DOCSLIB.ORG

Characterization of Candidate Exoplanet Companions from Hubble Space Telescope Astrometry, Ground-Based Radial Velocity, and Infrared Interferometry

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Characterization of Candidate Exoplanet Companions from Hubble Space Telescope Astrometry, Ground-Based Radial Velocity, and Infrared Interferometry INPE-00000-TDI/0000 CHARACTERIZATION OF CANDIDATE EXOPLANET COMPANIONS FROM HUBBLE SPACE TELESCOPE ASTROMETRY, GROUND-BASED RADIAL VELOCITY, AND INFRARED INTERFEROMETRY Eder Martioli Thesis submitted in partial fulfillment of the requirements for the degree of Ph.D. in Astrophysics, supervised by Drs. Francisco Jablonski, Barbara McArthur, and Fritz Benedict, approved in June 9, 2010. Original document registry: <http://urlib.net/xxx> INPE São José dos Campos 2010 PUBLISHED BY: Instituto Nacional de Pesquisas Espaciais - INPE Gabinete do Diretor (GB) Serviço de Informação e Documentação (SID) Caixa Postal 515 - CEP 12.245-970 São José dos Campos - SP - Brasil Tel.:(012) 3945-6911/6923 Fax: (012) 3945-6919 E-mail: [email protected] EDITORIAL COMMITTEE: Chairperson: Dr. Gerald Jean Francis Banon - Coordenação Observação da Terra (OBT) Members: Dr Maria do Carmo de Andrade Nono - Conselho de Pós-Graduação Dr. Haroldo Fraga de Campos Velho - Centro de Tecnologias Especiais (CTE) Dr Inez Staciarini Batista - Coordenação Ciências Espaciais e Atmosféricas (CEA) Marciana Leite Ribeiro - Serviço de Informação e Documentação (SID) Dr. Ralf Gielow - Centro de Previsão de Tempo e Estudos Climáticos (CPT) Dr. Wilson Yamaguti - Coordenação Engenharia e Tecnologia Espacial (ETE) DIGITAL LIBRARY: Dr. Gerald Jean Francis Banon - Coordenação Observação da Terra (OBT) Marciana Leite Ribeiro - Serviço de Informação e Documentação (SID) Jefferson Andrade Ancelmo - Serviço de Informação e Documentação (SID) Simone A. Del-Ducca Barbedo - Serviço de Informação e Documentação (SID) DOCUMENT REVIEW: Marciana Leite Ribeiro - Serviço de Informação e Documentação (SID) Marilcia Santos Melo Cid - Serviço de Informação e Documentação (SID) Yolanda Ribeiro da Silva Souza - Serviço de Informação e Documentação (SID) ELECTRONIC EDITING: Viveca SantAna Lemos - Serviço de Informação e Documentação (SID) INPE-00000-TDI/0000 CHARACTERIZATION OF CANDIDATE EXOPLANET COMPANIONS FROM HUBBLE SPACE TELESCOPE ASTROMETRY, GROUND-BASED RADIAL VELOCITY, AND INFRARED INTERFEROMETRY Eder Martioli Thesis submitted in partial fulfillment of the requirements for the degree of Ph.D. in Astrophysics, supervised by Drs. Francisco Jablonski, Barbara McArthur, and Fritz Benedict, approved in June 9, 2010. Original document registry: <http://urlib.net/xxx> INPE São José dos Campos 2010 Cataloging in Publication Data Martioli, Eder. Characterization of Candidate Exoplanet Companions From Cutter Hubble Space Telescope Astrometry, Ground-Based Radial Veloc- ity, and Infrared Interferometry / Eder Martioli. – São José dos Campos : INPE, 2010. ?? + 166 p. ; (INPE-00000-TDI/0000) Tese (Doutorado em Astrofísica) – Instituto Nacional de Pesquisas Espaciais, São José dos Campos, 2010. Orientadores : Francisco J. Jablonski; Barbara E. McArthur; G. Fritz Benedict. 1. Exoplanets. 2. Binary Stars. 3. Astrometry. 4. Radial Ve- locity. 5. Infrared Interferometry. CDU 000.000 Copyright c 2010 do MCT/INPE. Nenhuma parte desta publicação pode ser reproduzida, ar- mazenada em um sistema de recuperação, ou transmitida sob qualquer forma ou por qualquer meio, eletrônico, mecânico, fotográfico, reprográfico, de microfilmagem ou outros, sem a permissão escrita do INPE, com exceção de qualquer material fornecido especificamente com o propósito de ser entrado e executado num sistema computacional, para o uso exclusivo do leitor da obra. Copyright c 2010 by MCT/INPE. No part of this publication may be reproduced, stored in a retrieval system, or transmitted in any form or by any means, electronic, mechanical, photocopying, recording, microfilming, or