DOCSLIB.ORG

Radio Astronom1y G

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Radio Astronom1y G £t,: ,/ NATIONAL RADIO ASTRONOMY OBSERVATORY QUARTERLY REPORT October 1 - December 31, 1989 RADIO ASTRONOM1Y G.. '8 tO- C~oe'' n,'evI! I E. Vi. t-Li 1 2 1990 TABLE OF CONTENTS A. TELESCOPE USAGE ... .... ...... ............ 1 B. 140-FOOT OBSERVING PROGRAMS . .... .......... ... 1 C. 12-METER TELESCOPE ....... ..... ., .... ........ 5 D. VERY LARGE ARRAY ....... 1...................8 E. SCIENTIFIC HIGHLIGHTS .... ........ 19 F. PUBLICATIONS ............. G. CENTRAL DEVELOPMENT LABORATORY ........ 20 H. GREEN BANK ELECTRONICS . .. .a.. ...... 21 I. 12-METER ELECTRONICS ...... .. 0. I. 22 J. VLA ELECTRONICS ...... 0..... ..... .... a. 24 K. AIPS .... .............. ...... ............. 26 L. VLA COMPUTER ............. .. .0. .0. ... 27 M. VERY LONG BASELINE ARRAY . .. .0 .0 .0 .0 .0 . .0 .. 27 N. PERSONNEL .. ...... .... .0.0 . .0. .0. .. e. 30 APPENDIX A: List of NRAO Preprints A. TELESCOPE USAGE The NRAO telescopes have been scheduled for research and maintenance in the following manner during the fourth quarter of 1989. 140-ft 12-m VLA Scheduled observing (hrs) 1901.75 1583.50 1565.2 Scheduled maintenance and equipment changes 132.00 107.75 259.8 Scheduled tests and calibrations 20.75 425.75 327.1 Time lost 139.25 208.25 107.0 Actual observing 1762.50 1375.25 1458.2 B. 140-FOOT OBSERVING PROGRAMS The following line programs were conducted during this quarter. No. Observer(s) Program A-95 Avery, L (Herzberg) Observations at 18.2, 18.6, and Bell, M. (Herzberg) 23.7 GHz of cyanopolyynes in carbon Feldman, P. (Herzberg) stars part II. MacLeod, J. (Herzberg) Matthews, H. (Herzberg) B-493 Bania, T. (Boston) Measurements at 8.666 GHz of 3He + Rood, R. (Virginia) emission in HII regions and planetary Wilson, T. (MPIR, Bonn) nebulae. C-258 Clark, F. (AF Geophysics Lab) Studies at 23.7 GHz of ammonia in Mann, P. (Kentucky) infrared objects. LaHaise, W. (Kentucky) C-261 Cersosimo, J. (NAIC) Search at 8.880 GHz for the a and lines of carbon. C-263 Cersosimo, J. (NAIC) Studies of 18 cm recombination lines Onello, J. (SUNY, Cortland) from the diffuse interstellar gas. D-163 De Geus, E. (Maryland) Studies of HI around young open Leisawitz, D. (GSFC) clusters. D-164 da Costa, L. (CNPq, Brazil) Hydrogen observations of southern Giovanelli, R. (NAIC) low-surface brightness galaxies. Haynes, M. (Cornell) No. Observer(s) Program E-56 Elvis, M. (CFA) Hydrogen survey of the north ecliptic Lockman, F. J. pole. Morris, M. (UCLA) Likkel, L. (UCLA) M-283 Maddalena, R. Monitor at 1.3 cm unusual H20 emission from two IRAS sources. M-284 Madden, S. (Massachusetts) Time variability study at 1.5 cm of Brown, R. (Monash University) ammonia masers. Godfrey, P. (Monash University) Henkel, C. (MPIR, Bonn) Irvine, W. (Massachusetts) Wilson, T. (MPIR, Bonn) Maddalena, R. M-296 McCammon, D. (Wisconsin) Search for HI "edges." Jahoda, K. (GSFC) Snowden, S. (MPIR, Bonn) Lockman, F. J. M-301 Bally, J. (Bell Labs) Observations