knight, Steven D; Dhanak, Dashyant

2005-01-01

SB-706375 potently inhibited [125I]hU-II binding to both mammalian recombinant and ‘native' UT receptors (Ki 4.7±1.5 to 20.7±3.6 nM at rodent, feline and primate recombinant UT receptors and Ki 5.4±0.4 nM at the endogenous UT receptor in SJRH30 cells). Prior exposure to SB-706375 (1 μM, 30 min) did not alter [125I]hU-II binding affinity or density in recombinant cells (KD 3.1±0.4 vs 5.8±0.9 nM and Bmax 3.1±1.0 vs 2.8±0.8 pmol mg−1) consistent with a reversible mode of action. The novel, nonpeptidic radioligand [3H]SB-657510, a close analogue of SB-706375, bound to the monkey UT receptor (KD 2.6±0.4 nM, Bmax 0.86±0.12 pmol mg−1) in a manner that was inhibited by both U-II isopeptides and SB-706375 (Ki 4.6±1.4 to 17.6±5.4 nM) consistent with the sulphonamides and native U-II ligands sharing a common UT receptor binding domain. SB-706375 was a potent, competitive hU-II antagonist across species with pKb 7.29–8.00 in HEK293-UT receptor cells (inhibition of [Ca2+]i-mobilization) and pKb 7.47 in rat isolated aorta (inhibition of contraction). SB-706375 also reversed tone established in the rat aorta by prior exposure to hU-II (Kapp∼20 nM). SB-706375 was a selective U-II antagonist with ⩾100-fold selectivity for the human UT receptor compared to 86 distinct receptors, ion channels, enzymes, transporters and nuclear hormones (Ki/IC50>1 μM). Accordingly, the contractile responses induced in isolated aortae by KCl, phenylephrine, angiotensin II and endothelin-1 were unaltered by SB-706375 (1 μM). In summary, SB-706375 is a high-affinity, surmountable, reversible and selective nonpeptide UT receptor antagonist with cross-species activity that will assist in delineating the pathophysiological actions of U-II in mammals. PMID:15852036

Selected aspects of wide-field stellar interferometry

NASA Astrophysics Data System (ADS)

D'Arcio, Luigi Arsenio

1999-11-01

In Michelson stellar interferometry, the high-resolution information about the source structure is detected by performing observations with widely separated telescopes, interconnected to form an interferometer. At optical wavelengths, this method provides a technically viable approach for achieving angular resolutions in the milliarcsecond range, comparable to those of a 100 m diameter telescope, whose realization is beyond the immediate engineering capabilities. Considerable efforts are currently devoted to the definition of dedicated interferometric instruments, which will allow to address ambitious astronomical tasks such as high-resolution imaging, astrometry at microarcsecond level, and the direct detection of exoplanets. Astrometry and related techniques employ the so-called wide field-of-view interferometric mode, where phase measurements are performed simultaneously at two (or more) sources; often, the actual observable is the instantaneous phase difference of the two object signals. The future success of wide-field interferometry critically depends on the development of techniques for the accurate control of field-dependent (anisoplanatic) phase errors. In this thesis, we address two aspects of this problem in detail. The first one is theoretical in nature. For ground-based measurements, atmospheric turbulence is the largest source of random phase fluctuations between the on- and the off-axis fringes. We developed a model of the temporal power spectrum of this disturbance, whose validity is not limited to low frequencies only, as it is the case with earlier models. This extension opens the possibility of the analysis of dynamic issues, such as the determination of the allowable coherent integration time T for the off-axis fringes. The spectrum turns out to be well approximated by a sequences of four power-law branches. In first instance, its overall form is determined by the values of the baseline length, telescope diameter, and average beam separation in the atmosphere. Due to the rapid decorrelation of the on- and off-axis phases for increasing star separation theta, the useful field for wide-field interferometry is limited to about |theta|<1', the so-called very narrow angle regime. For high-accuracy applications, this range decreases to a few arcseconds. We estimated that for the VLTI along baselines operating at lambda=2.2 mu, a turbulence-related error of less than lambda/10 rms is only available for field angles smaller than 7.3'' and 5.8'', for UT-UT and AT-AT pairs respectively. The bulk of the spectral power is confined at relatively low frequencies, typically below 1 Hz. Both smaller star separations and larger telescope sizes contribute in lowering the spectral content at hight frequencies. We found that in general, as compared to blind observations, wide-field measurements can make use of significantly longer off-axis integration times T, even at rather big star separations. For the long UT-UT baseline operating at lambda=2.2 mu, we have calculated a 5 % fringe visibility loss is reached for T=740 ms, 2.1 s and 12.7 s for star separations of 30'', 10'', and 5'', respectively. These figures are about 2, 5 and 32 times higher than for a blind observation. Finally, we point out that for large telescopes a significant fraction of the total phase error due to anisoplanatic turbulence is contributed by wavefront modes higher than piston. Therefore, we generalized the formalism used in out study to the analysis of (Zernike) wavefront modes of arbitrary order. This thesis also addresses an instrumental aspect of the problem of the control of anisoplanatic phase errors. A Michelson interferometric imager is suitable for wide-field operation only if the configuration of the pupil images forms a scaled replica of the total array aperture. This implies the factual coincidence of the magnification factors M and pupil rotations phi of all interferometric arms: for the VLTI, the matching accuracy requirements are as severe as dM< 1.9e-3, dphi < 3.8''. We addressed the problem of measuring dM, dphi, to the accuracies expressed here above. In the selected approach, this is done by measuring the difference of the star separation vectors for the two interferometer arms, as measured at the corresponding pupil images. Variations of M and phi affect this quantity in orthogonal directions, which allows the simultaneous determination of both unknowns. The measurement makes use of two two-axis tilt sensors, that determine the angular separation vectors of the on- and off-axis beams, respectively, from the two interferometric arms. A 0.0075'' single-axis accuracy is required, together with a sufficiently high sensitivity for astronomical applications. This led to the choice of implementing the sensors as pupil plane devices, using the same interferometric tilt-detection principle as applied in Fine Guidance Sensors of the Hubble Space Telescope. The main challenge was to ensure equal responses for the two sensors, to within 0.0075''. Test measurements have shown that we succeeded in controlling mismatches between the sensors (including their mutual orientations, electronic gain and phase, linearity and signal normalization) a the 0.004'' level, and in performing beam recombination without introducing errors exceeding 0.006''. Pupil rotation alignment runs confirmed a 2'' overall measurement uncertainty for dphi, about half the 3.8'' calibration requirement. Finally, in this thesis we also developed a near-filed propagation method, intended for the diffraction-based analysis of optical systems with extremely high accuracy requirements (typically 1 deg in phase and 1.e-3 in field amplitude). Examples thereof are the nulling optics for planet detection and, outside the field of stellar interferometry, systems for the determination of the shape of mirrors for extreme-UV lithographic projection systems. The method is based on the local Fresnel approximation of the propagation integral, that we have solved analytically for rectangular domains and for triangular ones with an arched hypotenuse. This allows for an accurate computation of the field diffracted at the edges of complicated aperture shapes, without having to recur to time-consuming numerical quadrature techniques. The method has shown the ability to provide complex amplitude estimates that are consistently accurate to the specifications given above, and this in reasonable times. In a series of comparative tests, our method outperformed the Hopkins algorithm by typically a factor of fifty with respect to the computational speed.

Infrared spectroscopy of the transiting extrasolar planet HD 209458 b during secondary eclipse

NASA Astrophysics Data System (ADS)

Richardson, Lee Jeremy

2003-10-01

We present spectroscopic observations that place strong limits on the atmospheric structure of the transiting extrasolar planet HD 209458 b. The discovery of the transit has led to several new observations that have provided the most de tailed information on the physical properties of a planet outside the solar system. These observations have concentrated on the primary eclipse, the time at which the planet crosses in front of the star as seen from Earth. The measurements have determined the basic physical characteristics of the planet, including radius, mass, average density, and orbital inclination, and have even refined values of the stellar mass and radius. Transmission spectroscopy of the system during primary eclipse resulted in the first detection of the atmosphere of an extrasolar planet, with the measurement of the sodium doublet. The present work discusses the first reported attempts to detect the secondary eclipse, or the disappearance of the planet behind the star, in the infrared. We devise the method of ‘occultation spectroscopy’ to detect the planetary spectrum, by searching in combined light for subtle changes in the shape of the spectrum as the planet passes behind the star. Predicted secondary eclipse events were observed from the Very Large Telescope (VLT) on UT 8 and 15 July 2001 using the Infrared Spectrometer and Array Camera (3.5 3.7 μm). Further observations from the NASA Infrared Telescope Facility (IRTF) using the SpeX instrument (1.9 4.2 μm) included two predicted secondary eclipse events on UT 20 and 27 September 2001. Analysis of these data reveal a statistically significant non- detection of the planetary spectrum. The results place strong limits on the structure of the planetary atmosphere and reject widely-accepted models for the planet that assume the incident stellar radiation is completely absorbed and re-emitted in the substellar hemisphere. Situations that remain consistent with our data include an isothermal atmosphere or the presence of a high absorptive or reflective cloud. The latter case is also consistent with the observed low sodium abundance from transmission spectroscopy. These results represent the strongest limits to date on the temperature structure of the planetary atmosphere.

The overall computer/mobile devices usage time is related to newly diagnosed non-alcoholic fatty liver disease: a population-based study.

PubMed

Meng, Ge; Liu, Fangfang; Fang, Liyun; Li, Chunlei; Zhang, Qing; Liu, Li; Wu, Hongmei; Du, Huanmin; Shi, Hongbin; Xia, Yang; Guo, Xiaoyan; Liu, Xing; Bao, Xue; Su, Qian; Gu, Yeqing; Yu, Fei; Yang, Huijun; Yu, Bin; Sun, Shaomei; Wang, Xing; Zhou, Ming; Jia, Qiyu; Guo, Qi; Chen, Xin; Song, Kun; Wang, Guolin; Huang, Guowei; Niu, Kaijun

2016-11-01

The computer/mobile devices usage time (CMD-UT) is closely related to a sedentary lifestyle, which is an important risk factor for non-alcoholic fatty liver disease (NAFLD). But their direct relationship remains unclear. We aimed to examine the relationship between CMD-UT and newly diagnosed non-alcoholic fatty liver disease (NAFLD) in Chinese adults. This cross-sectional study was conducted on 7516 adults in Tianjin, China. The CMD-UT was collected via a questionnaire included five categories. NAFLD [with normal or elevated alanine transaminase (ALT) levels] was diagnosed by at least twice liver ultrasonography examinations and serum ALT concentrations (>41 U/L in males and >33 U/L in females). The prevalence of overall NAFLD, NAFLD with normal or elevated ALT levels was 18.2, 14.2, and 4.0%, respectively. After adjustments for potential confounding factors, the odds ratios (95% confidence interval) of having overall NAFLD by increasing CMD-UT levels were 1.00 for <1 h/d, 1.58 (1.22-2.05) for 1-3 h/d, 1.58 (1.18-2.11) for 3-5 h/d, 1.65 (1.21-2.27) for 5-10 h/d, and 1.99 (1.29-3.05) for ≥10h/d (P-trend for CMD-UT levels = 0.02), respectively. Similar relations were observed with the use of NAFLD with normal or elevated ALT levels. The present study is the first to find that CMD-UT levels are independently associated with NAFLD. Key Messages The computer/mobile devices usage time levels are independently associated with the prevalence of non-alcoholic fatty liver disease.

Metformin, an AMPK activator, stimulates the phosphorylation of aquaporin 2 and urea transporter A1 in inner medullary collecting ducts.

PubMed

Klein, Janet D; Wang, Yanhua; Blount, Mitsi A; Molina, Patrick A; LaRocque, Lauren M; Ruiz, Joseph A; Sands, Jeff M

2016-05-15

Nephrogenic diabetes insipidus (NDI) is characterized by production of very large quantities of dilute urine due to an inability of the kidney to respond to vasopressin. Congenital NDI results from mutations in the type 2 vasopressin receptor (V2R) in ∼90% of families. These patients do not have mutations in aquaporin-2 (AQP2) or urea transporter UT-A1 (UT-A1). We tested adenosine monophosphate kinase (AMPK) since it is known to phosphorylate another vasopressin-sensitive transporter, NKCC2 (Na-K-2Cl cotransporter). We found AMPK expressed in rat inner medulla (IM). AMPK directly phosphorylated AQP2 and UT-A1 in vitro. Metformin, an AMPK activator, increased phosphorylation of both AQP2 and UT-A1 in rat inner medullary collecting ducts (IMCDs). Metformin increased the apical plasma membrane accumulation of AQP2, but not UT-A1, in rat IM. Metformin increased both osmotic water permeability and urea permeability in perfused rat terminal IMCDs. These findings suggest that metformin increases osmotic water permeability by increasing AQP2 accumulation in the apical plasma membrane but increases urea permeability by activating UT-A1 already present in the membrane. Lastly, metformin increased urine osmolality in mice lacking a V2R, a mouse model of congenital NDI. We conclude that AMPK activation by metformin mimics many of the mechanisms by which vasopressin increases urine-concentrating ability. These findings suggest that metformin may be a novel therapeutic option for congenital NDI due to V2R mutations. Copyright © 2016 the American Physiological Society.

Metformin, an AMPK activator, stimulates the phosphorylation of aquaporin 2 and urea transporter A1 in inner medullary collecting ducts

PubMed Central

Wang, Yanhua; Blount, Mitsi A.; Molina, Patrick A.; LaRocque, Lauren M.; Ruiz, Joseph A.

2016-01-01

Nephrogenic diabetes insipidus (NDI) is characterized by production of very large quantities of dilute urine due to an inability of the kidney to respond to vasopressin. Congenital NDI results from mutations in the type 2 vasopressin receptor (V2R) in ∼90% of families. These patients do not have mutations in aquaporin-2 (AQP2) or urea transporter UT-A1 (UT-A1). We tested adenosine monophosphate kinase (AMPK) since it is known to phosphorylate another vasopressin-sensitive transporter, NKCC2 (Na-K-2Cl cotransporter). We found AMPK expressed in rat inner medulla (IM). AMPK directly phosphorylated AQP2 and UT-A1 in vitro. Metformin, an AMPK activator, increased phosphorylation of both AQP2 and UT-A1 in rat inner medullary collecting ducts (IMCDs). Metformin increased the apical plasma membrane accumulation of AQP2, but not UT-A1, in rat IM. Metformin increased both osmotic water permeability and urea permeability in perfused rat terminal IMCDs. These findings suggest that metformin increases osmotic water permeability by increasing AQP2 accumulation in the apical plasma membrane but increases urea permeability by activating UT-A1 already present in the membrane. Lastly, metformin increased urine osmolality in mice lacking a V2R, a mouse model of congenital NDI. We conclude that AMPK activation by metformin mimics many of the mechanisms by which vasopressin increases urine-concentrating ability. These findings suggest that metformin may be a novel therapeutic option for congenital NDI due to V2R mutations. PMID:26962099

Cluster Observations of Ion Dispersions near the Exterior Cusp

NASA Astrophysics Data System (ADS)

Escoubet, C.; Grison, B.; Berchem, J.; Trattner, K. J.; Pitout, F.; Richard, R. L.; Taylor, M. G.; Laakso, H. E.; Masson, A.; Dunlop, M. W.; Dandouras, I. S.; Reme, H.; Fazakerley, A. N.; Daly, P. W.

2013-12-01

The cusps are the places where the Earth's magnetic field lines, connected to the inner side of the magnetopause, converge. It is therefore the place where signatures of processes occurring near the subsolar point, in the tail lobes, as well as near the dawn and dusk flanks are observed. The main process that injects solar wind plasma into the polar cusp is now generally accepted to be magnetic reconnection. Depending on the IMF direction, this process will take place equatorward (for IMF southward), poleward (for IMF northward) or on the side (for IMF azimuthal) of the cusp. We report a Cluster crossing on 5 January 2002 near the exterior cusp on the southern dusk side. The IMF was mainly azimuthal (IMF-By around -5 nT), the solar wind speed around 280 km/s and the density around 5 cm-3. The four Cluster spacecraft were still in the "magnetotail" configuration with two perfect tetrahedra of 2000 km around apogee and turning into an elongated configuration near the magnetopause. C4 was the first spacecraft to enter the cusp around 19:52:04 UT, followed by C2 at 19:52:35 UT, C1 at 19:54:24 UT and C3 at 20:13:15 UT. C4 and C1 observed two ion energy dispersions at 20:10 UT and 20:40 UT and C3 at 20:35 UT and 21:15 UT. We will investigate the origin of the injections forming the dispersions and if these can be explained by the reconnection between the interplanetary magnetic field and the Earth's magnetic field.

VizieR Online Data Catalog: Potential exoplanet targets with Palomar/TripleSpec (Zellem+, 2014)

NASA Astrophysics Data System (ADS)

Zellem, R. T.; Griffith, C. A.; Deroo, P.; Swain, M. R.; Waldmann, I. P.

2017-05-01

We observed HD 209458b's emission with the 3.0 m NASA IRTF at the Mauna Kea Observatory and SpeX (Rayner et al. 2003PASP..115..362R), a near-IR spectrometer with a wavelength coverage of 2.0-4.2 um (K and L bands) and a resolution of R=2500, and with the 200 inch (5.08 m) Hale Telescope at the Palomar Observatory and TripleSpec, a near-IR spectrometer with a wavelength coverage of 1.0-2.4 um (J, H, and K bands) and a resolution of R=2500-2700. While low-resolution spectroscopic observations are incapable of observing the fine-scale structure of the spectral lines, the SpeX and TripleSpec spectral channels can be binned to increase the signal-to-noise ratio (S/N). We observed HD 209458b's 2011 September 9 (UT) secondary eclipse for ~8 hr, resulting in 1210 exposures of 10 s each in an ABBA nodding sequence. (1 data file).

Towards Cloud Processing of GGOS Big Data

NASA Astrophysics Data System (ADS)

Weston, Stuart; Kim, Bumjun; Litchfield, Alan; Gulyaev, Sergei; Hall, Dylan; Chorao, Carlos; Ruthven, Andrew; Davies, Glyn; Lagos, Bruno; Christie, Don

2017-04-01

We report on our initial steps towards development of a cloud-like correlation infrastructure for geodetic Very Long Baseline Interferometry (VLBI), which in its raw format is of the order of 10-100 TB (big data). Data is generated by multiple VLBI radio telescopes, and is then used by for geodetic, geophysical, and astrometric research and operational activities through the International VLBI Service (IVS), as well as for corrections of GPS satellite orbits. Currently IVS data is correlated in several international Correlators (Correlation Centres), which receive data from individual radio telescope stations either in hard drives via regular mail service or via fibre using e-transfer mode. The latter is strongly limited by connectivity of existing correlation centres, which creates bottle necks and slows down the turnover of the data. This becomes critical in many applications - for example, it currently takes 1-2 weeks to generate the dUT1 parameter for corrections of GNSS orbits while less than 1-2 days delay is desirable. We started with a blade server at the AUT campus to emulate a cloud server using Virtual Machines (VMWare). The New Zealand Data Head node is connected to the high speed (100 Gbps) network ring circuit courtesy of the Research and Education Advanced Network New Zealand (REANNZ), with the additional nodes at remote physical sites connected via 10 Gbps fibre. We use real Australian Long Baseline Array (LBA) observational data from 6 radio telescopes in Australia, South Africa and New Zealand (15 baselines) of 1.5 hours in duration making 8 TB to emulate data transfer from remote locations and to provide a meaningful benchmark dataset for correlation. Data was successfully transferred using bespoke UDT network transfer tools and correlated with the speed-up factor of 0.8 using DiFX software correlator. In partnership with the New Zealand office of Catalyst IT Ltd we have moved this environment into Catalyst Cloud and report on the first correlation of a VLBI Dataset in a true cloud environment.

8. DETAIL VIEW OF INCLINED OUTLET GATE WHEEL, LOOKING EAST ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

8. DETAIL VIEW OF INCLINED OUTLET GATE WHEEL, LOOKING EAST - High Mountain Dams in Upalco Unit, Kidney Lake Dam, Ashley National Forest, 4.7 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

3. OVERALL VIEW OF DAM, SHOWING UPSTREAM FACE, LOOKING EAST ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

3. OVERALL VIEW OF DAM, SHOWING UPSTREAM FACE, LOOKING EAST - High Mountain Dams in Upalco Unit, Kidney Lake Dam, Ashley National Forest, 4.7 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

5. VIEW OF OUTLET GATE WHEEL AND STEM, LOOKING NORTH ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. VIEW OF OUTLET GATE WHEEL AND STEM, LOOKING NORTH - High Mountain Dams in Upalco Unit, Island Lake Dam, Ashley National Forest, 4.8 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

4. VIEW SHOWING OUTLET GATE WHEEL AND STEM, LOOKING NORTH ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

4. VIEW SHOWING OUTLET GATE WHEEL AND STEM, LOOKING NORTH - High Mountain Dams in Upalco Unit, Clements Lake Dam, Ashley National Forest, 6.5 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

7. VIEW OF INCLINED OUTLET GATE WHEEL, STEM AND STEM ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

7. VIEW OF INCLINED OUTLET GATE WHEEL, STEM AND STEM GUIDE (15' HARDESTY MODEL 115 GATE), LOOKING NORTHWEST - High Mountain Dams in Bonneville Unit, Marjorie Lake Dam, Wasatch National Forest, Kamas, Summit County, UT

4. VIEW OF INCLINED OUTLET GATE, STEM, STEM GUIDE AND ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

4. VIEW OF INCLINED OUTLET GATE, STEM, STEM GUIDE AND WHEEL (10' HARDESTY VERTICAL LIFT GATE), LOOKING NORTHWEST - High Mountain Dams in Bonneville Unit, Pot Lake Dam, Wasatch National Forest, Kamas, Summit County, UT

2. OVERALL VIEW OF BROWN DUCK LAKE, LOOKING WEST ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

2. OVERALL VIEW OF BROWN DUCK LAKE, LOOKING WEST - High Mountain Dams in Upalco Unit, Brown Duck Lake Dam, Ashley National Forest, 4.4 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

Factors controlling threshold friction velocity in semiarid and arid areas of the United States

USGS Publications Warehouse

Marticorena, Beatrice; Bergametti, G.; Belnap, Jayne

1997-01-01

A physical model was developed to explain threshold friction velocities u*t for particles of the size 60a??120 I?m lying on a rough surface in loose soils for semiarid and arid parts of the United States. The model corrected for the effect of momentum absorption by the nonerodible roughness. For loose or disturbed soils the most important parameter that controls u*t is the aerodynamic roughness height z 0. For physical crusts damaged by wind the size of erodible crust pieces is important along with the roughness. The presence of cyanobacteriallichen soil crusts roughens the surface, and the biological fibrous growth aggregates soil particles. Only undisturbed sandy soils and disturbed soils of all types would be expected to be erodible in normal wind storms. Therefore disturbance of soils by both cattle and humans is very important in predicting wind erosion as confirmed by our measurements.

Deletion of the UT receptor gene results in the selective loss of urotensin-II contractile activity in aortae isolated from UT receptor knockout mice

PubMed Central

Behm, David J; Harrison, Stephen M; Ao, Zhaohui; Maniscalco, Kristeen; Pickering, Susan J; Grau, Evelyn V; Woods, Tina N; Coatney, Robert W; Doe, Christopher P A; Willette, Robert N; Johns, Douglas G; Douglas, Stephen A

2003-01-01

Urotensin-II (U-II) is among the most potent mammalian vasoconstrictors identified and may play a role in the aetiology of essential hypertension. Currently, only one mouse U-II receptor (UT) gene has been cloned. It is postulated that this protein is solely responsible for mediating U-II-induced vasoconstriction. This hypothesis has been investigated in the present study, which assessed basal haemodynamics and vascular reactivity to hU-II in wild-type (UT(+/+)) and UT receptor knockout (UT(−/−)) mice. Basal left ventricular end-diastolic and end-systolic volumes/pressures, stroke volumes, mean arterial blood pressures, heart rates, cardiac outputs and ejection fractions in UT(+/+) mice and in UT(−/−) mice were similar. Relative to UT(+/+) mouse isolated thoracic aorta, where hU-II was a potent spasmogen (pEC50=8.26±0.08) that evoked relatively little vasoconstriction (17±2% 60 mM KCl), vessels isolated from UT(−/−) mice did not respond to hU-II. However, in contrast, the superior mesenteric artery isolated from both the genotypes did not contract in the presence of hU-II. Reactivity to unrelated vasoconstrictors (phenylephrine, endothelin-1, KCl) and endothelium-dependent/independent vasodilator agents (carbachol, sodium nitroprusside) was similar in the aorta and superior mesenteric arteries isolated from both the genotypes. The present study is the first to directly link hU-II-induced vasoconstriction with the UT receptor. Deletion of the UT receptor gene results in loss of hU-II contractile action with no ‘nonspecific' alterations in vascular reactivity. However, as might be predicted based on the limited contractile efficacy recorded in vitro, the contribution that hU-II and its receptor make to basal systemic haemodynamics appears to be negligible in this species. PMID:12770952

Improving Childhood Asthma Outcomes in the United States. A Blueprint for Policy Action

DTIC Science & Technology

2002-01-01

would include family physicians, pediatricians, nurse practitioners, respiratory therapists, and pharmacists . Based on the NHLBI National Guidelines...C_4_C4_M_ In I ( Zf~qpqrsaJ JO -3 U! %L9 dol ul -0 -: L ’ V 11’ r-: m.N 12 .-- -1 ’ m m r 0 In 00 - UTIU~lSJO Uj~TE E)()SOS~Ip~UtIJ%9diU tITUIflS OJ UTI ~E ~a

Effect of protein supplementation on expression and distribution of urea transporter-B in lambs fed low-quality forage.

PubMed

Ludden, P A; Stohrer, R M; Austin, K J; Atkinson, R L; Belden, E L; Harlow, H J

2009-04-01

Two experiments were conducted to determine the effects of ruminal protein degradability, supplementation frequency, and increasing dietary protein on the expression and distribution of urea transporter-B (UT-B) in lambs fed low-quality forage (mature crested wheatgrass hay; 4.2 to 4.7% CP). In Exp. 1, 15 Dorset wether lambs (initial BW=45.8+/-1.3 kg) were blocked by initial BW and assigned to 1 of 3 treatments within a randomized complete block design for 28 d, with supplements fed to achieve 7, 10, or 13% total dietary CP. In Exp. 2, 13 Dorset wether lambs (initial BW=34+/-4 kg) were used in a completely randomized design and given 1 of 4 isonitrogenous supplements: 1) ruminally degradable protein (RDP) fed daily (n=3), 2) RDP fed on alternate days (n=3), 3) ruminally undegradable protein (RUP) fed on alternate days (n=3), or 4) a 50:50 mixture of RDP and RUP fed on alternate days (n=4) for 18 d. Alternate-day treatments were fed at twice that of daily supplementation. On the last day of both experiments, lambs were killed and samples taken for Western blot analyses for UT-B. Immunoblotting using a rabbit polyclonal antibody to UT-B confirmed the presence of distinct 32-kDa (consistent with a nonglycosylated UT-B protein) and 47-kDa (probable N-glycosylated form of UT-B) protein bands in all 9 tissues analyzed. In both experiments, the liver, dorsal rumen, reticulum, and ventral rumen displayed strong bands at 32 kDa and lighter bands at 47 kDa, whereas the cecum, large colon, spiral colon, and parotid salivary gland displayed slight 32-kDa bands and stronger, more visible bands at 47 kDa. Both protein bands were apparent in the kidney at similar visual intensities in Exp. 1, whereas the relative intensities of the 2 UT-B bands in the kidney were variable, and appeared somewhat reciprocal among animals in Exp. 2. Although the abundance of the 47-kDa UT-B band in the ventral rumen was greater (P=0.03) in lambs fed RDP daily in Exp. 2, no other treatment differences (P >or= 0.15 to 0.99) in the abundance of the 32- or 47-kDa UT-B proteins within tissues were observed in either experiment. Although protein supplementation strategy had little effect on UT-B expression in tissues other than the ventral rumen, differences in the degree of glycosylation of UT-B across tissues may provide insight into its regulation.

The Milky Way above La Silla

NASA Astrophysics Data System (ADS)

2004-09-01

Anybody who visits a high-altitude astronomical observatory at this time of the year will be impressed by the beauty of the Milky Way band that stretches across the sky. Compared to the poor views from cities and other human conglomerations, the dark and bright nebulae come into view together with an astonishing palette of clear stellar colours. This view above the ESO La Silla Observatory in the southernmost part of the Atacama desert was obtained some evenings ago by ESO Software Engineer Nico Housen. Normally stationed at the Paranal Observatory, he seized the opportunity of a visit to ESO's other observatory site to produce this amazing vista of the early evening scenery. To the left is the decommisioned 15-metre dish of the Swedish-ESO Submillimetre Telescope (SEST), and on the right in the background is the dome of the ESO 3.6-metre telescope, at the highest point of the mountain. The southern Milky Way is seen along the right border of the SEST and above the 3.6 metre telescope. There is an upside-down reflection of the sky and the horizon behind the photographer in the highly polished antenna dish of the SEST. Besides the reflection of the horizon (the darker part in the top of the dish) and the Milky Way (which runs as a thin cloud from the bottom of the dish up to the horizon) there is also a yellow area of light to the right. This is the reflection of the city lights of the city of La Serena, about 100 km away and too faint to disturb observations of celestial objects high above La Silla. The 3.6-m telescope began operations in 1976 and was ESO's largest telescope until the advent of the VLT at Paranal. Never endowed with a fancy name like the VLT Unit telescopes, the "3.6-m" houses several state-of-the-art astronomical instruments, including the ultra-precise HARPS facility that is used to hunt for exoplanets, cf. ESO PR 22/04. The SEST was for a long time the only instrument of its kind in the southern hemisphere. With it, ESO gained invaluable experience in ground-based non-optical observations, paving the way for the ALMA project. The Atacama Large Millimetre Array (ALMA) [1] is one of the largest ground-based astronomy projects of the next decade after the ESO VLT. Its construction started last year and will be completed by 2011. When ready, it will be the largest and most sensitive astronomical observatory of its kind, comprisiing some sixty-four 12-m antennas located on a 10-km wide plateau at a 5000-m elevation in the Atacama Desert. More information on ALMA can be found on ESO PR 29/03 or on the ESO ALMA web page. ESO PR Photo 27/04 may be reproduced if Nico Housen and the European Southern Observatory are mentioned as source. Technical information: The photo was obtained on September 4, 2004 at about 20:45 hrs local time (00:45 hrs UT) with a Nikon D100 digital camera with a Sigma 20mm/f1.8 lens. The exposure time was about 40 sec at 1600 ASA.

The Ground-Level Enhancements of 29 September and 22 October 1989

DTIC Science & Technology

1993-01-01

3409 September 29 OLE Static Zenith Auimuth Thmrahl lwuaae % m~GV -’O0-13:0 . T 130-,,14:00 UT : Mawson 42? N -3 2.5 1.7 42? S -3 2.5 1.7 620 N -5 1.3...seen by all stations except above 2 GV. J is in units of (cm- s ster GV)-. Source direc- Mawson and the second not seen by the low latitude stations...t989 October 22 GLE sun and further studies are continuing. The main GLE was complex with several peaks. We have Time T J J 1, per Source Source

Air impacts from three alternatives for producing JP-8 jet fuel.

PubMed

Kositkanawuth, Ketwalee; Gangupomu, Roja Haritha; Sattler, Melanie L; Dennis, Brian H; MacDonnell, Frederick M; Billo, Richard; Priest, John W

2012-10-01

To increase U.S. petroleum energy independence, the University of Texas at Arlington (UT Arlington) has developed a direct coal liquefaction process which uses a hydrogenated solvent and a proprietary catalyst to convert lignite coal to crude oil. This sweet crude can be refined to form JP-8 military jet fuel, as well as other end products like gasoline and diesel. This paper presents an analysis of air pollutants resulting from using UT Arlington's liquefaction process to produce crude and then JP-8, compared with 2 alternative processes: conventional crude extraction and refining (CCER), and the Fischer-Tropsch process. For each of the 3 processes, air pollutant emissions through production of JP-8 fuel were considered, including emissions from upstream extraction/ production, transportation, and conversion/refining. Air pollutants from the direct liquefaction process were measured using a LandTEC GEM2000 Plus, Draeger color detector tubes, OhioLumex RA-915 Light Hg Analyzer, and SRI 8610 gas chromatograph with thermal conductivity detector. According to the screening analysis presented here, producing jet fuel from UT Arlington crude results in lower levels of pollutants compared to international conventional crude extraction/refining. Compared to US domestic CCER, the UTA process emits lower levels of CO2-e, NO(x), and Hg, and higher levels of CO and SO2. Emissions from the UT Arlington process for producing JP-8 are estimated to be lower than for the Fischer-Tropsch process for all pollutants, with the exception of CO2-e, which were high for the UT Arlington process due to nitrous oxide emissions from crude refining. When comparing emissions from conventional lignite combustion to produce electricity, versus UT Arlington coal liquefaction to make JP-8 and subsequent JP-8 transport, emissions from the UT Arlington process are estimated to be lower for all air pollutants, per MJ of power delivered to the end user. The United States currently imports two-thirds of its crude oil, leaving its transportation system especially vulnerable to disruptions in international crude supplies. At current use rates, U.S. coal reserves (262 billion short tons, including 23 billion short tons lignite) would last 236 years. Accordingly, the University of Texas at Arlington (UT Arlington) has developed a process that converts lignite to crude oil, at about half the cost of regular crude. According to the screening analysis presented here, producing jet fuel from UT Arlington crude generates lower levels of pollutants compared to international conventional crude extraction/refining (CCER).

