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Nd AAS Meeting Abstracts
nd AAS Meeting Abstracts 101 – Kavli Foundation Lectureship: The Outreach Kepler Mission: Exoplanets and Astrophysics Search for Habitable Worlds 200 – SPD Harvey Prize Lecture: Modeling 301 – Bridging Laboratory and Astrophysics: 102 – Bridging Laboratory and Astrophysics: Solar Eruptions: Where Do We Stand? Planetary Atoms 201 – Astronomy Education & Public 302 – Extrasolar Planets & Tools 103 – Cosmology and Associated Topics Outreach 303 – Outer Limits of the Milky Way III: 104 – University of Arizona Astronomy Club 202 – Bridging Laboratory and Astrophysics: Mapping Galactic Structure in Stars and Dust 105 – WIYN Observatory - Building on the Dust and Ices 304 – Stars, Cool Dwarfs, and Brown Dwarfs Past, Looking to the Future: Groundbreaking 203 – Outer Limits of the Milky Way I: 305 – Recent Advances in Our Understanding Science and Education Overview and Theories of Galactic Structure of Star Formation 106 – SPD Hale Prize Lecture: Twisting and 204 – WIYN Observatory - Building on the 308 – Bridging Laboratory and Astrophysics: Writhing with George Ellery Hale Past, Looking to the Future: Partnerships Nuclear 108 – Astronomy Education: Where Are We 205 – The Atacama Large 309 – Galaxies and AGN II Now and Where Are We Going? Millimeter/submillimeter Array: A New 310 – Young Stellar Objects, Star Formation 109 – Bridging Laboratory and Astrophysics: Window on the Universe and Star Clusters Molecules 208 – Galaxies and AGN I 311 – Curiosity on Mars: The Latest Results 110 – Interstellar Medium, Dust, Etc. 209 – Supernovae and Neutron -
KING-MPIA-DOC-DET-004 Short Title KING 70 Cm Rocon Issue 2.169 Date June 18, 2021
KING { 70cm Telescope { RoCon Software Manual Doc. No. KING-MPIA-DOC-DET-004 Short Title KING 70 cm Rocon Issue 2.169 Date June 18, 2021 Prepared . .Richard . .J. Mathar . .. .([email protected], . .382) . .June . 18, . .2021 . Name Date Signature Approved ...................................................................N. Surname Name Date Signature Released . .N. Surname . Name Date Signature ii KING-MPIA-DOC-DET-004 { KING 70 cm Rocon { Issue 2.169 Change Record Issue Date Sect. Reason/Initiation/Documents/Remarks 1.055 2020-02-24 all created 2.169 June 18, 2021 all SVN version 44M KING-MPIA-DOC-DET-004 { KING 70 cm Rocon { Issue 2.169 iii Contents 1 OVERVIEW 1 1.1 Acronyms..........................................1 1.2 References..........................................2 2 OBSERVER 2 2.1 Basics of Operation.....................................2 2.2 Info pages..........................................2 2.3 Prerequisites........................................ 19 2.3.1 ccdread....................................... 19 2.3.2 Temperature log.................................. 22 2.4 FITS output........................................ 22 2.5 Temperatures........................................ 23 2.6 PyRAF........................................... 24 2.7 Jupyter........................................... 24 2.8 Pointing Model....................................... 25 2.8.1 Refractive index.................................. 25 2.8.2 Model Fit...................................... 26 2.9 Dome Slit Model..................................... -
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. -
Target Selection for the SUNS and DEBRIS Surveys for Debris Discs in the Solar Neighbourhood
Mon. Not. R. Astron. Soc. 000, 1–?? (2009) Printed 18 November 2009 (MN LATEX style file v2.2) Target selection for the SUNS and DEBRIS surveys for debris discs in the solar neighbourhood N. M. Phillips1, J. S. Greaves2, W. R. F. Dent3, B. C. Matthews4 W. S. Holland3, M. C. Wyatt5, B. Sibthorpe3 1Institute for Astronomy (IfA), Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ 2School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, KY16 9SS 3UK Astronomy Technology Centre (UKATC), Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ 4Herzberg Institute of Astrophysics (HIA), National Research Council of Canada, Victoria, BC, Canada 5Institute of Astronomy (IoA), University of Cambridge, Madingley Road, Cambridge, CB3 0HA Accepted 2009 September 2. Received 2009 July 27; in original form 2009 March 31 ABSTRACT Debris discs – analogous to the Asteroid and Kuiper-Edgeworth belts in the Solar system – have so far mostly been identified and studied in thermal emission shortward of 100 µm. The Herschel space observatory and the SCUBA-2 camera on the James Clerk Maxwell Telescope will allow efficient photometric surveying at 70 to 850 µm, which allow for the detection of cooler discs not yet discovered, and the measurement of disc masses and temperatures when combined with shorter wavelength photometry. The SCUBA-2 Unbiased Nearby Stars (SUNS) survey and the DEBRIS Herschel Open Time Key Project are complimentary legacy surveys observing samples of ∼500 nearby stellar systems. To maximise the legacy value of these surveys, great care has gone into the target selection process. This paper describes the target selection process and presents the target lists of these two surveys. -