of HI toward selected Maddalena, R. areas of Monoceros. Blitz, L. (Maryland) Pachowsky, R. (Maryland) S-330 Schloerb, F. (Massachussetts) OH observations of Comet Tacconi-Garman, L. (Massachusetts) P/Brorsen-Metcalf and C/Okazaki - Levy-Rudenko. T-268 DeFrees, D. (Molecular Research Search at 19 GHz for interstellar Inst.) C50. McLean, A. (Molecular Research Inst.) W-280 Wootten, H. A. H20 monitoring in star forming cores in rho Oph. The following pulsar programs were conducted during this quarter. No. Observer(s) Program B-484 Backer, D. (Berkeley) Timing observations at 750-800, and Foster, R. (Berkeley) 1355 MHz of PSR 1821-24 and other Taylor, J. (Princeton) millisecond pulsars. No. Observer(s) Program T-265 Taylor, J. (Princeton) Pulsar timing observations over the Stinebring, D. (Princeton) range 450-500, 750-800, and 1355 MHz. Dewey, R. (JPL) Nice, D. (Princeton) Thorsett, S. (Princeton) The following very long baseline programs were conducted, and the stations used for the observations are coded as follows: A Arecibo 1000 ft N NRL Maryland Pt. 85 ft B Effelsburg, MPIR 100 m No Noto, Sicily E Hartebeesthoek, South Africa 26 m O0 Owens Valley 130 ft F Fort Davis 85 ft Pt Pietown 25m G Green Bank 140 ft R Crimea, USSR 30 m H Hat Creek 26 m Sa Shanghai 25 m I Iowa 60 ft So Onsala 25 m Jb Jodrell Bank 250 ft Sn Onsala 20 m Km Haystack 120 ft T Torun 15 m Kp Kitt Peak 25 m Wn Westerbork n=l-14x26 m Lb Bologna 25 meter X Itapetinga 20 m Me Merlin Yn Socorro n=l-27x25 m No. Observer(s) Program AH-46V Wilkinson, P. (Manchester) Observations at 18 cm of 3C 380, with Akujor, C. (Nigeria) telescopes B, Jb, So, Lm, Wn, Km, G, F, O, Pt, and Kp. AH-7V Hewitt, J. (Haystack) Observations at 3.6 cm of reference sources for dMe stars, with telescopes G, H, and Pt. B-93V Booth, R. (Chalmers) Kus, A. (Chalmers) Observations at 3.6 cm of the core of Wilkinson, P. (Manchester) the steep spectrum compact QSO 3C 380, with telescopes B, Lm, Sn, Km, G, F, O, Y27, and Pt. B-94V Barthel, P. (Groningen) Studies at 6 cm of the cores in giant de Bruyn, A. (NFRA) core dominated quasars, with Schilizzi, R. (NFRA) telescopes B, Wn, Jb, So, Kin, G, H, O'Dea, C. (NRFA) I, O, F, and Y27. Wieringa, M. (Leiden) B-98V Bartel, N. (CFA) Observations of Cyg X-1 at 3.8 cm-- Lestrade, J.-F. (JPL) neutron star or black hole--with McClintock, J. (CFA) telescopes B, Lm, Sn, Km, G, F, O, Phillips, R. (Haystack) Y27, and Pt. Shapiro, I. (CFA) Preston, R. (JPL) 4 No. Observer(s) Program B-99V Bartel, N. (CFA) "World Array" bandwidth-synthesis Biretta, J. (CFA) observations of 3C 84 at 18 cm, with telescopes B, Lm, So, Wn, Jb, R, T, No, Kin, G, F, O, I, N, Y2 7 , Pt, Kp, and Me. F-23V Field, D. (Bristol, England) Observations at 18 cm of OH masers, Gray, M. (Bristol, England) with telescopes B, So, Jb, G, O, Pt, Cohen, M. (Caltech) and Sa. Zhou, Z. (Shanghai Observatory) Liang, S. (Shanghai Observatory) Winnberg, A. (Chalmers) Booth, R. (Chalmers) G-60V Giovannini, G. (Bologna) Observations at 6 cm of a sample of