otherwise, without written permission from INPE, with the exception of any material supplied specifically for the purpose of being entered and executed on a computer system, for exclusive use of the reader of the work. ii ATENÇÃO! A FOLHA DE APROVAÇÃO SERÁ INCLU- IDA POSTERIORMENTE. Doutorado em Astrofísica iii to my family. v ACKNOWLEDGEMENTS I would like to start by conveying my heartfelt gratitude to my parents, Aparecido and Iraci, my sister Lia and her family, my brother Cid and his family, and my dearest friend Carla, for their enormous support throughout my journey, and also for their caring and invaluable affection and friendship. I am also very appreciative to my advisor Francisco Jablonski who stood by me since the beginning of my graduate studies, and has made available his support in a number of ways. This thesis would not have been possible without the support of my co-advisors in Texas, Fritz Benedict and Barbara McArthur, those of whom provided me with the basic ideas and material for this thesis work. I am especially grateful for our fruitful discussions and for the continuous academic support they provided me at the time I was in Texas, and for their patience in keeping advising me through hundreds of emails, even after I came back to Brazil. I would also like to thank my colleagues Carla Gil and Ramarao Tata, who helped me in developing the pioneering work on the infrared interferometry experiment. They have also been decisive in the preparation of observing proposals, obtaining data, and in the data reduction and analysis. I am grateful for many of the personnel involved in my research work. Particularly, I would like to thank the competent work of clerical assistants at DAS-INPE, and at the University of Texas at Austin. Not to mention the always efficient work of clericals and technicians at the observatories. I would also like to thank the Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) agency for the financial support, and all the Brazilian and inter- national funds that I made use of for the development of my research. I am grateful for the support provided by NASA through grant GO-10704-10989, and 11210 from the Space Telescope Science Institute, for observations obtained from the Hobby- Ebberly Telescope at McDonald Observatory, and from the Very Large Telescope Array at European Southern Observatory. I would also like to thank the services provided by SIMBAD database, operated at CDS, Strasbourg, France, and NASA’s Astrophysics Data System Abstract Service. vii Finally, I should point up that I have not mentioned everyone who deserves being here. For this reason I would like to express my general but sincere gratitude to all of my friends, co-workers, and family members, who witnessed my quest and in some way supported me and made this thesis possible. These people surely know how important they were and still are to me. viii ABSTRACT This work presents the development of observational techniques and data analy- sis for the follow-up of RV-detected exoplanet candidates and low-mass compan- ions. We present high-cadence radial velocity data obtained with the HRS/HET combined with previously published data, and relative FGS/HST astrometry for HD 136118 and HD 33636. We perform a simultaneous analysis of these data in order to characterize the companion’s orbit thoroughly. This establishes the actual mass +22 of HD 136118 b, Mb = 63−13 MJ, in contrast to the minimum mass determined from the radial velocity data only, Mb sin i ∼ 12 MJ. Therefore, the low-mass companion to HD 136118 is now identified as a likely brown-dwarf residing in the “brown-dwarf desert”. We have performed a similar analysis for the object HD 33636. For this ob- ject we also present experimental AMBER/VLTI infrared interferometric data. The latter provides the measurement of visibility variations, which are consistent with an additional light that presents flux ratio of 30%, for a system with a G0 V primary star and an M-dwarf