5. VIEW SHOWING DOWNSTREAM FACE AND TOE OF DAM, LOOKING ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. VIEW SHOWING DOWNSTREAM FACE AND TOE OF DAM, LOOKING SOUTHWEST - High Mountain Dams in Upalco Unit, Kidney Lake Dam, Ashley National Forest, 4.7 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

7. VIEW OF INCLINED OUTLET GATE WHEEL AND STEM, LOOKING ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

7. VIEW OF INCLINED OUTLET GATE WHEEL AND STEM, LOOKING NORTH - High Mountain Dams in Upalco Unit, Kidney Lake Dam, Ashley National Forest, 4.7 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

2. VIEW SHOWING NATURAL SAND BEACH ON KIDNEY LAKE, LOOKING ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

2. VIEW SHOWING NATURAL SAND BEACH ON KIDNEY LAKE, LOOKING WEST - High Mountain Dams in Upalco Unit, Kidney Lake Dam, Ashley National Forest, 4.7 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

6. VIEW SHOWING DOWNSTREAM FACE AND TOE OF DAM, LOOKING ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

6. VIEW SHOWING DOWNSTREAM FACE AND TOE OF DAM, LOOKING SOUTHWEST - High Mountain Dams in Upalco Unit, Kidney Lake Dam, Ashley National Forest, 4.7 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

6. VIEW OF SHOWING DOWNSTREAM OUTLET PIPE AND COLLAR (12' ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

6. VIEW OF SHOWING DOWNSTREAM OUTLET PIPE AND COLLAR (12' DIAMETER CORRUGATED STEEL PIPE ENCASED IN 6' CONCRETE), LOOKING NORTH - High Mountain Dams in Bonneville Unit, Island Lake Dam, Wasatch National Forest, Kamas, Summit County, UT

5. VIEW OF UPRIGHT OUTLET GATE, STEM, STEM GUIDE AND ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. VIEW OF UPRIGHT OUTLET GATE, STEM, STEM GUIDE AND WHEEL (10' HARDESTY CAST IRON VERTICAL LIFT GATE), LOOKING WEST - High Mountain Dams in Bonneville Unit, Weir Lake Dam, Wasatch National Forest, Kamas, Summit County, UT

5. VIEW OF INCLINED OUTLET GATE WHEEL, STEM AND STEM ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. VIEW OF INCLINED OUTLET GATE WHEEL, STEM AND STEM GUIDE, (12' DIAMETER HARDESTY MODEL 112 CIRCULAR GATE), LOOKING NORTHEAST - High Mountain Dams in Bonneville Unit, Island Lake Dam, Wasatch National Forest, Kamas, Summit County, UT

4. VIEW OF INCLINED OUTLET GATE WHEEL AND STEM, LOOKING ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

4. VIEW OF INCLINED OUTLET GATE WHEEL AND STEM, LOOKING NORTHWEST - High Mountain Dams in Upalco Unit, Brown Duck Lake Dam, Ashley National Forest, 4.4 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

7. VIEW OF UPRIGHT OUTLET GATE, WHEEL STEM AND STEM ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

7. VIEW OF UPRIGHT OUTLET GATE, WHEEL STEM AND STEM GUIDE (14' DIAMETER CIRCULAR CALCO CAST IRON SLIDE GATE), LOOKING SOUTHEAST - High Mountain Dams in Bonneville Unit, Fire Lake Dam, Wasatch National Forest, Kamas, Summit County, UT

5. VIEW SHOWING INCLINED OUTLET GATE WHEEL, STEM AND STEM ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. VIEW SHOWING INCLINED OUTLET GATE WHEEL, STEM AND STEM GUIDE (28' WIDE HARDESTY CAST IRON SLIDE HEADGATE), LOOKING NORTHEAST - High Mountain Dams in Bonneville Unit, Duck Lake Dam, Wasatch National Forest, Kamas, Summit County, UT

Studies of Ionospheric Processes in the Atmosphere and the Laboratory

DTIC Science & Technology

2006-06-01

relevance to HAARP observations, and on vibrationally-excited levels of the O2 ground state [2] and the b1Σ +g excited state [3]. Synergy with the...UT [20] 29.4 (33) 260 0.94 .077 3/24/95 1737 UT 43.4 (44) 278 0.54 0.53 HAARP 62N, 145W 3/20/04 0617 UT [21] 54 (44) 290 0.33 0.54... HAARP 0.62 5.0E8 1.09E8 4.6 Studies of Ionospheric Processes in the Atmosphere and the Laboratory RTO-MP-IST-056 1 - 9 UNCLASSIFIED/UNLIMITED

Accurate procedure for deriving UTI at a submilliarcsecond accuracy from Greenwich Sidereal Time or from the stellar angle

NASA Astrophysics Data System (ADS)

Capitaine, N.; Gontier, A.-M.

1993-08-01

Present observations using modern astrometric techniques are supposed to provide the Earth orientation parameters, and therefore UT1, with an accuracy better than ±1 mas. In practice, UT1 is determined through the intermediary of Greenwich Sidereal Time (GST), using both the conventional relationship between Greenwich Mean Sidereal Time (GMST) and UTl (Aoki et al. 1982) and the so-called "equation of the equinoxes" limited to the first order terms with respect to the nutation quantities. This highly complex relation between sidereal time and UT1 is not accurate at the milliaresecond level which gives rise to spurious terms of milliaresecond amplitude in the derived UTl. A more complete relationship between GST and UT1 has been recommended by Aoki & Kinoshita (1983) and Aoki (1991) taking into account the second order terms in the difference between GST and GM ST, the largest one having an amplitude of 2.64 mas and a 18.6 yr-period. This paper explains how this complete expansion of GST implicitly uses the concept of "nonrotating origin" (NRO) as proposed by Guinot in 1979 and would, therefore, provide a more accurate value of UTl and consequently of the Earth's angular velocity. This paper shows, moreover, that such a procedure would be simplified and conceptually clarified by the explicit use of the NRO as previously proposed (Guinot 1979; Capitaine et al. 1986). The two corresponding options (implicit or explicit use of the NRO) are shown to be equivalent for defining the specific Earth's angle of rotation and then UT1. The of the use of such an accurate procedure which has been proposed in the new IERS standards (McCarthy 1992a) instead of the usual one are estimated for the practical derivation of UT1.

Cluster Observations of Particle Injections in the Exterior Cusp

NASA Astrophysics Data System (ADS)

Escoubet, C. P.; Grison, B.; Berchem, J.; Trattner, K. J.; Lavraud, B.; Pitout, F.; Soucek, J.; Richard, R. L.; Laakso, H. E.; Masson, A.; Dunlop, M. W.; Dandouras, I. S.; Reme, H.; Fazakerley, A. N.; Daly, P. W.

2014-12-01

The main process that injects solar wind plasma into the polar cusp is now generally accepted to be magnetic reconnection. Depending on the IMF direction, this process takes place equatorward (for IMF southward), poleward (for IMF northward) or on the dusk or dawn sides (for IMF azimuthal) of the cusp. We report a Cluster crossing on 5 January 2002 near the exterior cusp on the southern dusk side. The IMF was mainly azimuthal (IMF-By around -5 nT), the solar wind speed lower than usual around 280 km/s with the density of order 5 cm-3. The four Cluster spacecraft had an elongated configuration near the magnetopause. C4 was the first spacecraft to enter the cusp around 19:52:04 UT, followed by C2 at 19:52:35 UT, C1 at 19:54:24 UT and C3 at 20:13:15 UT. C4 and C1 observed two ion energy dispersions at 20:10 UT and 20:40 UT and C3 at 20:35 UT and 21:15 UT. Using the time of flight technique on the upgoing and downgoing ions, which leads to energy dispersions, we obtain distances of the ion sources between 14 and 20 RE from the spacecraft. Using Tsyganenko model, we find that these sources are located on the dusk flank, past the terminator. The first injection by C3 is seen at approximately the same time as the 2nd injection on C1 but their sources at the magnetopause were separated by more than 7 RE. This would imply that two distinct sources were active at the same time on the dusk flank of the magnetosphere. In addition, a flow reversal was observed at the magnetopause on C4 which would be an indication that reconnection is taking place near the exterior cusp.

Impact of aspirin on trophoblastic invasion in women with abnormal uterine artery Doppler at 11-14 weeks: a randomized controlled study.

PubMed

Scazzocchio, E; Oros, D; Diaz, D; Ramirez, J C; Ricart, M; Meler, E; González de Agüero, R; Gratacos, E; Figueras, F

2017-04-01

Defective trophoblastic invasion is a key feature in many cases of pre-eclampsia (PE). Uterine artery (UtA) Doppler is a validated non-invasive proxy for trophoblastic invasion. The aim of this study was to explore whether low-dose aspirin, administered from the first trimester, improves trophoblastic invasion, evaluated by UtA Doppler during the second and third trimesters in women defined as high risk by abnormal first-trimester UtA Doppler. This randomized Phase-II study had a triple-blind, parallel-arm, controlled design. Singleton pregnancies with abnormal mean UtA Doppler at 11-14 weeks and absence of other major risk factors for PE received 150 mg extended-release aspirin or identical-appearing placebo tablets from study inclusion to 28 weeks. Main outcome measure was UtA pulsatility index (PI) at 28 weeks' gestation. Secondary outcomes included frequency of development of PE and growth restriction/small-for-gestational age (SGA). A total of 155 women completed the follow-up and were analyzed. No difference in mean UtA-PI was found between women in the aspirin and placebo groups at 28 weeks (mean UtA-PI Z-score (mean ± SD), 0.99 ± 1.48 vs 0.85 ± 1.25; P = 0.52). Seven women developed PE: four (5%) in the aspirin group and three (4%) in the placebo group. There was a trend toward lower incidence of SGA in the aspirin group (8.8% vs 17.3%; P = 0.11). In women with defective trophoblastic invasion, as reflected by abnormal UtA Doppler, low-dose aspirin started in the first trimester does not have a significant effect on UtA impedance as pregnancy progresses; however, the study was underpowered to detect potential small effects . Copyright © 2016 ISUOG. Published by John Wiley & Sons Ltd. Copyright © 2016 ISUOG. Published by John Wiley & Sons Ltd.

Regulation of renal urea transport by vasopressin.

PubMed

Sands, Jeff M; Blount, Mitsi A; Klein, Janet D

2011-01-01

Terrestrial life would be miserable without the ability to concentrate urine. Production of concentrated urine requires complex interactions among the nephron segments and vasculature in the kidney medulla. In addition to water channels (aquaporins) and sodium transporters, urea transporters are critically important to the theories proposed to explain the physiologic processes occurring when urine is concentrated. Vasopressin (anti-diuretic hormone) is the key hormone regulating the production of concentrated urine. Vasopressin rapidly increases water and urea transport in the terminal inner medullary collecting duct (IMCD). Vasopressin rapidly increases urea permeability in the IMCD through increases in phosphorylation and apical plasma-membrane accumulation of the urea transporter A1 (UT-A1). Vasopressin acts through two cAMP-dependent signaling pathways in the IMCD: protein kinase A and exchange protein activated by cAMP Epac. Protein kinase A phosphorylates UT-A1 at serines 486 and 499. In summary, vasopressin regulates urea transport acutely by increasing UT-A1 phosphorylation and the apical plasma-membrane accumulation of UT-A1 through two cAMP-dependent pathways.

Issue des accouchements sur utérus cicatriciel dans un hôpital universitaire au Burkina

PubMed Central

Dembélé, Adama; Tarnagda, Zekiba; Ouédraogo, Jean Louis; Thiombiano, Oumarou; Bambara, Moussa

2012-01-01

Certains auteurs ont tendance à privilégier la césarienne comme méthode de prise en charge d'une parturiente porteuse d'un utérus cicatriciel. D'autres auteurs préconisent un accouchement par voie basse quand des paramètres cliniques précis sont observés. Le but de cette étude est d'analyser la prise en charge et l'issue des accouchements sur utérus cicatriciel au Centre Hospitalier Universitaire Souro Sanou de Bobo-Dioulasso et de la comparer aux différentes approches recommandées. Nous avons menés une étude transversale dans le Département de Gynécologie d'Obstétrique et de Médecine de la Reproduction du Centre Hospitalier Universitaire Sanou Souro de Bobo Dioulasso du 1er août 2006 au 1er août 2007 et a concerné 252 parturientes ayant un utérus cicatriciel parmi 4256 accouchements déroulés pendant la même période. Les accouchements sur utérus cicatriciels ont représenté 5,92 % de l'ensemble des accouchements dans notre département. La moyenne d'âge des patientes était de 26,2 ans et la parité moyenne de 4,3. Une césarienne d'emblée a été pratiquée chez 44% des parturientes ayant un utérus cicatriciel et 56 % parmi elles ont fait l'objet d'une épreuve utérine. Sur l'ensemble des épreuves utérines, 61% des parturientes ont accouché par voie basse. La mortalité maternelle était nulle et La mortalité périnatale était relativement importante. Les conditions d'acceptabilité de la voie basse ont été les mêmes chez toutes les patientes et un check liste a été proposé pour une meilleure prise en charge. L'épreuve utérine en salle d'accouchement doit être la règle à chaque fois que cela est possible chez une parturiente porteuse d'utérus cicatriciel. L’établissement d'un check liste pour accouchement par voie basse sur utérus cicatriciel facilite les prises de décision. PMID:23133695

On the Performance of Quorum Replication on the Internet

DTIC Science & Technology

2008-10-31

ISP in Cambridge, MA MA2 ISP in Cambridge, MA MA3 ISP in Martha’s Vineyard, MA MA4 ISP in Massachusetts, MA MD ISP in Laurel, MD MEX National...1523 171 96% 58% MA2 28% 742 1517 230 94% 59% NC 32% 465 616 255 90% 63% ISR2 3% 424 70 400 100% 97% UT1 27% 979 1847 189 96% 55% MA1 29% 645 712 238... MA2 UT2 UT1 CA1 AUS NC NZ TW KR CA2 CA3 Fig. 4. Our crumbling wall quorum system. of the first row are in North America. TW, which has lossy

The Calibration Units of the KM3NeT neutrino telescope

NASA Astrophysics Data System (ADS)

Baret, B.; Keller, P.; Clark, M. Lindsey

2016-04-01

KM3NeT is a network of deep-sea neutrino telescopes to be deployed in the Mediterranean Sea that will perform neutrino astronomy and oscillation studies. It consists of three-dimensional arrays of thousands of optical modules that detect the Cherenkov light induced by charged particles resulting from the interaction of a neutrino with the surrounding medium. The performance of the neutrino telescope relies on the precise timing and positioning calibration of the detector elements. Other environmental conditions which may affect light and sound transmission, such as water temperature and salinity, must also be continuously monitored. This contribution describes the technical design of the first Calibration Unit, to be deployed on the French site as part of KM3NeT Phase 1.

CRTS-II Detection of Increased Optical Activity from CTA 102

NASA Astrophysics Data System (ADS)

Djorgovski, S. G.; Drake, A. J.; Mahabal, A. A.; Graham, M. J.; Christensen, E.; Larson, S. M.

2017-12-01

We report the detection of significant optical brightening of FSRQ CTA 102 by CRTS-II on 2017 Dec. 8.15 UT. At that time CTA 102 was seen to have risen approximately 1.4 mags (to V_CSS = 14.15) compared with previous observations taken on 2017 Nov. 23 UT. Additional survey observations taken on 2017 Dec. 15 UT show CTA 102 at V_CSS = 14.05.

VizieR Online Data Catalog: The populations of Carina. II. Abundances (Norris+, 2017)

NASA Astrophysics Data System (ADS)

Norris, J. E.; Yong, D.; Venn, K. A.; Gilmore, G.; Casagrande, L.; Dotter, A.

2017-08-01

Our selection of objects is based on unpublished CCD V, I observations that we have made of the Carina galaxy. High-resolution, moderate-S/N spectra were obtained of 39 Carina red giants, during 2007 November-2008 March, with the FLAMES system at the 8.2m Kueyen (VLT/UT2) telescope at Cerro Paranal. The spectra cover the wavelength ranges 4800-5750Å and 5840-6800Å. The resolving power was R=47000. Photometry has been obtained from several sources: P. B. Stetson provided us with homogenized BVI, M. J. Irwin furnished JHK from ESO VISTA survey photometry, and M. Gullieuszik supplied BVIJHKs. (12 data files).

An afocal telescope configuration for the ESA Ariel mission

NASA Astrophysics Data System (ADS)

Da Deppo, V.; Middleton, K.; Focardi, M.; Morgante, G.; Pace, E.; Claudi, R.; Micela, G.

2017-09-01

ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) is one of the three candidates for the next ESA medium-class science mission (M4) expected to be launched in 2026. This mission will be devoted to observing spectroscopically in the infrared (IR) a large population of known transiting planets in the neighborhood of the Solar System, opening a new discovery space in the field of extrasolar planets and enabling the understanding of the physics and chemistry of these far away worlds. ARIEL is based on a 1-m class telescope ahead of two spectrometer channels covering the band 1.95 to 7.8 microns. In addition there are four photometric channels: two wide band, also used as fine guidance sensors, and two narrow band. During its 3.5 years of operations from L2 orbit, ARIEL will continuously observe exoplanets transiting their host star. The ARIEL optical design is conceived as a fore-module common afocal telescope that will feed the spectrometer and photometric channels. The telescope optical design is composed of an off-axis portion of a two-mirror classic Cassegrain coupled to a tertiary off-axis paraboloidal mirror. The telescope and optical bench operating temperatures, as well as those of some subsystems, will be monitored and fine tuned/stabilised mainly by means of a thermal control subsystem (TCU-Telescope Control Unit) working in closed-loop feedback and hosted by the main Payload electronics unit, the Instrument Control Unit (ICU). Another important function of the TCU will be to monitor the telescope and optical bench thermistors when the Payload decontamination heaters will be switched on (when operating the instrument in Decontamination Mode) during the Commissioning Phase and cyclically, if required. Then the thermistors data will be sent by the ICU to the On Board Computer by means of a proper formatted telemetry. The latter (OBC) will be in charge of switching on and off the decontamination heaters on the basis of the thermistors readout values.

5. VIEW OF UPRIGHT OUTLET GATE WHEEL, STEM AND STEM ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. VIEW OF UPRIGHT OUTLET GATE WHEEL, STEM AND STEM GUIDE, LOOKING NORTHWEST - High Mountain Dams in Upalco Unit, Drift Lake Dam, Ashley National Forest, 11.4 miles Northwest of Swift Creek Campground, Mountain Home, Duchesne County, UT

Role of thin descending limb urea transport in renal urea handling and the urine concentrating mechanism

PubMed Central

Lei, Tianluo; Zhou, Lei; Layton, Anita T.; Zhou, Hong; Zhao, Xuejian; Bankir, Lise

2011-01-01

Urea transporters UT-A2 and UT-B are expressed in epithelia of thin descending limb of Henle's loop and in descending vasa recta, respectively. To study their role and possible interaction in the context of the urine concentration mechanism, a UT-A2 and UT-B double knockout (UT-A2/B knockout) mouse model was generated by targeted deletion of the UT-A2 promoter in embryonic stem cells with UT-B gene knockout. The UT-A2/B knockout mice lacked detectable UT-A2 and UT-B transcripts and proteins and showed normal survival and growth. Daily urine output was significantly higher in UT-A2/B knockout mice than that in wild-type mice and lower than that in UT-B knockout mice. Urine osmolality in UT-A2/B knockout mice was intermediate between that in UT-B knockout and wild-type mice. The changes in urine osmolality and flow rate, plasma and urine urea concentration, as well as non-urea solute concentration after an acute urea load or chronic changes in protein intake suggested that UT-A2 plays a role in the progressive accumulation of urea in the inner medulla. These results suggest that in wild-type mice UT-A2 facilitates urea absorption by urea efflux from the thin descending limb of short loops of Henle. Moreover, UT-A2 deletion in UT-B knockout mice partially remedies the urine concentrating defect caused by UT-B deletion, by reducing urea loss from the descending limbs to the peripheral circulation; instead, urea is returned to the inner medulla through the loops of Henle and the collecting ducts. PMID:21849488

Role of thin descending limb urea transport in renal urea handling and the urine concentrating mechanism.

PubMed

Lei, Tianluo; Zhou, Lei; Layton, Anita T; Zhou, Hong; Zhao, Xuejian; Bankir, Lise; Yang, Baoxue

2011-12-01

Urea transporters UT-A2 and UT-B are expressed in epithelia of thin descending limb of Henle's loop and in descending vasa recta, respectively. To study their role and possible interaction in the context of the urine concentration mechanism, a UT-A2 and UT-B double knockout (UT-A2/B knockout) mouse model was generated by targeted deletion of the UT-A2 promoter in embryonic stem cells with UT-B gene knockout. The UT-A2/B knockout mice lacked detectable UT-A2 and UT-B transcripts and proteins and showed normal survival and growth. Daily urine output was significantly higher in UT-A2/B knockout mice than that in wild-type mice and lower than that in UT-B knockout mice. Urine osmolality in UT-A2/B knockout mice was intermediate between that in UT-B knockout and wild-type mice. The changes in urine osmolality and flow rate, plasma and urine urea concentration, as well as non-urea solute concentration after an acute urea load or chronic changes in protein intake suggested that UT-A2 plays a role in the progressive accumulation of urea in the inner medulla. These results suggest that in wild-type mice UT-A2 facilitates urea absorption by urea efflux from the thin descending limb of short loops of Henle. Moreover, UT-A2 deletion in UT-B knockout mice partially remedies the urine concentrating defect caused by UT-B deletion, by reducing urea loss from the descending limbs to the peripheral circulation; instead, urea is returned to the inner medulla through the loops of Henle and the collecting ducts.

ON THE APPARENT ORBITAL INCLINATION CHANGE OF THE EXTRASOLAR TRANSITING PLANET TrES-2b

DOE Office of Scientific and Technical Information (OSTI.GOV)

Scuderi, Louis J.; Dittmann, Jason A.; Males, Jared R.

2010-05-01

On 2009 June 15 UT the transit of TrES-2b was detected using the University of Arizona's 1.55 m Kuiper Telescope with 2.0-2.5 millimag rms accuracy in the I band. We find a central transit time of T{sub c} = 2454997.76286 {+-} 0.00035 HJD, an orbital period of P = 2.4706127 {+-} 0.0000009 days, and an inclination angle of i = 83.{sup 0}92 {+-} 0{sup 0}.05, which is consistent with our re-fit of the original I-band light curve of O'Donovan et al. where we find i = 83.{sup 0}84 {+-} 0{sup 0}.05. We calculate an insignificant inclination change of {Delta}i =more » -0.{sup 0}08 {+-} 0{sup 0}.07 over the last three years, and as such, our observations rule out, at the {approx}11{sigma} level, the apparent change of orbital inclination to i{sub predicted} = 83.{sup 0}35 {+-} 0{sup 0}.1 as predicted by Mislis and Schmitt and Mislis et al. for our epoch. Moreover, our analysis of a recently published Kepler Space Telescope light curve for TrES-2b finds an inclination of i = 83.{sup 0}91 {+-} 0.{sup 0}03 for a similar epoch. These Kepler results definitively rule out change in i as a function of time. Indeed, we detect no significant changes in any of the orbital parameters of TrES-2b.« less

Evaluation of three elevated mist-net systems for sampling birds

USGS Publications Warehouse

Meyers, J.M.; Pardieck, K.L.

1993-01-01

Three light-weight, low-canopy mist-net systems were developed and tested in dry tropical scrub, mangrove and forest habitats. One plastic (polyvinyl chloride) and two aluminum pole systems (with and without pulleys) were used to support mist nets to heights of up to 7.3 m. Although the aluminum telescoping-pole system (without pulleys) was expensive initially ( 79-141/unit (US)), its use reduced capture of nontarget species and may have increased capture of target species when compared with ground-level netting. In one year, its use also reduced labor costs by 756, which completely offset the higher cost of the aluminum telescoping-pole system when compared to the plastic-pole system ( 19/unit). Unlike the plastic-pole system, the aluminum telescoping-pole system was adjustable to any height within its range of 1.8 to 7.3 m, was 1.5 m higher, was more efficient to operate in the field, and was easily moved to new locations. For capture of psittacines, the pulleys of the aluminum telescoping-pole system were not necessary, but their use may assist in efficiently retrieving large numbers of birds from the nets. The aluminum telescoping-pole system was efficient in capturing psittacines, columbids, passerines and possibly chiropterans in habitats with canopies lt 10 m or in the forest subcanopy.

Automated ambiguity estimation for VLBI Intensive sessions using L1-norm

NASA Astrophysics Data System (ADS)

Kareinen, Niko; Hobiger, Thomas; Haas, Rüdiger

2016-12-01

Very Long Baseline Interferometry (VLBI) is a space-geodetic technique that is uniquely capable of direct observation of the angle of the Earth's rotation about the Celestial Intermediate Pole (CIP) axis, namely UT1. The daily estimates of the difference between UT1 and Coordinated Universal Time (UTC) provided by the 1-h long VLBI Intensive sessions are essential in providing timely UT1 estimates for satellite navigation systems and orbit determination. In order to produce timely UT1 estimates, efforts have been made to completely automate the analysis of VLBI Intensive sessions. This involves the automatic processing of X- and S-band group delays. These data contain an unknown number of integer ambiguities in the observed group delays. They are introduced as a side-effect of the bandwidth synthesis technique, which is used to combine correlator results from the narrow channels that span the individual bands. In an automated analysis with the c5++ software the standard approach in resolving the ambiguities is to perform a simplified parameter estimation using a least-squares adjustment (L2-norm minimisation). We implement L1-norm as an alternative estimation method in c5++. The implemented method is used to automatically estimate the ambiguities in VLBI Intensive sessions on the Kokee-Wettzell baseline. The results are compared to an analysis set-up where the ambiguity estimation is computed using the L2-norm. For both methods three different weighting strategies for the ambiguity estimation are assessed. The results show that the L1-norm is better at automatically resolving the ambiguities than the L2-norm. The use of the L1-norm leads to a significantly higher number of good quality UT1-UTC estimates with each of the three weighting strategies. The increase in the number of sessions is approximately 5% for each weighting strategy. This is accompanied by smaller post-fit residuals in the final UT1-UTC estimation step.

GNOSIS: a novel near-infrared OH suppression unit at the AAT

NASA Astrophysics Data System (ADS)

Trinh, C. Q.; Ellis, S. C.; Lawrence, J. S.; Horton, A. J.; Bland-Hawthorn, J.; Leon-Saval, S. G.; Bryant, J.; Case, S.; Colless, M.; Couch, W.; Freeman, K.; Gers, L.; Glazebrook, K.; Haynes, R.; Lee, S.; Löhmannsröben, H.-G.; Miziarski, S.; O'Byrne, J.; Rambold, W.; Roth, M. M.; Schmidt, B.; Shortridge, K.; Smedley, S.; Tinney, C. G.; Xavier, P.; Zheng, J.

2012-09-01

GNOSIS has provided the first on-telescope demonstration of a concept to utilize complex aperioidc fiber Bragg gratings to suppress the 103 brightest atmospheric hydroxyl emission doublets between 1.47-1.7 μm. The unit is designed to be used at the 3.9-meter Anglo-Australian Telescope (AAT) feeding the IRIS2 spectrograph. Unlike previous atmospheric suppression techniques GNOSIS suppresses the lines before dispersion. We present the results of laboratory and on-sky tests from instrument commissioning. These tests reveal excellent suppression performance by the gratings and high inter-notch throughput, which combine to produce high fidelity OH-free spectra.

E-ELT M5 field stabilisation unit scale 1 demonstrator design and performances evaluation

NASA Astrophysics Data System (ADS)

Casalta, J. M.; Barriga, J.; Ariño, J.; Mercader, J.; San Andrés, M.; Serra, J.; Kjelberg, I.; Hubin, N.; Jochum, L.; Vernet, E.; Dimmler, M.; Müller, M.

2010-07-01

The M5 Field stabilization Unit (M5FU) for European Extremely Large Telescope (E-ELT) is a fast correcting optical system that shall provide tip-tilt corrections for the telescope dynamic pointing errors and the effect of atmospheric tiptilt and wind disturbances. A M5FU scale 1 demonstrator (M5FU1D) is being built to assess the feasibility of the key elements (actuators, sensors, mirror, mirror interfaces) and the real-time control algorithm. The strict constraints (e.g. tip-tilt control frequency range 100Hz, 3m ellipse mirror size, mirror first Eigen frequency 300Hz, maximum tip/tilt range +/- 30 arcsec, maximum tiptilt error < 40 marcsec) have been a big challenge for developing the M5FU Conceptual Design and its scale 1 demonstrator. The paper summarises the proposed design for the final unit and demonstrator and the measured performances compared to the applicable specifications.

Peripheral markers of central fatigue in trained and untrained during uncompensable heat stress.

PubMed

Wright, Heather E; Selkirk, Glen A; Rhind, Shawn G; McLellan, Tom M

2012-03-01

The development of fatigue is more pronounced in the heat than thermoneutral environments; however, it is unclear whether biomarkers of central fatigue are consistent with the higher core temperature (T (c)) tolerated by endurance trained (TR) versus untrained (UT) during exertional heat stress (EHS). The purpose of this study was to examine the indicators of central fatigue during EHS in TR versus UT. Twelve TR and 11 UT males (mean ± SE [Formula: see text] = 70 ± 2 and 50 ± 1 mL kg LBM(-1) min(-1), respectively) walked on a treadmill to exhaustion (EXH) in 40°C (dry) wearing protective clothing. Venous blood was obtained at PRE and 0.5°C T (c) increments from 38 to 40°C/EXH. Free tryptophan (f-TRP) decreased dramatically at 39.5°C for the TR. Branch chain amino acids decreased with T (c) and were greater for UT than TR at EXH. Tyrosine and phenylalanine remained unchanged. Serum S100β was undetectable (<5 pg mL(-1)). Albumin was greater for the UT from PRE to 39.0°C and at EXH. Prolactin (PRL) responded to relative thermal strain with similar EXH values despite higher T (c) tolerated for TR (39.7 ± 0.09°C) than UT (39.0 ± 0.09°C). The high EXH PRL values for both groups support its use as a biomarker of the serotonin and dopamine interplay within the brain during the development of central fatigue.

ACE ID genotype and the muscle strength and size response to unilateral resistance training.

PubMed

Pescatello, Linda S; Kostek, Matthew A; Gordish-Dressman, Heather; Thompson, Paul D; Seip, Richard L; Price, Thomas B; Angelopoulos, Theodore J; Clarkson, Priscilla M; Gordon, Paul M; Moyna, Niall M; Visich, Paul S; Zoeller, Robert F; Devaney, Joseph M; Hoffman, Eric P

2006-06-01

To examine associations among the angiotensin I-converting enzyme (ACE) insertion (I)/deletion (D) polymorphism and the response to a 12-wk (2 d.wk) unilateral, upper-arm resistance training (RT) program in the trained (T, nondominant) and untrained (UT, dominant) arms. Subjects were 631 (mean+/-SEM, 24.2+/-0.2 yr) white (80%) men (42%) and women (58%). The ACE ID genotype was in Hardy-Weinberg equilibrium with frequencies of 23.1, 46.1, and 30.8% for ACE II, ID, and DD, respectively (chi=1.688, P=0.430). Maximum voluntary contraction (MVC) and one-repetition maximum (1RM) assessed peak elbow flexor muscle strength. Magnetic resonance imaging measured biceps muscle cross-sectional area (CSA). Multiple variable and repeated-measures ANCOVA tested whether muscle strength and size differed at baseline and pre- to post-RT among T and UT and ACE ID genotype. Baseline muscle strength and size were greater in UT than T (P<0.001) and did not differ among ACE ID genotype in either arm (P >or= 0.05). In T, MVC increases were greater for ACE II/ID (22%) than DD (17%) (P<0.05), whereas 1RM (51%) and CSA (19%) gains were not different among ACE ID genotype pre- to post-RT (P >or= 0.05). In UT, MVC increased among ACE II/ID (7%) (P<0.001) but was similar among ACE DD (2%) pre- to post-RT (P >or= 0.05). In UT, 1RM (11%) and CSA (2%) increases were greater for ACE DD/ID than ACE II (1RM, 7%; CSA, -0.1%) (P<0.05). ACE ID genotype explained approximately 1% of the MVC response to RT in T and approximately 2% of MVC, 2% of 1RM, and 4% of CSA response in UT (P<0.05). ACE ID genotype is associated with the contralateral effects of unilateral RT, perhaps more so than with the muscle strength and size adaptations that result from RT.

Robust Ambiguity Estimation for an Automated Analysis of the Intensive Sessions

NASA Astrophysics Data System (ADS)

Kareinen, Niko; Hobiger, Thomas; Haas, Rüdiger

2016-12-01

Very Long Baseline Interferometry (VLBI) is a unique space-geodetic technique that can directly determine the Earth's phase of rotation, namely UT1. The daily estimates of the difference between UT1 and Coordinated Universal Time (UTC) are computed from one-hour long VLBI Intensive sessions. These sessions are essential for providing timely UT1 estimates for satellite navigation systems. To produce timely UT1 estimates, efforts have been made to completely automate the analysis of VLBI Intensive sessions. This requires automated processing of X- and S-band group delays. These data often contain an unknown number of integer ambiguities in the observed group delays. In an automated analysis with the c5++ software the standard approach in resolving the ambiguities is to perform a simplified parameter estimation using a least-squares adjustment (L2-norm minimization). We implement the robust L1-norm with an alternative estimation method in c5++. The implemented method is used to automatically estimate the ambiguities in VLBI Intensive sessions for the Kokee-Wettzell baseline. The results are compared to an analysis setup where the ambiguity estimation is computed using the L2-norm. Additionally, we investigate three alternative weighting strategies for the ambiguity estimation. The results show that in automated analysis the L1-norm resolves ambiguities better than the L2-norm. The use of the L1-norm leads to a significantly higher number of good quality UT1-UTC estimates with each of the three weighting strategies.