Wehrle, A. (Caltech) Fanaroff-Riley Type I radio galaxies, Comoretto, G. (Arcetri) with telescopes at B, Jb, So, Wn, Km, Feretti, L. (Bologna) G, F, O, Y2 7 , and Pt. Venturi, T. (Bologna) G-61V Garrett, M. (Manchester) Observations at 18 cm of the Wilkinson, P. (Manchester) gravitationally lensed quasar Walsh, D. (Manchester) 0957+561 A,B, with telescopes B, So, Porcas, R. (MPIR, Bonn) Lm, Wn, Jb, G, Y1 , O, and Pt. Quirrenbach, A. (MPIR, Bonn) G-62V Gwinn, C. (CFA) Study at 18 cm the OH magamaser in Moran, J. (CFA) IIIZw 035, with telescopes B, G, Y2 7 , Reid, M. (CFA) Pt, and A. Zheng, X. (Nanjing) Peng, Y. (Nanjing) H-51V Heflin, M. (MIT) Observations at 18 cm of the Lawrence, C. (Caltech) gravitational lens system 2016+112, Burke, B. (MIT) with telescopes B, Wn, Jb, Km, G, F, Shapiro, I. (MIT) 0, Y27 , and A. K-24V Kus, A. (Chalmers) Observations at 3.6 cm of the core of Booth, R. (Chalmers) the steep spectrum compact QSO 3C Mareki, A. (Torun) 386, with telescopes B, Lm, Sn, Km, G, F, O, Y2 7 , and Pt. L-57V Mutel, R. (Iowa) Measure at 18 cm the inner scale of Spangler, S. (Iowa) interstellar turbulence, with telescopes B, Lm, Wn, Kin, G, F, O, and Y27 * No. Observer(s) Program M-103V Mutel, R. (Iowa) Measure at 18 cm the inner scale of Spangler, S. (Iowa) interstellar turbulence, with telescopes B, Lm, Wn, Km, G, F, O, and Y27 . N-18V Neff, S. (Goddard) High resolution observations at 18 cm Antonucci, R. (Calif., Santa of the NGC 1068 core, with telescopes Barbara) B, Lm, G, O, and Y27 . Pedlar, A. (MRAO) O-5V O'Dea, C. (NRFA) Observations at 6 cm of gigahertz Baum, S. (NFRA) peaked spectrum sources, with Murphy, D. (JPL) telescopes B, Wn, Jb, So, Km, G, O, F, Y27 , and Pt. P-91V Phillips, R. (Haystack) Studies of hot O-giant stars at Titus, M. (Haystack) 18 cm, with telescopes G, O, Y27 , and Lestrade, J-F. (JPL) Pt. P-95V Pauliny-Toth, I. (MPIR, Bonn) Observations at 18 cm of 3C 454.3, Porcas, R. (MPIR, Bonn) with telescopes B, Jb, So, Lm, Wn, R, Zensus, A. T, Km, G, O, Pt, E, and Me. Kellermann, K. P-98V Pearson, T. (Caltech) Second epoch maps and spectra of four Readhead, A. (Caltech) sources at 18 cm, with telescopes B, So, Lm, Wn, Jb, No, Kin, G, O, Y1 , Pt, Kp, and La. S-84V Sakurai, T. (Iowa) Studies at 18 cm of the density Spangler, S. (Iowa) turbulence in the outer corona and Cairns, I. (Iowa) solar wind, with telescopes N, I, 0, Mutel, R. (Iowa) F, and Y27- Armstrong, J. (JPL) W-54V Walker, R. C. Third epoch observations at 18 cm of Benson, J. 3C 120, with telescopes B, Jb, Wn, Unwin, S. (Caltech) So, Lm, T, R, No, K, G, N, I, F, O, Pilbratt, G. (ESA) Y1 , Pt, Kp, and A. C. 12-METER TELESCOPE The following line programs were conducted during this quarter. No. Observer(s) Program A-94 Adler, D. (Illinois) Study of the structure of the Allen, R. (Illinois) interstellar medium in the spiral Lo, K. (Illinois) galaxy M83. Sukumar, S. (Illinois) No. Observer(s) Program B-526 Buhl, D. (GSFC) Study of CO in the atmospheres of Chin, G. (GSFC) Venus and Jupiter. Goldstein, J.