companion. ix CARACTERIZAÇÃO DE CANDIDATOS A EXOPLANETAS VIA ASTROMETRIA COM O TELESCÓPIO ESPACIAL, MEDIDAS EM TERRA DE VELOCIDADES RADIAIS E INTERFEROMETRIA NO INFRAVERMELHO RESUMO Neste trabalho desenvolvem-se técnicas observacionais e análise de dados para o estudo de candidatos a exoplanetas e companheiras de baixa massa detectados via velocidades radiais. Apresentamos medidas de alta-cadência de velocidades radiais obtidas com o Espectrógrafo de Alta Resolução no Telescópio Hobby-Eberly, com- binado com dados publicados anteriormente, e medidas astrométricas com o instru- mento FGS-1r no Telescópio Espacial Hubble dos sistemas HD 136118 e HD 33636. Realizamos a análise simultânea desses dados para caracterização completa da ór- bita das companheiras. O trabalho resultou na determinação da massa verdadeira de +22 HD 136118 b, Mb = 63−13 MJ, em contraste com a massa mínima determinada ante- riormente via velocidades radiais, Mb sin i ∼ 12 MJ. Portanto, HD 136118 b é identi- ficada como uma provável anã-marrom que reside no “deserto das anã-marrons”. Re- alizamos uma análise semelhante para os dados do também candidato a exoplaneta HD 33636. Para este objeto, apresentamos medidas interferométricas experimentais no infravermelho com o instrumento AMBER no VLTI. Esse experimento resultou na medida de variações na visibilidade consistentes com uma luz adicional que ap- resenta razão de fluxos de aproximadamente 30%, para um sistema binaário que constitui-se de uma estrela primária do tipo G0 V e uma companheira anã do tipo M. xi LIST OF FIGURES Page 3.1 Ellipse geometry................................ 15 3.2 Simple representation of the binary brightness distribution and the bi- nary parameters. ............................... 26 4.1 HRS optical layout. Source: http://www.as.utexas.edu/mcdonald. 33 4.2 HRS System Parameters. Source: http://www.as.utexas.edu/mcdonald. 33 4.3 HRS design parameters. Source: http://www.as.utexas.edu/mcdonald.
Load more

Recommended publications
  • Radio and IR Interferometry of Sio Maser Stars
    Cosmic Masers - from OH to H0 Proceedings IAU Symposium No. 287, 2012 c International Astronomical Union 2012 R.S. Booth, E.M.L. Humphreys & W.H.T. Vlemmings, eds. doi:10.1017/S1743921312006989 Radio and IR interferometry of SiO maser stars Markus Wittkowski1, David A. Boboltz2,MalcolmD.Gray3, Elizabeth M. L. Humphreys1 Iva Karovicova4, and Michael Scholz5,6 1 ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei M¨unchen, Germany 2 US Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392-5420, USA 3 Jodrell Bank Centre for Astrophysics, Alan Turing Building, University of Manchester, Manchester M13 9PL, UK 4 Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl 17, 69117 Heidelberg, Germany 5 Zentrum f¨ur Astronomie der Universit¨at Heidelberg (ZAH), Institut f¨ur Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany 6 Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney NSW 2006, Australia Abstract. Radio and infrared interferometry of SiO maser stars provide complementary infor- mation on the atmosphere and circumstellar environment at comparable spatial resolution. Here, we present the latest results on the atmospheric structure and the dust condensation region of AGB stars based on our recent infrared spectro-interferometric observations, which represent the environment of SiO masers. We discuss, as an example, new results from simultaneous VLTI and VLBA observations of the Mira variable AGB star R Cnc, including VLTI near- and mid- infrared interferometry, as well as VLBA observations of the SiO maser emission toward this source. We present preliminary results from a monitoring campaign of high-frequency SiO maser emission toward evolved stars obtained with the APEX telescope, which also serves as a pre- cursor of ALMA images of the SiO emitting region.
    [Show full text]
  • Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
    Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born.