Ucam Installation Manual
UCam Installation Manual Version 0.3 Stewart McLay 5th March 2010 Acknowledgements Professor Vikram Dhillon who was P.I. for the UltraCam instrument the project from which UCam was born. The UCam development team has involved several members of UK ATC staff. Valuable contributions were made by: David Atkinson, Steven Beard, Derek Ives, Stewart McLay, Chris Tierney and Andy Vick. The Enhanced Machine Controller (EMC) project for their knowledge base wiki which has been a valuable source of information for installing RTAI on Debian Linux. 2 Table of Contents 1Introduction........................................................................................................................................5 1.1About UltraCam..........................................................................................................................5 1.2About ARC Controller................................................................................................................5 1.3About UK Astronomy Technology Centre.................................................................................6 1.4Acronyms And Abbreviations.....................................................................................................6 1.5Stylistic Conventions..................................................................................................................6 2How To Install Debian Linux.............................................................................................................8 2.1Debian Releases..........................................................................................................................8 -
Atmospheric Velocity Fields in Tepid Main Sequence Stars
A&A 503, 973–984 (2009) Astronomy DOI: 10.1051/0004-6361/200912083 & c ESO 2009 Astrophysics Atmospheric velocity fields in tepid main sequence stars, J. D. Landstreet1,2, F. Kupka3,6,H.A.Ford2,4,5,T.Officer2,T.A.A.Sigut2, J. Silaj2, S. Strasser2, and A. Townshend2 1 Armagh Observatory, College Hill, Armagh BT61 9DG, Northern Ireland 2 Department of Physics & Astronomy, University of Western Ontario, London, ON N6A 3K7, Canada e-mail: [email protected] 3 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany 4 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia 5 Australia Telescope National Facility, CSIRO, Epping, NSW 1710, Australia 6 Observatoire de Paris, LESIA, CNRS UMR 8109, 92195, Meudon, France Received 16 March 2009 / Accepted 11 June 2009 ABSTRACT −1 Context. The line profiles of the stars with ve sin i below a few km s can reveal direct signatures of local velocity fields such as convection in stellar atmospheres. This effect is well established in cool main sequence stars, and has been detected and studied in three A stars. Aims. This paper reports observations of main sequence B, A and F stars (1) to identify additional stars with sufficiently low values of ve sin i to search for spectral line profile signatures of local velocity fields and (2) to explore how the signatures of the local velocity fields in the atmosphere depend on stellar parameters such as effective temperature and peculiarity type. Methods. We have carried out a spectroscopic survey of B and A stars of low ve sin i at high resolution. -
Data Reduction Helpdesk First Responder Guidelines Kathleen Labrie