Load more

Recommended publications
  • II Publications, Presentations
    II Publications, Presentations 1. Refereed Publications Izumi, K., Kotake, K., Nakamura, K., Nishida, E., Obuchi, Y., Ohishi, N., Okada, N., Suzuki, R., Takahashi, R., Torii, Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, Y., Ueda, A., Yamazaki, T.: 2010, DECIGO and DECIGO Search for Gravitational-wave Inspiral Signals Associated with pathfinder, Class. Quantum Grav., 27, 084010. Short Gamma-ray Bursts During LIGO's Fifth and Virgo's First Aoki, K.: 2010, Broad Balmer-Line Absorption in SDSS Science Run, ApJ, 715, 1453-1461. J172341.10+555340.5, PASJ, 62, 1333. Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, All- Aoki, K., Oyabu, S., Dunn, J. P., Arav, N., Edmonds, D., Korista sky search for gravitational-wave bursts in the first joint LIGO- K. T., Matsuhara, H., Toba, Y.: 2011, Outflow in Overlooked GEO-Virgo run, Phys. Rev. D, 81, 102001. Luminous Quasar: Subaru Observations of AKARI J1757+5907, Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, PASJ, 63, S457. Search for gravitational waves from compact binary coalescence Aoki, W., Beers, T. C., Honda, S., Carollo, D.: 2010, Extreme in LIGO and Virgo data from S5 and VSR1, Phys. Rev. D, 82, Enhancements of r-process Elements in the Cool Metal-poor 102001. Main-sequence Star SDSS J2357-0052, ApJ, 723, L201-L206. Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, Arai, A., et al. including Yamashita, T., Okita, K., Yanagisawa, TOPICAL REVIEW: Predictions for the rates of compact K.: 2010, Optical and Near-Infrared Photometry of Nova V2362 binary coalescences observable by ground-based gravitational- Cyg: Rebrightening Event and Dust Formation, PASJ, 62, wave detectors, Class.
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Dust and Molecular Shells in Asymptotic Giant Branch Stars⋆⋆⋆⋆⋆⋆
    A&A 545, A56 (2012) Astronomy DOI: 10.1051/0004-6361/201118150 & c ESO 2012 Astrophysics Dust and molecular shells in asymptotic giant branch stars,, Mid-infrared interferometric observations of R Aquilae, R Aquarii, R Hydrae, W Hydrae, and V Hydrae R. Zhao-Geisler1,2,†, A. Quirrenbach1, R. Köhler1,3, and B. Lopez4 1 Zentrum für Astronomie der Universität Heidelberg (ZAH), Landessternwarte, Königstuhl 12, 69120 Heidelberg, Germany e-mail: [email protected] 2 National Taiwan Normal University, Department of Earth Sciences, 88 Sec. 4, Ting-Chou Rd, Wenshan District, Taipei, 11677 Taiwan, ROC 3 Max-Planck-Institut für Astronomie, Königstuhl 17, 69120 Heidelberg, Germany 4 Laboratoire J.-L. Lagrange, Université de Nice Sophia-Antipolis et Observatoire de la Cˆote d’Azur, BP 4229, 06304 Nice Cedex 4, France Received 26 September 2011 / Accepted 21 June 2012 ABSTRACT Context. Asymptotic giant branch (AGB) stars are one of the largest distributors of dust into the interstellar medium. However, the wind formation mechanism and dust condensation sequence leading to the observed high mass-loss rates have not yet been constrained well observationally, in particular for oxygen-rich AGB stars. Aims. The immediate objective in this work is to identify molecules and dust species which are present in the layers above the photosphere, and which have emission and absorption features in the mid-infrared (IR), causing the diameter to vary across the N-band, and are potentially relevant for the wind formation. Methods. Mid-IR (8–13 μm) interferometric data of four oxygen-rich AGB stars (R Aql, R Aqr, R Hya, and W Hya) and one carbon- rich AGB star (V Hya) were obtained with MIDI/VLTI between April 2007 and September 2009.