Millimeter and X-Ray Emission from the 5 July 2012 Solar Flare

NASA Astrophysics Data System (ADS)

Tsap, Y. T.; Smirnova, V. V.; Motorina, G. G.; Morgachev, A. S.; Kuznetsov, S. A.; Nagnibeda, V. G.; Ryzhov, V. S.

2018-03-01

The 5 July 2012 solar flare SOL2012-07-05T11:44 (11:39 - 11:49 UT) with an increasing millimeter spectrum between 93 and 140 GHz is considered. We use space and ground-based observations in X-ray, extreme ultraviolet, microwave, and millimeter wave ranges obtained with the Reuven Ramaty High-Energy Solar Spectroscopic Imager, Solar Dynamics Observatory (SDO), Geostationary Operational Environmental Satellite, Radio Solar Telescope Network, and Bauman Moscow State Technical University millimeter radio telescope RT-7.5. The main parameters of thermal and accelerated electrons were determined through X-ray spectral fitting assuming the homogeneous thermal source and thick-target model. From the data of the Atmospheric Imaging Assembly/SDO and differential-emission-measure calculations it is shown that the thermal coronal plasma gives a negligible contribution to the millimeter flare emission. Model calculations suggest that the observed increase of millimeter spectral flux with frequency is determined by gyrosynchrotron emission of high-energy (≳ 300 keV) electrons in the chromosphere. The consequences of the results are discussed in the light of the flare-energy-release mechanisms.

SAAO's new robotic telescope and WiNCam (Wide-field Nasmyth Camera)

NASA Astrophysics Data System (ADS)

Worters, Hannah L.; O'Connor, James E.; Carter, David B.; Loubser, Egan; Fourie, Pieter A.; Sickafoose, Amanda; Swanevelder, Pieter

2016-08-01

The South African Astronomical Observatory (SAAO) is designing and manufacturing a wide-field camera for use on two of its telescopes. The initial concept was of a Prime focus camera for the 74" telescope, an equatorial design made by Grubb Parsons, where it would employ a 61mmx61mm detector to cover a 23 arcmin diameter field of view. However, while in the design phase, SAAO embarked on the process of acquiring a bespoke 1-metre robotic alt-az telescope with a 43 arcmin field of view, which needs a homegrown instrument suite. The Prime focus camera design was thus adapted for use on either telescope, increasing the detector size to 92mmx92mm. Since the camera will be mounted on the Nasmyth port of the new telescope, it was dubbed WiNCam (Wide-field Nasmyth Camera). This paper describes both WiNCam and the new telescope. Producing an instrument that can be swapped between two very different telescopes poses some unique challenges. At the Nasmyth port of the alt-az telescope there is ample circumferential space, while on the 74 inch the available envelope is constrained by the optical footprint of the secondary, if further obscuration is to be avoided. This forces the design into a cylindrical volume of 600mm diameter x 250mm height. The back focal distance is tightly constrained on the new telescope, shoehorning the shutter, filter unit, guider mechanism, a 10mm thick window and a tip/tilt mechanism for the detector into 100mm depth. The iris shutter and filter wheel planned for prime focus could no longer be accommodated. Instead, a compact shutter with a thickness of less than 20mm has been designed in-house, using a sliding curtain mechanism to cover an aperture of 125mmx125mm, while the filter wheel has been replaced with 2 peripheral filter cartridges (6 filters each) and a gripper to move a filter into the beam. We intend using through-vacuum wall PCB technology across the cryostat vacuum interface, instead of traditional hermetic connector-based wiring. This has advantages in terms of space saving and improved performance. Measures are being taken to minimise the risk of damage during an instrument change. The detector is cooled by a Stirling cooler, which can be disconnected from the cooler unit without risking damage. Each telescope has a dedicated cooler unit into which the coolant hoses of WiNCam will plug. To overcome an inherent drawback of Stirling coolers, an active vibration damper is incorporated. During an instrument change, the autoguider remains on the telescope, and the filter magazines, shutter and detector package are removed as a single unit. The new alt-az telescope, manufactured by APM-Telescopes, is a 1-metre f/8 Ritchey-Chrétien with optics by LOMO. The field flattening optics were designed by Darragh O'Donoghue to have high UV throughput and uniform encircled energy over the 100mm diameter field. WiNCam will be mounted on one Nasmyth port, with the second port available for SHOC (Sutherland High-speed Optical Camera) and guest instrumentation. The telescope will be located in Sutherland, where an existing dome is being extensively renovated to accommodate it. Commissioning is planned for the second half of 2016.

Musculoskeletal health profile for elite female footballers versus untrained young women before and after 16 weeks of football training.

PubMed

Jackman, Sarah R; Scott, Suzanne; Randers, Morten Bredsgaard; Orntoft, Christina; Blackwell, Jamie; Zar, Abdossaleh; Helge, Eva Wulff; Mohr, Magni; Krustrup, Peter

2013-01-01

We investigated the musculoskeletal health profile of elite female football players (ET) in comparison to untrained (UT) young women subjected to 16 weeks of football training (2 × 1 h per week). DXA scans, blood sampling, sprint testing and Flamingo postural balance testing were carried out for 27 Danish national team players and 28 untrained women, with eight women being tested after training. At baseline total BMD and BMC were 13% (1.305 ± 0.050 versus 1.159 ± 0.056 g · cm(-2)) and 23% (3047 ± 235 versus 2477 ± 526 g) higher (P <0.001) and leg BMD and BMC were 24 and 28% higher (P <0.01) in ET than in UT. Resting plasma osteocalcin was 45% higher in ET than in UT (28.8 ± 10.9 versus 19.9 ± 9.9 µg · L(-1), P <0.05). Total lean body mass was 14% higher (50.4 ± 3.3 versus 44.3 ± 4.0 kg) in ET compared with UT, with no difference in total body mass. The number of Flamingo test falls was 56-63% less (P <0.01) and 30 m sprinting speed was 31% faster (P <0.001) in ET than UT. After 16 weeks of football training for UT, lean body mass increased by 1.4 ± 0.5 kg and the number of left leg falls decreased by 29% (P <0.05). No significant changes occurred in BMD or BMC, but plasma osteocalcin increased (P <0.05) by 37%. In summary, elite women footballers have an impressive musculoskeletal health profile compared with untrained controls, but short-term football training seems to reduce the risk of falls and increase bone formation.

6. VIEW SHOWING CREST OF DAM AND OUTLET GATE WHEEL, ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

6. VIEW SHOWING CREST OF DAM AND OUTLET GATE WHEEL, STEM AND STEM GUIDE, LOOKING SOUTHEAST - High Mountain Dams in Upalco Unit, Milk Lake Dam, Ashley National Forest, 9.4 miles Northwest of Swift Creek Campground, Mountain Home, Duchesne County, UT

6. VIEW OF OUTLET GATE WHEEL AND STEM, WITH OUTLET ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

6. VIEW OF OUTLET GATE WHEEL AND STEM, WITH OUTLET CHANNEL IN BACKGROUND, LOOKING SOUTHEAST - High Mountain Dams in Upalco Unit, Island Lake Dam, Ashley National Forest, 4.8 miles North of Miners Gulch Campground, Mountain Home, Duchesne County, UT

Cerebro-renal interactions: impact of uremic toxins on cognitive function.

PubMed

Watanabe, Kimio; Watanabe, Tsuyoshi; Nakayama, Masaaki

2014-09-01

Cognitive impairment (CI) associated with chronic kidney disease (CKD) has received attention as an important problem in recent years. Causes of CI with CKD are multifactorial, and include cerebrovascular disease, renal anemia, secondary hyperparathyroidism, dialysis disequilibrium, and uremic toxins (UTs). Among these causes, little is known about the role of UTs. We therefore selected 21 uremic compounds, and summarized reports of cerebro-renal interactions associated with UTs. Among the compounds, uric acid, indoxyl sulfate, p-cresyl sulfate, interleukin 1-β, interleukin 6, TNF-α, and PTH were most likely to affect the cerebro-renal interaction dysfunction; however, sufficient data have not been obtained for other UTs. Notably, most of the data were not obtained under uremic conditions; therefore, the impact and mechanism of each UT on cognition and central nervous system in uremic state remains unknown. At present, impacts and mechanisms of UT effects on cognition are poorly understood. Clarifying the mechanisms and establishing novel therapeutic strategies for cerebro-renal interaction dysfunction is expected to be subject of future research. Copyright © 2014 Elsevier Inc. All rights reserved.

Development of Primary Volatile Production in COMET C/20O9 Pl (GARRADD) During its 2011-2O12 Apparition

NASA Technical Reports Server (NTRS)

Mumma, M. J.; {agamomo. :/; Vo; DiSanti, M. A.; Bonev, B. P.; Lippi, M.; Boehnhardt, H.; Keane, J. V.; Meech, K. J.; Blake, G. A.

2012-01-01

We quantified primary volatiles in comet C/2009 Pl (Garradd) through pre- and post-perihelion observations acquired during its apparition in 2011-12 [1,2,3]. Detected volatiles include H2O, CO, CH4, C2H2, C2H6, HCN, NH3, H2CO, and CH3OH. We present production rates and chemical abundance ratios (relative to water) for all species, and I-D spatial profiles for multiple primary volatiles. We discuss these findings in the context of an emerging taxonomy based on primary volatiles in comets [4]. We used three spectrometer/telescope combinations. On UT 20ll August 7 (Rh 2.4 AU) and September 17-21 (Rh 2.0 AU), we used CRIRES at ESO's Very Large Telescope (VLT) [1]. On September 8 and 9 (Rh 2.1 AU), we used NIRSPEC at Keck-2 and CSHELL at IRTF [2]. Using NIRSPEC on October 13 and 2012 January 08 (Rh 1.83 and 1.57 AU, respectively), we detected nine primary volatiles pre-perihelion, and six post-perihelion [3]. CO was enriched in Garradd while C2H2 was strongly depleted. C2H6 and CH3OH displayed abundances close to those measured for the majority of Oort cloud comets observed to date. The high fractional abundance of CO identifies comet C12009 P1 as a CO-rich comet. Spatial profiles revealed notable differences among individual primary species. Given the relatively large heliocentric distance of C/2009 Pl, we explored the effect of water not being fully sublimated within our field of view and we identi$, the "missing" water fraction needed to reconcile the retrieved abundance ratios with the mean values found for "organics-normal" comets.

A close look into the carbon disk at the core of the planetary nebula CPD-56°8032

NASA Astrophysics Data System (ADS)

Chesneau, O.; Collioud, A.; De Marco, O.; Wolf, S.; Lagadec, E.; Zijlstra, A. A.; Rothkopf, A.; Acker, A.; Clayton, G. C.; Lopez, B.

2006-09-01

Aims.We present high spatial resolution observations of the dusty core of the Planetary Nebula with Wolf-Rayet central star CPD-56°8032, for which indications of a compact disk have been found by HST/SITS observations. Methods: .These observations were taken with the mid-infrared interferometer VLTI/MIDI in imaging mode providing a typical 300 mas resolution and in interferometric mode using UT2-UT3 47m baseline providing a typical spatial resolution of 20 mas. We also made use of unpublished HST/ACS images in the F435W and F606W filters. Results: .The visible HST images exhibit a complex multilobal geometry dominated by faint lobes. The farthest structures are located at 7 arcsec from the star. The mid-IR environment of CPD-56°8032 is dominated by a compact source, barely resolved by a single UT telescope in a 8.7 μm filter (Δ λ=1.6~μm, contaminated by PAH emission). The infrared core is almost fully resolved with the three 40-45 m projected baselines ranging from -5° to 51° but smooth oscillating fringes at low level have been detected in spectrally dispersed visibilities. This clear signal is interpreted in terms of a ring structure which would define the bright inner rim of the equatorial disk. Geometric models allowed us to derive the main geometrical parameters of the disk. For instance, a reasonably good fit is reached with an achromatic and elliptical truncated Gaussian with a radius of 97±11 AU, an inclination of 28±7° and a PA for the major axis at 345° ±7°. Furthermore, we performed some radiative transfer modeling aimed at further constraining the geometry and mass content of the disk, by taking into account the MIDI dispersed visibilities, spectra, and the large aperture SED of the source. These models show that the disk is mostly optically thin in the N band and highly flared. As a consequence of the complex flux distribution, an edge-on inclination is not excluded by the data.

Modelling of Lunar Laser Ranging in the Geocentric Frame and Comparison with the Common-View Double-Difference Lunar Laser Ranging Approach

NASA Astrophysics Data System (ADS)

Svehla, D.; Rothacher, M.

2016-12-01

Is it possible to process Lunar Laser Ranging (LLR) measurements in the geocentric frame in a similar way SLR measurements are modelled for GPS satellites and estimate all global reference frame parameters like in the case of GPS? The answer is yes. We managed to process Lunar laser measurements to Apollo and Luna retro-reflectors on the Moon in a similar way we are processing SLR measurements to GPS satellites. We make use of the latest Lunar libration models and DE430 ephemerides given in the Solar system baricentric frame and model uplink and downlink Lunar laser ranges in the geocentric frame as one way measurements, similar to SLR measurements to GPS satellites. In the first part of this contribution we present the estimation of the Lunar orbit as well as the Earth orientation parameters (including UT1 or UT0) with this new formulation. In the second part, we form common-view double-difference LLR measurements between two Lunar retro-reflectors and two LLR telescopes to show the actual noise of the LLR measurements. Since, by forming double-differences of LLR measurements, all range biases are removed and orbit errors are significantly reduced (the Lunar orbit is much farther away than the GPS orbits), one can consider double-difference LLR as an "orbit-free" and "bias-free" differential approach. In the end, we make a comparison with the SLR double-difference approach with Galileo satellites, where we already demonstrated submillimeter precision, and discuss possible combination of LLR and SLR to GNSS satellites using double-difference approach.

Lessons Learned and Lessons To Be Learned: An Overview of Innovative Network Learning Environments.

ERIC Educational Resources Information Center

Jacobson, Michael J.; Jacobson, Phoebe Chen

This paper provides an overview of five innovative projects involving network learning technologies in the United States: (1) the MicroObservatory Internet Telescope is a collection of small, high-quality, and low-maintenance telescopes operated by the Harvard-Smithsonian Center for Astrophysics (Massachusetts), which may be used remotely via the…

Usability Tests in Medicine: A Cost-Benefit Analysis for Hospitals Before Acquiring Medical Devices for Theatre.

PubMed

Gonser, Phillipp; Fuchsberger, Thomas; Matern, Ulrich

2017-08-01

The use of active medical devices in clinical routine should be as safe and efficient as possible. Usability tests (UTs) help improve these aspects of medical devices during their development, but UTs can be of use for hospitals even after a product has been launched. The present pilot study examines the costs and possible benefits of UT for hospitals before buying new medical devices for theatre. Two active medical devices with different complexity were tested in a standardized UT and a cost-benefit analysis was carried out assuming a different device bought at the same price with a higher usability could increase the efficiency of task solving and due to that save valuable theatre time. The cost of the UT amounted up to €19.400. Hospitals could benefit from UTs before buying new devices for theatre by reducing time-consuming operator errors and thereby increase productivity and patient safety. The possible benefits amounted from €23.300 to €1.570.000 (median = €797.000). Not only hospitals could benefit economically from investing in a UT before deciding to buy a medical device, but especially patients would profit from a higher usability by reducing possible operator errors and increase safety and performance of use.

Analysis of readability and quality of web pages addressing both common and uncommon topics in pediatric surgery.

PubMed

Adorisio, Ottavio; Silveri, Massimiliano; Rivosecchi, Massimo; Tozzi, Alberto Eugenio; Scottoni, Federico; Buonuomo, Paola Sabrina

2012-06-01

The quality medical information on Internet is highly variable. The aim of this study is to determine if Web pages addressing four common pediatric surgical topics (CT) and four uncommon pediatric surgical topics (UT) differ significantly in terms of quality and/or characteristics. We performed an Internet search regarding four CT, addressing more frequent clinical conditions with an incidence≤1:1.500 children (inguinal hernia, varicocele, umbilical hernia, and phimosis) and four UT addressing less frequent clinical conditions with an incidence≥1:1.500 children (anorectal malformation, intestinal atresia, gastroschisis, and omphalocele), using a popular search engine (Google). We evaluated readability with the Flesch reading ease (FRE) and the Flesch-Kincaid grade (FKG) and quality of content using the site checker of the HON Code of Conduct (HON code) for each website. In this study, 30/40 websites addressing CT versus 33/50 addressing UT responded to our criteria. No differences statistically significant in advertisements between the two groups were found (15 vs. 16%) (p>0.05). No differences were found in terms of time from last update, owner/author type, financial disclosure, accreditation, or advertising. CT had higher quality level according to the HON code (6.54±1.38 vs. 5.05±1.82) (p<0.05). Mean FRE was 47.38±14.27 versus 46.24±14.56, respectively, for CT and UT (p>0.05). The mean FKG was 8.1±1.9 for CT versus 8±1.9 for UT (p>0.05). Websites devoted to pediatric surgical topics have higher readability and quality information for disease diagnosis and natural history. Otherwise, the quality of pediatric surgical information on the Internet is high for CT and UT. A high reading level is required to use these resources. Copyright © 2012 by Thieme Medical Publishers 333 Seventh Avenue, New York, NY 10001, USA.

Educational Opportunities for the 2014 Opposition of Mars

NASA Astrophysics Data System (ADS)

Albin, Edward F.

2013-10-01

Mars reaches opposition and is well placed for public viewing on April 8, 2014 at 20:57 UT. The opposition timeline and educational opportunities are considered, with emphasis on programs presented at the Fernbank Science Center in Atlanta, Georgia. Educational programs include a planetarium presentation, observations of Mars through telescopes, and activities associated with the ongoing Curiosity Rover (MSL) / anticipated Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft. When at opposition in 2014, Mars will have an apparent diameter of 15.1 arcseconds and will be visible in the evening sky for a little over a year until it is lost in the glare of the Sun in late April 2015. At closest approach, the planet will be a bit more than 57 million miles (92 million kilometers) from the Earth. Mars is especially well placed in the evening sky for viewing between the months of March and May of 2014. During this period, the planet can be found in retrograde motion within the constellation pattern of Virgo. Fernbank Science Center will offer public viewing of Mars through the observatory’s 36-inch (0.9 meter) reflecting telescope on Thursday and Friday evenings. The observatory is open immediately after the evening planetarium program. We anticipate showing a fulldome planetarium presentation about Mars entitled, "Mars Quest," which includes a live update about the Red Planet and how to find it among the stars in the current evening sky.

Simultaneous observations of Ellerman bombs by NST and IRIS

NASA Astrophysics Data System (ADS)

Kim, Y. H.; Yurchyshyn, V.; Cho, I. H.; Lee, J.; Park, Y. D.; Yang, H.; Ahn, K.; Goode, P.

2015-12-01

In this study, we present the simultaneous observations of Ellerman bombs made by New Solar Telescope (NST) of Big Bear Solar Observatory (BBSO) and Interface Region Imaging Spectrograph (IRIS) in space. The data obtained during joint NST-IRIS observations on 30 and 31 in July 2014. We observed two representative events on both days. The first one was a relatively weak Ellerman bomb occurred around 19:20 UT on 30 July 2014. IRIS observed this event by sit-and-stare mode thus we analyzed high cadence spectral data and slit-jaw data simultaneously. We found that this event was a hot explosion that occurred by magnetic reconnection in the lower atmosphere of the Sun. The second event was quite strong Ellerman bomb (20:20 UT on 31 July 2014) that is well observed by NST FISS (Fast Imaging Solar Spectrograph), while there was no IRIS spectral data. We had IRIS slit-jaw data only. The Ellerman bomb was clearly coincident with the IRIS brightening at the same location. Since the Ellerman bombs are usually believed to occur in the photosphere with no coronal emission, it should be explained its higher atmospheric emission in IRIS data. We will present the result of simultaneous observations by IRIS and NST instruments and discuss physical connection between Ellerman bombs and IRIS brightenings.

Systems Engineering Body of Knowledge and Its Integration with Software Engineering

DTIC Science & Technology

2011-05-01

e pro ess ona  soc e es  y  end of 2012. 801/27/2010 4/25/2011 9 Topic 2 (Article Title)Part 1 Related Topics Article Structure Lorem ipsum dolor  sit...amet[1], consectetuer adipiscing elit, sed diam nonummy nibh euismod tincidunt ut laoreet dolore magna aliquam erat volutpat. Ut wisi enim ad minim...veniam, quis nostrud exerci tation ullamcorper suscipit lobortis nisl ut aliquip ex ea commodo consequat. Duis autem vel eum iriure dolor [2] in

Transport characteristics of urea transporter-B.

PubMed

Yang, Baoxue

2014-01-01

UT-B represents the major urea transporter in erythrocytes, in addition to being expressed in kidney descending vasa recta, brain, spleen, ureter, bladder, and testis. Expression of urea transporter UT-B confers high urea permeability to mammalian erythrocytes. Erythrocyte membranes are also permeable to various urea analogues, suggesting common transport pathways for urea and structurally similar solutes. UT-B is highly permeable to urea and the chemical analogues formamide, acetamide, methylurea, methylformamide, ammonium carbamate, and acrylamide, each with a Ps > 5.0 × 10(-6) cm/s at 10 °C. The amides formamide, acetamide, acrylamide, and butyramide efficiently diffuse across lipid bilayers. The urea analogues dimethylurea, acryalmide, methylurea, thiourea, and methylformamide inhibit UT-B-mediated urea transport by >60 % by a pore-blocking mechanism. UT-B is also a water channel in erythrocytes and has a single-channel water permeability that is similar to aquaporin-1. Whether UT-B is an NH3 channel still needs further study. Urea permeability (Purea) in erythrocytes differs between different mammals. Carnivores (dog, fox, cat) exhibit high Purea. In contrast, herbivores (cow, donkey, sheep) show much lower Purea. Erythrocyte Purea in human and pig (omnivores) was intermediate. Rodents and lagomorphs (mouse, rat, rabbit) have Purea intermediate between carnivores and omnivores. Birds that do not excrete urea and do not express UT-B in their erythrocytes have very low values. In contrast to Purea, water permeability is relatively similar in all mammals studied. This chapter will provide information about the transporter characteristics of UT-B.

Deer Creek Dam, Dam, 1,204 feet/238 degrees from intersection of ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

Deer Creek Dam, Dam, 1,204 feet/238 degrees from intersection of dam complex access road and U.S. Highway 189 to center of dam, 874 feet/352 degrees from Hydroelectric Powerplant (HAER UT-93-B) to center of dam, Charleston, Wasatch County, UT

Regulation of Renal Urea Transport by Vasopressin

PubMed Central

Sands, Jeff M.; Blount, Mitsi A.; Klein, Janet D.

2011-01-01

Terrestrial life would be miserable without the ability to concentrate urine. Production of concentrated urine requires complex interactions among the nephron segments and vasculature in the kidney medulla. In addition to water channels (aquaporins) and sodium transporters, urea transporters are critically important to the theories proposed to explain the physiologic processes occurring when urine is concentrated. Vasopressin (anti-diuretic hormone) is the key hormone regulating the production of concentrated urine. Vasopressin rapidly increases water and urea transport in the terminal inner medullary collecting duct (IMCD). Vasopressin rapidly increases urea permeability in the IMCD through increases in phosphorylation and apical plasma-membrane accumulation of the urea transporter A1 (UT-A1). Vasopressin acts through two cAMP-dependent signaling pathways in the IMCD: protein kinase A and exchange protein activated by cAMP Epac. Protein kinase A phosphorylates UT-A1 at serines 486 and 499. In summary, vasopressin regulates urea transport acutely by increasing UT-A1 phosphorylation and the apical plasma-membrane accumulation of UT-A1 through two cAMP-dependent pathways. PMID:21686211

Isometric muscle activation of the serratus anterior and trapezius muscles varies by arm position: a pilot study with healthy volunteers with implications for rehabilitation.

PubMed

Miyasaka, Junsuke; Arai, Ryuzo; Ito, Taisuke; Shingu, Nobuyuki; Hasegawa, Satoshi; Ibuki, Satoko; Ichihashi, Noriaki; Matsuda, Shuichi; Moritani, Toshio

2017-07-01

This study aimed to determine the most appropriate angle and moving direction of the arm for improving coordination of the periscapular muscles, including the serratus anterior (SA), upper trapezius (UT), middle trapezius (MT), and lower trapezius (LT). Muscle activation amplitudes were evaluated in the SA, UT, MT, and LT in 11 healthy subjects by use of surface electromyography. The subjects were asked to maintain the arm position at 5 elevated positions with maximal effort against applied manual forces, which were directed from upper to lower (test 1), lower to upper (test 2), posterior to anterior in the frontal plane and lateral to medial in the sagittal plane (test 3), and anterior to posterior in the frontal plane and medial to lateral in the sagittal plane (test 4). The relative activity of the UT with respect to the SA, MT, and LT was calculated, resulting in the UT/SA, UT/MT, and UT/LT ratios. Test 4 in all positions but 150° of elevation in the frontal plane showed high activity of the SA with a low UT/SA ratio. High MT activity with a low UT/MT ratio was observed during test 3 at the 90° elevated position, whereas high LT activity without UT hyperactivation was not found. To strengthen the periscapular muscles in the balanced condition, horizontal adduction is recommended for the SA. Horizontal abduction at the 90° elevated position should be effective for the MT. Because no technique in this study was effective for the LT, further studies are needed. Copyright © 2016 Journal of Shoulder and Elbow Surgery Board of Trustees. Published by Elsevier Inc. All rights reserved.

Backfilling behavior of a mixed aggregate based on construction waste and ultrafine tailings

PubMed Central

Zhang, Qinli; Xiao, Chongchun; Chen, Xin

2017-01-01

To study the possibility of utilizing mixed construction waste and ultrafine tailings (CW&UT) as a backfilling aggregate that can be placed underground in a mine, physicochemical evaluation, proportioning strength tests, and pumpability experiments were conducted. It was revealed that mixed CW&UT can be used as a backfilling aggregate due to the complementarities of their physicochemical properties. In addition, as the results of the proportioning strength tests show, the compressive strength of a cemented CW&UT backfilling specimen cured for 28 days, with a mass fraction of 72–74%, a cement-sand ratio of 1:12, and a CW proportion of 30%, is higher than 1.0 MPa, which meets the safety requirements and economic consideration of backfilling technology in many underground metal mines, and can also be enhanced with an increase in the cement-sand ratio. The results of the pumpability experiments show that cemented backfilling slurry based on CW&UT can be transported to the stope underground with a common filling pump, with a 16.6 MPa maximum pressure, with the condition that the time of emergency shut-down is less than approximately 20 min. All in all, the research to utilize mixed CW&UT as a backfilling aggregate can not only provide a way to dispose of CW&UT but also will bring large economic benefits and can provide constructive guidance for environmental protection. PMID:28662072

Backfilling behavior of a mixed aggregate based on construction waste and ultrafine tailings.

PubMed

Chen, Qiusong; Zhang, Qinli; Xiao, Chongchun; Chen, Xin

2017-01-01

To study the possibility of utilizing mixed construction waste and ultrafine tailings (CW&UT) as a backfilling aggregate that can be placed underground in a mine, physicochemical evaluation, proportioning strength tests, and pumpability experiments were conducted. It was revealed that mixed CW&UT can be used as a backfilling aggregate due to the complementarities of their physicochemical properties. In addition, as the results of the proportioning strength tests show, the compressive strength of a cemented CW&UT backfilling specimen cured for 28 days, with a mass fraction of 72-74%, a cement-sand ratio of 1:12, and a CW proportion of 30%, is higher than 1.0 MPa, which meets the safety requirements and economic consideration of backfilling technology in many underground metal mines, and can also be enhanced with an increase in the cement-sand ratio. The results of the pumpability experiments show that cemented backfilling slurry based on CW&UT can be transported to the stope underground with a common filling pump, with a 16.6 MPa maximum pressure, with the condition that the time of emergency shut-down is less than approximately 20 min. All in all, the research to utilize mixed CW&UT as a backfilling aggregate can not only provide a way to dispose of CW&UT but also will bring large economic benefits and can provide constructive guidance for environmental protection.

Increased Upper Trapezius Muscle Stiffness in Overhead Athletes with Rotator Cuff Tendinopathy

PubMed Central

Leong, Hio Teng; Hug, François; Fu, Siu Ngor

2016-01-01

Although excessive tension of the upper trapezius (UT) is thought to contribute to rotator cuff tendinopathy, no study examined UT tension in athletes with and without rotator cuff tendinopathy. Here we used UT shear modulus measured using ultrasound shear wave elastography as an index of muscle stiffness/tension. The aims of this study were twofold: 1) to determine whether the UT muscle shear modulus is altered in athletes with rotator cuff tendinopathy compared to asymptomatic athletes, and 2) to detect optimal cut-off points of UT shear modulus in identifying athletes with rotator cuff tendinopathy. Forty-three male volleyball players (17 asymptomatic and 26 with rotator cuff tendinopathy, mean age = 22.9±3.5 years) participated in the study. UT shear modulus was quantified during active arm holding at 30° and 60° of shoulder abduction and passive arm positioning at 0°, 30° and 60° of shoulder abduction. During the active tasks, the UT shear modulus was higher in athletes with rotator cuff tendinopathy than the asymptomatic athletes (p = 0.002), regardless the arm position. During the passive tasks, athletes with rotator cuff tendinopathy exhibited a higher UT shear modulus than asymptomatic athletes only at 0° of shoulder abduction (13.0±2.5 kPa vs 10.2±1.8 kPa, p = 0.001). When considering the active task, an optimal cut-off shear modulus of 12.0 kPa at 30° of shoulder abduction (sensitivity = 0.84, specificity = 0.57, AUC = 0.757, p = 0.008) and 9.5 kPa at 60° of shoulder abduction (sensitivity = 0.88, specificity = 0.67, AUC = 0.816, p = 0.002) was detected. When considering the passive task at 0° of shoulder abduction, a cut-off of 12.2 kPa was found (sensitivity = 0.73, AUC = 0.817, p = 0.001). Findings from the present study show that monitoring passive and active UT muscle shear modulus may provide important information for the prevention/rehabilitation of rotator cuff tendinopathy. PMID:27159276

Increased Upper Trapezius Muscle Stiffness in Overhead Athletes with Rotator Cuff Tendinopathy.

PubMed

Leong, Hio Teng; Hug, François; Fu, Siu Ngor

2016-01-01

Although excessive tension of the upper trapezius (UT) is thought to contribute to rotator cuff tendinopathy, no study examined UT tension in athletes with and without rotator cuff tendinopathy. Here we used UT shear modulus measured using ultrasound shear wave elastography as an index of muscle stiffness/tension. The aims of this study were twofold: 1) to determine whether the UT muscle shear modulus is altered in athletes with rotator cuff tendinopathy compared to asymptomatic athletes, and 2) to detect optimal cut-off points of UT shear modulus in identifying athletes with rotator cuff tendinopathy. Forty-three male volleyball players (17 asymptomatic and 26 with rotator cuff tendinopathy, mean age = 22.9±3.5 years) participated in the study. UT shear modulus was quantified during active arm holding at 30° and 60° of shoulder abduction and passive arm positioning at 0°, 30° and 60° of shoulder abduction. During the active tasks, the UT shear modulus was higher in athletes with rotator cuff tendinopathy than the asymptomatic athletes (p = 0.002), regardless the arm position. During the passive tasks, athletes with rotator cuff tendinopathy exhibited a higher UT shear modulus than asymptomatic athletes only at 0° of shoulder abduction (13.0±2.5 kPa vs 10.2±1.8 kPa, p = 0.001). When considering the active task, an optimal cut-off shear modulus of 12.0 kPa at 30° of shoulder abduction (sensitivity = 0.84, specificity = 0.57, AUC = 0.757, p = 0.008) and 9.5 kPa at 60° of shoulder abduction (sensitivity = 0.88, specificity = 0.67, AUC = 0.816, p = 0.002) was detected. When considering the passive task at 0° of shoulder abduction, a cut-off of 12.2 kPa was found (sensitivity = 0.73, AUC = 0.817, p = 0.001). Findings from the present study show that monitoring passive and active UT muscle shear modulus may provide important information for the prevention/rehabilitation of rotator cuff tendinopathy.

MAGNETOMETER - TRI-AXIS SENSOR UNIT - GEMINI-TITAN (GT)-12 EXPERIMENT MSC-3 (M405) - MSC

NASA Image and Video Library

1966-10-01

S66-09379 (1 Oct. 1966) --- Tri-Axis Magnetometer-Sensor Unit mounted on telescoping boom. Cable connects Sensor Unit with Electronics Unit mounted on retrograde beam in retrograde adapter section. Objective of experiment is to monitor the direction and amplitude of Earth's magnetic field (Gemini-12). Photo credit: NASA

High-Resolution Mid-IR Imaging of Jupiter's Great Red Spot: Comparing Cassini, VLT and Subaru Observations

NASA Astrophysics Data System (ADS)

Fletcher, Leigh N.; Orton, G. S.; Yanamandra-Fisher, P.; Irwin, P. G. J.; Baines, K. H.; Edkins, E.; Line, M. R.; Mousis, O.; Parrish, P. D.; Vanzi, L.; Fuse, T.; Fujoyoshi, T.