Data Reduction Helpdesk First Responder Guidelines Kathleen Labrie Science Users Support Department V2.0 – 14 November 2019 Revision History V1.0 – 16 January 2018 Kathleen Labrie V1.1 – 12 March 2018 Kathleen Labrie V2.0 – 14 November 2019 Kathleen Labrie Document ID: DPSG-USER-101_DRHDFirstResponderGuidelines Document Purpose This document aims to help the Tier 1 assignee respond to the data reduction tickets in a manner that will gather the necessary information for understanding and debugging the problem reported by the users in a timely manner. Intended Audience This document is intended primarily for Tier 1 Data Reduction Helpdesk assignee, who are often NGO members. Members of the Science Users Support Department new to handling data reduction tickets should also read this. Table of Contents 1. Introduction ............................................................................................................................. 2 2. Preparations – Assembling your First-aid Kit .......................................................................... 2 2.1 Choosing a platform ....................................................................................................... 2 2.2 AstroConda .................................................................... Error! Bookmark not defined. 2.3 IRAF and Gemini IRAF .................................................................................................. 3 2.3.1 IRAF .......................................................................................................................... -
AT 2016Dah and at 2017Fyp: the First Classical Novae Discovered Within A
MNRAS 000,1{22 (2020) Preprint 21 April 2020 Compiled using MNRAS LATEX style file v3.0 AT 2016dah and AT 2017fyp: the first classical novae discovered within a tidal stream M. J. Darnley,1? A. M. Newsam,1y K. Chinetti,1;2 I. D. W. Hawkins,1 A. L. Jannetta,1;3 M. M. Kasliwal,2 J. C. McGarry,1;4 M. M. Shara,5 M. Sitaram,1;6 S. C. Williams7;8;9 1Astrophysics Research Institute, Liverpool John Moores University, IC2 Liverpool Science Park, Liverpool, L3 5RF, UK 2Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 3INTO Newcastle University, The INTO Building, Newcastle University, NE1 7RU, UK 4Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK 5Department of Astrophysics, American Museum of Natural History, 79th Street and Central Park West, New York, NY 10024, USA 6Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA 7Finnish Centre for Astronomy with ESO (FINCA), Quantum, Vesilinnantie 5, University of Turku, 20014 Turku, Finland 8Department of Physics and Astronomy, University of Turku, 20014 Turku, Finland 9Physics Department, Lancaster University, Lancaster, LA1 4YB, UK Accepted 2020 April 20. Received 2020 April 20; in original form 2020 March 10 ABSTRACT AT 2016dah and AT 2017fyp are fairly typical Andromeda Galaxy (M 31) classical novae. AT 2016dah is an almost text book example of a `very fast' declining, yet uncommon, Fe ii`b' (broad-lined) nova, discovered during the rise to peak optical luminosity, and decaying with a smooth broken power-law light curve. -
The Significant Properties of Software: a Study
The Significant Properties of Software: A Study Brian Matthews, Brian McIlwrath, David Giaretta, Esther Conway STFC Rutherford Appleton Laboratory Chilton OX11 0QX UK December 2008 Significant Properties of Software Revision History: Version Date Authors Sections Affected / Comments 0.1 18/02/2008 BMM Outline 0.5 05/03/2008 BMM First Draft 0.6 09/03/2008 DG DG added section on OAIS/CASPAR 0.7 11/03/2008 BMM Added section on StarLink + revisions. 0.8 23/03/2008 BMcI, EC, BMM Expanded use cases 1.0 28/03/2008 BMM, BMcI First Complete release version 1.1 23/12/2008 BMM Final Revision 2 Significant Properties of Software Executive Summary ...................................................................................................... 5 Recommendations ..................................................................................................................... 6 1 Background to the Study ....................................................................................... 9 1.1 Introduction ................................................................................................................... 9 1.2 Significant Properties .................................................................................................. 10 2 Scope of Study .................................................................................................... 12 2.1 Definition of Software ................................................................................................ 12 2.2 Diversity of Software ................................................................................................. -
The Full Appendices with All References