    [Show full text]
  • Meeting Program
    A A S MEETING PROGRAM 211TH MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY WITH THE HIGH ENERGY ASTROPHYSICS DIVISION (HEAD) AND THE HISTORICAL ASTRONOMY DIVISION (HAD) 7-11 JANUARY 2008 AUSTIN, TX All scientific session will be held at the: Austin Convention Center COUNCIL .......................... 2 500 East Cesar Chavez St. Austin, TX 78701 EXHIBITS ........................... 4 FURTHER IN GRATITUDE INFORMATION ............... 6 AAS Paper Sorters SCHEDULE ....................... 7 Rachel Akeson, David Bartlett, Elizabeth Barton, SUNDAY ........................17 Joan Centrella, Jun Cui, Susana Deustua, Tapasi Ghosh, Jennifer Grier, Joe Hahn, Hugh Harris, MONDAY .......................21 Chryssa Kouveliotou, John Martin, Kevin Marvel, Kristen Menou, Brian Patten, Robert Quimby, Chris Springob, Joe Tenn, Dirk Terrell, Dave TUESDAY .......................25 Thompson, Liese van Zee, and Amy Winebarger WEDNESDAY ................77 We would like to thank the THURSDAY ................. 143 following sponsors: FRIDAY ......................... 203 Elsevier Northrop Grumman SATURDAY .................. 241 Lockheed Martin The TABASGO Foundation AUTHOR INDEX ........ 242 AAS COUNCIL J. Craig Wheeler Univ. of Texas President (6/2006-6/2008) John P. Huchra Harvard-Smithsonian, President-Elect CfA (6/2007-6/2008) Paul Vanden Bout NRAO Vice-President (6/2005-6/2008) Robert W. O’Connell Univ. of Virginia Vice-President (6/2006-6/2009) Lee W. Hartman Univ. of Michigan Vice-President (6/2007-6/2010) John Graham CIW Secretary (6/2004-6/2010) OFFICERS Hervey (Peter) STScI Treasurer Stockman (6/2005-6/2008) Timothy F. Slater Univ. of Arizona Education Officer (6/2006-6/2009) Mike A’Hearn Univ. of Maryland Pub. Board Chair (6/2005-6/2008) Kevin Marvel AAS Executive Officer (6/2006-Present) Gary J. Ferland Univ. of Kentucky (6/2007-6/2008) Suzanne Hawley Univ.
    [Show full text]
  • Overview on Spectral Line Source Finding and Visualisation
    CSIRO PUBLISHING Publications of the Astronomical Society of Australia, 2012, 29, 359–370 http://dx.doi.org/10.1071/AS12030 Overview on Spectral Line Source Finding and Visualisation B. S. Koribalski CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia Email: [email protected] Abstract: Here I will outline successes and challenges for finding spectral line sources in large data cubes that are dominated by noise. This is a 3D challenge as the sources we wish to catalog are spread over several spatial pixels and spectral channels. While 2D searches can be applied, e.g. channel by channel, optimal searches take into account the 3-dimensional nature of the sources. In this overview I will focus on HI 21-cm spectral line source detection in extragalactic surveys, in particular HIPASS, the HI Parkes All-Sky Survey and WALLABY, the ASKAP HI All-Sky Survey. I use the original HIPASS data to highlight the diversity of spectral signatures of galaxies and gaseous clouds, both in emission and absorption. Among others, I report the À1 discovery of a 680 km s wide HI absorption trough in the megamaser galaxy NGC 5793. Issues such as source confusion and baseline ripples, typically encountered in single-dish HI surveys, are much reduced in interferometric HI surveys. Several large HI emission and absorption surveys are planned for the Australian Square Kilometre Array Pathfinder (ASKAP): here we focus on WALLABY, the 21-cm survey of the sky (d , þ308; z , 0.26) which will take about one year of observing time with ASKAP.