2008-09-01

In the eight years since the Cassini fly-by of Jupiter, the spatial resolution of ground-based observations of Jupiter's giant anticyclonic storm systems (the Great Red Spot, Oval BA and others) using 8m-class telescopes has surpassed the resolution of the Cassini/CIRS maps. We present a time-series of mid-IR imaging of the Great Red Spot (GRS) and its environs from the VISIR instrument on the Very Large Telescope (UT3/Melipal) and the COMICS instrument on the Subaru telescope (Hawaii). The NEMESIS optimal-estimation retrieval algorithm (Irwin et al., 2008) is used to analyse both the 7-25 micron filtered imaging from 2005-2008 and Cassini/CIRS 7-16 micron data from 2000. We demonstrate the ability to map temperatures in the 100-400 mbar range, NH3, aerosol opacity and the para-H2 fraction from the filtered imaging. Furthermore, the Cassini/CIRS spectra are used to map the PH3 mole fraction around the GRS. The thermal field, gaseous composition and aerosol distribution are used as diagnostics for the atmospheric motion associated with the GRS. Changes in the atmospheric state in response to close encounters with Oval BA and other vortices will be assessed. These results will be discussed in light of their implications for the planning of the Europa-Jupiter System Mission.

A Case for Thinking Without Consciousness.

PubMed

Dijksterhuis, Ap; Strick, Madelijn

2016-01-01

People can engage in prolonged thought processes, such as when they are facing an important decision or when they are working on a scientific discovery. Such thought processes can take months or even years. We argue that while people engage in such thinking, they make progress not only when they consciously think but also sometimes when they are consciously thinking about something else-that is, while they think unconsciously. We review the literature on unconscious thought (UT) processes and conclude that there is indeed quite some evidence for UT. Conceptualized as a form of unconscious goal pursuit, UT is likely to be especially fruitful for thought processes that are complex, important, or interesting to the thinker. In addition, we discuss other characteristics of the UT process. We end with proposing Type 3 processes, in addition to Type 1 and Type 2 (or Systems 1 and 2) processes, to accommodate prolonged thought processes in models on thought. © The Author(s) 2015.

6. VIEW SHOWING UPRIGHT OUTLET GATE WHEEL, STEM AND STEM ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

6. VIEW SHOWING UPRIGHT OUTLET GATE WHEEL, STEM AND STEM GUIDE, WITH LOG ACCESS STRUCTURE, LOOKING WEST - High Mountain Dams in Upalco Unit, Bluebell Lake Dam, Ashley National Forest, 11.2 miles Northwest of Swift Creek Campground, Mountain Home, Duchesne County, UT

3. OVERALL VIEW OF DEER LAKE AND UPRIGHT OUTLET GATE ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

3. OVERALL VIEW OF DEER LAKE AND UPRIGHT OUTLET GATE WHEEL, STEM AND STEM GUIDE, LOOKING NORTH - High Mountain Dams in Upalco Unit, Deer Lake Dam, Ashley National Forest, 5.8 miles North of Swift Creek Campground, Mountain Home, Duchesne County, UT

5. VIEW SHOWING UPRIGHT OUTLET GATE WHEEL, STEM AND STEM ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. VIEW SHOWING UPRIGHT OUTLET GATE WHEEL, STEM AND STEM GUIDE, WITH LOG ACCESS STRUCTURE, LOOKING SOUTHEAST - High Mountain Dams in Upalco Unit, Bluebell Lake Dam, Ashley National Forest, 11.2 miles Northwest of Swift Creek Campground, Mountain Home, Duchesne County, UT

The First Use of Coordinated Ionospheric Radio and Optical Observations Over Italy: Convergence of High-and Low-Latitude Storm-Induced Effects

NASA Astrophysics Data System (ADS)

Cesaroni, C.; Alfonsi, L.; Pezzopane, M.; Martinis, C.; Baumgardner, J.; Wroten, J.; Mendillo, M.; Musicò, E.; Lazzarin, M.; Umbriaco, G.

2017-11-01

Ionospheric storm effects at midlatitudes were analyzed using different ground-based instruments distributed in Italy during the 13-15 November 2012 geomagnetic storm. These included an all-sky imager (ASI) in Asiago (45.8°N, 11.5°E), a network of dual-frequeny Global Navigation Satellite Systems receivers (Rete Integrata Nazionale GPS network), and ionosondes in Rome (41.8°N, 12.5°E) and San Vito (40.6°N, 17.8°E). GPS measurements showed an unusual enhancement of total electron content (TEC) in southern Italy, during the nights of 14 and 15 November. The ASI observed colocated enhancements of 630 nm airglow at the same time, as did variations in NmF2 measured by the ionosondes. Moreover, wave-like perturbations were identified propagating from the north. The Ensemble Empirical Mode Decomposition, applied to TEC values revealed the presence of traveling ionospheric disturbances (TIDs) propagating southward between 01:30 UT and 03:00 UT on 15 November. These TIDs were characterized by weak TEC oscillations ( ±0.5 TEC unit), period of 45 min, and velocity of 500 m/s typical of large-scale TIDs. Optical images showed enhanced airglow entering the field of view of the ASI from the N-NE at 02:00 UT and propagating to the S-SW, reaching the region covered by the GPS stations after 03:00 UT, when TEC fluctuations are very small ( ±0.2 TEC unit). The enhancement of TEC and airglow observed in southern Italy could be a consequence of a poleward expansion of the northern crest of the equatorial ionization anomaly. The enhanced airglow propagating from the north and the TEC waves resulted from energy injected at auroral latitudes as confirmed by magnetometer observations in Scandinavia.

Pro-am collaborations with the Faulkes Telescopes, and the benefit to education, science and outreach awareness

NASA Astrophysics Data System (ADS)

Howes, N.; Miles, R.; Roche, P.

2013-09-01

The Faulkes Telescope Project is an educational and research arm of the Las Cumbres Observatory Global Telescope Network (LCOGTN). It has two 2-metre robotic telescopes, located at Haleakala on Maui (FT North) and Siding Spring in Australia (FT South). It is planned for these telescopes to be complemented by a research network of multiple 1-metre telescopes, along with an educational network of multiple 0.4-metre telescopes, providing 24-hour coverage of both northern and southern hemispheres. The telescope network is unique in that it provides school students with access to research grade instrumentation in the United Kingdom and several other countries across Europe as well as in Hawaii. Over the past few years, amateur astronomers have increasingly been working with schools suggesting projects which have provided valuable scientific input to professional astronomers. This poster aims to present several of the key results and observations where professional astronomers have cited and used this data obtained with the Faulkes Telescope, notably - Observations and results from the global campaign on Comet C/2007 Q3 ; Ref.[2] - Observations of the fragmentation of Comet 168P; Ref.[3] - Observations relating to the evolution of Comet C/2012 S1; Ref.[4] - Observations and imaging of the Jupiter-family comet, P/2010 TO20; Ref.[5

An afocal telescope configuration for the ESA ARIEL mission

NASA Astrophysics Data System (ADS)

Da Deppo, Vania; Focardi, Mauro; Middleton, Kevin; Morgante, Gianluca; Pascale, Enzo; Grella, Samuele; Pace, Emanuele; Claudi, Riccardo; Amiaux, Jérôme; Colomé Ferrer, Josep; Hunt, Thomas; Rataj, Miroslaw; Sierra-Roig, Carles; Ficai Veltroni, Iacopo; Eccleston, Paul; Micela, Giuseppina; Tinetti, Giovanna

2017-12-01

Atmospheric Remote-Sensing Infrared Exoplanet Large Survey (ARIEL) is a candidate as an M4 ESA mission to launch in 2026. During its 3.5 years of scientific operations, ARIEL will observe spectroscopically in the infrared (IR) a large population of known transiting planets in the neighbourhood of the solar system. ARIEL aims to give a breakthrough in the observation of exoplanet atmospheres and understanding of the physics and chemistry of these far-away worlds. ARIEL is based on a 1 m class telescope feeding a collimated beam into two separate instrument modules: a spectrometer module covering the waveband between 1.95 and 7.8 μm and a combined fine guidance system/visible photometer/NIR spectrometer. The telescope configuration is a classic Cassegrain layout used with an eccentric pupil and coupled to a tertiary off-axis paraboloidal mirror. To constrain the thermo-mechanically induced optical aberrations, the primary mirror (M1) temperature will be monitored and finely tuned using an active thermal control system based on thermistors and heaters. They will be switched on and off to maintain the M1 temperature within ± 1 K by the telescope control unit (TCU). The TCU is a payload electronics subsystem also responsible for the thermal control of the spectrometer module detectors as well as the secondary mirror mechanism and IR calibration source management. The TCU, being a slave subsystem of the instrument control unit, will collect the housekeeping data from the monitored subsystems and will forward them to the master unit. The latter will run the application software, devoted to the main spectrometer management and to the scientific data on-board processing.

Developing Hypothetical Inhibition Mechanism of Novel Urea Transporter B Inhibitor

NASA Astrophysics Data System (ADS)

Li, Min; Tou, Weng Ieong; Zhou, Hong; Li, Fei; Ren, Huiwen; Chen, Calvin Yu-Chian; Yang, Baoxue

2014-07-01

Urea transporter B (UT-B) is a membrane channel protein that specifically transports urea. UT-B null mouse exhibited urea selective urine concentrating ability deficiency, which suggests the potential clinical applications of the UT-B inhibitors as novel diuretics. Primary high-throughput virtual screening (HTVS) of 50000 small-molecular drug-like compounds identified 2319 hit compounds. These 2319 compounds were screened by high-throughput screening using an erythrocyte osmotic lysis assay. Based on the pharmacological data, putative UT-B binding sites were identified by structure-based drug design and validated by ligand-based and QSAR model. Additionally, UT-B structural and functional characteristics under inhibitors treated and untreated conditions were simulated by molecular dynamics (MD). As the result, we identified four classes of compounds with UT-B inhibitory activity and predicted a human UT-B model, based on which computative binding sites were identified and validated. A novel potential mechanism of UT-B inhibitory activity was discovered by comparing UT-B from different species. Results suggest residue PHE198 in rat and mouse UT-B might block the inhibitor migration pathway. Inhibitory mechanisms of UT-B inhibitors and the functions of key residues in UT-B were proposed. The binding site analysis provides a structural basis for lead identification and optimization of UT-B inhibitors.

The transverse technique; a complementary approach to the measurement of first-trimester uterine artery Doppler.

PubMed

Drouin, Olivier; Johnson, Jo-Ann; Chaemsaithong, Piya; Metcalfe, Amy; Huber, Janie; Schwarzenberger, Jill; Winters, Erin; Stavness, Lesley; Tse, Ada W T; Lu, Jing; Lim, Wan Teng; Leung, Tak Yeung; Bujold, Emmanuel; Sahota, Daljit; Poon, Liona C

2017-10-04

The objectives of this study were to 1) define the protocol for the first-trimester assessment of the uterine artery pulsatility index (UtA-PI) using the new transverse technique, 2) evaluate UtA-PI measured by the transverse approach versus that obtained by the conventional sagittal approach, and 3) determine if accelerated onsite training (both methods) of inexperienced sonographers can achieve reproducible UtA-PI measurements compared to that measured by an experienced sonographer. The study consists of 2 parts conducted in 2 centers (Part 1, Calgary, Canada and Part 2, Hong Kong). Part 1 Prospective observational study of women with singleton pregnancies between 11-13+6 weeks' gestation. UtA-PI measurements were performed using the 2 techniques (4 sonographers trained in both methods, 10 cases each) and measurement indices (PI), time required and subjective difficulty to obtain satisfactory measurements were compared. One sample t-test and Wilcoxon rank sign test was used when appropriate. Bland-Altman difference plots were used to assess measurement agreement, and intra-class correlation (ICC) was used to evaluate measurement reliability. A target plot was used to assess measures of central tendency and dispersion. Part 2 One experienced and three inexperienced sonographers prospectively measured the UtA-PI at 11-13+6 weeks' gestation in two groups of women (42 and 35, respectively), with singleton pregnancies using both approaches. Inexperienced sonographers underwent accelerated on-site training by the experienced sonographer. Measurement approach and sonographer order were on a random basis. ICC, Bland-Altman and Passing-Bablok analyses were performed to assess measurement agreement, reliability and effect of accelerated training. Part 1 We observed no difference in the mean time to acquire the measurements (Sagittal: 118 seconds vs Transverse: 106 seconds, p=0.38). The 4 sonographers reported the transverse technique was subjectively easier to perform (p=0.04). The bias (95% LOA) and the ICC between sagittal and transverse measurements was -0.05 (-0.48 to 0.37) and 0.94 for the mean UtA-PIs respectively. Measurements obtained using the transverse technique after correcting for gestation were significantly closer to the expected distribution than the sagittal technique. Part 2 There were no significant differences in the median UtA-PI measurements using the different approaches for both experienced and inexperienced sonographers (p>0.05 for all sonographers). Mean UtA-PI measurement reliability between approaches was high for the experienced (ICC=0.92) and inexperienced sonographers (ICC>0.81). UtA-PI measurement approaches did not deviate from linearity whilst biases ranged from -0.10 to 0.07. Median time required was similar (sagittal vs. transverse: 56.11 sec vs. 49.29 sec; p=0.054). This novel transverse approach for the measurement of UtA-PI in the first-trimester appears comparable to the sagittal approach and can be used in first-trimester preeclampsia screening. Providing accelerated onsite training can be helpful to improve UtA-PI measurement reliability and could potentially facilitate the broad implementation of first-trimester preeclampsia screening. This article is protected by copyright. All rights reserved.

Novel FR-900493 Analogues That Inhibit the Outgrowth of Clostridium difficile Spores

PubMed Central

2018-01-01

The spectrum of antibacterial activity for the nucleoside antibiotic FR-900493 (1) can be extended by chemical modifications. We have generated a small focused library based on the structure of 1 and identified UT-17415 (9), UT-17455 (10), UT-17460 (11), and UT-17465 (12), which exhibit anti-Clostridium difficile growth inhibitory activity. These analogues also inhibit the outgrowth of C. difficile spores at 2× minimum inhibitory concentration. One of these analogues, 11, relative to 1 exhibits over 180-fold and 15-fold greater activity against the enzymes, phospho-MurNAc-pentapeptide translocase (MraY) and polyprenyl phosphate-GlcNAc-1-phosphate transferase (WecA), respectively. The phosphotransferase inhibitor 11 displays antimicrobial activity against several tested bacteria including Bacillus subtilis, Clostridium spp., and Mycobacterium smegmatis, but no growth inhibitory activity is observed against the other Gram-positive and Gram-negative bacteria. The selectivity index (Vero cell cytotoxicity/C. difficileantimicrobial activity) of 11 is approximately 17, and 11 does not induce hemolysis even at a 100 μM concentration. PMID:29503973

Observation of a rapid decrease in the brightness of the coma of 2060 Chiron in 1990 January

DOE Office of Scientific and Technical Information (OSTI.GOV)

Buratti, B.J.; Dunbar, R.S.

Photometric observations of 2060 Chiron in the V and R filters were obtained with the 1.5-m telescope on Palomar Mountain during a 7-hr period on January 20, 1990 (UT). A general decrease of about 10 percent in integrated brightness occurred in both filters. No color dependence to the decrease was observed. A small (about 0.02 mag) rotational light curve, far smaller than the 0.09 mag (peak-to-peak) one observed by Bus et al. (1989) is superposed on the general decrease. On January 29, 1990, Luu and Jewitt (1990) observed an impulsive brightening of Chiron of approximately the same magnitude and timemore » scale as the presently observed decrease in brightness. The combined results provide evidence that Chiron is currently exhibiting short-term fluctuations in the brightness of its coma, in addition to its well-established general decrease in brightness. 14 refs.« less

The NST observation of a small loop eruption in He I D3 line on 2016 May 30

NASA Astrophysics Data System (ADS)

Kim, Yeon-Han; Xu, Yan; Bong, Su-Chan; Lim, Eunkyung; Yang, Heesu; Park, Young-Deuk; Yurchyshyn, Vasyl B.; Ahn, Kwangsu; Goode, Philip R.

2017-08-01

Since the He I D3 line has a unique response to a flare impact on the low solar atmosphere, it can be a powerful diagnostic tool for energy transport processes. In order to obtain comprehensive data sets for studying solar flare activities in D3 spectral line, we performed observations for several days using the 1.6m New Solar Telescope of Big Bear Solar Observatory (BBSO) in 2015 and 2016, equipped with the He I D3 filter, the photospheric broadband filter, and Near IR imaging spectrograph (NIRIS). On 2016 May 30, we observed a small loop eruption in He I D3 images associated with a B class brightening, which is occurred around 17:10 UT in a small active region, and dynamic variations of photospheric features in G-band images. Accordingly, the cause of the loop eruption can be magnetic reconnection driven by photospheric plasma motions. In this presentation, we will give the observation results and the interpretation.

Temporal frequency of radio emissions for the April 25, 1984 flare

NASA Technical Reports Server (NTRS)

Wells, G. D.; Hausman, B. A.; Kroehl, H. W.

1986-01-01

The National Geophysical Data Center archives data of the solar-terrestrial environment. The USAF Radio Solar Telescope Network (RSTN) data allow performance of time series analysis to determine temporal oscillations as low as three seconds. The X13/3B flare which erupted in region 4474 (S12E43) on the 24 to 25 of April 1984, was selected. The soft X-rays, 1 to 8 A, remained above X-levels for 50 minutes and the radio emissions measured at Learmonth Solar Observatory reached a maximum of 3.15 x 10 to the 5th power SFUs at 410 MHz at 0000UT. A power spectral analysis of the fixed frequency RSTN data from Learmonth shows possible quasi-periodic fluctuations in the range two to ten seconds. Repetition rates or quasi-periodicities, in the case of the power spectral analysis, generally showed the same trends as the average solar radio flux at 245 and 8800 MHz. The quasi-periodicities at 1415 MHz showed no such trends.

Small-Molecule Inhibitors of Urea Transporters

PubMed Central

Verkman, Alan S.; Esteva-Font, Cristina; Cil, Onur; Anderson, Marc O.; Li, Fei; Li, Min; Lei, Tianluo; Ren, Huiwen; Yang, Baoxue

2015-01-01

Urea transporter (UT) proteins, which include isoforms of UT-A in kidney tubule epithelia and UT-B in vasa recta endothelia and erythrocytes, facilitate urinary concentrating function. Inhibitors of urea transporter function have potential clinical applications as sodium-sparing diuretics, or ‘urearetics,’ in edema from different etiologies, such as congestive heart failure and cirrhosis, as well as in syndrome of inappropriate antidiuretic hormone (SIADH). High-throughput screening of drug-like small molecules has identified UT-A and UT-B inhibitors with nanomolar potency. Inhibitors have been identified with different UT-A versus UT-B selectivity profiles and putative binding sites on UT proteins. Studies in rodent models support the utility of UT inhibitors in reducing urinary concentration, though testing in clinically relevant animal models of edema has not yet been done. PMID:25298345

Discovery and Classification of Nova in M31 : P60-M31-081230

NASA Astrophysics Data System (ADS)

Kasliwal, M. M.; Rau, A.; Salvato, M.; Cenko, S. B.; Ofek, E. O.; Quimby, R.; Kulkarni, S. R.

2009-01-01

On UT 2008 Dec 30.207, P60-FasTING (Palomar 60-inch Fast Transients In Nearby Galaxies) discovered an optical transient in M31 at RA(J2000) = 00:43:05.027, DEC(J2000)=+41:17:52.25, offset from the nucleus by 233.4"E,103.8"N. P60-M31-081230 had a brightness of g = 20.5 +/- 0.2 at discovery. It was not detected by P60 to g > 22.0 on Dec 29.140. There is no counterpart in SIMBAD. Follow-up spectroscopy with the Double Beam Spectrograph on the Palomar Hale telescope on Dec 31.104 revealed prominent Balmer emission and strong P Cygni profiles of several Fe II lines.

A comparison of LOD and UT1-UTC forecasts by different combined prediction techniques

NASA Astrophysics Data System (ADS)

Kosek, W.; Kalarus, M.; Johnson, T. J.; Wooden, W. H.; McCarthy, D. D.; Popiński, W.

Stochastic prediction techniques including autocovariance, autoregressive, autoregressive moving average, and neural networks were applied to the UT1-UTC and Length of Day (LOD) International Earth Rotation and Reference Systems Servive (IERS) EOPC04 time series to evaluate the capabilities of each method. All known effects such as leap seconds and solid Earth zonal tides were first removed from the observed values of UT1-UTC and LOD. Two combination procedures were applied to predict the resulting LODR time series: 1) the combination of the least-squares (LS) extrapolation with a stochastic predition method, and 2) the combination of the discrete wavelet transform (DWT) filtering and a stochastic prediction method. The results of the combination of the LS extrapolation with different stochastic prediction techniques were compared with the results of the UT1-UTC prediction method currently used by the IERS Rapid Service/Prediction Centre (RS/PC). It was found that the prediction accuracy depends on the starting prediction epochs, and for the combined forecast methods, the mean prediction errors for 1 to about 70 days in the future are of the same order as those of the method used by the IERS RS/PC.

Nitrogen oxides and ozone in the tropopause region of the Northern Hemisphere: Measurements from commercial aircraft in 1995/1996 and 1997

NASA Astrophysics Data System (ADS)

Brunner, Dominik; Staehelin, Johannes; Jeker, Dominique; Wernli, Heini; Schumann, Ulrich

2001-11-01

Measurements of nitrogen oxides (NO and NO2) and ozone (O3) were performed from a Swissair B-747 passenger aircraft in two extended time periods (May 1995 to May 1996, August to November 1997) in the framework of the Swiss NOXAR and the European POLINAT 2 project. The measurements were obtained on a total of 623 flights between Europe and destinations in the United States and the Far East. NO2 measurements were obtained only after December 1995 and were less precise than the NO measurements. Therefore daytime NO2 values were derived from measured NO and O3 concentrations assuming photostationary equilibrium. The completed NOx data set (measured NO, measured NO2 during night, and calculated NO2 during day) includes a complete annual cycle and is the most extensive and representative data set currently available for the upper troposphere (UT) and the lower stratosphere (LS) covering a significant proportion of the northern hemisphere between 15°N and 65°N. NOx concentrations in midlatitudes (30°-60°N) showed a marked seasonal variation both in the UT and the LS with a maximum in summer (median/mean values of 159/264 pptv in UT, 199/237 pptv in LS) and a minimum in winter (51/99 pptv in UT, 67/91 pptv in LS). Mean NOx concentrations were generally much higher than the respective median values, in particular in the UT, which reflects the important contribution from comparatively few very high concentrations observed in large-scale convection/lightning and small-scale aircraft plumes. Seasonal mean NOx concentrations in the UT were up to 3-4 times higher over continental regions than over the North Atlantic during summer. Lightning production of NO and convective vertical transport from the polluted boundary layer thus appear to have dominated the upper tropospheric NOx budget over these continental regions, particularly during summer. Ozone concentrations at aircraft cruising levels typically varied by an order of magnitude due to the strong vertical gradient in the LS. Seasonal mean values were dominated by large-scale dynamical processes controlling the altitude of the tropopause and the O3 abundance in the LS. O3 in the UT in midlatitudes showed a broad maximum between June and August, typical of observations in the free troposphere.

Toward Adaptive X-Ray Telescopes

NASA Technical Reports Server (NTRS)

O'Dell, Stephen L.; Atkins, Carolyn; Button, Tim W.; Cotroneo, Vincenzo; Davis, William N.; Doel, Peer; Feldman, Charlotte H.; Freeman, Mark D.; Gubarev, Mikhail V.; Kolodziejczak, Jeffrey J.;

Toward active x-ray telescopes

NASA Astrophysics Data System (ADS)

O'Dell, Stephen L.; Atkins, Carolyn; Button, Timothy W.; Cotroneo, Vincenzo; Davis, William N.; Doel, Peter; Feldman, Charlotte H.; Freeman, Mark D.; Gubarev, Mikhail V.; Kolodziejczak, Jeffery J.; Michette, Alan G.; Ramsey, Brian D.; Reid, Paul B.; Rodriguez Sanmartin, Daniel; Saha, Timo T.; Schwartz, Daniel A.; Trolier-McKinstry, Susan; Wilke, Rudeger H. T.; Willingale, Richard; Zhang, William W.

2011-09-01

Future x-ray observatories will require high-resolution (< 1") optics with very-large-aperture (> 25 m2) areas. Even with the next generation of heavy-lift launch vehicles, launch-mass constraints and aperture-area requirements will limit the areal density of the grazing-incidence mirrors to about 1 kg/m2 or less. Achieving sub-arcsecond x-ray imaging with such lightweight mirrors will require excellent mirror surfaces, precise and stable alignment, and exceptional stiffness or deformation compensation. Attaining and maintaining alignment and figure control will likely involve active (in-space adjustable) x-ray optics. In contrast with infrared and visible astronomy, active optics for x-ray astronomy is in its infancy. In the middle of the past decade, two efforts began to advance technologies for adaptive x-ray telescopes: The Smart X-ray Optics (SXO) Basic Technology project in the United Kingdom (UK) and the Generation-X (Gen-X) concept studies in the United States (US). This paper discusses relevant technological issues and summarizes progress toward active x-ray telescopes.

The Near-Earth Encounter of Asteroid 308635 (2005 YU55): Thermal IR Observations

NASA Astrophysics Data System (ADS)

Lim, Lucy F.; Emery, J. P.; Moskovitz, N. A.; Busch, M. W.; Yang, B.; Granvik, M.

2012-10-01

The near-Earth approach (0.00217 AU, or 0.845 lunar distances) of the C-type asteroid 308635 (2005 YU55) in November 2011 presented a rare opportunity for detailed observations of a low-albedo NEA in this size range. As part of a multi-telescope campaign to measure visible and infrared spectra and photometry, we obtained mid-infrared ( 8 to 22 micron) photometry and spectroscopy of 2005 YU55 using Michelle [1] on the Gemini North telescope on UT November 9 and 10, 2011. An extensive radar campaign [2] together with optical lightcurves [3,4] established the rotation state of YU55. In addition, the radar imaging resulted in a shape model for the asteroid, detection of numerous boulders on its surface, and a preliminary estimate of its equatorial diameter at 380 +/- 20 m. In a preliminary analysis, applying the radar and lightcurve-derived parameters to a rough-surface thermophysical model fit to the Gemini/Michelle thermal emission photometry results in a thermal inertia range of approximately 500 to 1500 J m-2 s-1/2 K-1, with the low-thermal-inertia solution corresponding to the small end of the radar size range and vice versa. Updates to these results will be presented and modeling of the thermal contribution to the measured near-infrared spectra from Palomar/Triplespec and IRTF/SpeX will also be discussed. The authors gratefully acknowledge the assistance of observatory staff and the support of the NASA NEOO program (LFL and JPE), the Carnegie fellowship (NAM), and NASA AES, NSF, and the NRAO Jansky Fellowship (MWB). [1] De Buizer, J. and R. Fisher, Proc. Hris (2005), pp. 84-87. [2] Busch, M.W. et al., ACM (2012), abstract #6179. [3] Warner, B., MPBull 39 (2), 84 [4] Pravec, P.

EIT And SXT Observations of a Quiet-Region Filament Ejection: First Eruption, Then Reconnection

NASA Technical Reports Server (NTRS)

Sterling, Alphonse C.; Moore, Ronald L.; Thompson, Barbara J.

2001-01-01

We observe a slow-onset quiet-region filament eruption with the Extreme Ultraviolet Imaging Telescope (EIT) on the Solar Heliospheric Observatory (SOHO) and the Soft X-ray Telescope (SXT) on Yohkoh. This event occurred on 1999 April 18 and was likely the origin of a coronal mass ejection detected by SOHO at 08:30 UT on that day. In the EIT observation, one-half of the filament shows two stages of evolution: stage 1 is a slow, roughly constant upward movement at approximately 1 km/s lasting approximately 0.5 hr, and stage 2 is a rapid upward eruption at approximately 16 km/s occurring just before the filament disappears into interplanetary space. The other half of the filament shows little motion along the line of sight during the time of stage 1 but erupts along with the rest of the filament during stage 2. There is no obvious emission from the filament in the SXT observation until stage 2; at that time, an arcade of EUV and soft X-ray loops forms first at the central location of the filament and then expands outward along the length of the filament channel. A plot of EUV intensity versus time of the central portion of the filament (where the postflare loops initially form) shows a flat profile during stage 1 and a rapid upturn after the start of stage 2. This light curve is delayed from what would be expected if 'tether-cutting' reconnection in the core of the erupting region were responsible for the initiation of the eruption. Rather, these observations suggest that a loss of stability of the magnetic field holding the filament initiates the eruption, with reconnection in the core region occurring only as a by-product.

Li depletion in solar analogues with exoplanets. Extending the sample

NASA Astrophysics Data System (ADS)

Delgado Mena, E.; Israelian, G.; González Hernández, J. I.; Sousa, S. G.; Mortier, A.; Santos, N. C.; Adibekyan, V. Zh.; Fernandes, J.; Rebolo, R.; Udry, S.; Mayor, M.

2014-02-01

Aims: We want to study the effects of the formation of planets and planetary systems on the atmospheric Li abundance of planet host stars. Methods: In this work we present new determinations of lithium abundances for 326 main sequence stars with and without planets in the Teff range 5600-5900 K. The 277 stars come from the HARPS sample, the remaining targets were observed with a variety of high-resolution spectrographs. Results: We confirm significant differences in the Li distribution of solar twins (Teff = T⊙ ± 80 K, log g = log g⊙ ± 0.2 and [Fe/H] = [Fe/H]⊙ ± 0.2): the full sample of planet host stars (22) shows Li average values lower than "single" stars with no detected planets (60). If we focus on subsamples with narrower ranges in metallicity and age, we observe indications of a similar result though it is not so clear for some of the subsamples. Furthermore, we compare the observed spectra of several couples of stars with very similar parameters that show differences in Li abundances up to 1.6 dex. Therefore we show that neither age, mass, nor metallicity of a parent star is the only cause for enhanced Li depletion in solar analogues. Conclusions: We conclude that another variable must account for that difference and suggest that this could be the presence of planets that causes additional rotationally induced mixing in the external layers of planet host stars. Moreover, we find indications that the amount of depletion of Li in planet-host solar-type stars is higher when the planets are more massive than Jupiter. Based on observations collected at the La Silla Observatory, ESO (Chile), with the HARPS spectrograph at the 3.6 m ESO telescope, with CORALIE spectrograph at the 1.2 m Euler Swiss telescope and with the FEROS spectrograph at the 1.52 m ESO telescope; at the Paranal Observatory, ESO (Chile), using the UVES spectrograph at the VLT/UT2 Kueyen telescope, and with the FIES, SARG, and UES spectrographs at the 2.5 m NOT, the 3.6 m TNG and the 4.2 WHT, respectively, operated on the island of La Palma in the Spanish Observatorio del Roque de los Muchachos.Table 6 is available in electronic form at http://www.aanda.org

Protective effect of Uncaria tomentosa extract against oxidative stress and genotoxicity induced by glyphosate-Roundup® using zebrafish (Danio rerio) as a model.

PubMed

Santo, Glaucia Dal; Grotto, Alan; Boligon, Aline A; Da Costa, Bárbara; Rambo, Cassiano L; Fantini, Emily A; Sauer, Elisa; Lazzarotto, Luan M V; Bertoncello, Kanandra T; Júnior, Osmar Tomazelli; Garcia, Solange C; Siebel, Anna M; Rosemberg, Denis B; Magro, Jacir Dal; Conterato, Greicy M M; Zanatta, Leila

2018-04-01

Oxidative stress and DNA damage are involved in the glyphosate-based herbicide toxicity. Uncaria tomentosa (UT; Rubiaceae) is a plant species from South America containing bioactive compounds with known beneficial properties. The objective of this work was to evaluate the antioxidant and antigenotoxic potential of UT extract in a model of acute exposure to glyphosate-Roundup® (GR) in zebrafish (Danio rerio). We showed that UT (1.0 mg/mL) prevented the decrease of brain total thiols, the increase of lipid peroxidation in both brain and liver, and the decrease of liver GPx activity caused after 96 h of GR (5.0 mg/L) exposure. In addition, UT partially protected against the increase of micronucleus frequency induced by GR exposure in fish brain. Overall, our results indicate that UT protects against damage induced by a glyphosate-based herbicide by providing antioxidant and antigenotoxic effects, which may be related to the phenolic compounds identified in the extract.

Geophysical excitation of LOD/UT1 estimated from the output of the global circulation models of the atmosphere - ERA-40 reanalysis and of the ocean - OMCT

NASA Astrophysics Data System (ADS)

Korbacz, A.; Brzeziński, A.; Thomas, M.

2008-04-01

We use new estimates of the global atmospheric and oceanic angular momenta (AAM, OAM) to study the influence on LOD/UT1. The AAM series was calculated from the output fields of the atmospheric general circulation model ERA-40 reanalysis. The OAM series is an outcome of global ocean model OMCT simulation driven by global fields of the atmospheric parameters from the ERA- 40 reanalysis. The excitation data cover the period between 1963 and 2001. Our calculations concern atmospheric and oceanic effects in LOD/UT1 over the periods between 20 days and decades. Results are compared to those derived from the alternative AAM/OAM data sets.

SPM-Twin Telescopes: Project Overview

NASA Astrophysics Data System (ADS)

González, J. J.