Breakthrough Listen Exotica Catalog References 1 APPENDIX A. THE PROTOTYPE SAMPLE A.1. Minor bodies We classify Solar System minor bodies according to both orbital family and composition, with a small number of additional subtypes. Minor bodies of specific compositions might be selected by ETIs for mining (c.f., Papagiannis 1978). From a SETI perspective, orbital families might be targeted by ETI probes to provide a unique vantage point over bodies like the Earth, or because they are dynamically stable for long periods of time and could accumulate a large number of artifacts (e.g., Benford 2019). There is a large overlap in some cases between spectral and orbital groups (as in DeMeo & Carry 2014), as with the E-belt and E-type asteroids, for which we use the same Prototype. For asteroids, our spectral-type system is largely taken from Tholen(1984) (see also Tedesco et al. 1989). We selected those types considered the most significant by Tholen(1984), adding those unique to one or a few members. Some intermediate classes that blend into larger \complexes" in the more recent Bus & Binzel(2002) taxonomy were omitted. In choosing the Prototypes, we were guided by the classifications of Tholen(1984), Tedesco et al.(1989), and Bus & Binzel(2002). The comet orbital classifications were informed by Levison(1996). \Distant minor bodies", adapting the \distant objects" term used by the Minor Planet Center,1 refer to outer Solar System bodies beyond the Jupiter Trojans that are not comets. The spectral type system is that of Barucci et al. (2005) and Fulchignoni et al.(2008), with the latter guiding our Prototype selection. -
Pyraf FAQ Pyraf Pyraf FAQ
1/12/2018 PyRAF FAQ PyRAF PyRAF FAQ Last edited: 6 Jan 2017. 0. Support Status Due to reduced budgets for HST, we can only provide minimal pyraf support. If you have a problem that cannot be solved quickly by our first tier support, we may be unable to help. This is unfortunate, but it is the best we can do with the resources available. 1. Installation 1.1. How do I download and install PyRAF? 1.2. I am on a Mac. Can I use PyRAF with/without running X11? 1.3. Can I run PyRAF without IRAF? 1.4. What are the errors about Python.h / numpy.h ? 1.5. Can I run PyRAF with the 64-bit version of IRAF (v2.15.*)? 1.6. Does PyRAF run on OSX Mountain Lion (10.8)? 1.7. How do I run PyRAF on Windows? 1.8. Does PyRAF work under Python 3? 1.9. What is "X11/X.h: No such file or directory"? 1.10. Does PyRAF work within IPython Notebook? 1.11. Do you support other downloads of PyRAF? 2. Startup 2.1. How do I execute a Python script during startup? 2.2. How can I make my PyRAF session start up faster? 2.3. Why do I get messages about the "CL script cache" when I start up? 2.4. Why does PyRAF fail on startup with a message about togl.so? 2.5. How can I tell PyRAF that I want to run without graphics? 2.6. Why do I see "Could not import aqutil"? What's that? 2.7. -
Atmospheric Velocity Fields in Tepid Main Sequence Stars
Astronomy & Astrophysics manuscript no. 12083top c ESO 2018 June 8, 2018 Atmospheric velocity fields in tepid main sequence stars⋆,⋆⋆ J. D. Landstreet1,2, F. Kupka3,6, H. A. Ford2,4,5, T.Officer2, T. A. A. Sigut2, J. Silaj2, S. Strasser2, and A. Townshend2 1 Armagh Observatory, College Hill, Armagh BT61 9DG, Northern Ireland 2 Department of Physics & Astronomy, University of Western Ontario, London, ON N6A 3K7, Canada 3 Max-Planck-Institut f¨ur Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany 4 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia. 5 Australia Telescope National Facility, CSIRO, Epping, NSW 1710, Australia. 6 Observatoire de Paris, LESIA, CNRS UMR 8109, F-92195, Meudon, France Received September 1, 2009; accepted August 1, 2019 ABSTRACT −1 Context. The line profiles of the stars with ve sin i below a few km s can reveal direct signatures of local velocity fields such as convection in stellar atmospheres. This effect is well established in cool main sequence stars, and has been detected and studied in three A stars. Aims. This paper reports observations of main sequence B, A and F stars (1) to identify additional stars with sufficiently low values of ve sin i to search for spectral line profile signatures of local velocity fields, and (2) to explore how the signatures of the local velocity fields in the atmosphere depend on stellar parameters such as effective temperature and peculiarity type. Methods. We have carried out a spectroscopic survey of B and A stars of low ve sin i at high resolution.