    [Show full text]
  • Staffbrochure200903e.Pdf
    天文及天文物理研究所天文及天文物理研究所 Institute of Astronomy and Astrophysics Academia Sinica SMSMAA TAOTAOSS Institute of Astronomy and Astrophysics P.O. Box 23-141, Taipei 106, Taiwan, R.O.C Tel: 886-2-33652200 Fax: 886-2-23677849 Website: http://www.asiaa.sinica.edu.tw AMAMiiBABA AALMALMA TiARTiARAA 目錄 AMiBA TAOSS CFHTCFHT ALMA TIARA SMA Contents 02 Introduction 04 Administration 05 Advisory Panel Members 06 Research Fellows & Specialists 38 Adjunct Research Fellows 40 Postdoctoral Fellows 42 Visiting Scholars 44 List of Personnel Institute of Astronomy & Astrophysics Introduction The Institute of Astronomy and Astrophysics (ASIAA) was established in 1993 after approval by the Academia Sinica Council upon the recommendation of Academician C.C. Lin. It started as a Preparatory Office inaugurated with Prof. Frank H. Shu chairing the Advisory Panel, and with Dr. Typhoon Lee as the first director. Succeeding directors have been Prof. Chi Yuan (1994-1997), Prof. Fred K.Y. Lo (1997-2002), Prof. Sun Kwok (2003-2005), and Prof. Paul T.P. Ho (2002-2003, and Sept. 2005 - present). ASIAA currently has about 140 members, including research scien- tists, post-doctoral fellows, engineers, and technical and administrative staff. ASIAA is interna- tional and has members from many foreign countries, including Australia, Canada, France, India, Japan, Korea, Malaysia, Switzerland, U.S.A., and Vietnam. ASIAA is officially still a Preparatory Office, which means that the major decisions, such as hiring, are made in fact by the Advisory Panel. The Advisory Panel provides oversight and advice to ASIAA, and helps formulate the future planning of the institute. ASIAA plans to become a full-fledged institute in a couple of years and grow by a factor of two in size in five to ten years.
    [Show full text]
  • Atlas Menor Was Objects to Slowly Change Over Time
    C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts.
    [Show full text]
  • HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land
    HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land 1 Executive Summary • There are now 420 peer-reviewed HET publications – Fifteen papers published in 2019 – As of 27 November, nineteen published papers in 2020 • HET papers have 29363 citations – Average of 70, median of 39 citations per paper – H-number of 90 – 81 papers have ≥ 100 citations; 175 have ≥ 50 cites • Wide angle surveys account for 26% of papers and 35% of citations. • Synoptic (e.g., planet searches) and Target of Opportunity (e.g., supernovae and γ-ray bursts) programs have produced 47% of the papers and 47% of the citations, respectively. • Listing of the HET papers (with ADS links) is given at http://personal.psu.edu/dps7/hetpapers.html 2 HET Program Classification Code TypeofProgram Examples 1 ToO Supernovae,Gamma-rayBursts 2 Synoptic Exoplanets,EclipsingBinaries 3 OneorTwoObjects HaloofNGC821 4 Narrow-angle HDF,VirgoCluster 5 Wide-angle BlazarSurvey 6 HETTechnical HETQueue 7 HETDEXTheory DarkEnergywithBAO 8 Other HETOptics Programs also broken down into “Dark Time”, “Light Time”, and “Other”. 3 Peer-reviewed Publications • There are now 420 journal papers that either use HET data or (nine cases) use the HET as the motivation for the paper (e.g., technical papers, theoretical studies). • Except for 2005, approximately 22 HET papers were published each year since 2002 through the shutdown. A record 44 papers were published in 2012. • In 2020 a total of fifteen HET papers appeared; nineteen have been published to date in 2020. • Each HET partner has published at least 14 papers using HET data. • Nineteen papers have been published from NOAO time.
