SAS-2019 the Symposium on Telescope Science
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FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
FOR an ADVANCED Oaoi
.' ' ' > \ .\i I X-732-67-363 < I A COMPUTER, CONTROL SYSTEM I FOR AN ADVANCED OAOi ) I i I , 1 \ i J'OHN A. ,HRASTAR , P 1 (ACCESSION NUMBER) (THRU) I P > . -. c (PAGES) / + AUGUST 1967 - I . \ \ I, I \ / - k d - GO~DARD'SPACE FLIGHT CENTER ' GREENBELT, MARYLAND . .r A COMPUTER CONTROL SYSTEM FOR AN ADVANCED OAO John A. Hrastar August 1967 Goddard Space Flight Center Greenbelt, Maryland A COMPUTER CONTROL SYSTEM FOR AN ADVANCED OAO John A. Hrastar SUMMARY The purpose of the study covered by this report was to determine the feasibility of using an on-board digital computer and strap-down inertial reference unit for attitude control of an advanced OAO space- craft. An integrated, three axis control law was assumed which had been previously proven stable in the large. The principal advantage of this type of control system is the ability to complete three axis reori- entations over large angles. This system, although apparently complex, has the effect of simplifying the overall system. This is because a re- orientation is a simple extension of a hold or point operation, i.e., mode switching may be simplified. The study indicates that a system of this type is feasible and offers many advantages over present systems. The time for a reorientation using this type of control is considerably shorter than the time required using more conventional methods. The computer and inertial reference unit usedinthe study had the characteristics of systems presently under development. Feasibility, therefore is within the present state of the art, requiring only continued development of these systems. -
The Impact of the Astro2010 Recommendations on Variable Star Science
The Impact of the Astro2010 Recommendations on Variable Star Science Corresponding Authors Lucianne M. Walkowicz Department of Astronomy, University of California Berkeley [email protected] phone: (510) 642–6931 Andrew C. Becker Department of Astronomy, University of Washington [email protected] phone: (206) 685–0542 Authors Scott F. Anderson, Department of Astronomy, University of Washington Joshua S. Bloom, Department of Astronomy, University of California Berkeley Leonid Georgiev, Universidad Autonoma de Mexico Josh Grindlay, Harvard–Smithsonian Center for Astrophysics Steve Howell, National Optical Astronomy Observatory Knox Long, Space Telescope Science Institute Anjum Mukadam, Department of Astronomy, University of Washington Andrej Prsa,ˇ Villanova University Joshua Pepper, Villanova University Arne Rau, California Institute of Technology Branimir Sesar, Department of Astronomy, University of Washington Nicole Silvestri, Department of Astronomy, University of Washington Nathan Smith, Department of Astronomy, University of California Berkeley Keivan Stassun, Vanderbilt University Paula Szkody, Department of Astronomy, University of Washington Science Frontier Panels: Stars and Stellar Evolution (SSE) February 16, 2009 Abstract The next decade of survey astronomy has the potential to transform our knowledge of variable stars. Stellar variability underpins our knowledge of the cosmological distance ladder, and provides direct tests of stellar formation and evolution theory. Variable stars can also be used to probe the fundamental physics of gravity and degenerate material in ways that are otherwise impossible in the laboratory. The computational and engineering advances of the past decade have made large–scale, time–domain surveys an immediate reality. Some surveys proposed for the next decade promise to gather more data than in the prior cumulative history of astronomy. -
Whole Earth Telescope Observations of AM Canum Venaticorum – Discoseismology at Last