2007-06-01

The SPM-Twin Project is an international initiative for a pair of 6.5-m telescopes, at the San Pedro Mártir Observatory (SPM), to provide a limber, and highly competitive, platform for discovery by focusing on scientific niches technically difficult for existing or planned larger aperture telescopes, and by exploiting the superiority of the SPM site. The telescopes are based on the proven and highly efficient Magellan concept, but each with a distinct optimization to cover two complementary but mutually exclusive aspects: (a) the "Standard Field Telescope" would have a field of view of 15'- 30', capable of observing in the optical through the thermal infrared (0.4 - 24 μm) and prepared for adaptive optics, and (b) the "Wide Field Telescope" (WFT) with a field of view of 1.5° or more, capable of multi-object fiber spectroscopy, integral field unit (IFU) spectroscopy, and potentially narrow-band imaging as well. The WFT spectroscopy would extend from 0.36 to 1.8 μm, and would contain several thousand fibers. We present a general overview of the project.

Progress on the Construction of The PS2 Telescope

NASA Astrophysics Data System (ADS)

Morgan, Jeffrey S.

2011-01-01

The PS2 telescope is the second in a series of 4 telescopes that are being fabricated for the Pan-STARRS project. Its fabrication is currently in progress and this talk will discuss the current state of this fabrication. The optics for this telescope consist of the primary and secondary mirrors along with 3 large corrector lenses. These have already been purchased from Rayleigh Optical Corporation and are mostly complete. We will show the interferometric measurements of the completed elements. The site and enclosure for PS2 have been chosen to be the old LURE north dome which sits adjacent to the current PS1 telescope on Haleakala, Maui. We will show design renderings for the renovations of this enclosure for the PS2 telescope. The design of the PS2 telescope has small, but significant differences that have been initiated by our experience with PS1. We will discuss these changes. Finally, we will discuss the fabrication schedule for PS2. The Pan-STARRS construction project is led by the University of Hawaii Institute for Astronomy with funding support from the United States Air Force AFRL and in partnership with the Maui High Performance Computing Center and MIT Lincoln Laboratory.

2. Photocopied from Photo 11456, Wheelon Station Special Folder, Engineering ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

2. Photocopied from Photo 11456, Wheelon Station Special Folder, Engineering Dept., Utah Power & Light Co., Salt Lake City, Utah. 'WHEELON HYDRO-ELECTRIC PLANT (7125 KW). INTERIOR OF MAIN BUILDING SHOWING FOUR 1000 KW UNITS. NOV 1914.' - Utah Sugar Company, Wheelon Hydoelectric Plant, Bear River, Fielding, Box Elder County, UT

77 FR 56608 - Designation for the Pocatello, ID; Evansville, IN; and Salt Lake City, UT Areas

Federal Register 2010, 2011, 2012, 2013, 2014

2012-09-13

...GIPSA is announcing the designation of Idaho Grain Inspection Service (Idaho); Ohio Valley Grain Inspection, Inc. (Ohio Valley); and Utah Depart of Agriculture and Food (Utah) to provide official services under the United States Grain Standards Act (USGSA), as amended.

8. VIEW OF STEEL, STOCKDRAWN EARTH SCRAPER USED TO SCAPE ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

8. VIEW OF STEEL, STOCK-DRAWN EARTH SCRAPER USED TO SCAPE EARTH BORROW MATERIAL AND TRANSPORT IT TO DAM DURING CONSTRUCTION, LOOKING SOUTH - High Mountain Dams in Upalco Unit, Five Point Lake Dam, Ashley National Forest, 12 miles Northwest of Swift Creek Campground, Mountain Home, Duchesne County, UT

View of the cinder block milking barn (UT126D) and attached ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

View of the cinder block milking barn (UT-126-D) and attached livestock barn (UT-126-B) with large barn (UT-126-A) in the foreground, looking east-northeast - Thomas Powers Ranch, Milking Barn, 4137 North Highway 224, Snyderville, Summit County, UT

COSAGE (Concepts Analysis Agency’s Combat Sample Generator) Analysis and Design Report. Volume 1.

DTIC Science & Technology

1984-04-29

CM. C4UT.TI ON 12 5..j FUNCTION m2-. WLr 12 j -1 ---VUTINE w-fA.NEPT 112 5 3 ; CUTINE CA S. =V3L 1 1 5- P JU T loE z- 4 L 0Y.L C T FR S 11 55 P;ICESS... CUTINE PLAT.COUNT 5 -7 1 1 OUT I N PROX.CHiEOK 5 * 14ROUTINE Sw IT CH FrO 5 Figu, .- Modules Ranked by Functional IF Tests Conti nued 3-30 -SCIENCE...2 ; CUTIN -" ...CR T=CT 231 ;OUTI- = Kv .Ir UT T 232 UuTIN.-- Mi 3s.I~d3UT , 2 3 Z Ru T iiM d:’ 3 N-l 2". OUT:N .44 1’ ,1 L3i R OUT INE %4 l Nk 0 (3o

Anti-inflammatory and antioxidant activities of cat's claw (Uncaria tomentosa and Uncaria guianensis) are independent of their alkaloid content.

PubMed

Sandoval, M; Okuhama, N N; Zhang, X J; Condezo, L A; Lao, J; Angeles', F M; Musah, R A; Bobrowski, P; Miller, M J S

2002-05-01

Cat's claw is an herbal medicine from the Amazon that is used widely to treat inflammatory disorders. The purpose of this study was to characterize the antioxidative and antiinflammatory properties of cat's claw, Uncaria tomentosa (UT) and Uncaria guianensis (UG). Alkaloids and flavanols were determined using reversed-phase HPLC; scavenging of 1,1-diphenyl-2-picrilhydrazyl (DPPH), hydroxyl radicals, and lipid peroxidation by spectrophotometry; and TNFalpha production by ELISA. Anti-inflammatory activity was assessed in vitro by inhibition of TNFalpha and nitrite production from RAW 264.7 cells exposed to LPS (50 ng/ml) and in vivo using the indomethacin-induced gastritis model. Apoptosis was assessed using the TUNEL technique and TNFalpha mRNA by in situ RT-PCR. In each of the antioxidant assays tested, UG was more potent than UT (P < 0.01). The total oxindole and pentacyclic alkaloid content of UT was 35-fold > UG. The IC50 value for inhibition of TNFalpha production was significantly (P < 0.01) higher for UT (14.1 ng/ml) vs UG (9.5 ng/ml), yet at concentrations that were considerable lower than that required for antioxidant activity. Non-alkaloid HPLC fractions from UT decreased LPS-induced TNFalpha and nitrite production in RAW 264.7 cells (P < 0.01) at a concentration range comparable to the parent botanical. Oral pretreatment for 3 d with UT protected against indomethacin-induced gastritis, and prevented TNFalpha mRNA expression and apoptosis. These results indicate that while both species of cat's claw provide effective antioxidant and anti-inflammatory activities, U. guianensis is more potent. In conclusion, the presence of oxindole or pentacyclic alkaloids did not influence the antioxidant and anti-inflammatory properties of cat's claw.

Concentrically trained cyclists are not more susceptible to eccentric exercise-induced muscle damage than are stretch-shortening exercise-trained runners.

PubMed

Snieckus, Audrius; Kamandulis, Sigitas; Venckūnas, Tomas; Brazaitis, Marius; Volungevičius, Gintautas; Skurvydas, Albertas

2013-03-01

Here, we test the hypothesis that continuous concentric exercise training renders skeletal muscles more susceptible to damage in response to eccentric exercise. Elite road cyclists (CYC; n = 10, training experience 8.1 ± 2.0 years, age 22.9 ± 3.7 years), long-distance runners (LDR; n = 10, 9.9 ± 2.3 years, 24.4 ± 2.5 years), and healthy untrained (UT) men (n = 10; 22.4 ± 1.7 years) performed 100 submaximal eccentric contractions at constant angular velocity of 60° s(-1). Concentric isokinetic peak torque, isometric maximal voluntary contraction (MVC), and electrically induced knee extension torque were measured at baseline and immediately and 48 h after an eccentric exercise bout. Muscle soreness was assessed and plasma creatine kinase (CK) activity was measured at baseline and 48 h after exercise. Voluntary and electrically stimulated knee extension torque reduction were significantly greater (p < 0.05) in UT than in LDR and CYC. Immediately and 48 h after exercise, MVC decreased by 32 % and 20 % in UT, 20 % and 5 % in LDR, and 25 % and 6 % in CYC. Electrically induced 20 Hz torque decreased at the same times by 61 and 29 % in UT, 40 and 17 % in LDR, and 26 and 14 % in CYC. Muscle soreness and plasma CK activity 48 h after exercise did not differ significantly between athletes and UT subjects. In conclusion, even though elite endurance athletes are more resistant to eccentric exercise-induced muscle damage than are UT people, stretch-shortening exercise-trained LDR have no advantage over concentrically trained CYC.

Enhanced Right-Chamber Remodeling in Endurance Ultra-Trail Athletes Compared to Marathon Runners Detected by Standard and Speckle-Tracking Echocardiography

PubMed Central

Ujka, Kristian; Bastiani, Luca; D'Angelo, Gennaro; Catuzzo, Bruna; Tonacci, Alessandro; Mrakic-Sposta, Simona; Vezzoli, Alessandra; Giardini, Guido; Pratali, Lorenza

2017-01-01

Background: Strenuous and endurance exercise training have been associated with morphological and functional heart remodeling. Two-dimensional speckle-tracking echocardiography (STE) is a novel technique that allows an accurate quantification of global myocardium deformation. Our aim was to evaluate together left and right cardiac remodeling in different long-distance running athletes: marathon runners (42 km) (M) and endurance mountain runners (>300 Km) (UT). Methods: A total of 92 athletes (70 males, 76%) including 47 M [age 45 ± 7 years; training: 18 (9–53) years*days/week], 45 UT [age 42 ± 9, training: 30 (15–66) years*days/week] underwent conventional echocardiography and STE (Beyond Diogenes 2.0, AMID) during the agonistic season. Results: Right ventricle (RV) end-diastolic area (p = 0.026), fractional area changing (FAC) (p = 0.008) and RV global longitudinal strain (GLS) were significantly increasedin UT athletes. Furthermore, UT showed larger right atrium (RA) volume (p = 0.03), reduced RA GLS and significantly increased RA global circumferential strain (GCS) compared to M. After adjustment for age, sex, and HR as covariates, UT showed a reduced RA GLS (OR 0.907; CI 0.856–0.961) and increased RV FAC (OR 1.172; CI: 1.044–1.317) compared to M. Conclusion: Athletes enrolled in UT endurance activities showed RV and RA morphological and functional remodeling to increased preload in comparison with M runners characterized by increased RV FAC and reduced RA GLS. Follow-up studies are needed to better assess the long-term clinical impact of these modifications. 2D STE is a useful tool for investigating the deformation dynamic in different sports specialties. PMID:28790928

Identification of the Quality Spot Welding used Non Destructive Test-Ultrasonic Testing: (Effect of Welding Time)

NASA Astrophysics Data System (ADS)

Sifa, A.; Endramawan, T.; Badruzzaman

2017-03-01

Resistance Spot Welding (RSW) is frequently used as one way of welding is used in the manufacturing process, especially in the automotive industry [4][5][6][7]. Several parameters influence the process of welding points. To determine the quality of a welding job needs to be tested, either by damaging or testing without damage, in this study conducted experimental testing the quality of welding or identify quality of the nugget by using Non-Destructive Test (NDT) -Ultrasonic Testing (UT), in which the identification of the quality of the welding is done with parameter thickness of worksheet after welding using NDT-UT with use same material worksheet and have more thickness of worksheet, the thickness of the worksheet single plate 1mm, with the capability of propagation Ultrasonic Testing (UT) standard limited> 3 mm [1], welding process parameters such as the time difference between 1-10s and the welding current of 8 KV, visually Heat Affected Zone ( HAZ ) have different results due to the length of time of welding. UT uses a probe that is used with a frequency of 4 MHz, diameter 10 mm, range 100 and the couplant used is oil. Identification techniques using drop 6dB, with sound velocity 2267 m / s of Fe, with the result that the effect of the Welding time affect the size of the HAZ, identification with the lowest time 1s show results capable identified joined through NDT - UT.

Optical and system engineering in the development of a high-quality student telescope kit

NASA Astrophysics Data System (ADS)

Pompea, Stephen M.; Pfisterer, Richard N.; Ellis, Scott; Arion, Douglas N.; Fienberg, Richard Tresch; Smith, Thomas C.

2010-07-01

The Galileoscope student telescope kit was developed by a volunteer team of astronomers, science education experts, and optical engineers in conjunction with the International Year of Astronomy 2009. This refracting telescope is in production with over 180,000 units produced and distributed with 25,000 units in production. The telescope was designed to be able to resolve the rings of Saturn and to be used in urban areas. The telescope system requirements, performance metrics, and architecture were established after an analysis of current inexpensive telescopes and student telescope kits. The optical design approaches used in the various prototypes and the optical system engineering tradeoffs will be described. Risk analysis, risk management, and change management were critical as was cost management since the final product was to cost around 15 (but had to perform as well as 100 telescopes). In the system engineering of the Galileoscope a variety of analysis and testing approaches were used, including stray light design and analysis using the powerful optical analysis program FRED.

Observation of Markarian 421 in TeV Gamma Rays Over a 14-Year Time Span

NASA Technical Reports Server (NTRS)

Acciari, V. A.; Arlen, T.; Aune, T.; Benbow, W.; Bird, R.; Bouvier, A.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; McEnery, Julie E.

2013-01-01

The variability of the blazar Markarian 421 in TeV gamma rays over a 14-year time period has been explored with theWhipple 10 m telescope. It is shown that the dynamic range of its flux variations is large and similar to that in X-rays. A correlation between the X-ray and TeV energy bands is observed during some bright flares and when the complete data sets are binned on long timescales. The main database consists of 878.4 hours of observation with theWhipple telescope, spread over 783 nights. The peak energy response of the telescope was 400 GeV with 20% uncertainty. This is the largest database of any TeV-emitting active galactic nucleus (AGN) and hence was used to explore the variability profile of Markarian 421. The time-averaged flux from Markarian 421 over this period was 0.446+/-0.008 Crab flux units. The flux exceeded 10 Crab flux units on three separate occasions. For the 2000-2001 season the average flux reached 1.86 Crab units, while in the 1996-1997 season the average flux was only 0.23 Crab units.

Movement of NH3 through the human urea transporter B: a new gas channel

PubMed Central

Musa-Aziz, Raif; Enkavi, Giray; Mahinthichaichan, P.; Tajkhorshid, Emad; Boron, Walter F.

2013-01-01

Aquaporins and Rh proteins can function as gas (CO2 and NH3) channels. The present study explores the urea, H2O, CO2, and NH3 permeability of the human urea transporter B (UT-B) (SLC14A1), expressed in Xenopus oocytes. We monitored urea uptake using [14C]urea and measured osmotic water permeability (Pf) using video microscopy. To obtain a semiquantitative measure of gas permeability, we used microelectrodes to record the maximum transient change in surface pH (ΔpHS) caused by exposing oocytes to 5% CO2/33 mM HCO3− (pHS increase) or 0.5 mM NH3/NH4+ (pHS decrease). UT-B expression increased oocyte permeability to urea by >20-fold, and Pf by 8-fold vs. H2O-injected control oocytes. UT-B expression had no effect on the CO2-induced ΔpHS but doubled the NH3-induced ΔpHS. Phloretin reduced UT-B-dependent urea uptake (Jurea*) by 45%, Pf* by 50%, and (−ΔpHS*)NH3 by 70%. p-Chloromercuribenzene sulfonate reduced Jurea* by 25%, Pf* by 30%, and (ΔpHS*)NH3 by 100%. Molecular dynamics (MD) simulations of membrane-embedded models of UT-B identified the monomeric UT-B pores as the main conduction pathway for both H2O and NH3 and characterized the energetics associated with permeation of these species through the channel. Mutating each of two conserved threonines lining the monomeric urea pores reduced H2O and NH3 permeability. Our data confirm that UT-B has significant H2O permeability and for the first time demonstrate significant NH3 permeability. Thus the UTs become the third family of gas channels. Inhibitor and mutagenesis studies and results of MD simulations suggest that NH3 and H2O pass through the three monomeric urea channels in UT-B. PMID:23552862

Tolerance of uncertainty: Conceptual analysis, integrative model, and implications for healthcare.

PubMed

Hillen, Marij A; Gutheil, Caitlin M; Strout, Tania D; Smets, Ellen M A; Han, Paul K J

2017-05-01

Uncertainty tolerance (UT) is an important, well-studied phenomenon in health care and many other important domains of life, yet its conceptualization and measurement by researchers in various disciplines have varied substantially and its essential nature remains unclear. The objectives of this study were to: 1) analyze the meaning and logical coherence of UT as conceptualized by developers of UT measures, and 2) develop an integrative conceptual model to guide future empirical research regarding the nature, causes, and effects of UT. A narrative review and conceptual analysis of 18 existing measures of Uncertainty and Ambiguity Tolerance was conducted, focusing on how measure developers in various fields have defined both the "uncertainty" and "tolerance" components of UT-both explicitly through their writings and implicitly through the items constituting their measures. Both explicit and implicit conceptual definitions of uncertainty and tolerance vary substantially and are often poorly and inconsistently specified. A logically coherent, unified understanding or theoretical model of UT is lacking. To address these gaps, we propose a new integrative definition and multidimensional conceptual model that construes UT as the set of negative and positive psychological responses-cognitive, emotional, and behavioral-provoked by the conscious awareness of ignorance about particular aspects of the world. This model synthesizes insights from various disciplines and provides an organizing framework for future research. We discuss how this model can facilitate further empirical and theoretical research to better measure and understand the nature, determinants, and outcomes of UT in health care and other domains of life. Uncertainty tolerance is an important and complex phenomenon requiring more precise and consistent definition. An integrative definition and conceptual model, intended as a tentative and flexible point of departure for future research, adds needed breadth, specificity, and precision to efforts to conceptualize and measure UT. Copyright © 2017 The Authors. Published by Elsevier Ltd.. All rights reserved.

Clinical utility of third-trimester uterine artery Doppler in the prediction of brain hemodynamic deterioration and adverse perinatal outcome in small-for-gestational-age fetuses.

PubMed

Cruz-Martinez, R; Savchev, S; Cruz-Lemini, M; Mendez, A; Gratacos, E; Figueras, F

2015-03-01

To assess the clinical value of third-trimester uterine artery (UtA) Doppler ultrasound in the prediction of hemodynamic deterioration and adverse perinatal outcome in term small-for-gestational-age (SGA) fetuses. UtA Doppler parameters, cerebroplacental ratio (CPR) and fetal middle cerebral artery (MCA) pulsatility index (PI) were evaluated weekly, starting from the time of SGA diagnosis until 24 h before induction of labor, in a cohort of 327 SGA fetuses with normal umbilical artery PI (< 95th centile), delivered at > 37 weeks' gestation. Differences in the sequence of CPR and MCA-PI changes < 5th centile, between the group with normal UtA Doppler indices at diagnosis and those with abnormal UtA indices, were analyzed by survival analysis. In addition, the use of UtA Doppler value, alone or in combination with a brain Doppler scan before delivery, to predict the risk of Cesarean section, Cesarean section for non-reassuring fetal status (NRFS), neonatal acidosis and neonatal hospitalization was evaluated by logistic regression analysis, adjusted for gestational age at birth and birth-weight percentile. Abnormal UtA Doppler at diagnosis of SGA was associated with a higher risk of developing abnormal brain Doppler indices before induction of labor than in those with a normal UtA at diagnosis (62.7% vs 34.6%, respectively; P < 0.01). Compared to those with normal UtA Doppler indices, those with abnormal UtA Doppler findings were associated with a higher risk of intrapartum Cesarean section (52.2% vs 37.3%, respectively; P = 0.03), Cesarean section for NRFS (35.8% vs 23.1%, respectively; P = 0.03), neonatal acidosis (10.4% vs 7.7%, respectively; P = 0.47) and neonatal hospitalization (23.9% vs 16.5%, respectively; P = 0.16). Logistic regression analysis indicated that UtA Doppler findings were not significantly associated with adverse perinatal outcome independent of brain Doppler findings. UtA Doppler indices predict adverse perinatal outcome, but do not help to improve the predictive value of brain Doppler indices. However, at the time of SGA diagnosis they identify the subgroup of fetuses at highest risk of progression to abnormal brain Doppler findings. Copyright © 2014 ISUOG. Published by John Wiley & Sons Ltd.

Very high cloud detection in more than two decades of HIRS data

NASA Astrophysics Data System (ADS)

Kolat, Utkan; Menzel, W. Paul; Olson, Erik; Frey, Richard

2013-04-01

This paper reports on the use of High-resolution Infrared Radiation Sounder (HIRS) measurements to infer the presence of upper tropospheric and lower stratospheric (UT/LS) clouds. UT/LS cloud detection is based on the fact that, when viewing an opaque UT/LS cloud that fills the sensor field of view, positive lapse rates above the tropopause cause a more absorbing CO2 or H2O-sensitive spectral band to measure a brightness temperature warmer than that of a less absorbing or nearly transparent infrared window spectral band. The HIRS sensor has flown on 16 polar-orbiting satellites from TIROS-N through NOAA-19 and Metop-A and -B, forming the only 30 year record that includes H2O and CO2-sensitive spectral bands enabling the detection of these UT/LS clouds. Comparison with collocated Cloud-Aerosol Lidar with Orthogonal Polarization data reveals that 97% of the HIRS UT/LS cloud determinations are within 2.5 km of the tropopause (defined as the coldest level in the National Centers for Environmental Prediction Global Data Assimilation System); more clouds are found above the tropopause than below. From NOAA-14 data spanning 1995 through 2005, we find indications of UT/LS clouds in 0.7% of the observations from 60N to 60S using CO2 absorption bands; however, in the region of the Inter-Tropical Convergence Zone (ITCZ), this increases to 1.7%. During El Niño years, UT/LS clouds shift eastward out of their normal location in the western Pacific region. Monthly trends from 1987 through 2011 using data from NOAA-10 onwards show decreases in UT/LS cloud detection in the region of the ITCZ from 1987 until 1996, increases until 2001, and decreases thereafter.

Approaches to reduce urinary tract injury during management of placenta accreta, increta, and percreta: a systematic review.

PubMed

Tam Tam, Kiran Babu; Dozier, James; Martin, James Nello

2012-04-01

A systematic review of the literature was conducted to answer the following question: are there enhancements to standard peripartum hysterectomy technique that minimize unintentional urinary tract (UT) injury in pregnancies complicated by invasive placental attachment (INPLAT)? A PubMed search of English language articles on INPLAT published by June 2010 was conducted. Data regarding the following parameters was required for inclusion in the quantitative analysis of the review's objective: (1) type of INPLAT, (2) details pertaining to medical and surgical management of INPLAT, and (3) complications, if any, associated with management. An attempt was made to identify approaches that may lower the risk of unintentional UT injury. Most cases (285 of 292) were managed by hysterectomy. There were 83 (29%) cases of unintentional UT injury. Antenatal diagnosis of INPLAT lowered the rate of UT injury (39% vs. 63%; P = 0.04). Information regarding surgical technique or medical management was available for 90 cases; 14 of these underwent a standard hysterectomy technique. Methotrexate treatment and 11 modifications of the surgical technique were associated with 16% unintentional UT injury rate as opposed to 57% for standard hysterectomy (P = 0.002). The use of ureteral stents reduced risk of urologic injury (P = 0.01). Multiple logistic regression analysis identified antenatal diagnosis as the significant predictor of an intact UT. Antenatal diagnosis of INPLAT is paramount to minimize UT injury. Utilization of management modifications identified in this review may reduce urologic injury due to INPLAT.

Cluster Observations of reconnection along the dusk flank of the magnetosphere

NASA Astrophysics Data System (ADS)

Escoubet, C.-Philippe; Grison, Benjamin; Berchem, Jean; Trattner, Karlheinz; Lavraud, Benoit; Pitout, Frederic; Soucek, Jan; Richard, Robert; Laakso, Harri; Masson, Arnaud; Dunlop, Malcolm; Dandouras, Iannis; Reme, Henri; Fazakerley, Andrew; Daly, Patrick

2015-04-01

Magnetic reconnection is generally accepted to be the main process that transfers particles and energy from the solar wind to the magnetosphere. The location of the reconnection site depends on the orientation of the interplanetary magnetic field (IMF) in the solar wind: on the dayside magnetosphere for an IMF southward, on the lobes for an IMF northward and on the flanks for an IMF in the East-West direction. Since most of observations of reconnection events have sampled a limited region of space simultaneously it is still not yet know if the reconnection line is extended over large regions of the magnetosphere or if is patchy and made of many reconnection lines. We report a Cluster crossing on 5 January 2002 near the exterior cusp on the southern dusk side where we observe multiple sources of reconnection/injections. The IMF was mainly azimuthal (IMF-By around -5 nT), the solar wind speed lower than usual around 280 km/s with the density of order 5 cm-3. The four Cluster spacecraft had an elongated configuration near the magnetopause. C4 was the first spacecraft to enter the cusp around 19:52:04 UT, followed by C2 at 19:52:35 UT, C1 at 19:54:24 UT and C3 at 20:13:15 UT. C4 and C1 observed two ion energy dispersions at 20:10 UT and 20:40 UT and C3 at 20:35 UT and 21:15 UT. Using the time of flight technique on the upgoing and downgoing ions, which leads to energy dispersions, we obtain distances of the ion sources between 14 and 20 RE from the spacecraft. The slope of the ion energy dispersions confirmed these distances. Using Tsyganenko model, we find that these sources are located on the dusk flank, past the terminator. The first injection by C3 is seen at approximately the same time as the 2nd injection on C1 but their sources at the magnetopause were separated by more than 7 RE. This would imply that two distinct sources were active at the same time on the dusk flank of the magnetosphere. In addition, a flow reversal was observed at the magnetopause on C4 which would be an indication that reconnection is also taking place near the exterior cusp quasi-simultaneously.

With the VLT Interferometer towards Sharper Vision

NASA Astrophysics Data System (ADS)

2000-05-01

The Nova-ESO VLTI Expertise Centre Opens in Leiden (The Netherlands) European science and technology will gain further strength when the new, front-line Nova-ESO VLTI Expertise Centre (NEVEC) opens in Leiden (The Netherlands) this week. It is a joint venture of the Netherlands Research School for Astronomy (NOVA) (itself a collaboration between the Universities of Amsterdam, Groningen, Leiden, and Utrecht) and the European Southern Observatory (ESO). It is concerned with the Very Large Telescope Interferometer (VLTI). The Inauguration of the new Centre will take place on Friday, May 26, 2000, at the Gorlaeus Laboratory (Lecture Hall no. 1), Einsteinweg 55 2333 CC Leiden; the programme is available on the web. Media representatives who would like to participate in this event and who want further details should contact the Nova Information Centre (e-mail: jacques@astro.uva.nl; Tel: +31-20-5257480 or +31-6-246 525 46). The inaugural ceremony is preceded by a scientific workshop on ground and space-based optical interferometry. NEVEC: A Technology Centre of Excellence As a joint project of NOVA and ESO, NEVEC will develop in the coming years the expertise to exploit the unique interferometric possibilities of the Very Large Telescope (VLT) - now being built on Paranal mountain in Chile. Its primary goals are the * development of instrument modeling, data reduction and calibration techniques for the VLTI; * accumulation of expertise relevant for second-generation VLTI instruments; and * education in the use of the VLTI and related matters. NEVEC will develop optical equipment, simulations and software to enable interferometry with VLT [1]. The new Center provides a strong impulse to Dutch participation in the VLTI. With direct involvement in this R&D work, the scientists at NOVA will be in the front row to do observations with this unique research facility, bound to produce top-level research and many exciting new discoveries. The ESO VLTI at Paranal ESO PR Photo 14a/00 ESO PR Photo 14a/00 [Preview - JPEG: 359 x 400 pix - 120k] [Normal - JPEG: 717 x 800 pix - 416k] [High-Res - JPEG: 2689 x 3000 pix - 6.7M] Caption : A view of the Paranal platform with the four 8.2-m VLT Unit Telescopes (UTs) and the foundations for the 1.8-m VLT Auxiliary Telescopes (ATs) that together will be used as the VLT Interferometer (VLTI). The three ATs will move on rails (yet to be installed) between the thirty observing stations above the holes that provide access to the underlying tunnel system. The light beams from the individual telescopes will be guided towards the centrally located, partly underground Interferometry Laboratory in which the VLTI instruments will be set up. This photo was obtained in December 1999 at which time some construction materials were still present on the platform; they were electronically removed in this reproduction. The ESO VLT facility at Paranal (Chile) consists of four Unit Telescopes with 8.2-m mirrors and several 1.8-m auxiliary telescopes that move on rails, cf. PR Photo 14a/00 . While each of the large telescopes can be used individually for astronomical observations, a prime feature of the VLT is the possibility to combine all of these telescopes into the Very Large Telescope Interferometer (VLTI) . In the interferometric mode, the light beams from the VLT telescopes are brought together at a common focal point in the Interferometry Laboratory that is placed at the centre of the observing platform on top of Paranal. In principle, this can be done in such a way that the resulting (reconstructed) image appears to come from a virtual telescope with a diameter that is equal to the largest distance between two of the individual telescopes, i.e., up to about 200 metres. The theoretically achievable image sharpness of an astronomical telescope is proportional to its diameter (or, for an interferometer, the largest distance between two of its component telescopes). The interferometric observing technique will thus allow the VLTI to produce images as sharp as 0.001 arcsec (at wavelength 1 µm) - this corresponds to viewing the shape of a golfball at more than 8,000 km distance. The VLTI will do even better when this technique is later extended to shorter wavelengths in the visible part of the spectrum - it may ultimately distinguish human-size objects on the surface of the Moon (a 2-metre object at this distance, about 400,000 km, subtends an angle of about 0.001 arcsec). However, interferometry with the VLT demands that the wavefronts of light from the individual telescopes that are up to 200 meters apart must be matched exactly, with less than 1 wavelength of difference. This demands continuous mechanical stability to a fraction of 1 µm (0.001 mm) for the heavy components over such large distances, and is a technically formidable challenge. This is achieved by electronic feed-back loops that measure and adjust the distances during the observations. In addition, continuous and automatic correction of image distortions from air turbulence in the telescopes' field of view is performed by means of adaptive optics [2]. VLTI technology at ESO, industry and institutes The VLT Interferometer is based on front-line technologies introduced and advanced by ESO, and its many parts are now being constructed at various sites in Europe. ESO PR Photo 14b/00 ESO PR Photo 14b/00 [Preview - JPEG: 359 x 400 pix - 72k] [Normal - JPEG: 717 x 800 pix - 200k] [High-Res - JPEG: 2687 x 3000 pix - 1.3M] Caption : Schematic lay-out of the VLT Interferometer. The light from a distant celestial objects enters two of the VLT telescopes and is reflected by the various mirrors into the Interferometric Tunnel, below the observing platform on the top of Paranal. Two Delay Lines with moveable carriages continuously adjust the length of the paths so that the two beams interfere constructively and produce fringes at the interferometric focus in the laboratory. In 1998, Fokker Space (also in Leiden, The Netherlands) was awarded a contract for the delivery of the three Delay Lines of the VLTI. This mechanical-optical system will compensate the optical path differences of the light beams from the individual telescopes. It is necessary to ensure that the light from all telescopes arrives in the same phase at the focal point of the interferometer. Otherwise, the very sharp interferometric images cannot be obtained. More details are available in the corresponding ESO PR 04/98 and recent video sequences, included in ESO Video News Reel No. 9 and Video Clip 04a/00 , cf. below. Also in 1998, the company AMOS (Liège, Belgium) was awarded an ESO contract for the delivery of the three 1.8-m Auxiliary Telescopes (ATs) and of the full set of on-site equipment for the 30 AT observing stations, cf. ESO PR Photos 25a-b/98. This work is now in progress at the factory - various scenes are incorporated into ESO Video News Reel No. 9 and Video Clip 04b/00 . Several instruments for imaging and spectroscopy are currently being developed for the VLTI. The first will be the VLT Interferometer Commissioning Instrument (VINCI) that is the test and first-light instrument for the VLT Interferometer. It is being built by a consortium of French and German institutes under ESO contract. The VLTI Near-Infrared / Red Focal Instrument (AMBER) is a collaborative project between five institutes in France, Germany and Italy, under ESO contract. It will operate with two 8.2-m UTs in the wavelength range between 1 and 2.5 µm during a first phase (2001-2003). The wavelength coverage will be extended in a second phase down to 0.6 µm (600 nm) at the time the ATs become operational. Main scientific objectives are the investigation at very high-angular resolution of disks and jets around young stellar objects and dust tori at active galaxy nuclei with spectroscopic observations. The Phase-Referenced Imaging and Microarcsecond Astrometry (PRIMA) device is managed by ESO and will allow simultaneous interferometric observations of two objects - each with a maximum size of 2 arcsec - and provide exceedingly accurate positional measurements. This will be of importance for many different kinds of astronomical investigations, for instance the search for planetary companions by means of accurate astrometry. The MID-Infrared interferometric instrument (MIDI) is a project collaboration between eight institutes in France, Germany and the Netherlands [1], under ESO contract. The actual design of MIDI is optimized for operation at 10 µm and a possible extension to 20 µm is being considered. Notes [1] The NEVEC Centre is involved in the MIDI project for the VLTI. Another joint project between ESO and NOVA is the Wide-Field Imager OMEGACAM for the VLT Survey Telescope (VST) that will be placed at Paranal. [2] Adaptive Optics systems allow to continuously "re-focus" an astronomical telescope in order to compensate for the atmospheric turbulence and thus to obtain the sharpest possible images. The work at ESO is described on the Adaptive Optics Team Homepage. VLTI-related videos now available In conjunction with the Inauguration of the NEVEC Centre (Leiden, The Netherlands) on May 26, 2000, ESO has issued ESO Video News Reel No. 9 (May 2000) ( "The Sharpest Vision - Interferometry with the VLT" ). Tapes with this VNR, suitable for transmission and in full professional quality (Betacam, etc.), are now available for broadcasters upon request; please contact the ESO EPR Department for more details. Extracts from this VNR are available as ESO Video Clips 04a/00 and 04b/00 . ESO PR Video Clip 04a/00 [160x120 pix MPEG-version] ESO PR Video Clip 04a/00 (2600 frames/1:44 min) [MPEG Video+Audio; 160x120 pix; 2.4Mb] [MPEG Video+Audio; 320x240 pix; 4.8 Mb] [RealMedia; streaming; 33kps] [RealMedia; streaming; 200kps] ESO Video Clip 04a/00 shows some recent tests with the prototype VLT Delay Line carriage at FOKKER Space (Leiden, The Netherlands. This device is crucial for the proper functioning of the VLTI and will be mounted in the main interferometric tunnel at Paranal. Contents: Outside view of the FOKKER site. The carriage on rails. The protecting cover is removed. View towards the cat's eye. The carriage moves on the rails. ESO PR Video Clip 04b/00 [160x120 pix MPEG-version] ESO PR Video Clip 04b/00 (3425 frames/2:17 min) [MPEG Video+Audio; 160x120 pix; 3.2Mb] [MPEG Video+Audio; 320x240 pix; 6.3 Mb] [RealMedia; streaming; 33kps] [RealMedia; streaming; 200kps] ESO Video Clip 04b/00 shows the construction of the 1.8-m VLT Auxiliary Telescopes at AMOS (Liège, Belgium). Contents: External view of the facility. Computer drawing of the mechanics. The 1.8-m mirror (graphics). Construction of the centerpiece of the telescope tube. Mechanical parts. Checking the optical shape of an 1.8-m mirror. Mirror cell with supports for the 1.8-m mirror. Test ramp with rails on which the telescope moves and an "observing station" (the hole). The telescope yoke that will support the telescope tube. Both clips are available in four versions: two MPEG files and two streamer-versions of different sizes; the latter require RealPlayer software. They may be freely reproduced if ESO is mentioned as source. Most of the ESO PR Video Clips at the ESO website provide "animated" illustrations of the ongoing work and events at the European Southern Observatory. The most recent clip was: ESO PR Video Clip 03/00 with a trailer for "Physics on Stage" (2 May 2000). Information is also available on the web about other ESO videos.