    [Show full text]
  • Resolving the AGN and Host Emission in the Mid-Infrared Using A
    Draft version February 23, 2015 Preprint typeset using LATEX style emulateapj v. 5/2/11 RESOLVING THE AGN AND HOST EMISSION IN THE MID-INFRARED USING A MODEL-INDEPENDENT SPECTRAL DECOMPOSITION Antonio Hernan´ -Caballero,1 Almudena Alonso-Herrero,1 Evanthia Hatziminaoglou,2 Henrik W. W. Spoon,3 Cristina Ramos Almeida,4,5 Tanio D´ıaz Santos,6,7 Sebastian F. H¨onig,8 Omaira Gonzalez´ -Mart´ın,9 and Pilar Esquej10 Draft version February 23, 2015 ABSTRACT We present results on the spectral decomposition of 118 Spitzer Infrared Spectrograph (IRS) spectra from local active galactic nuclei (AGN) using a large set of Spitzer/IRS spectra as templates. The templates are themselves IRS spectra from extreme cases where a single physical component (stellar, interstellar, or AGN) completely dominates the integrated mid-infrared emission. We show that a linear combination of one template for each physical component reproduces the observed IRS spectra of AGN hosts with unprecedented fidelity for a template fitting method, with no need to model extinction separately. We use full probability distribu- tion functions to estimate expectation values and uncertainties for observables, and find that the decomposition results are robust against degeneracies. Furthermore, we compare the AGN spectra derived from the spec- tral decomposition with sub-arcsecond resolution nuclear photometry and spectroscopy from ground-based observations. We find that the AGN component derived from the decomposition closely matches the nuclear spectrum, with a 1-σ dispersion of 0.12 dex in luminosity and typical uncertainties of ∼0.19 in the spectral index and ∼0.1 in the silicate strength.
    [Show full text]
  • Extended H I Disks in Dust–Lane Elliptical Galaxies1
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Extended H I disks in dust{lane elliptical galaxies1 Thomas A. Oosterloo ASTRON, PO Box 2, 7990 AA, Dwingeloo, The Netherlands Raffaella Morganti ASTRON, PO Box 2, 7990 AA, Dwingeloo, The Netherlands Elaine M. Sadler School of Physics, University of Sydney, NSW 2006, Australia Daniela Vergani Dipartimento di Astronomia, Universit`a di Bologna, via Zamboni 33, I-40126 Bologna, Italy Nelson Caldwell Smithsonian Institution, Steward Observatory, 949 N Cherry Avenue, Tucson Arizona 85719, USA ABSTRACT –2– We present the results of H I observations of five dust-lane ellipticals with the Aus- tralia Telescope Compact Array. Two galaxies (NGC 3108 and NGC 1947) are detected, and sensitive upper limits are obtained for the other three. In the two detected galaxies, the H I is distributed in a regular, extended and warped disk-like structure of low surface brightness. Adding data from the literature, we find that several more dust-lane ellipti- cals have regular H I structures. This H I is likely to be a remnant of accretions/mergers which took place a considerable time ago, and in which a significant fraction of the gas survived to form a disk. The presence of regular H I structures suggests that some mergers lead to galaxies with extended low surface brightness density gas disks. These gas disk will evolve very slowly and these elliptical galaxies will remain gas rich for a long period of time. One of the galaxies we observed (NGC 3108) has a very large amount of neutral 9 hydrogen (MHI =4:5 10 M ; MHI=LB 0:09), which is very regularly distributed × ∼ in an annulus extending to a radius of 6 Reff .