Astron. Astrophys. 332, 939–957 (1998) ASTRONOMY AND ASTROPHYSICS Whole Earth Telescope observations of AM Canum Venaticorum – discoseismology at last J.-E. Solheim1;14, J.L. Provencal2;15, P.A. Bradley2;16, G. Vauclair3, M.A. Barstow4, S.O. Kepler5, G. Fontaine6, A.D. Grauer7, D.E. Winget2, T.M.K. Marar8, E.M. Leibowitz9, P.-I. Emanuelsen1, M. Chevreton10, N. Dolez3, A. Kanaan5, P. Bergeron6, C.F. Claver2;17, J.C. Clemens2;18, S.J. Kleinman2, B.P. Hine12, S. Seetha8, B.N. Ashoka8, T. Mazeh9, A.E. Sansom4;19, R.W. Tweedy4, E.G. Meistasˇ 11;13, A. Bruvold1, and C.M. Massacand1 1 Nordlysobservatoriet, Institutt for Fysikk, Universitetet i Tromsø, N-9037 Tromsø, Norway 2 McDonald Observatory and Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA 3 Observatoire Midi–Pyrenees, 14 Avenue E. Belin, F-31400 Toulouse, France 4 Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, UK 5 Instituto de Fisica, Universidade Federal do Rio Grande do Sul, 91500-970 Porto Alegre - RS, Brazil 6 Department de Physique, Universite´ de Montreal,´ C.P. 6128, Succ A., Montreal,´ PQ H3C 3J7, Canada 7 Department of Physics and Astronomy, University of Arkansas, 2801 S. University Ave, Little Rock, AR 72204, USA 8 Technical Physics Division, ISRO Satelite Centre, Airport Rd, Bangalore, 560 017 India 9 University of Tel Aviv, Department of Physics and Astronomy, Ramat Aviv, Tel Aviv 69978, Israel 10 Observatoire de Paris-Meudon, F-92195 Meudon Principal Cedex, France 11 Institute of Material Research and Applied Sciences, Vilnius University, Ciurlionio 29, Vilnius 2009, Lithuania 12 NASA Ames Research Center, M.S. -
1000 Cataclysmic Variables from the Catalina Real-Time Transient Survey
MNRAS 443, 3174–3207 (2014) doi:10.1093/mnras/stu1377 1000 cataclysmic variables from the Catalina Real-time Transient Survey E. Breedt,1‹ B. T. Gansicke,¨ 1 A. J. Drake,2 P. Rodr´ıguez-Gil,3,4 S. G. Parsons,5 T. R. Marsh,1 P. Szkody,6 M. R. Schreiber5 and S. G. Djorgovski2 1Department of Physics, University of Warwick, Coventry, CV4 7AL, UK 2California Institute of Technology, 1200 E. California Blvd, CA 91225, USA 3Instituto de Astrof´ısica de Canarias, V´ıa Lactea´ s/n, La Laguna, E-38205, Santa Cruz de Tenerife, Spain 4Departamento de Astrof´ısica, Universidad de La Laguna, La Laguna, E-38206, Santa Cruz de Tenerife, Spain 5Instituto de F´ısica y Astronom´ıa, Universidad de Valpara´ıso, Avenida Gran Bretana 1111, 2360102 Valpara´ıso, Chile 6Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580, USA Downloaded from Accepted 2014 July 6. Received 2014 July 5; in original form 2014 May 13 ABSTRACT Over six years of operation, the Catalina Real-time Transient Survey (CRTS) has identified http://mnras.oxfordjournals.org/ 1043 cataclysmic variable (CV) candidates – the largest sample of CVs from a single survey to date. Here, we provide spectroscopic identification of 85 systems fainter than g ≥ 19, including three AM Canum Venaticorum binaries, one helium-enriched CV, one polar and one new eclipsing CV. We analyse the outburst properties of the full sample and show that it contains a large fraction of low-accretion-rate CVs with long outburst recurrence times. We argue that most of the high-accretion-rate dwarf novae in the survey footprint have already been found and that future CRTS discoveries will be mostly low-accretion-rate systems. -
Exploring the Brown Dwarf Desert C
Astronomy & Astrophysics manuscript no. draft c ESO 2018 March 5, 2018 MOA-2007-BLG-197: Exploring the brown dwarf desert C. Ranc1; 35, A. Cassan1; 35, M. D. Albrow2; 35, D. Kubas1; 35, I. A. Bond3; 36, V. Batista1; 35, J.-P. Beaulieu1; 35, D. P. Bennett4; 36, M. Dominik5; 35, Subo Dong6; 37, P. Fouqué7; 8; 35, A. Gould9; 37, J. Greenhilly10; 35, U. G. Jørgensen11; 35, N. Kains12; 5; 35, J. Menzies13; 35, T. Sumi14; 36, E. Bachelet15; 35, C. Coutures1; 35, S. Dieters1; 35, D. Dominis Prester16; 35, J. Donatowicz17; 35, B. S. Gaudi9; 37, C. Han18; 37, M. Hundertmark5; 11, K. Horne5; 35, S. R. Kane19; 35, C.-U. Lee20; 37, J.-B. Marquette1; 35, B.