    [Show full text]
  • Evidence for Very Extended Gaseous Layers Around O-Rich Mira Variables and M Giants B
    The Astrophysical Journal, 579:446–454, 2002 November 1 # 2002. The American Astronomical Society. All rights reserved. Printed in U.S.A. EVIDENCE FOR VERY EXTENDED GASEOUS LAYERS AROUND O-RICH MIRA VARIABLES AND M GIANTS B. Mennesson,1 G. Perrin,2 G. Chagnon,2 V. Coude du Foresto,2 S. Ridgway,3 A. Merand,2 P. Salome,2 P. Borde,2 W. Cotton,4 S. Morel,5 P. Kervella,5 W. Traub,6 and M. Lacasse6 Received 2002 March 15; accepted 2002 July 3 ABSTRACT Nine bright O-rich Mira stars and five semiregular variable cool M giants have been observed with the Infrared and Optical Telescope Array (IOTA) interferometer in both K0 (2.15 lm) and L0 (3.8 lm) broad- band filters, in most cases at very close variability phases. All of the sample Mira stars and four of the semire- gular M giants show strong increases, from ’20% to ’100%, in measured uniform-disk (UD) diameters between the K0 and L0 bands. (A selection of hotter M stars does not show such a large increase.) There is no evidence that K0 and L0 broadband visibility measurements should be dominated by strong molecular bands, and cool expanding dust shells already detected around some of these objects are also found to be poor candi- dates for producing these large apparent diameter increases. Therefore, we propose that this must be a con- tinuum or pseudocontinuum opacity effect. Such an apparent enlargement can be reproduced using a simple two-component model consisting of a warm (1500–2000 K), extended (up to ’3 stellar radii), optically thin ( ’ 0:5) layer located above the classical photosphere.
    [Show full text]
  • Catching up with Barnard's Star. Dave Eagle Within the Constellation Of
    Catching Up with Barnard’s Star. Dave Eagle Within the constellation of Ophiuchus lies Barnard’s Star. It is a fairly faint red dwarf star of magnitude 9.53, six light years from Earth, so is fairly close to us. Its luminosity is 1/2,500th that of the Sun and 16% its mass. The diameter is estimated at about 140,000 miles, so it’s quite a small, faint star and well below naked eye visibility. So why is this star so well known? In 1916 Edward Barnard looked at a photographic plate of the area. When he compared this to a similar plate made in 1894, he noticed that one of the stars had moved between the time of the two plates being taken. Although all the stars in the sky in reality are all moving quite fast, from our remote vantage point on Earth most stars appear to appear virtually static during our lifetime as their apparent motion is extremely small. Barnard’s star, being so close and moving so fast, is one of the stars that bucks this trend. So fast indeed that it will subtend the apparent diameter equivalent to the Moon or Sun in about 176 years. So compared to other stars it is really shifting. The star is travelling at 103 miles per second and is approaching us at about 87 miles per second. In about 8,000 years it will become the closest star to us, at just under 4 light years and will have brightened to magnitude 8.6. Peter van de Camp caused great excitement in the 1960’s when he claimed to have discovered a planet (or more) around the star, due to wobbles superimposed on its movement.
    [Show full text]
  • 100 Closest Stars Designation R.A
    100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79,
    [Show full text]
  • August 13 2016 7:00Pm at the Herrett Center for Arts & Science College of Southern Idaho
    Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Saturday, August 13th 2016 7:00pm at the Herrett Center for Arts & Science College of Southern Idaho. Public Star Party Follows at the Colleagues, Centennial Observatory Club Officers It's that time of year: The City of Rocks Star Party. Set for Friday, Aug. 5th, and Saturday, Aug. 6th, the event is the gem of the MVAS year. As we've done every Robert Mayer, President year, we will hold solar viewing at the Smoky Mountain Campground, followed by a [email protected] potluck there at the campground. Again, MVAS will provide the main course and 208-312-1203 beverages. Paul McClain, Vice President After the potluck, the party moves over to the corral by the bunkhouse over at [email protected] Castle Rocks, with deep sky viewing beginning sometime after 9 p.m. This is a chance to dig into some of the darkest skies in the west. Gary Leavitt, Secretary [email protected] Some members have already reserved campsites, but for those who are thinking of 208-731-7476 dropping by at the last minute, we have room for you at the bunkhouse, and would love to have to come by. Jim Tubbs, Treasurer / ALCOR [email protected] The following Saturday will be the regular MVAS meeting. Please check E-mail or 208-404-2999 Facebook for updates on our guest speaker that day. David Olsen, Newsletter Editor Until then, clear views, [email protected] Robert Mayer Rick Widmer, Webmaster [email protected] Magic Valley Astronomical Society is a member of the Astronomical League M-51 imaged by Rick Widmer & Ken Thomason Herrett Telescope Shotwell Camera https://herrett.csi.edu/astronomy/observatory/City_of_Rocks_Star_Party_2016.asp Calendars for August Sun Mon Tue Wed Thu Fri Sat 1 2 3 4 5 6 New Moon City Rocks City Rocks Lunation 1158 Castle Rocks Castle Rocks Star Party Star Party Almo, ID Almo, ID 7 8 9 10 11 12 13 MVAS General Mtg.