Replicated Wolter-I X-ray Optics for Lightweight, High Angular Resolution, Large Collecting Area X-Ray Telescopes

NASA Technical Reports Server (NTRS)

Joy, M.; Bilbro, J.; Elsner, R.; Jones, W.; Kolodziejczak, J.; Petruzzo, J.; ODell, S.; Weisskopf, M.

1997-01-01

The next generation of orbiting x-ray observatories will require high angular resolution telescopes that have an order of magnitude greater collecting area in the 0.1-10 keV spectral region than those currently under construction, but with a much lower weight and cost per unit area. Replicated Wolter-I x-ray optics have the potential to meet this requirement. The currently demonstrated capabilities of replicated Wolter-I optics will be described, and a development plan for creating lightweight, high angular resolution, large effective area x-ray telescopes will be presented.

DOE Office of Scientific and Technical Information (OSTI.GOV)

Hirano, Teruyuki; Masuda, Kento; Suto, Yasushi

We report a joint analysis of the Rossiter-McLaughlin (RM) effect with Subaru and the Kepler photometry for the Kepler Object of Interest (KOI) 94 system. The system is comprised of four transiting planet candidates with orbital periods of 22.3 (KOI-94.01), 10.4 (KOI-94.02), 54.3 (KOI-94.03), and 3.7 (KOI-94.04) days from the Kepler photometry. We performed the radial velocity (RV) measurement of the system with the Subaru 8.2 m telescope on UT 2012 August 10, covering a complete transit of KOI-94.01 for {approx}6.7 hr. The resulting RV variation due to the RM effect spectroscopically confirms that KOI-94.01 is indeed the transiting planetmore » and implies that its orbital axis is well aligned with the stellar spin axis; the projected spin-orbit angle {lambda} is estimated as -6{sup +13}{sub -11} deg. This is the first measurement of the RM effect for a multiple transiting system. Remarkably, the archived Kepler light curve around BJD = 2455211.5 (date in UT 2010 January 14/15) indicates a 'double-transit' event of KOI-94.01 and KOI-94.03, in which the two planets transit the stellar disk simultaneously. Moreover, the two planets partially overlap with each other, and exhibit a 'planet-planet eclipse' around the transit center. This provides a rare opportunity to put tight constraints on the configuration of the two transiting planets by joint analysis with our Subaru RM measurement. Indeed, we find that the projected mutual inclination of KOI-94.01 and KOI-94.03 is estimated to be {delta} = -1.{sup 0}15 {+-} 0.{sup 0}55. Implications for the migration model of multiple planet systems are also discussed.« less

Giant Eyes for the VLT Interferometer

NASA Astrophysics Data System (ADS)

2001-11-01

First Scientific Results with Combined Light Beams from Two 8.2-m Unit Telescopes Summary It started as a preparatory technical experiment and it soon developed into a spectacular success. Those astronomers and engineers who were present in the control room that night now think of it as the scientific dawn of the Very Large Telescope Interferometer (VLTI) . On October 29, 2001, ANTU and MELIPAL , two of the four VLT 8.2-m Unit Telescopes at the ESO Paranal Observatory, were linked for the first time. Light from the southern star Achernar (Alpha Eridani) was captured by the two telescopes and sent to a common focus in the observatory's Interferometric Laboratory. Following careful adjustments of the optical paths, interferometric fringes were soon recorded there, proving that the beams from the two telescopes had been successfully combined "in phase" . From an analysis of the observed pattern (the "fringe contrast"), the angular diameter of Achernar was determined to be 1.9 milli-arcsec. At the star's distance (145 light-years), this corresponds to a size of 13 million km. The observation is equivalent to measuring the size of a 4-metre long car on the surface of the Moon. This result marks the exciting starting point for operations with the Very Large Telescope Interferometer (VLTI) and it was immediately followed up by other scientific observations. Among these were the first measurements of the diameters of three red dwarf stars ("Kapteyn's star" - HD 33793, HD 217987 and HD 36395), a precise determination of the variable diameters of the pulsating Cepheid stars Beta Doradus and Zeta Geminorum (of great importance for the calibration of the universal distance scale), as well as a first interferometric measurement of the core of Eta Carinae , an intriguing, massive southern object that may possibly become the next supernova in our galaxy. This milestone is another important step towards the ultimate goal of the VLT project - to combine all four 8.2-m telescopes into the most powerful optical/infrared telescope system on Earth. When ready, it will be able to reveal at least 15 times finer details in astronomical objects than what is possible with any existing, single ground-based telescope. PR Photo 30a/01 : Overview of the VLT Interferometer . PR Photo 30b/01 : "Joint" stellar light-spot produced via ANTU and MELIPAL at the VLTI focus. PR Photo 30c/01 : Interferometric fringes from the star Achernar . PR Photo 30d/01 : Time sequence of fringes from Achernar. PR Photo 30e/01 : "Visibility curve" of the star Psi Phoenicis . Scientific Appendix First VLTI observations with two 8.2-m telescopes ESO PR Photo 30a/01 ESO PR Photo 30a/01 [Preview - JPEG: 357 x 400 pix - 82k] [Normal - JPEG: 713 x 800 pix - 208k] [Hi-Res - JPEG: 2673 x 3000 pix - 1.4M] ESO PR Photo 30b/01 ESO PR Photo 30b/01 [Preview - JPEG: 400 x 350 pix - 57k] [Normal - JPEG: 800 x 700 pix - 176k] Caption : PR Photo 30a/01 : Overview of the VLT Interferometer as it was operated when the light beams from two of the 8.2-m telescopes were combined. The VINCI instrument that was used for the present test, is located at the common focus in the Interferometric Laboratory. PR Photo 30b/01 shows one of the first "joint" light-spots from a star as seen at this VLTI focus and resulting from the superposition of light collected with the 8.2-m VLT ANTU and MELIPAL telescopes. Despite the long optical paths (about 200 m), the quality is excellent (FWHM = 0.45 arcsec). Note that this is not (yet) an image of the stellar surface. At 1 o'clock in the morning of October 30, 2001, ESO astronomers and engineers working in the VLTI Control Room successfully combined the light from ANTU and MELIPAL , two of the four 8.2-m VLT Unit Telescopes at the Paranal Observatory. The same night, a series of high-resolution test observations with the VINCI instrument [1] at the focus of the VLT Interferometer (VLTI) proved that this complex system was functioning extremely well, and within the technical specifications . Following about seven months after the moment of "VLTI first light" during which the light beams from two small test telescopes were combined - as described in detail in ESO Press Release 06/01 - this accomplishment above all serves as a demonstration of the possibilities and potential of interferometric observations with the four giant VLT telescopes. The two large telescopes used for the present test are separated by 102 metres. In order to properly combine the starlight received by them, a train of 25 mirrors is needed . All of them must be adjusted with a precision of one thousandth of a millimetre or better. As can be seen on PR Photo 30a/01 , the light from the observed star is first directed towards the Nasmyth focus by three mirrors in the telescope tube. From here, it continues towards the intermediate Coudé focus below the telescope and then onwards through a subterranean light duct to the VLTI Delay Lines that are installed in the Interferometric Tunnel . At the end of this long chain of mirrors and after traveling a distance of approximately 200 metres, the light finally reaches the VINCI instrument in which the two beams interact coherently (in phase) to produce "interferometric fringes". The tests have shown that the starlight arrives at the VINCI instrument with a pointing accuracy of about 1 arcsecond and, even more important, with a long-term tracking stability of the order of 0.2 arcseconds per hour. In fact, the image quality measured at the focus of VINCI is essentially identical to that of the individual telescopes at the Nasmyth (and Cassegrain) foci. Stellar images as sharp as 0.4 arcsec (note that this is the size of the "seeing disk" FWHM, not yet a real image of the stellar surface; the VLTI will start producing two-dimensional images of stars and other objects at a later stage) have been obtained at the interferometric focus, cf. PR Photo 30b/01 . The installation of an Adaptive Optics system (see below) will later reduce the image size to the theoretical limit of 0.057 arcsec (for observations with an 8.2-m telescope in the infrared K-band at wavelength 2.2 µm (or 0.032 arcsec in the J-band at 1.2 µm). First scientific results already during the test observations ESO PR Photo 30c/01 ESO PR Photo 30c/01 [Preview - JPEG: 400 x 368 pix - 50k] [Normal - JPEG: 800 x 736 pix - 136k] ESO PR Photo 30d/01 ESO PR Photo 30d/01 [Preview - JPEG: 400 x 332 pix - 168k] [Normal - JPEG: 800 x 663 pix - 440k] Caption : PR Photo 30c/01 shows the interferometric fringes of the star Achernar , as observed on the computer screen in the VLTI Control Room, at the moment of "First Light" with two 8.2-m VLT telescopes. PR Photo 30d/01 displays the time evolution of the interferometric fringes obtained on Achernar . Each horizontal scan represents a recorded fringe pattern, with time running vertically from bottom to top. PR Photo 30c/01 was extracted from one of these scans. The technical demonstration being so successful, the ESO astronomers and engineers involved in the development of the VLTI immediately decided to go one step further. And indeed, the interferometric fringes recorded with the light beams from two 8.2-m VLT telescopes during these initial technical tests have already led to some very valuable scientific results. The first star to be observed - the brightest star in the southern constellation Eridanus (The River) and known as Alpha Eridani or Achernar - is quite different from our Sun. It is estimated to be several times more massive and, with a surface temperature of about 20000 degrees, it is about three times hotter than our local star. The distance to Achernar has been measured by the ESA HIPPARCOS satellite as about 145 light-years, and from its apparent brightness, it is found to be almost 1000 times more luminous than the Sun. Consequently, it depletes its energy resources much faster and has a much shorter life expectancy (about 100 million years) than the Sun (about 10,000 million years). The new measurement with the VLTI found the angular diameter of Achernar to be 0.00192 ± 0.00005 arcsec . This is equivalent to the angle subtended by a 1 Euro coin (diameter 23.25 mm) as seen from a distance of 2500 km, or by a car (4 metres long) on the surface of the Moon. At the indicated distance, this angle also shows that the real size of Achernar is about 13 million kilometres, and that it is therefore nearly ten times larger than our Sun. Following that first observation, and in spite of the many technical tests scheduled at this moment of the VLTI commissioning work, the astronomers were able to carry out several other scientific observations. During this exciting first period of operation, among others, measurements were made of three red dwarf stars, three stars surrounded by disks, one red giant star, two Cepheid stars and one luminous blue variable star. Preliminary results from some of these observations are described in the Appendix. Angular measurements with the VLTI like the present ones will soon become routine and will allow astronomers to measure accurately the physical characteristics of many different types of stars. For instance, the precise measurement of the angular diameter of Achernar will make it possible to deduce directly and accurately its surface temperature, an important information for our understanding of the formation and evolution of such hot and massive stars. From 40-cm to 8.2-m The present event follows after half a year of much hard work by ESO astronomers and engineers. Earlier this year, the VLTI achieved "first fringes" by combining two small 40-cm siderostat telescopes ( ESO PR 06/01 ). Since then, ESO astronomers and engineers have upgraded the VLTI and are preparing it for regular observations that will start next year. The present results obtained with the combination of two giant telescopes constitute one important milestone along this road. Between March and October 2001, about 1000 individual measurements were carried out on celestial objects with the light beams from the small test telescopes. This process is on-going, as part of the commissioning of the VLTI, and is aimed at a detailed technical characterization of the interferometer and thorough knowledge of its performance. Such observations mainly serve to obtain technical data. Nevertheless, some of them also provide interesting scientific results . For example, during the week just prior to the first fringes now achieved with two large telescopes, nearly 150 measurements were obtained over 4 nights. Among them, five Mira stars (a type of large and cool, pulsating stars) and two close binary stellar systems were observed - some of them had never before been studied interferometrically. Moreover, a large number of objects were observed for calibration. These data are now being evaluated, and will help astronomers to refine their understanding of the capabilities of the VLTI - they will soon become available to the astronomical community via the VLT archive. In the same period, substantial additions were made to the system, e.g., a third Delay Line was installed in the Interferometric Tunnel. This allows the use of the telescopes on the east side of the beam combination laboratory (including MELIPAL) and also to combine the light beams from up to three telescopes at a later moment. The additional mirrors needed in order to permit the combination of the light from the two 8.2-m telescopes were installed. The extensive software that controls the telescopes and the instruments has undergone several revisions to accommodate the increased needs required by the more complex system of Unit Telescopes, delay lines and test instruments. At the same time, the overall reliability of the facility has been constantly improved. The path that the light travels from the two 8.2-m telescopes to the VINCI instrument must be kept constant to within a fraction of a micron , or better than one thousandth of a millimetre! Although it is therefore extremely sensitive to even very small disturbances, the VLT Interferometer has proven to be remarkably reliable and robust. For instance, an earthquake of magnitude 4+ on the Richter scale happened in August 2001 in the middle of a series of interferometric measurements. However, thanks to the many safeguards and compensatory measures built into the system, the VLTI continued to function all through the tremor. The observations were barely affected by the ground vibrations. It should also be noted that, unlike the 40-cm siderostat telescopes, the 8.2-m telescopes are so large that the images they produce are significantly affected by atmospheric turbulence. In order to overcome this problem, ESO is now developing a system of "Adaptive Optics" correctors ( MACAO ) which will "remove" the distortions introduced by the atmospheres by means of small, rapidly reacting computer-controlled deformable mirrors. From 2003, this system will increase the sensitivity of the VLTI by a factor of about 100 (5 magnitudes) compared to the present observations without adaptive optics. VLT Instrumentation The next steps in the VLTI project will be the integration of a new instrument working at a wavelength of 10 µm (the Mid-Infrared interferometric instrument for the VLTI (MIDI) ) in the middle of 2002, the addition of a fringe tracker ( FINITO ) and then of a 3-way, 3-photometric bands instrument (the near-infrared/red VLTI focal instrument (AMBER) ) at the beginning of 2003. Following closely will be the addition of three 1.8-m movable telescopes dedicated to interferometry, and of the Adaptive Optics system. With all these components in place, the VLTI will represent the most powerful interferometer available in the southern hemisphere, and will enable scientific investigations on a wide range of topics ranging from the direct detection of planets around other stars, to the formation and early evolution of stars, to the study of extragalactic objects. A dedication to Ariela Rijo On behalf of the staff, the Director of the Paranal Observatory adds this message: "The Paranal Observatory, while very pleased at the present success of the first fringes from two of the 8.2-m telescopes, at the same time is greatly saddened by the loss of our colleague Ariela Rijo who passed away on October 31" . "She was a wonderful person and an excellent colleague who contributed greatly to the implementation of the VLTI on Paranal. The Paranal Observatory dedicates this result to her memory". Note [1]: The VINCI instrument was built under ESO contract at the Observatoire de Paris (France) and the camera in this instrument was delivered by the MPI for Extraterrestrial Physics (Garching, Germany). The detector and the detector electronics was supplied by ESO. Scientific Appendix: First VLTI stellar measurements with two UTs ESO PR Photo 30e/01 ESO PR Photo 30e/01 [Preview - JPEG: 343 x 400 pix - 39k] [Normal - JPEG: 686 x 800 pix - 82k] Caption : PR Photo 30d/01 shows the "visibility curve" for the red giant star Psi Phoenicis as measured on two nights (16 data sets; three points to the right) with two VLT UTs (ANTU + MELIPAL) for three different positions in the sky and on four nights with the 40-cm test siderostats on a shorter 16-m baseline (8 data sets; one point to the left); see the text below. From the fitted curve, a preliminary value of the angular diameter is 8.21 ± 0.02 milli-arcsec (mas). This appendix presents some technical details of the measurements, obtained with the VLTI and two UTs during the first three test nights. While it must be emphasized that the stated results are still provisional, they clearly indicate the excellent performance of the VLTI already at this early stage and, not least, the great potential for important fundamental observations with this facility. Note in particular, that the quoted errors reflect the statistical uncertainty in the data only and that additional calibration errors must later be taken into account. The observational data were taken on a variety of astronomical objects, including three red dwarfs, three stars surrounded by disks, one red giant, two Cepheids and one luminous blue variable. All of these measurements were calibrated by observing a reference star of known angular size. Each data set required about ten minutes of continuous observations. Fringes were found on all pointed objects within a few minutes of time and kept for up to several hours. All data were deemed to be of high quality and will be analyzed in detail within the next weeks. A preliminary data reduction was possible for part of these objects and it gave the results listed below (all quoted values are uniform disk diameters): * For the blue dwarf Alpha Eridani , on which first fringes were found, 11 data sets were taken within three nights and an angular diameter of 1.92 ± 0.05 milli-arcsec (mas) could be estimated, which is precisely in line with previous measurements. * The nearby red dwarf HD 217987 was measured to have a diameter of 0.92 ± 0.05 mas, resulting from two data sets. This is the first measurement of the angular diameter of a star as small as a type M0 dwarf , and one of the very few available for cool main sequence stars in general. * The giant star HD 36167 was found from four data sets to have a diameter of 3.32 ± 0.02 mas. This measurement constitutes a significant refinement of the earlier, indirect estimate of 3.55 ± 0.06 mas (Cohen M. et al. 1999, Astronomical Journal 117, 1864). * For the three stars which are known to be surrounded by a disk, the following results were obtained: Epsilon Eridani 2.20 ± 0.02 mas (8 data sets in two nights); Fomalhaut (Alpha Piscis Austrini) 2.31 ± 0.02 mas (4 data sets); Beta Pictoris unresolved (4 data sets). Further analysis is expected to put a significant lower limit on the visibility for the latter star. * The two Cepheids Zeta Geminorum and Beta Doradus showed diameters of 1.78 ± 0.02 mas (7 data sets) and 2.00 ± 0.04 mas (6 data sets), respectively. The diameter of Zeta Geminorum has been measured before by three different interferometers. Its diameter is expected to vary between about 1.5 mas and 1.8 mas within ten days. On the date the VLTI data was taken, its phase was close to the foreseen maximum diameter. Beta Doradus has never been measured before. * The red giant Psi Phoenicis was measured on two nights (16 data sets) with the UTs for three different positions in the sky, hence with three different projected baselines. Some weeks earlier it had been measured on four nights with the 40-cm test siderostats (8 data sets) on a shorter 16-m baseline. The star was well resolved already in the previous measurements, but the addition of the data recently obtained with the UTs is of fundamental importance because with their longer baseline and larger light-gathering power, it now becomes possible to obtain visibility measurements beyond the first null, cf. PR Photo 30e/01 . Such measurements in the future will enable astronomers to measure fine details such as limb-darkening and deviations from spherical symmetry. The preliminary diameter value for this star is 8.21 ± 0.02 mas. * The enigmatic object Eta Carinae is a luminous blue variable, a supermassive star, which underwent a massive outburst in the 1840's. This outburst was responsible for the creation of the surrounding Homunculus Nebula . The central object is not well understood, but is likely to have a complex structure and therefore the first interferometric measurement with the VLTI is of great importance. Fringes with a low contrast (amplitude of about 20%) were detected, indicating that the central object is resolved on a scale of a few milliarcseconds. More observations will be obtained to further investigate this peculiar object.

RNA-Seq analysis of glycosylation related gene expression in STZ-induced diabetic rat kidney

USDA-ARS?s Scientific Manuscript database

The UT-A1 urea transporter is crucial to the kidney’s ability to generate the concentrated urine. Native UT-A1 from kidney inner medulla (IM) is a heavily glycosylated protein with two glycosylation forms of 97 and 117 kDa. In diabetes, protein abundance, particularly the 117 kD isoform, is si...

Multi-point observations of Ion Dispersions near the Exterior Cusp with Cluster

NASA Astrophysics Data System (ADS)

Escoubet, C.-Philippe; Grison, Benjamin; Berchem, Jean; Trattner, Kralheinz; Pitout, Frederic; Richard, Robert; Taylor, Matt; Soucek, Jan; Laakso, Harri; Masson, Arnaud; Dunlop, Malcolm; Dandouras, Iannis; Reme, Henri; Fazakerley, Andrew; Daly, Patrick

2014-05-01

The exterior cusp is the most external region of the polar magnetosphere in direct contact with the plasma and the magnetic field from the solar wind. Unlike the rest of the magnetopause surface, the exterior cusp is a singular region with small and turbulent magnetic field and where large entry of plasma from solar origin takes place. The main process that injects solar wind plasma into the polar cusp is now generally accepted to be magnetic reconnection. Depending on the IMF direction, this process will take place equatorward (for IMF southward), poleward (for IMF northward) or on the dusk or dawn sides (for IMF azimuthal) of the cusp. We report a Cluster crossing on 5 January 2002 near the exterior cusp on the southern dusk side. The IMF was mainly azimuthal (IMF-By around -5 nT), the solar wind speed lower than usual around 280 km/s and the density around 5 cm-3. The four Cluster spacecraft were still in the "magnetotail" configuration with two perfect tetrahedra of 2000 km around apogee and turning into an elongated configuration near the magnetopause. C4 was the first spacecraft to enter the cusp around 19:52:04 UT, followed by C2 at 19:52:35 UT, C1 at 19:54:24 UT and C3 at 20:13:15 UT. C4 and C1 observed two ion energy dispersions at 20:10 UT and 20:40 UT and C3 at 20:35 UT and 21:15 UT. Using the time of flight technique on the upgoing and downgoing ions in the dispersions, we obtain an altitude of the sources of these ions between 14 and 20 RE. Using Tsyganenko model, these sources are located on the dusk flank, past the terminator. In addition, before entering the cusp, the magnetopause crossing was characterized by a large shear in By and bipolar plasma flows, suggesting that reconnection was taking place near the exterior cusp. We will discuss the extent of the reconnection line along the flank of the magnetopause based on these observations.

Mare and foal survival and subsequent fertility of mares treated for uterine torsion.

PubMed

Spoormakers, T J P; Graat, E A M; ter Braake, F; Stout, T A E; Bergman, H J

2016-03-01

Previous surveys have reported that mare and foal survival after correction of uterine torsion (UT) varies from 60 to 84% and from 30 to 54%, respectively. Furthermore, resolution via a standing flank laparotomy (SFL) has been associated with better foal, but not mare, survival. To compare the success of SFL with other correction methods (e.g. midline or flank laparotomy under general anaesthesia; correction per vaginam). Retrospective analysis of clinical records. Data on correction technique, stage of gestation, degree of rotation, survival and subsequent fertility for 189 mares treated for UT at 3 equine referral hospitals in The Netherlands during 1987-2007 were analysed. Mean stage of gestation at diagnosis was 283 days (range 153-369 days), with the majority of UTs (77.5%) occurring before Day 320 of gestation. After correction of UT, 90.5% of mares and 82.3% of foals survived to hospital discharge, between 3 and 39 days later, and to foaling. Multivariable logistic regression indicated that correction method and stage of gestation at UT affected survival of foals and mares. For foals, survival was 88.7% after SFL compared with 35.0% after other methods (P = 0.001). When UT occurred at <320 days, 90.6% of foals survived, compared with 56.1% at ≥320 days (P = 0.007). For mare survival, an interaction between stage of gestation and correction method was detected (P = 0.02), with higher survival after SFL (97.1%) than other methods (50.0%) at <320 days of gestation (P<0.01). When UT occurred at ≥320 days, mare survival did not differ between techniques (76.0 vs. 68.8%; P = 0.6). Of 123 mares that were bred again, 93.5% became pregnant; fertility did not differ between mares treated by SFL (93.9%) and other techniques (87.5%; P = 0.9). Standing flank laparotomy is the surgical technique of choice for resolving uncomplicated equine UT (i.e. with no coexisting gastrointestinal lesions) except when the stage of gestation exceeds 320 days. © 2015 EVJ Ltd.

The emerging physiological roles of the SLC14A family of urea transporters

PubMed Central

Stewart, Gavin

2011-01-01

In mammals, urea is the main nitrogenous breakdown product of protein catabolism and is produced in the liver. In certain tissues, the movement of urea across cell membranes is specifically mediated by a group of proteins known as the SLC14A family of facilitative urea transporters. These proteins are derived from two distinct genes, UT-A (SLC14A2) and UT-B (SLC14A1). Facilitative urea transporters play an important role in two major physiological processes – urinary concentration and urea nitrogen salvaging. Although UT-A and UT-B transporters both have a similar basic structure and mediate the transport of urea in a facilitative manner, there are a number of significant differences between them. UT-A transporters are mainly found in the kidney, are highly specific for urea, have relatively lower transport rates and are highly regulated at both gene expression and cellular localization levels. In contrast, UT-B transporters are more widespread in their tissue location, transport both urea and water, have a relatively high transport rate, are inhibited by mercurial compounds and currently appear to be less acutely regulated. This review details the fundamental research that has so far been performed to investigate the function and physiological significance of these two types of urea transporters. PMID:21449978

Computer-generated scenes depicting the HST capture and EVA repair mission

NASA Image and Video Library

1993-11-12

Computer generated scenes depicting the Hubble Space Telescope capture and a sequence of planned events on the planned extravehicular activity (EVA). Scenes include the Remote Manipulator System (RMS) arm assisting two astronauts changing out the Wide Field/Planetary Camera (WF/PC) (48699); RMS arm assisting in the temporary mating of the orbiting telescope to the flight support system in Endeavour's cargo bay (48700); Endeavour's RMS arm assisting in the "capture" of the orbiting telescope (48701); Two astronauts changing out the telescope's coprocessor (48702); RMS arm assistign two astronauts replacing one of the telescope's electronic control units (48703); RMS assisting two astronauts replacing the fuse plugs on the telescope's Power Distribution Unit (PDU) (48704); The telescope's High Resolution Spectrograph (HRS) kit is depicted in this scene (48705); Two astronauts during the removal of the high speed photometer and the installation of the COSTAR instrument (48706); Two astronauts, standing on the RMS, during installation of one of the Magnetic Sensing System (MSS) (48707); High angle view of the orbiting Space Shuttle Endeavour with its cargo bay doors open, revealing the bay's pre-capture configuration. Seen are, from the left, the Solar Array Carrier, the ORU Carrier and the flight support system (48708); Two astronauts performing the replacement of HST's Rate Sensor Units (RSU) (48709); The RMS arm assisting two astronauts with the replacement of the telescope's solar array panels (48710); Two astronauts replacing the telescope's Solar Array Drive Electronics (SADE) (48711).

"First Light" Approaches for Fourth VLT Unit Telescope

NASA Astrophysics Data System (ADS)

2000-08-01

These days, the ESO staff at Paranal is having a strong feeling of "déja-vu". Only seven months after the third 8.2-m VLT Unit Telescope, MELIPAL , achieved "First Light", this crucial moment is now rapidly approaching for YEPUN , the fourth and last of the giants at the ESO observatory. Following successful coating with a thin layer of aluminium in early June 2000, the 8.2-m primary Zerodur mirror (M1) was placed in its supporting cell and safely attached to the mechanical structure of YEPUN on July 31. On August 26, the 1.1-m M2 Beryllium Mirror for YEPUN was coated. Again, this delicate operation went very well and the measured reflectivity was excellent, about 91%. The M2 mirror and its support were then assembled and successfully installed at the telescope on Sunday, August 27. Before the optical mirrors were installed, and with dummies in their place, careful tests were made of most telescope functions. In particular, this included accurate balancing of the 450-tonnes telescope frame on its hydrostatic oil bearings, as well as precise adjustment of all motions. It now remains for the ESO engineers to do the final performance optimization of the entire telescope. The work on the fourth telescope has been particularly noticeable because a large proportion of the assembly, integration, tuning and testing was organised and executed by ESOs young group of capable engineers and technicians. As the engineering staff at Paranal has grown and during the earlier work on the first three telescopes, they have been acquiring the necessary expertise to autonomously integrate and maintain the 8.2-m telescopes. During the coming "First Light" observations, light from the selected celestial objects will be registered by the VLT Test Camera at the Cassegrain Focus. This comparatively simple instrument was also used for the consecutive "First Light" events for ANTU ( May 1998 ), KUEYEN ( March 1999 ) and MELIPAL ( January 2000 ). It is mounted on the telescope's optical axis within the M1 Mirror Cell, just behind the main mirror. It is planned to make one or more of these first images available on the web soon thereafter. This is the caption to ESO PR Photos 21a-b/00 . They may be reproduced, if credit is given to the European Southern Observatory. Note, however, that since these photos were electronically recorded and were primarily obtained to document the ongoing activities at Paranal, they are not of full professional quality for photographic reproduction.

The Validity of the Baby and Infant Screen for Children with aUtIsm Traits: Part 1 (BISCUIT-- Part 1)

ERIC Educational Resources Information Center

Matson, Johnny L.; Wilkins, Jonathan; Fodstad, Jill C.

2011-01-01

A top priority in the field of autism spectrum disorders (ASD) is the development of precise early diagnostic tools that can be completed with minimal time and training. We report on the convergent and divergent validity of the Baby and Infant Screen for Children with aUtIsm Traits (BISCUIT), specifically the BISCUIT-Part 1. Previous research with…

SWIFT observations and flash ionization features in the spectrum of DLT17h/SN 2017ahn

NASA Astrophysics Data System (ADS)

Tartaglia, L.; Hosseinzadeh, G.; Sand, D.; Valenti, S.; Wyatt, S.; Arcavi, I.; Howell, D. A.; McCully, C.

2017-02-01

We report follow-up observations of the Type II DLT17h/SN 2017ahn (ATels #10058, #10059) in the UV domain with the SWIFT satellite (Gehrels et al. 2004). Three target of opportunity observations were obtained on 2017-02-08.6 ( 3.0 ks), 2017-02-09.2 ( 3.2 ks) and 2017-02-09.6 ( 3.2 ks). DLT17h was detected in the Swift UV/Optical Telescope (UVOT; Roming et al. 2005) data with the following apparent magnitudes: JD | Mag | Err | Filter 2457793.121 | 16.99 | 0.10 | V 2457793.131 | 16.65 | 0.06 | UVM2 2457793.146 | 16.49 | 0.07 | UVW1 2457793.148 | 16.43 | 0.06 | U 2457793.149 | 17.42 | 0.06 | B 2457793.151 | 16.62 | 0.08 | UVW2 2457793.722 | 15.84 | 0.06 | UVM2 2457793.750 | 15.64 | 0.06 | UVW1 2457793.751 | 15.76 | 0.06 | U 2457793.751 | 16.76 | 0.05 | B 2457793.753 | 15.78 | 0.07 | UVW2 2457793.754 | 16.58 | 0.07 | V 2457794.081 | 15.72 | 0.06 | U 2457794.082 | 16.64 | 0.06 | B 2457794.085 | 16.50 | 0.08 | V 2457794.112 | 15.77 | 0.08 | UVW1 2457794.115 | 15.78 | 0.08 | UVW2 2457794.120 | 15.72 | 0.07 | UVM2 We also report the presence of flash ionization features (H-alpha, H-beta, He I, He II, and N IV emission with electron-scattering profiles; see Gal-Yam et al. 2014, Nature, 509, 471) in spectra of DLT17h/SN 2017ahn taken on 2017 February 9 UT with the robotic FLOYDS instrument mounted on the Las Cumbres Observatory 2-meter telescope on Haleakala, Hawai'i.