-G. Park20; 37, K. R. Pollard2; 35, K. C. Sahu12; 35, R. Street21; 35, Y. Tsapras21; 22; 35, J. Wambsganss22; 35, A. Williams23; 24; 35, M. Zub22; 35, F. Abe25; 36, A. Fukui26; 36, Y. Itow25; 36, K. Masuda25; 36, Y. Matsubara25; 36, Y. Muraki25; 36, K. Ohnishi27; 36, N. Rattenbury28; 36, To. Saito29; 36, D. J. Sullivan30; 36, W. L. Sweatman31; 36, P. J. Tristram32; 36, P. C. M. Yock33; 36, and A. Yonehara34; 36 (Affiliations can be found after the references) Received <date> / accepted <date> ABSTRACT We present the analysis of MOA-2007-BLG-197Lb, the first brown dwarf companion to a Sun-like star detected through gravitational microlensing. The event was alerted and followed-up photometrically by a network of telescopes from the PLANET, MOA, and µFUN collaborations, and observed at high angular resolution using the NaCo instrument at the VLT. -
Superwasp Observations of Long Timescale Photometric Variations in Cataclysmic Variables
A&A 514, A30 (2010) Astronomy DOI: 10.1051/0004-6361/200912650 & c ESO 2010 Astrophysics SuperWASP observations of long timescale photometric variations in cataclysmic variables N. L. Thomas1,A.J.Norton1, D. Pollacco2,R.G.West3,P.J.Wheatley4, B. Enoch5, and W. I. Clarkson6 1 Department of Physics and Astronomy, The Open University, Milton Keynes MK7 6AA, UK e-mail: [email protected] 2 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University, University Road, Belfast BT7 1NN, UK 3 Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK 4 Department of Physics, University of Warwick, Coventry CV4 7AL, UK 5 SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK 6 STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA Received 7 June 2009 / Accepted 26 January 2010 ABSTRACT Aims. We investigated whether the predictions and results of Stanishev et al. (2002, A&A, 394, 625) concerning a possible relation- ship between eclipse depths in PX And and its retrograde disc precession phase, could be confirmed in long term observations made by SuperWASP. In addition, two further CVs (DQ Her and V795 Her) in the same SuperWASP data set were investigated to see whether evidence of superhump periods and disc precession periods were present and what other, if any, long term periods could be detected. Methods. Long term photometry of PX And, V795 Her and DQ Her was carried out and Lomb-Scargle periodogram analysis under- taken on the resulting light curves. For the two eclipsing CVs, PX And and DQ Her, we analysed the potential variations in the depth of the eclipse with cycle number. -
Variable Star Classification and Light Curves Manual
Variable Star Classification and Light Curves An AAVSO course for the Carolyn Hurless Online Institute for Continuing Education in Astronomy (CHOICE) This is copyrighted material meant only for official enrollees in this online course. Do not share this document with others. Please do not quote from it without prior permission from the AAVSO. Table of Contents Course Description and Requirements for Completion Chapter One- 1. Introduction . What are variable stars? . The first known variable stars 2. Variable Star Names . Constellation names . Greek letters (Bayer letters) . GCVS naming scheme . Other naming conventions . Naming variable star types 3. The Main Types of variability Extrinsic . Eclipsing . Rotating . Microlensing Intrinsic . Pulsating . Eruptive . Cataclysmic . X-Ray 4. The Variability Tree Chapter Two- 1. Rotating Variables . The Sun . BY Dra stars . RS CVn stars . Rotating ellipsoidal variables 2. Eclipsing Variables . EA . EB . EW . EP . Roche Lobes 1 Chapter Three- 1. Pulsating Variables . Classical Cepheids . Type II Cepheids . RV Tau stars . Delta Sct stars . RR Lyr stars . Miras . Semi-regular stars 2. Eruptive Variables . Young Stellar Objects . T Tau stars . FUOrs . EXOrs . UXOrs . UV Cet stars . Gamma Cas stars . S Dor stars . R CrB stars Chapter Four- 1. Cataclysmic Variables . Dwarf Novae . Novae . Recurrent Novae . Magnetic CVs . Symbiotic Variables . Supernovae 2. Other Variables . Gamma-Ray Bursters . Active Galactic Nuclei 2 Course Description and Requirements for Completion This course is an overview of the types of variable stars most commonly observed by AAVSO observers. We discuss the physical processes behind what makes each type variable and how this is demonstrated in their light curves. Variable star names and nomenclature are placed in a historical context to aid in understanding today’s classification scheme. -