    [Show full text]
  • 190 Index of Names
    Index of names Ancora Leonis 389 NGC 3664, Arp 005 Andriscus Centauri 879 IC 3290 Anemodes Ceti 85 NGC 0864 Name CMG Identification Angelica Canum Venaticorum 659 NGC 5377 Accola Leonis 367 NGC 3489 Angulatus Ursae Majoris 247 NGC 2654 Acer Leonis 411 NGC 3832 Angulosus Virginis 450 NGC 4123, Mrk 1466 Acritobrachius Camelopardalis 833 IC 0356, Arp 213 Angusticlavia Ceti 102 NGC 1032 Actenista Apodis 891 IC 4633 Anomalus Piscis 804 NGC 7603, Arp 092, Mrk 0530 Actuosus Arietis 95 NGC 0972 Ansatus Antliae 303 NGC 3084 Aculeatus Canum Venaticorum 460 NGC 4183 Antarctica Mensae 865 IC 2051 Aculeus Piscium 9 NGC 0100 Antenna Australis Corvi 437 NGC 4039, Caldwell 61, Antennae, Arp 244 Acutifolium Canum Venaticorum 650 NGC 5297 Antenna Borealis Corvi 436 NGC 4038, Caldwell 60, Antennae, Arp 244 Adelus Ursae Majoris 668 NGC 5473 Anthemodes Cassiopeiae 34 NGC 0278 Adversus Comae Berenices 484 NGC 4298 Anticampe Centauri 550 NGC 4622 Aeluropus Lyncis 231 NGC 2445, Arp 143 Antirrhopus Virginis 532 NGC 4550 Aeola Canum Venaticorum 469 NGC 4220 Anulifera Carinae 226 NGC 2381 Aequanimus Draconis 705 NGC 5905 Anulus Grahamianus Volantis 955 ESO 034-IG011, AM0644-741, Graham's Ring Aequilibrata Eridani 122 NGC 1172 Aphenges Virginis 654 NGC 5334, IC 4338 Affinis Canum Venaticorum 449 NGC 4111 Apostrophus Fornac 159 NGC 1406 Agiton Aquarii 812 NGC 7721 Aquilops Gruis 911 IC 5267 Aglaea Comae Berenices 489 NGC 4314 Araneosus Camelopardalis 223 NGC 2336 Agrius Virginis 975 MCG -01-30-033, Arp 248, Wild's Triplet Aratrum Leonis 323 NGC 3239, Arp 263 Ahenea
    [Show full text]
  • New Constraints on the Formation and Settling of Dust in the Atmospheres of Young M and L Dwarfs?,??,???
    A&A 564, A55 (2014) Astronomy DOI: 10.1051/0004-6361/201323016 & c ESO 2014 Astrophysics New constraints on the formation and settling of dust in the atmospheres of young M and L dwarfs?;??;??? E. Manjavacas1, M. Bonnefoy1;2, J. E. Schlieder1, F. Allard3, P. Rojo4, B. Goldman1, G. Chauvin2, D. Homeier3, N. Lodieu5;6, and T. Henning1 1 Max Planck Institute für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] 2 UJF-Grenoble1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR5274, Grenoble 38041, France 3 CRAL-ENS, 46 allée d’Italie, 69364 Lyon Cedex 07, France 4 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile 5 Instituto de Astrofísica de Canarias (IAC), Vía Láctea s/n, 38206 La Laguna, Tenerife, Spain 6 Departamento de Astrofísica, Universidad de La Laguna (ULL), 38205 La Laguna, Tenerife, Spain Received 8 November 2013 / Accepted 6 February 2014 ABSTRACT Context. Gravity modifies the spectral features of young brown dwarfs (BDs). A proper characterization of these objects is crucial for the identification of the least massive and latest-type objects in star-forming regions, and to explain the origin(s) of the peculiar spectrophotometric properties of young directly imaged extrasolar planets and BD companions. Aims. We obtained medium-resolution (R ∼ 1500−1700) near-infrared (1.1−2.5 µm) spectra of seven young M9.5–L3 dwarfs clas- sified at optical wavelengths. We aim to empirically confirm the low surface gravity of the objects in the near-infrared. We also test whether self-consistent atmospheric models correctly represent the formation and the settling of dust clouds in the atmosphere of young late-M and L dwarfs.
    [Show full text]