PRELIMINARY ANALYSIS OF SOHO/STEREO OBSERVATIONS OF SUNGRAZING COMET ISON (C/2012 S1) AROUND PERIHELION

DOE Office of Scientific and Technical Information (OSTI.GOV)

Knight, Matthew M.; Battams, Karl, E-mail: knight@lowell.edu

2014-02-20

We present photometric and morphological analysis of the behavior of sungrazing comet C/2012 S1 ISON in Solar and Heliospheric Observatory (SOHO) and Solar TErrestrial RElations Observatory (STEREO) images around its perihelion on 2013 November 28.779 UT. ISON brightened gradually November 20-26 with a superimposed outburst on November 21.3-23.5. The slope of brightening changed about November 26.7 and was significantly steeper in SOHO's orange and clear filter images until November 27.9 when it began to flatten out, reaching a peak about November 28.1 (r {sub H} ≈ 17 R {sub ☉}), then fading before brightening again from November 28.6 (r {submore » H} ≈ 5 R {sub ☉}) until disappearing behind the occulting disk. ISON brightened continuously as it approached perihelion while visible in all other telescopes/filters. The central condensation disappeared about November 28.5 and the leading edge became progressively more elongated until perihelion. These photometric and morphological behaviors are reminiscent of the tens of meter-sized Kreutz comets regularly observed by SOHO and STEREO and strongly suggest that the nucleus of ISON was destroyed prior to perihelion. This is much too small to support published gas production rates and implies significant mass loss and/or disruption in the days and weeks leading up to perihelion. No central condensation was seen post-perihelion. The post-perihelion lightcurve was nearly identical in all telescopes/filters and fell slightly steeper than r{sub H}{sup −2}. This implies that the brightness was dominated by reflected solar continuum off of remnant dust in the coma/tail and that any remaining active nucleus was <10 m in radius.« less

EIT and SXT Observations of a Quiet Region Filament Ejection: First Eruption, Then Reconnection

NASA Technical Reports Server (NTRS)

Sterling, Alphonse C.; Moore, Ronald L.; Thompson, Barbara J.; Six, N. Frank (Technical Monitor)

2001-01-01

We observe a slow-onset quiet-region filament eruption with the EUV Imaging Telescope (EIT) on SOHO, and the Soft X-ray Telescope (SXT) on Yohkoh. This event occurred on 1999 April 18, and was likely the origin of a coronal mass ejection (CME) detected by SOHO at 08:30 UT on that day. In EIT, one-half of the filament shows two stages of evolution: Stage I is a slow, roughly constant upward movement at approx. 1 km per second lasting approximately 6.5 hours, and Stage 2 is a rapid upward eruption at approximately 16 kilometers per second occurring just before the filament disappears into interplanetary space. The other half of the filament shows little motion along the line-of-sight during the time of Stage 1, but erupts along with the rest of the filament during Stage 2. There is no obvious emission from the filament in SXT until Stage 2; at that time an arcade of EUV and soft X-ray loops forms first at the central location of the filament, and then expands outward along the length of the filament channel. A plot of EUV intensity versus time of the central portion of the filament (where the postflare loops initially form) shows a flat profile during Stage 1, and a rapid upturn after the start of Stage 2. This lightcurve is delayed from what would be expected if "tether-cutting" reconnection in the core of the erupting region were responsible for the initiation of the eruption. Rather, these observations suggest that a loss of stability of the magnetic field holding the filament initiates the eruption, with reconnection in the core region occurring only as a byproduct.

4-station ultra-rapid EOP experiment with e-VLBI technique and automated correlation/analysis

NASA Astrophysics Data System (ADS)

Kurihara, S.; Nozawa, K.; Haas, R.; Lovell, J.; McCallum, J.; Quick, J.; Hobiger, T.

2013-08-01

Since 2007, the Geospatial Information Authority of Japan (GSI) and the Onsala Space Observatory (OSO) have performed the ultra-rapid dUT1 experiments, which can provide us with near real-time dUT1 value. Its technical knowledge has already been adopted for the regular series of the Tsukuba-Wettzell intensive session. Now we tried some 4-station ultra-rapid EOP experiments in association with Hobart and HartRAO so that we can estimate not only dUT1 but also the two polar motion parameters. In this experiment a new analysis software c5++ developed by the National Institute of Information and Communications Technology (NICT) was used. We describe past developments and an overview of the experiment, and conclude with its results in this report.

Adaptive Optics Facility: control strategy and first on-sky results of the acquisition sequence

NASA Astrophysics Data System (ADS)

Madec, P.-Y.; Kolb, J.; Oberti, S.; Paufique, J.; La Penna, P.; Hackenberg, W.; Kuntschner, H.; Argomedo, J.; Kiekebusch, M.; Donaldson, R.; Suarez, M.; Arsenault, R.

2016-07-01

The Adaptive Optics Facility is an ESO project aiming at converting Yepun, one of the four 8m telescopes in Paranal, into an adaptive telescope. This is done by replacing the current conventional secondary mirror of Yepun by a Deformable Secondary Mirror (DSM) and attaching four Laser Guide Star (LGS) Units to its centerpiece. In the meantime, two Adaptive Optics (AO) modules have been developed incorporating each four LGS WaveFront Sensors (WFS) and one tip-tilt sensor used to control the DSM at 1 kHz frame rate. The four LGS Units and one AO module (GRAAL) have already been assembled on Yepun. Besides the technological challenge itself, one critical area of AOF is the AO control strategy and its link with the telescope control, including Active Optics used to shape M1. Another challenge is the request to minimize the overhead due to AOF during the acquisition phase of the observation. This paper presents the control strategy of the AOF. The current control of the telescope is first recalled, and then the way the AO control makes the link with the Active Optics is detailed. Lab results are used to illustrate the expected performance. Finally, the overall AOF acquisition sequence is presented as well as first results obtained on sky with GRAAL.

The triggering and subsequent development of a solar flare

NASA Technical Reports Server (NTRS)

Vorpahl, J. A.

1975-01-01

High temporal and spatial resolution solar X-ray pictures of a flare at 1827 UT on 5 September 1973 were taken with the S-056 telescope on the Apollo telescope mount. Photographs taken at 9 sec intervals allow detailed information to be obtained about the site of the energy release, as well as about the evolution of the flare itself. Observations suggest that the flare occurred in an entire arcade of loops rather than in any single loop. Sequential brightening of different X-ray features indicates that some excitation moved perpendicular to the magnetic field of the arcade at velocities of 180 to 280 km/sec. The most intense X-ray features were located in places where the magnetic field composing the arcade had a small radius of curvature with horizontal field gradients higher than the surroundings region and where the axis of the arcade changed direction. It was felt that the arcade geometry strongly influenced the propagation of the triggering disturbance, as well as the storage and site of the subsequent deposition of energy. A magnetosonic wave is suggested as the propagating mechanism triggering instabilities that may have existed in the preflare structure.

LCOGT Imaging Lab

NASA Astrophysics Data System (ADS)

Tufts, Joseph R.; Lobdill, Rich; Haldeman, Benjamin J.; Haynes, Rachel; Hawkins, Eric; Burleson, Ben; Jahng, David

2008-07-01

The Las Cumbres Observatory Global Telescope Network (LCOGT) is an ambitious project to build and operate, within 5 years, a worldwide robotic network of 50 0.4, 1, and 2 m telescopes sharing identical instrumentation and optimized for precision photometry of time-varying sources. The telescopes, instrumentation, and software are all developed in house with two 2 m telescopes already installed. The LCOGT Imaging Lab is responsible for assembly and characterization of the network's cameras and instrumentation. In addition to a fully equipped CNC machine shop, two electronics labs, and a future optics lab, the Imaging Lab is designed from the ground up to be a superb environment for bare detectors, precision filters, and assembled instruments. At the heart of the lab is an ISO class 5 cleanroom with full ionization. Surrounding this, the class 7 main lab houses equipment for detector characterization including QE and CTE, and equipment for measuring transmission and reflection of optics. Although the first science cameras installed, two TEC cooled e2v 42-40 deep depletion based units and two CryoTiger cooled Fairchild Imaging CCD486-BI based units, are from outside manufacturers, their 18 position filter wheels and the remainder of the network's science cameras, controllers, and instrumentation will be built in house. Currently being designed, the first generation LCOGT cameras for the network's 1 m telescopes use existing CCD486-BI devices and an in-house controller. Additionally, the controller uses digital signal processing to optimize readout noise vs. speed, and all instrumentation uses embedded microprocessors for communication over ethernet.

TEMTADS Adjunct Sensor Systems Hand-Held EMI Sensor for Cued UXO Discrimination (ESTCP MR-200807) and Man-Portable EMI Array for UXO Detection and Discrimination (ESTCP MR-200909)

DTIC Science & Technology

2012-04-05

C la ss ifi ca tio n TY PE D ep th (M ) A zi m ut h (D eg re es ) D ip (D eg re es ) 1 2 3...Naval Research Laboratory Washington, DC 20375-5320 NRL/MR/ 6110 --12-9401 TEMTADS Adjunct Sensor Systems Hand-held EMI Sensor for Cued UXO...NUMBER 5b. GRANT NUMBER 5c. PROGRAM ELEMENT NUMBER 5d. PROJECT NUMBER 5e. TASK NUMBER 5f. WORK UNIT NUMBER 2 . REPORT TYPE1. REPORT DATE (DD-MM-YYYY) 4

Thienoquinolins exert diuresis by strongly inhibiting UT-A urea transporters

PubMed Central

Ren, Huiwen; Wang, Yanhua; Xing, Yongning; Ran, Jianhua; Liu, Ming; Lei, Tianluo; Zhou, Hong; Li, Runtao; Sands, Jeff M.

2014-01-01

Urea transporters (UT) play an important role in the urine concentration mechanism by mediating intrarenal urea recycling, suggesting that UT inhibitors could have therapeutic use as a novel class of diuretic. Recently, we found a thienoquinolin UT inhibitor, PU-14, that exhibited diuretic activity. The purpose of this study was to identify more potent UT inhibitors that strongly inhibit UT-A isoforms in the inner medullary collecting duct (IMCD). Efficient thienoquinolin UT inhibitors were identified by structure-activity relationship analysis. Urea transport inhibition activity was assayed in perfused rat terminal IMCDs. Diuretic activity of the compound was determined in rats and mice using metabolic cages. The results show that the compound PU-48 exhibited potent UT-A inhibition activity. The inhibition was 69.5% with an IC50 of 0.32 μM. PU-48 significantly inhibited urea transport in perfused rat terminal IMCDs. PU-48 caused significant diuresis in UT-B null mice, which indicates that UT-A is the target of PU-48. The diuresis caused by PU-48 did not change blood Na+, K+, or Cl− levels or nonurea solute excretion in rats and mice. No toxicity was detected in cells or animals treated with PU-48. The results indicate that thienoquinolin UT inhibitors induce a diuresis by inhibiting UT-A in the IMCD. This suggests that they may have the potential to be developed as a novel class of diuretics with fewer side effects than classical diuretics. PMID:25298523

Thienoquinolins exert diuresis by strongly inhibiting UT-A urea transporters.

PubMed

Ren, Huiwen; Wang, Yanhua; Xing, Yongning; Ran, Jianhua; Liu, Ming; Lei, Tianluo; Zhou, Hong; Li, Runtao; Sands, Jeff M; Yang, Baoxue

2014-12-15

Urea transporters (UT) play an important role in the urine concentration mechanism by mediating intrarenal urea recycling, suggesting that UT inhibitors could have therapeutic use as a novel class of diuretic. Recently, we found a thienoquinolin UT inhibitor, PU-14, that exhibited diuretic activity. The purpose of this study was to identify more potent UT inhibitors that strongly inhibit UT-A isoforms in the inner medullary collecting duct (IMCD). Efficient thienoquinolin UT inhibitors were identified by structure-activity relationship analysis. Urea transport inhibition activity was assayed in perfused rat terminal IMCDs. Diuretic activity of the compound was determined in rats and mice using metabolic cages. The results show that the compound PU-48 exhibited potent UT-A inhibition activity. The inhibition was 69.5% with an IC50 of 0.32 μM. PU-48 significantly inhibited urea transport in perfused rat terminal IMCDs. PU-48 caused significant diuresis in UT-B null mice, which indicates that UT-A is the target of PU-48. The diuresis caused by PU-48 did not change blood Na(+), K(+), or Cl(-) levels or nonurea solute excretion in rats and mice. No toxicity was detected in cells or animals treated with PU-48. The results indicate that thienoquinolin UT inhibitors induce a diuresis by inhibiting UT-A in the IMCD. This suggests that they may have the potential to be developed as a novel class of diuretics with fewer side effects than classical diuretics. Copyright © 2014 the American Physiological Society.

EEJ and EIA variations during modeling substorms with different onset moments

NASA Astrophysics Data System (ADS)

Klimenko, V. V.; Klimenko, M. V.

2015-11-01

This paper presents the simulations of four modeling substorms with different moment of substorm onset at 00:00 UT, 06:00 UT, 12:00 UT, and 18:00 UT for spring equinoctial conditions in solar activity minimum. Such investigation provides opportunity to examine the longitudinal dependence of ionospheric response to geomagnetic substorms. Model runs were performed using modified Global Self-consistent Model of the Thermosphere, Ionosphere and Protonosphere (GSM TIP). We analyzed GSM TIP simulated global distributions of foF2, low latitude electric field and ionospheric currents at geomagnetic equator and their disturbances at different UT moments substorms. We considered in more detail the variations in equatorial ionization anomaly, equatorial electrojet and counter equatorial electrojet during substorms. It is shown that: (1) the effects in EIA, EEJ and CEJ strongly depend on the substorm onset moment; (2) disturbances in equatorial zonal current density during substorm has significant longitudinal dependence; (3) the observed controversy on the equatorial ionospheric electric field signature of substorms can depend on the substorm onset moments, i.e., on the longitudinal variability in parameters of the thermosphere-ionosphere system.

75 FR 62627 - Environmental Impact Statement; Davis County, UT

Federal Register 2010, 2011, 2012, 2013, 2014

2010-10-12

... County, UT AGENCY: Federal Highway Administration (FHWA), DOT. ACTION: Notice of Intent. SUMMARY: FWHA is... cooperation with the Utah Department of Transportation (UDOT), will prepare an EIS on a proposal to address... and need and are based on agency and public input. These alternatives include: (1) Taking no action...

Wind ripples in low density atmospheres

NASA Technical Reports Server (NTRS)

Miller, J. S.; Marshall, J. R.; Greeley, R.

1987-01-01

The effect of varying fluid density (rho) on particle transport was examined by conducting tests at atmospheric pressures between 1 and 0.004 bar in the Martian Surface Wind Tunnel (MARSWIT). This study specifically concerns the effect of varying rho on the character of wind ripples, and elicits information concerning generalized ripple models as well as specific geological circumstances for ripple formation such as those prevailing on Mars. Tests were conducted primarily with 95 micron quartz sand, and for each atmospheric pressure chosen, tests were conducted at two freestream wind speeds: 1.1 U*(t) and 1.5 U*(t), where U*(t) is saltation threshold. Preliminary analysis of the data suggests: (1) ballistic ripple wavelength is not at variance with model predictions; (2) an atmospheric pressure of approximately 0.2 bar could represent a discontinuity in ripple behavior; and (4) ripple formation on Mars may not be readily predicted by extrapolation of terrestrial observations.

GNSS Observations of Ionospheric Variations During the 21 August 2017 Solar Eclipse

NASA Astrophysics Data System (ADS)

Coster, Anthea J.; Goncharenko, Larisa; Zhang, Shun-Rong; Erickson, Philip J.; Rideout, William; Vierinen, Juha

2017-12-01

On 21 August 2017, during daytime hours, a total solar eclipse with a narrow ˜160 km wide umbral shadow occurred across the continental United States. Totality was observed from the Oregon coast at ˜9:15 local standard time (LST) (17:20 UT) to the South Carolina coast at ˜13:27 LST (18:47 UT). A dense network of Global Navigation Satellite Systems (GNSS) receivers was utilized to produce total electron content (TEC) and differential TEC. These data were analyzed for the latitudinal and longitudinal response of the TEC and for the presence of traveling ionospheric disturbances (TIDs) during eclipse passage. A significant TEC depletion, in some cases greater than 60%, was observed associated with the eclipse shadow, exceeding initial model predictions of 35%. Evidence of enhanced large-scale TID activity was detected over the United States prior to and following the large TEC depletion observed near the time of totality. Signatures of enhanced TEC structures were observed over the Rocky Mountain chain during the main period of TEC depletion.

MROI Array telescopes: the relocatable enclosure domes

NASA Astrophysics Data System (ADS)

Marchiori, G.; Busatta, A.; Payne, I.

2016-07-01

The MROI - Magdalena Ridge Interferometer is a project which comprises an array of up to 10 1.4m diameter mirror telescopes arranged in a "Y" configuration. Each of these telescopes will be housed inside a Unit Telescope Enclosure (UTE) which are relocatable onto any of 28 stations. EIE GROUP Srl, Venice - Italy, was awarded the contract for the design, the construction and the erection on site of the MROI by the New Mexico Institute of Mining and Technology. The close-pack array of the MROI - including all 10 telescopes, several of which are at a relative distance of less than 8m center to center from each other - necessitated an original design for the Unit Telescope Enclosure (UTE). This innovative design enclosure incorporates a unique dome/observing aperture system to be able to operate in the harsh environmental conditions encountered at an altitude of 10,460ft (3,188m). The main characteristics of this Relocatable Enclosure Dome are: a Light insulated Steel Structure with a dome made of composites materials (e.g. glass/carbon fibers, sandwich panels etc.), an aperture motorized system for observation, a series of louvers for ventilation, a series of electrical and plants installations and relevant auxiliary equipment. The first Enclosure Dome is now under construction and the completion of the mounting on site id envisaged by the end of 2016. The relocation system utilizes a modified reachstacker (a transporter used to handle freight containers) capable of maneuvering between and around the enclosures, capable of lifting the combined weight of the enclosure with the telescope (30tons), with minimal impacts due to vibrations.

Reactive Nitrogen Distribution and Partitioning in the North American Troposphere and Lowermost Stratosphere

NASA Technical Reports Server (NTRS)

Singh, H. B.; Salas, L.; Herlth, D.; Kolyer, R.; Czech, E.; Crawford, J. H.; Pierce, R. B.; Sachse, G. W.; Blake, D. R.; Cohen, R. C.;

Evaluation of biochemical markers combined with uterine artery Doppler parameters in fetuses with growth restriction: a case-control study.

PubMed

Zamarian, Ana Cristina Perez; Araujo Júnior, Edward; Daher, Sílvia; Rolo, Liliam Cristine; Moron, Antonio Fernandes; Nardozza, Luciano Marcondes Machado

2016-10-01

Assessing the biochemical markers levels and the uterine artery Doppler (UtA) parameters in fetuses with growth restriction (FGR). Prospective case-control study included 66 patients with diagnosis of FGR and 64 healthy pregnancies at 24-41 weeks of gestation. For both groups, maternal circulating concentrations of biochemical factors of soluble fms-like tyrosine kinase-1 (sFlt-1), soluble endoglin(sEng), adiponectin, A disintegrin and metalloproteinases (ADAM-12), pregnancy-associated plasma protein-A (PAPP-A), angiopoietin-2 (ANGI-2), vascular endothelial growth factor (VEGF) and transforming growth factor-β (TGF-β) were assayed by ELISA and UtA by Doppler were performed. ANOVA, Mann-Whitney tests and Pearson correlation coefficient were applied to compare the biochemical factors, UtA Doppler and EFW Z-score between the groups. Concentrations of sFlt-1, sEng, PAPP-A were significantly higher in FGR than controls (p < 0.0001, p = 0.02 and p = 0.03, respectively), but concentration of ANGI-2 (p < 0.0001) was significantly lower in FGR than controls and ADAM-12 levels had a tendency to be lower in the FGR, though not statistically significant (p = 0.059). Increased sEng concentrations were correlated with abnormal UtA Doppler in FGR. Fetal growth restriction fetuses showed increased serum levels of sFlt-1, sEng and PAPP-A with levels of ANGI-2 decreased and a positive association between elevated concentrations of sEng and changing impedance of UtA Doppler were observed.

TCS and peripheral robotization and upgrade on the ESO 1-meter telescope at La Silla Observatory

NASA Astrophysics Data System (ADS)

Ropert, S.; Suc, V.; Jordán, A.; Tala, M.; Liedtke, P.; Royo, S.

2016-07-01

In this work we describe the robotization and upgrade of the ESO 1m telescope located at La Silla Observatory. The ESO 1m telescope was the first telescope installed in La Silla, in 1966. It now hosts as a main instrument the FIber Dual EchellE Optical Spectrograph (FIDEOS), a high resolution spectrograph designed for precise Radial Velocity (RV) measurements on bright stars. In order to meet this project's requirements, the Telescope Control System (TCS) and some of its mechanical peripherals needed to be upgraded. The TCS was also upgraded into a modern and robust software running on a group of single board computers interacting together as a network with the CoolObs TCS developed by ObsTech. One of the particularities of the CoolObs TCS is that it allows to fuse the input signals of 2 encoders per axis in order to achieve high precision and resolution of the tracking with moderate cost encoders. One encoder is installed on axis at the telescope and the other on axis at the motor. The TCS was also integrated with the FIDEOS instrument system so that all the system can be controlled through the same remote user interface. Our modern TCS unit allows the user to run observations remotely through a secured internet web interface, minimizing the need of an on-site observer and opening a new age in robotic astronomy for the ESO 1m telescope.

VizieR Online Data Catalog: The Gemini Observation Log (CADC, 2001-)

NASA Astrophysics Data System (ADS)

Association of Universities For Research in Astronomy

2018-01-01

This database contains a log of the Gemini Telescope observations since 2001, managed by the Canadian Astronomical Data Center (CADC). The data are regularly updated (see the date of the last version at the end of this file). The Gemini Observatory consists of twin 8.1-meter diameter optical/infrared telescopes located on two of the best observing sites on the planet. From their locations on mountains in Hawai'i and Chile, Gemini Observatory's telescopes can collectively access the entire sky. Gemini is operated by a partnership of five countries including the United States, Canada, Brazil, Argentina and Chile. Any astronomer in these countries can apply for time on Gemini, which is allocated in proportion to each partner's financial stake. (1 data file).

Accouchements sur utérus cicatriciel en République Démocratique du Congo: épreuve utérine et facteurs déterminants de l’issue

PubMed Central

Momat, Félix Kitenge wa; Zalagile, Pierre Akilimali; Mukalenge, Faustin Chenge; Luboya, Oscar Numbi; Kalala, Cléophas Tshibangu; Mashinda, Désiré; Grangé, Gilles; Mukuku, Olivier; Kaj, Fanny Malonga; Lubamba, Chamy Cham; Bwama, Joseph Bagambe; Mukoko, Célestin Kayembe; Kakoma, Jean Baptiste; Kalungwe, Justin Kizonde

2017-01-01

Introduction L'objectif était d'identifier les principaux facteurs de risque associés à un échec d'épreuve utérine et définir un score prédictif d'accouchement sur utérus cicatriciel en République Démocratique du Congo. Méthodes Étude multicentrique, transversale et analytique des patientes porteuses d'un utérus cicatriciel sur la période du 1er janvier au 31 décembre 2013 dans quatre maternités de la République Démocratique du Congo (RDC). Un modèle de régression logistique a été construit pour identifier les facteurs associés à l'échec de l'épreuve utérine. De ce modèle, un score prédictif a été construit pour prédire l'échec de l'épreuve utérine dans les maternités de la RDC. La courbe ROC a été utilisée pour évaluer la capacité du score construit à identifier les patientes à risque de connaitre un échec de l'épreuve utérine. Le cut off point du score prédictif a été déterminé en fonction de la sensibilité et spécificité optimale via l'index de Youden. Tous les tests ont été réalisés au seuil de signification α=0,05. Résultats Deux types de facteurs explicatifs de l'échec de l'épreuve utérine ont été retenus. Il s'agit d'un facteur sociodémographique (âge maternel) et de trois facteurs obstétricaux (hauteur utérine, présentation du fœtus et rupture prématurée des membranes). Le score de prédiction a été défini pour prédire l'échec de l'épreuve utérine. La construction de ce score s'est basée sur quatre éléments : l'âge maternel, l'état de la poche des eaux à l'admission, la hauteur utérine et la présentation fœtale. Le score minimal est de 4 et le score maximal est de 16. Le seuil est de 7. Un Score total supérieur ou égal à 7 traduit un risque d'échec de l'épreuve utérine. Conclusion L'utilisation de ce score prédictif chez les patientes pourra améliorer la qualité dans les indications de la voie haute, l'augmentation des taux de césariennes prophylactiques ainsi que la meilleure sélection des patientes soumises à l'épreuve utérine. Ceci pourra également contribuer à la réduction de la morbi-mortalité fœto-maternelle liée à la gestion de l'accouchement sur utérus cicatriciels. PMID:28819492

Causes of high O3 in the lower free troposphere over the Pacific Northwest as observed at the Mt. Bachelor Observatory

NASA Astrophysics Data System (ADS)

Ambrose, J. L.; Reidmiller, D. R.; Jaffe, D. A.

2011-09-01

We measured O3, CO, Hg, sub-micron particle scattering of mid-visible light (σsp), and water vapor (WV) at the Mt. Bachelor Observatory (MBO) in central Oregon, USA since 2004. The data were used to identify sources of large ozone enhancements in the lower free troposphere (FT). A total of 25 high-ozone events, defined as time periods when the 8-h averaged O3 mixing ratio was >70.0 ppbv, were recorded. The events occurred between early March and late September. For 18 of the 25 event days we were able to identify sources based on (1) relative enhancements of O3, CO, Hg and WV compared with the corresponding monthly distributions and (2) supporting data from the Hybrid Single-Particle Lagrangian Integrated Trajectory (HYSPLIT) model, the Navy Aerosol Analysis and Prediction System (NAAPS) global aerosol model, and Moderate Resolution Imaging Spectroradiometer (MODIS) satellite-derived active fire counts from the Fire Information for Resource Management System (FIRMS). Our analysis suggests that enhanced O3 levels during all the identified events were transported to MBO in the FT and were driven mostly by subsidence of O3-rich air masses from the upper troposphere/lower stratosphere (UT/LS), Asian long range transport (ALRT) and mixed ALRT + UT/LS influences. The UT/LS events were depleted in CO and total atmospheric mercury (TAM) compared to monthly median values. Levels of O3 and CO tended to be anti-correlated during UT/LS events, consistent with transport from clean regions in the UT. Conversely, the ALRT events were characterized by concomitant enhancements in CO and TAM with mean values during each event that were >70th percentile values for the months during which the events occurred. Unlike for UT/LS events, levels of O3 and CO during ALRT events tended to be correlated, consistent with photochemical O3 production in polluted air masses transported across the Pacific. The mixed ALRT + UT/LS events exhibited characteristics that were intermediate between those of the ALRT and UT/LS events. For the classifiable cases the fractional distribution of each event type was: UT/LS, ˜44% (n = 8); ALRT + UT/LS, ˜33% (n = 6); ALRT, ˜22% (n = 4). In terms of the total number of classifiable high-ozone event hours UT/LS, ALRT + UT/LS and ALRT events accounted for ˜52% (t = 85), ˜36% (t = 59) and ˜13% (t = 21), respectively. The results indicate that downward mixing of O3-rich air masses from the UT/LS together with trans-Pacific transport of urban/industrial and biomass burning emissions from the Asian continent are the most important mechanisms for delivering high O3 levels (i.e., 8-h averages >70.0 ppbv) to the lower FT in the Pacific Northwest.

Absence of PKC-Alpha Attenuates Lithium-Induced Nephrogenic Diabetes Insipidus

PubMed Central

Sim, Jae H.; Himmel, Nathaniel J.; Redd, Sara K.; Pulous, Fadi E.; Rogers, Richard T.; Black, Lauren N.; Hong, Seongun M.; von Bergen, Tobias N.; Blount, Mitsi A.

2014-01-01

Lithium, an effective antipsychotic, induces nephrogenic diabetes insipidus (NDI) in ∼40% of patients. The decreased capacity to concentrate urine is likely due to lithium acutely disrupting the cAMP pathway and chronically reducing urea transporter (UT-A1) and water channel (AQP2) expression in the inner medulla. Targeting an alternative signaling pathway, such as PKC-mediated signaling, may be an effective method of treating lithium-induced polyuria. PKC-alpha null mice (PKCα KO) and strain-matched wild type (WT) controls were treated with lithium for 0, 3 or 5 days. WT mice had increased urine output and lowered urine osmolality after 3 and 5 days of treatment whereas PKCα KO mice had no change in urine output or concentration. Western blot analysis revealed that AQP2 expression in medullary tissues was lowered after 3 and 5 days in WT mice; however, AQP2 was unchanged in PKCα KO. Similar results were observed with UT-A1 expression. Animals were also treated with lithium for 6 weeks. Lithium-treated WT mice had 19-fold increased urine output whereas treated PKCα KO animals had a 4-fold increase in output. AQP2 and UT-A1 expression was lowered in 6 week lithium-treated WT animals whereas in treated PKCα KO mice, AQP2 was only reduced by 2-fold and UT-A1 expression was unaffected. Urinary sodium, potassium and calcium were elevated in lithium-fed WT but not in lithium-fed PKCα KO mice. Our data show that ablation of PKCα preserves AQP2 and UT-A1 protein expression and localization in lithium-induced NDI, and prevents the development of the severe polyuria associated with lithium therapy. PMID:25006961

Chronic use of chloroquine disrupts the urine concentration mechanism by lowering cAMP levels in the inner medulla

PubMed Central

von Bergen, Tobias N.

2012-01-01

Chloroquine, a widely used anti-malaria drug, has gained popularity for the treatment of rheumatoid arthritis, systemic lupus erythematosus (SLE), and human immunodeficiency virus (HIV). Unfortunately, chloroquine may also negatively impact renal function for patients whose fluid and electrolyte homeostasis is already compromised by diseases. Chronic administration of chloroquine also results in polyuria, which may be explained by suppression of the antidiuretic response of vasopressin. Several of the transporters responsible for concentrating urine are vasopressin-sensitive including the urea transporters UT-A1 and UT-A3, the water channel aquaporin-2 (AQP2), and the Na+-K+-2Cl− cotransporter (NKCC2). To examine the effect of chloroquine on these transporters, Sprague-Dawley rats received daily subcutaneous injections of 80 mg·kg−1·day−1 of chloroquine for 4 days. Twenty-four hour urine output was twofold higher, and urine osmolality was decreased by twofold in chloroquine-treated rats compared with controls. Urine analysis of treated rats detected the presence chloroquine as well as decreased urine urea and cAMP levels compared with control rats. Western blot analysis showed a downregulation of AQP2 and NKCC2 transporters; however, UT-A1 and UT-A3 abundances were unaffected by chloroquine treatment. Immunohistochemistry showed a marked reduction of UT-A1 and AQP2 in the apical membrane in inner medullary collecting ducts of chloroquine-treated rats. In conclusion, chloroquine-induced polyuria likely occurs as a result of lowered cAMP production. These findings suggest that chronic chloroquine treatment would exacerbate the already compromised fluid homeostasis observed in diseases like chronic kidney disease. PMID:22791344

Microstructure and properties of ultrafine grained structure of Cu-Zn-Si alloy fabricated by heavy cold rolling

NASA Astrophysics Data System (ADS)

Miura, H.; Kobayashi, T.; Kobayashi, M.

2014-08-01

Cu-18.2Zn-1.5Si-0.25Fe (mass%) alloy was heavily cold rolled. Ultrafine grained (UFGed) structure, containing a mixture of lamellar and mechanical twins, was easily and homogeneously formed. The average grain size was approximately 100 nm. The as-rolled sample showed quite high ultimate tensile strength (UTS) over 1 GPa. The UTS was higher than those obtained by multi directional forging. When the samples were annealed at relatively low temperatures between 553 K and 653 K, they showed slight hardening followed by large softening due to occurrence of static recrystallization (SRX). Annealing of UFGed structure at relatively low temperature of around 0.4 Tm caused extensive SRX that, in turn, induces ultrafine RXed grained structure. The grain size of the RXed sample was as fine as 200 nm. Although the annealing induced recovery of ductility while UTS gradually reduces, UTS over 1 GPa with ductility of 15 % were attained. The RXed grains mainly contained ultrafine annealing twins. Therefore, UFGed structure and superior mechanical properties could be achieved by a simple process of cold rolling, i.e., without severe plastic deformation.

Awa1p on the cell surface of sake yeast inhibits biofilm formation and the co-aggregation between sake yeasts and Lactobacillus plantarum ML11-11.

PubMed

Hirayama, Satoru; Shimizu, Masashi; Tsuchiya, Noriko; Furukawa, Soichi; Watanabe, Daisuke; Shimoi, Hitoshi; Takagi, Hiroshi; Ogihara, Hirokazu; Morinaga, Yasushi

2015-05-01

We examined mixed-species biofilm formation between Lactobacillus plantarum ML11-11 and both foaming and non-foaming mutant strains of Saccharomyces cerevisiae sake yeasts. Wild-type strains showed significantly lower levels of biofilm formation compared with the non-foaming mutants. Awa1p, a protein involved in foam formation during sake brewing, is a glycosylphosphatidylinositol (GPI)-anchored protein and is associated with the cell wall of sake yeasts. The AWA1 gene of the non-foaming mutant strain Kyokai no. 701 (K701) has lost the C-terminal sequence that includes the GPI anchor signal. Mixed-species biofilm formation and co-aggregation of wild-type strain Kyokai no. 7 (K7) were significantly lower than K701 UT-1 (K701 ura3/ura3 trp1/trp1), while the levels of strain K701 UT-1 carrying the AWA1 on a plasmid were comparable to those of K7. The levels of biofilm formation and co-aggregation of the strain K701 UT-1 harboring AWA1 with a deleted GPI anchor signal were similar to those of K701 UT-1. These results clearly demonstrate that Awa1p present on the surface of sake yeast strain K7 inhibits adhesion between yeast cells and L. plantarum ML11-11, consequently impeding mixed-species biofilm formation. Copyright © 2014 The Society for Biotechnology, Japan. Published by Elsevier B.V. All rights reserved.