Arxiv:1810.09864V2 [Astro-Ph.SR] 6 Nov 2018
Manuscript for Revista Mexicana de Astronomía y Astrofísica (2007) EXTENSIVE PHOTOMETRY OF V1838 AQL DURING THE 2013 SUPEROUTBURST J. Echevarría1, E. de Miguel2, J. V. Hernández Santisteban3, R. Michel4, R. Costero1, L. J. Sánchez1, A. Ruelas-Mayorga1, J. Olivares5, D. González-Buitrago6, J.L. Jones7, A. Oskanen8, W. Goff9, J. Ulowetz10, G. Bolt11, R. Sabo12, F.-J Hambsch13, D. Slauson14, and W. Stein15 Draft version: September 6, 2021 RESUMEN Presentamos un estudio fotométrico detallado de la super-erupción de V1838 Aql, una variable cataclísmica recientemente descubierta, desde el máx- imo en 2013 hasta su regreso al mínimo. Examinamos en detalle la evolución de los superhumps. Determinamos el período orbital Porb = 0:05698(9) d a partir de la periodicidad de los superhumps tempranos. Comparando los períodos de superhumps en las etapas A y B con el valor del período orbital, derivamos un valor del cambio en el período orbital de = 0:024(2) y un cociente de masa para el sistema de q = 0:10(1). Sugerimos que V1838 Aql se está acercando al mínimo período orbital, por lo que la secundaria sería una estrella de baja masa y no un objeto sub-estelar. ABSTRACT We present an in-depth photometric study of the 2013 superoutburst of the recently discovered cataclysmic variable V1838 Aql and subsequent pho- tometry near its quiescent state. A careful examination of the development of the superhumps is presented. Our best determination of the orbital period is Porb = 0:05698(9) days, based on the periodicity of early superhumps. Com- paring the superhump periods at stages A and B with the early superhump 1Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, Ciudad Universitaria, México D.F., C.P. -
Open Batalha-Dissertation.Pdf
The Pennsylvania State University The Graduate School Eberly College of Science A SYNERGISTIC APPROACH TO INTERPRETING PLANETARY ATMOSPHERES A Dissertation in Astronomy and Astrophysics by Natasha E. Batalha © 2017 Natasha E. Batalha Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy August 2017 The dissertation of Natasha E. Batalha was reviewed and approved∗ by the following: Steinn Sigurdsson Professor of Astronomy and Astrophysics Dissertation Co-Advisor, Co-Chair of Committee James Kasting Professor of Geosciences Dissertation Co-Advisor, Co-Chair of Committee Jason Wright Professor of Astronomy and Astrophysics Eric Ford Professor of Astronomy and Astrophysics Chris Forest Professor of Meteorology Avi Mandell NASA Goddard Space Flight Center, Research Scientist Special Signatory Michael Eracleous Professor of Astronomy and Astrophysics Graduate Program Chair ∗Signatures are on file in the Graduate School. ii Abstract We will soon have the technological capability to measure the atmospheric compo- sition of temperate Earth-sized planets orbiting nearby stars. Interpreting these atmospheric signals poses a new challenge to planetary science. In contrast to jovian-like atmospheres, whose bulk compositions consist of hydrogen and helium, terrestrial planet atmospheres are likely comprised of high mean molecular weight secondary atmospheres, which have gone through a high degree of evolution. For example, present-day Mars has a frozen surface with a thin tenuous atmosphere, but 4 billion years ago it may have been warmed by a thick greenhouse atmosphere. Several processes contribute to a planet’s atmospheric evolution: stellar evolution, geological processes, atmospheric escape, biology, etc. Each of these individual processes affects the planetary system as a whole and therefore they all must be considered in the modeling of terrestrial planets. -