Innovative enclosure dome/observing aperture system design for the MROI Array Telescopes

NASA Astrophysics Data System (ADS)

Busatta, A.; Marchiori, G.; Mian, S.; Payne, I.; Pozzobon, M.

2010-07-01

The close-pack array of the MROI necessitated an original design for the Unit Telescope Enclosure (UTE) at Magdalena Ridge Observatory. The Magdalena Ridge Observatory Interferometer (MROI) is a project which comprises an array of up to ten (10) 1.4m diameter mirror telescopes arranged in a "Y" configuration. Each of these telescopes will be housed inside a Unit Telescope Enclosure (UTE) which are relocatable onto any of 28 stations. The most compact configuration includes all ten telescopes, several of which are at a relative distance of less than 8m center to center from each other. Since the minimum angle of the field of regard is 30° with respect to the horizon, it is difficult to prevent optical blockage caused by adjacent UTEs in this compact array. This paper presents the design constraints inherent in meeting the requirement for the close-pack array. An innovative design enclosure was created which incorporates an unique dome/observing aperture system. The description of this system focuses on how the field of regard requirement led to an unique and highly innovative concept that had to be able to operate in the harsh environmental conditions encountered at an altitude of 10,460ft (3,188m). Finally, we describe the wide use of composites materials and structures (e.g. glass/carbon fibres, sandwich panels etc.) on the aperture system which represents the only way to guarantee adequate thermal and environmental protection, compactness, structural stability and limited power consumption due to reduced mass.

VizieR Online Data Catalog: The magnetic field of L1544. I. NIR data (Clemens+, 2016)

NASA Astrophysics Data System (ADS)

Clemens, D. P.; Tassis, K.; Goldsmith, P. F.

2017-04-01

NIR imaging polarimetric observations of L1544 were conducted on the UT nights of 2013 January 20, 2015 October 27 and 31, 2015 November 1 and 2, and 2016 January 27 and 31 using the Mimir instrument on the 1.83m Perkins Telescope, located outside Flagstaff, Arizona. Six pointing centers ("fields") were selected toward a Center direction (RAJ200=05:04:16.6, DEJ2000=+25:10:48), the four equatorial NSEW directions offset by 6 arcmin from the Center, and one field to the NW offset mostly diagonally by about 10.9 arcmin. In addition, the AllWISE (Cutri+ 2013, II/328) catalog entries for the field shown in Figure 1 were fetched, resulting in 3616 stars with a detection in at least the WISE W1 (3.6um) band or W2 (4.5um) band. These were positionally matched to the H-band catalog, yielding 1262 matches. The properties of the 450 H-band stars without WISE star matches and the WISE stars without H-band star matches were similar in being fainter than the subset of stars with H-to-WISE matches. The combined data set of 1712 stars is listed in Table 1. (1 data file).

MUSE field splitter unit: fan-shaped separator for 24 integral field units

NASA Astrophysics Data System (ADS)

Laurent, Florence; Renault, Edgard; Anwand, Heiko; Boudon, Didier; Caillier, Patrick; Kosmalski, Johan; Loupias, Magali; Nicklas, Harald; Seifert, Walter; Salaun, Yves; Xu, Wenli

2014-07-01

MUSE (Multi Unit Spectroscopic Explorer) is a second generation Very Large Telescope (VLT) integral field spectrograph developed for the European Southern Observatory (ESO). It combines a 1' x 1' field of view sampled at 0.2 arcsec for its Wide Field Mode (WFM) and a 7.5"x7.5" field of view for its Narrow Field Mode (NFM). Both modes will operate with the improved spatial resolution provided by GALACSI (Ground Atmospheric Layer Adaptive Optics for Spectroscopic Imaging), that will use the VLT deformable secondary mirror and 4 Laser Guide Stars (LGS) foreseen in 2015. MUSE operates in the visible wavelength range (0.465-0.93 μm). A consortium of seven institutes is currently commissioning MUSE in the Very Large Telescope for the Preliminary Acceptance in Chile, scheduled for September, 2014. MUSE is composed of several subsystems which are under the responsibility of each institute. The Fore Optics derotates and anamorphoses the image at the focal plane. A Splitting and Relay Optics feed the 24 identical Integral Field Units (IFU), that are mounted within a large monolithic instrument mechanical structure. Each IFU incorporates an image slicer, a fully refractive spectrograph with VPH-grating and a detector system connected to a global vacuum and cryogenic system. During 2012 and 2013, all MUSE subsystems were integrated, aligned and tested to the P.I. institute at Lyon. After successful PAE in September 2013, MUSE instrument was shipped to the Very Large Telescope in Chile where it was aligned and tested in ESO integration hall at Paranal. After, MUSE was directly transferred in monolithic way onto VLT telescope where the first light was achieved. This paper describes the MUSE main optical component: the Field Splitter Unit. It splits the VLT image into 24 subfields and provides the first separation of the beam for the 24 Integral Field Units. This talk depicts its manufacturing at Winlight Optics and its alignment into MUSE instrument. The success of the MUSE alignment is demonstrated by the excellent results obtained onto MUSE positioning, image quality and throughput onto the sky. MUSE commissioning at the VLT is planned for September, 2014.

Uterine disease and its effect on subsequent reproductive performance of dairy cattle: a comparison of two cow-side diagnostic methods.

PubMed

Šavc, Miha; Duane, Mary; O'Grady, Luke E; Somers, Joris R; Beltman, Marijke E

2016-11-01

The aim of this study was to compare vaginal mucus scoring and ultrasonographic assessment of uterine content as predictors of future reproductive performance of dairy cows. Holstein-Friesian cows (n = 493) from seven commercial dairy farms were enrolled in this study. All cows received one prebreeding examination (PBE) between 21 and 38 days after parturition. During the PBE, vaginal mucus was scored (MS) and the transrectal ultrasonographic examination of the uterus to assess content (UTS) took place. The MS was scored on a scale of 0 to 3 using a Metricheck device and appearance of the uterus on transrectal ultrasound was scored on a scale of 0 to 4 based on the presence and consistency of intraluminal fluid. Other data collected from each cow included the farm ID (F_ID), conception rate to first service, length of breeding window, lactation number, calving month, body condition score (BCS) at calving, BCS loss after calving, BCS at PBE, days in milk at PBE, 305 day milk yield, economic breeding index (EBI), EBI fertility subindex and EBI health subindex. For each cow these parameters were analyzed using univariate Cox proportional hazard model to evaluate the effect of variables on the reproductive performance, measured as positive pregnancy status (PS) at the end of the breeding season. Receiver-operating characteristic analysis of the diagnostic tests compared with each other took place as well. Cows with positive UTS were 7.75 times more likely to have a positive MS as well (P < 0.01). The PS hazard ratios for cows with UTS0, 1, 2, 3, and 4 were 1; 0.84; 0.53; 0.78; 0.28, respectively (P < 0.001). For the cows with MS0, 1, 2, and 3, the PR hazard ratios were 1; 1.02; 0.51; 0.75; respectively (P = 0.01). Conception rate to first service, breeding window, and PS were significantly better for the cows with UTS0, 1 and 2 compared with the cows with UTS3-4 and MS2+3 (68%; 18%, [P = 0.020]; 29; 75 days, [P = 0.001]; 95%; 55%; [P = 0.010], respectively). There was a significant effect of days in milk at PBE in relation to the subsequent PS (P = 0.04). Cows in lactation number 5 or more were less likely (r = 0.69) to get in calf before the end of the breeding season than cows in their first lactation. Cows that calved later in the season were less likely to become pregnant before the end of the breeding season (P < 0.03). Younger cows (lactation <5) and cows with MS and UTS scores of 0 and -1 had significantly better reproductive performance (P < 0.04). Receiver-operating characteristic analysis showed that MS did not always reflect UTS, but cows with positive UTS were 7.75 times more likely to have a positive MS (P < 0.01) and a high UTS had a larger negative effect on time to PS than a high MS (P < 0.05). In conclusion, both prebreeding vaginal mucus evaluation with the Metricheck device and an ultrasound scan of the uterus serve as a good predictor of the subsequent PS. There is overlap between the two systems, but the best predictor for future reproductive outcome of the cow is a combination of both. Copyright © 2016 Elsevier Inc. All rights reserved.

Expression of urea transporters and their regulation.

PubMed

Klein, Janet D

2014-01-01

UT-A and UT-B families of urea transporters consist of multiple isoforms that are subject to regulation of both acutely and by long-term measures. This chapter provides a brief overview of the expression of the urea transporter forms and their locations in the kidney. Rapid regulation of UT-A1 results from the combination of phosphorylation and membrane accumulation. Phosphorylation of UT-A1 has been linked to vasopressin and hyperosmolality, although through different kinases. Other acute influences on urea transporter activity are ubiquitination and glycosylation, both of which influence the membrane association of the urea transporter, again through different mechanisms. Long-term regulation of urea transport is most closely associated with the environment that the kidney experiences. Low-protein diets may influence the amount of urea transporter available. Conditions of osmotic diuresis, where urea concentrations are low, will prompt an increase in urea transporter abundance. Although adrenal steroids affect urea transporter abundance, conflicting reports make conclusions tenuous. Urea transporters are upregulated when P2Y2 purinergic receptors are decreased, suggesting a role for these receptors in UT regulation. Hypercalcemia and hypokalemia both cause urine concentration deficiencies. Urea transporter abundances are reduced in aging animals and animals with angiotensin-converting enzyme deficiencies. This chapter will provide information about both rapid and long-term regulation of urea transporters and provide an introduction into the literature.

Hypovolemic intolerance to lower body negative pressure in female runners.

PubMed

Morikawa, T; Sagawa, S; Torii, R; Endo, Y; Yamazaki, F; Shiraki, K

2001-12-01

An attenuated baroreflex response and orthostatic intolerance have been reported in endurance-trained male athletes; however, it is still unknown whether this occurs also in females. The purpose of the present study was to examine whether endurance exercise-trained women had a predisposition to orthostatic compromise, and if so, what causative factor(s) may induce orthostatic intolerance. We studied cardiovascular and hormonal responses to graded lower body negative pressure (LBNP) (0 to -60 mm Hg) in 26 middle-distance female runners (18.6 +/- 0.1 yr) as the exercise-trained (ET) subjects and 23 age-matched untrained (UT) control subjects. On the basis of the occurrence of syncope episodes during LBNP, ET and UT subjects were further allocated to two groups; ET with presyncope (ET+syncope) and without presyncope (ET-syncope) and UT with presyncope (UT+syncope) and without presyncope (UT-syncope). Occurrence of presyncope episodes during LBNP was higher in ET (65.4%, P < 0.05) than that for UT (34.8%). Leg compliance was higher (P < 0.05) in ET than in UT. LBNP reduced stroke volume (SV) more (P < 0.05), increased heart rate (HR) higher (P < 0.05), and increased forearm vascular resistance (FVR) more in ET+syncope as compared with the other groups. Response of vasoactive hormones to LBNP was higher in ET+syncope (P < 0.05) than that of the other groups except for norepinephrine (NE); high in both ET+syncope and UT+syncope. The relationship between SV and NE, an index of sympathetic neuronal response, had no training-related changes during LBNP. We conclude that exercise-trained females have a high incidence of orthostatic intolerance during LBNP, with a greater reduction of SV independent of changes in baroreflex and neurohumoral function. A lower incidence of LBNP intolerance in UT may be accounted for by a lower reduction of SV during LBNP. An increase in leg compliance in the exercise-trained females may play an important role in inducing pronounced reduction of SV and hence the intolerance to LBNP.

Observations of the eclipsing binary b Persei

NASA Astrophysics Data System (ADS)

Templeton, Matthew R.

2015-01-01

Dr. Robert Zavala (USNO-Flagstaff) et al. request V time-series observations of the bright variable star b Persei 7-21 January 2015 UT, in hopes of catching a predicted eclipse on January 15. This is a follow-up to the February 2013 campaign announced in Alert Notice 476, and will be used as a photometric comparison for upcoming interferometric observations with the Navy Precision Optical Interferometer (NPOI) in Arizona. b Per (V=4.598, B-V=0.054) is ideal for photoelectric photometers or DSLR cameras. Telescopic CCD observers may observe by stopping down larger apertures. Comparison and check stars assigned by PI: Comp: SAO 24412, V=4.285, B-V = -0.013; Check: SAO 24512, V=5.19, B-V = -0.05. From the PI: "[W]e wanted to try and involve AAVSO observers in a follow up to our successful detection of the b Persei eclipse of Feb 2013, AAVSO Alert Notice 476 and Special Notice 333. Our goal now is to get good time resolution photometry as the third star passes in front of the close ellipsoidal binary. The potential for multiple eclipses exists. The close binary has a 1.5 day orbital period, and the eclipsing C component requires about 4 days to pass across the close binary pair. The primary eclipse depth is 0.15 magnitude. Photometry to 0.02 or 0.03 mags would be fine to detect this eclipse. Eclipse prediction date (JD 2457033.79 = 2015 01 11 UT, ~+/- 1 day) is based on one orbital period from the 2013 eclipse." More information is available at PI's b Persei eclipse web page: http://inside.warren-wilson.edu/~dcollins/bPersei/. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Observations should be submitted to the AAVSO International Database. See full Alert Notice for more details and information on the targets.

78 FR 45848 - Amendment of Class E Airspace; Salt Lake City, UT

Federal Register 2010, 2011, 2012, 2013, 2014

2013-07-30

... Salt Lake City, UT, to accommodate aircraft using Area Navigation (RNAV) Global Positioning System (GPS) and Instrument Landing System (ILS) or Localizer (LOC) standard instrument approach procedures at Salt..., and makes a minor change to the legal description of Class E airspace extending upward from 1,200 feet...

Use of anaerobic hydrolysis pretreatment to enhance ultrasonic disintegration of excess sludge.

PubMed

Li, Xianjin; Zhu, Tong; Shen, Yang; Chai, Tianyu; Xie, Yuanhua; You, Meiyan; Wang, Youzhao

2016-01-01

To improve the excess sludge disintegration efficiency, reduce the sludge disintegration cost, and increase sludge biodegradability, a combined pretreatment of anaerobic hydrolysis (AH) and ultrasonic treatment (UT) was proposed for excess sludge. Results showed that AH had an advantage in dissolving flocs, modifying sludge characteristics, and reducing the difficulty of sludge disintegration, whereas UT was advantageous in damaging cell walls, releasing intracellular substances, and decomposing macromolecular material. The combined AH-UT process was an efficient method for excess sludge pretreatment. The optimized solution involved AH for 3 days, followed by UT for 10 min. After treatment, chemical oxygen demand, protein, and peptidoglycan concentrations reached 3,949.5 mg O2/L, 752.5 mg/L and 619.1 mg/L, respectively. This work has great significance for further engineering applications, namely, reducing energy consumption, increasing the sludge disintegration rate, and improving the biochemical properties of sludge.

Pre-heated dual-cured resin cements: analysis of the degree of conversion and ultimate tensile strength.

PubMed

França, Flávio Álvares; Oliveira, Michele de; Rodrigues, José Augusto; Arrais, César Augusto Galvão

2011-01-01

This study evaluated the degree of conversion (DC) and ultimate tensile strength (UTS) of dual-cured resin cements heated to 50º C prior to and during polymerization. Disc- and hourglass-shaped specimens of Rely X ARC (RX) and Variolink II (VII) were obtained using addition silicon molds. The products were manipulated at 25º C or 50º C and were subjected to 3 curing conditions: light-activation through a glass slide or through a pre-cured 2-mm thick resin composite disc, or they were allowed to self-cure (SC). All specimens were dark-stored dry for 15 days. For DC analysis, the resin cements were placed into the mold located on the center of a horizontal diamond on the attenuated total reflectance element in the optical bench of a Fourier Transformed Infrared spectrometer. Infrared spectra (n = 6) were collected between 1680 and 1500 cm-1, and DC was calculated by standard methods using changes in ratios of aliphatic-to-aromatic C=C absorption peaks from uncured and cured states. For UTS test, specimens (n = 10) were tested in tension in a universal testing machine (crosshead speed of 1 mm/min) until failure. DC and UTS data were submitted to 2-way ANOVA, followed by Tukey's test (α= 5%). Both products showed higher DC at 50º C than at 25º C in all curing conditions. No significant difference in UTS was noted between most light-activated groups at 25º C and those at 50º C. VII SC groups showed higher UTS at 50º C than at 25º C (p < 0.05). Increased temperature led to higher DC, but its effects on resin cement UTS depended on the curing condition.

Poland and the United States: Achieving American National Interests in Eastern Europe in the 1990s

DTIC Science & Technology

1990-09-01

RESTRIC-IVE VIARK %NGS UNCLASSIFIED ___________________ 2a SECURITY CLASSIFICATION AUTHORITY 3 DiS7RI8UT1ON, AVALAB; L ,7Y OF RE.POR’ 2b...DECLASSIFCA71ONiDOWNGRADtNG SCHEDULE Approved for public release; dis - tribution is unlimited 4 PERFORMING ORGANIZATION REPORT NUMBER(S) S MONITORING ORGAN:ZATIO0...3b TIME COVERED ~ DA’E OF REPORT (Year, Montt., D3a ) 5PC C JIidster’s Thesis FROM --- __ - 0__T 199, ’ - L =’I’ 12 3 16 SUPPLEMENT7ARY NOTATION The

KSC-08pd2124

NASA Image and Video Library

2008-07-24

CAPE CANAVERAL, Fla. – In Orbiter Processing Facility 1 at NASA's Kennedy Space Center, a worker from United Space Alliance supervises the closure of the payload bay doors on space shuttle Atlantis. The payload bay has been thoroughly cleaned and is ready to receive the carriers transporting the instruments and equipment needed to service the Hubble Space Telescope. Atlantis is targeted to launch Oct. 8 on the STS-125 mission to service Hubble. The mission crew will perform history-making, on-orbit “surgery” on two important science instruments aboard the telescope. After capturing the telescope, two teams of spacewalking astronauts will perform the repairs during five planned spacewalks. Photo credit: NASA/Jack Pfaller

KSC-08pd2121

NASA Image and Video Library

2008-07-24

CAPE CANAVERAL, Fla. – In Orbiter Processing Facility 1 at NASA's Kennedy Space Center, a worker from United Space Alliance prepares to close the payload bay doors on space shuttle Atlantis. The payload bay has been thoroughly cleaned and is ready to receive the carriers transporting the instruments and equipment needed to service the Hubble Space Telescope. Atlantis is targeted to launch Oct. 8 on the STS-125 mission to service Hubble. The mission crew will perform history-making, on-orbit “surgery” on two important science instruments aboard the telescope. After capturing the telescope, two teams of spacewalking astronauts will perform the repairs during five planned spacewalks. Photo credit: NASA/Jack Pfaller

VizieR Online Data Catalog: Variables in Centaurus field F170 (Pietrukowicz+, 2012)

NASA Astrophysics Data System (ADS)

Pietrukowicz, P.; Minniti, D.; Alonso-Garcia; J.; Hempel, M.

2011-10-01

VJHKs photometry of stars in two VIMOS disc fields: F167 and F170. Data table with 333 variables detected in the field F170 in Centaurus. The optical observations were taken with the 8.2-m Unit Telescope 3 + VIMOS imager with a scale of 0.205"/pix at ESO Very Large Telescope at Paranal Observatory. Date of the observations: Apr 11-12, 2005. The infrared observations were obtained with the 4.1-m VISTA telescope + VIRCAM with a scale of 0.34"/pix also at Paranal Observatory. Date of the observations: Mar-Apr 2010. (4 data files).

Construction of a self-cloning system in the unicellular green alga Pseudochoricystis ellipsoidea.

PubMed

Kasai, Yuki; Oshima, Kohei; Ikeda, Fukiko; Abe, Jun; Yoshimitsu, Yuya; Harayama, Shigeaki

2015-01-01

Microalgae have received considerable interest as a source of biofuel production. The unicellular green alga Pseudochoricystis ellipsoidea (non-validated scientific name) strain Obi appears to be suitable for large-scale cultivation in outdoor open ponds for biodiesel production because it accumulates lipids to more than 30 % of dry cell weight under nitrogen-depleted conditions. It also grows rapidly under acidic conditions at which most protozoan grazers of microalgae may not be tolerant. The lipid productivity of this alga could be improved using genetic engineering techniques; however, genetically modified organisms are the subject of regulation by specific laws. Therefore, the aim of this study was to develop a self-cloning-based positive selection system for the breeding of P. ellipsoidea. In this study, uracil auxotrophic mutants were isolated after the mutagenesis of P. ellipsoidea using either ultraviolet light or a transcription activator-like effector nuclease (TALEN) system. The cDNA of the uridine monophosphate synthase gene (PeUMPS) of P. ellipsoidea was cloned downstream of the promoter of either a beta-tubulin gene (PeTUBULIN1) or the gene for the small subunit of ribulose 1,5-bisphosphate carboxylase/oxygenase (PeRBCS) to construct the pUT1 or pUT2 plasmid, respectively. These constructs were introduced into uracil auxotroph strains, and genetically complementary transformants were isolated successfully on minimal agar plates. Use of Noble agar as the solidifying agent was essential to avoid the development of false-positive colonies. It took more than 6 weeks for the formation of colonies of pUT1 transformants, whereas pUT2 transformants formed colonies in 2 weeks. Real-time PCR revealed that there were more PeUMPS transcripts in pUT2 transformants than in pUT1 transformants. Uracil synthesis (Ura(+)) transformants were also obtained using a gene cassette consisting solely of PeUMPS flanked by the PeRBCS promoter and terminator. A self-cloning-based positive selection system for the genetic transformation of P. ellipsoidea was developed. Self-cloned P. ellipsoidea strains will require less-stringent containment measures for large-scale outdoor cultivation.

THE VOLATILE COMPOSITION OF COMET C/2003 K4 (LINEAR) AT NEAR-IR WAVELENGTHS—COMPARISONS WITH RESULTS FROM THE NANÇAY RADIO TELESCOPE AND FROM THE ODIN, SPITZER, AND SOHO SPACE OBSERVATORIES

DOE Office of Scientific and Technical Information (OSTI.GOV)

Paganini, L.; Mumma, M. J.; Villanueva, G. L.

2015-07-20

We observed comet C/2003 K4 (LINEAR) using NIRSPEC at the Keck Observatory on UT 2004 November 28, when the comet was at 1.28 AU from the Sun (post-perihelion) and 1.38 AU from Earth. We detected six gaseous species (H{sub 2}O, OH*, C{sub 2}H{sub 6}, CH{sub 3}OH, CH{sub 4}, and HCN) and obtained upper limits for three others (H{sub 2}CO, C{sub 2}H{sub 2}, and NH{sub 3}). Our results indicate a water production rate of (1.72 ± 0.18) × 10{sup 29} molecules s{sup −1}, in reasonable agreement with production rates from SOHO (on the same day), Odin (one day earlier), and Nançaymore » (about two weeks earlier). We also report abundances (relative to water) for seven trace species: CH{sub 3}OH (∼1.8%), CH{sub 4} (∼0.9%), and C{sub 2}H{sub 6} (∼0.4%) that were consistent with mean values among Oort cloud (OC) comets, while NH{sub 3} (<0.55%), HCN (∼0.07%), H{sub 2}CO (<0.07%), and C{sub 2}H{sub 2} (<0.04%) were “lower” than the mean values in other OC comets. We extracted inner-coma rotational temperatures for four species (H{sub 2}O, C{sub 2}H{sub 6}, CH{sub 3}OH, and CH{sub 4}), all of which are consistent with 70 K (within 1σ). The extracted ortho-para ratio for water was 3.0 ± 0.15, corresponding to spin temperatures larger than 39 K (at the 1σ level) and agreeing with those obtained with the Spitzer Space Telescope at the 2σ level.« less

Distinct sources of particles near the cusp and the dusk flank of the magnetosphere

NASA Astrophysics Data System (ADS)

Escoubet, C. P.; Grison, B.; Berchem, J.; Trattner, K. J.; Lavraud, B.; Pitout, F.; Soucek, J.; Richard, R. L.; Laakso, H. E.; Masson, A.; Dunlop, M.; Dandouras, I. S.; Rème, H.; Fazakerley, A. N.; Daly, P. W.

2015-12-01

At the magnetopause, the location of the magnetic reconnection sites depends on the orientation of the interplanetary magnetic field (IMF) in the solar wind: on the dayside magnetosphere for an IMF southward, on the lobes for an IMF northward and on the flanks for an IMF in the East-West direction. Since most of observations of reconnection events have sampled a limited region of space simultaneously it is still not yet know if the reconnection line is extended over large regions of the magnetosphere or if is patchy and made of many reconnection lines. We report a Cluster crossing on 5 January 2002 near the exterior cusp on the southern dusk side where we observe multiple sources of reconnection/injections. The IMF was mainly azimuthal (IMF-By around -5 nT), the solar wind speed lower than usual around 280 km/s with the density of order 5 cm-3. The four Cluster spacecraft had an elongated configuration near the magnetopause. C4 was the first spacecraft to enter the cusp around 19:52:04 UT, followed by C2 at 19:52:35 UT, C1 at 19:54:24 UT and C3 at 20:13:15 UT. C4 and C1 observed two ion energy dispersions at 20:10 UT and 20:40 UT and C3 at 20:35 UT and 21:15 UT. Using the time of flight technique on the upgoing and downgoing ions, which leads to energy dispersions, we obtain distances of the ion sources between 14 and 20 RE from the spacecraft. The slope of the ion energy dispersions confirmed these distances. Using Tsyganenko model, we find that these sources are located on the dusk flank, past the terminator. The first injection by C3 is seen at approximately the same time as the 2nd injection on C1 but their sources at the magnetopause were separated by more than 7 RE. This would imply that two distinct sources were active at the same time on the dusk flank of the magnetosphere. In addition, a flow reversal was observed at the magnetopause on C4 which would be an indication that reconnection is also taking place near the exterior cusp quasi-simultaneously. A three-dimensional global magnetohydrodynamic (MHD) simulation will be used to determine the global topology of the magnetic field during the event.

Localization and regulation of a facilitative urea transporter in the kidney of the red-eared slider turtle (Trachemys scripta elegans).

PubMed

Uchiyama, Minoru; Kikuchi, Ryosuke; Konno, Norifumi; Wakasugi, Tatsuya; Matsuda, Kouhei

2009-01-01

Urea is the major excretory end product of nitrogen metabolism in most chelonian reptiles. In the present study, we report the isolation of a 1632 base pair cDNA from turtle kidney with one open reading frame putatively encoding a 403-residue protein, the turtle urea transporter (turtle UT). The first cloned reptilian UT has high homology with UTs (facilitated urea transporters) cloned from vertebrates, and most closely resembles the UT-A subfamily. Injection of turtle UT cRNA into Xenopus oocytes induced a 6-fold increase in [(14)C]urea uptake that was inhibited by phloretin. The turtle UT mRNA expression and tissue distribution were examined by RT-PCR with total RNA from various tissues. Expression of turtle UT mRNA was restricted to the kidney, and no signal was detected in the other tissues, such as brain, heart, alimentary tract and urinary bladder. An approximately 58 kDa protein band was detected in membrane fractions of the kidney by western blot using an affinity-purified antibody that recognized turtle UT expressed in Xenopus oocytes. In an immunohistochemical study using the anti-turtle UT antibody, UT-immunopositive cells were observed along the distal tubule but not in the collecting duct. In turtles under dry conditions, plasma osmolality and urea concentration increased, and using semi-quantitative RT-PCR the UT mRNA expression level in the kidney was found to increase 2-fold compared with control. The present results, taken together, suggest that the turtle UT probably contributes to urea transport in the distal tubule segments of the kidney in response to hyperosmotic stress under dry conditions.

Effects of augmented trunk stabilization with external compression support on shoulder and scapular muscle activity and maximum strength during isometric shoulder abduction.

PubMed

Jang, Hyun-jeong; Kim, Suhn-yeop; Oh, Duck-won

2015-04-01

The aim of the present study was to investigate the effects of augmented trunk stabilization with external compression support (ECS) on the electromyography (EMG) activity of shoulder and scapular muscles and shoulder abductor strength during isometric shoulder abduction. Twenty-six women volunteered for the study. Surface EMG was used to monitor the activity of the upper trapezius (UT), lower trapezius (LT), serratus anterior (SA), and middle deltoid (MD), and shoulder abductor strength was measured using a dynamometer during three experimental conditions: (1) no external support (condition-1), (2) pelvic support (condition-2), and (3) pelvic and thoracic supports (condition-3) in an active therapeutic movement device. EMG activities were significantly lower for UT and higher for MD during condition 3 than during condition 1 (p < 0.05). The MD/UT ratio was significantly higher during condition 3 than during conditions 1 and 2, and higher during condition 2 than during condition 1 (p < 0.05). Shoulder abductor strength was significantly higher during condition 3 than during condition 1 (p < 0.05). These findings suggest that augmented trunk stabilization with the ECS may be advantageous with regard to reducing the compensatory muscle effort of the UT during isometric shoulder abduction and increasing shoulder abductor strength. Copyright © 2014 Elsevier Ltd. All rights reserved.

An Overview of Integration and Test of the James Webb Space Telescope Integrated Science Instrument Module

NASA Technical Reports Server (NTRS)

Drury, Michael; Becker, Neil; Bos, Brent; Davila, Pamela; Frey, Bradley; Hylan, Jason; Marsh, James; McGuffey, Douglas; Novak, Maria; Ohl, Raymond;

Astrometric confirmation of young low-mass binaries and multiple systems in the Chamaeleon star-forming regions

NASA Astrophysics Data System (ADS)

Vogt, N.; Schmidt, T. O. B.; Neuhäuser, R.; Bedalov, A.; Roell, T.; Seifahrt, A.; Mugrauer, M.

2012-10-01

Context. The star-forming regions in Chamaeleon (Cha) are one of the nearest (distance ~ 165 pc) and youngest (age ~ 2 Myr) conglomerates of recently formed stars and the ideal target for population studies of star formation. Aims: We investigate a total of 16 Cha targets that have been suggested, but not confirmed, to be binaries or multiple systems in previous literature. Methods: We used the adaptive optics instrument Naos-Conica (NACO) at the Very Large Telescope Unit Telescope (UT) 4 / YEPUN of the Paranal Observatory, at 2-5 different epochs, in order to obtain relative and absolute astrometric measurements, as well as differential photometry in the J, H, and K band. On the basis of known proper motions and these observations, we analyse the astrometric results in our proper motion diagram (PMD: angular separation / position angle versus time), to eliminate possible (non-moving) background stars, establish co-moving binaries and multiples, and search for curvature as indications for orbital motion. Results: All previously suggested close components are co-moving and no background stars are found. The angular separations range between 0.07 and 9 arcsec, corresponding to projected distances between the components of 6-845 AU. Thirteen stars are at least binaries and the remaining three (RX J0919.4-7738, RX J0952.7-7933, VW Cha) are confirmed high-order multiple systems with up to four components. In 13 cases, we found significant slopes in the PMDs, which are compatible with orbital motion whose periods (estimated from the observed gradients in the position angles) range from 60 to 550 years. However, in only four cases there are indications of a curved orbit, the ultimate proof of a gravitational bond. Conclusions: A statistical study based on the 2MASS catalogue confirms the high probability of all 16 stellar systems being gravitationally bound. Most of the secondary components are well above the mass limit of hydrogen burning stars (0.08 M⊙), and have masses twice as high as this value or more. Massive primary components appear to avoid the simultaneous formation of equal-mass secondary components, while extremely low-mass secondary components are hard to find for both high and low mass primaries owing to the much higher dynamic range and the faintness of the secondaries. Based on observations made with ESO telescopes at the Paranal Observatory under program IDs 076.C-0292(A), 078.C-0535(A), 080.C-0424(A), 082.C-0489(A), 084.C-0364(B), 086.C-0638(A) & 086.C-0600(B), the Hubble Space Telescope under program ID GO-8716 and data obtained from the ESO/ST-ECF Science Archive Facility from the Paranal Observatory under program IDs 075.C-0042(A), 076.C-0579(A), 278.C-5070(A) and from the Hubble Space Telescope under programme IDs SNAP-7387, GO-11164. Appendix A is available in electronic form at http://www.aanda.org

Evaluation of transit signal priority strategies for bus rapid transit project on 3500 South Street in Salt Lake County, UT.

DOT National Transportation Integrated Search

2013-07-01

Bus Rapid Transit (BRT) is becoming one of the most popular transit services in the United States. BRT is a viable option for many cities and can offer commuters travel times comparable to those experienced in private cars. With about 100 miles of BR...

The Knowledge Product Lifecycle and the Strategic Dashboard

ERIC Educational Resources Information Center

Glessner, Linda L.; Gillis, Denise

2012-01-01

Several years ago, the Continuing and Innovative Education (CIE) leadership team at UT-Austin took a hard look at the unit through the lens of customers to reevaluate their programs and services and the role they played in serving the lifelong educational needs of their constituents. Their goal was to provide continuous learning for a productive,…

The aspen mortality summit; December 18 and 19, 2006; Salt Lake City, UT

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Dale L. Bartos; Wayne D. Shepperd

2010-01-01

The USDA Forest Service Rocky Mountain Research Station sponsored an aspen summit meeting in Salt Lake City, Utah, on December 18 and19, 2006, to discuss the rapidly increasing mortality of aspen (Populus tremuloides) throughout the western United States. Selected scientists, university faculty, and managers from Federal, State, and non-profit agencies with experience...