    [Show full text]
  • Occurrence and Core-Envelope Structure of 1–4× Earth-Size Planets Around Sun-Like Stars
    Occurrence and core-envelope structure of 1–4× SPECIAL FEATURE Earth-size planets around Sun-like stars Geoffrey W. Marcya,1, Lauren M. Weissa, Erik A. Petiguraa, Howard Isaacsona, Andrew W. Howardb, and Lars A. Buchhavec aDepartment of Astronomy, University of California, Berkeley, CA 94720; bInstitute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822; and cHarvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 02138 Edited by Adam S. Burrows, Princeton University, Princeton, NJ, and accepted by the Editorial Board April 16, 2014 (received for review January 24, 2014) Small planets, 1–4× the size of Earth, are extremely common planets. The Doppler reflex velocity of an Earth-size planet − around Sun-like stars, and surprisingly so, as they are missing in orbiting at 0.3 AU is only 0.2 m s 1, difficult to detect with an − our solar system. Recent detections have yielded enough informa- observational precision of 1 m s 1. However, such Earth-size tion about this class of exoplanets to begin characterizing their planets show up as a ∼10-sigma dimming of the host star after occurrence rates, orbits, masses, densities, and internal structures. coadding the brightness measurements from each transit. The Kepler mission finds the smallest planets to be most common, The occurrence rate of Earth-size planets is a major goal of as 26% of Sun-like stars have small, 1–2 R⊕ planets with orbital exoplanet science. With three years of Kepler photometry in periods under 100 d, and 11% have 1–2 R⊕ planets that receive 1–4× hand, two groups worked to account for the detection biases in the incident stellar flux that warms our Earth.
    [Show full text]
  • METEOR CSILLAGÁSZATI ÉVKÖNYV 2019 Meteor Csillagászati Évkönyv 2019
    METEOR CSILLAGÁSZATI ÉVKÖNYV 2019 meteor csillagászati évkönyv 2019 Szerkesztette: Benkő József Mizser Attila Magyar Csillagászati Egyesület www.mcse.hu Budapest, 2018 Az évkönyv kalendárium részének összeállításában közreműködött: Tartalom Bagó Balázs Görgei Zoltán Kaposvári Zoltán Kiss Áron Keve Kovács József Bevezető ....................................................................................................... 7 Molnár Péter Sánta Gábor Kalendárium .............................................................................................. 13 Sárneczky Krisztián Szabadi Péter Cikkek Szabó Sándor Szőllősi Attila Zsoldos Endre: 100 éves a Nemzetközi Csillagászati Unió ........................191 Zsoldos Endre Maria Lugaro – Kereszturi Ákos: Elemkeletkezés a csillagokban.............. 203 Szabó Róbert: Az OGLE égboltfelmérés 25 éve ........................................218 A kalendárium csillagtérképei az Ursa Minor szoftverrel készültek. www.ursaminor.hu Beszámolók Mizser Attila: A Magyar Csillagászati Egyesület Szakmailag ellenőrizte: 2017. évi tevékenysége .........................................................................242 Szabados László Kiss László – Szabó Róbert: Az MTA CSFK Csillagászati Intézetének 2017. évi tevékenysége .........................................................................248 Petrovay Kristóf: Az ELTE Csillagászati Tanszékének működése 2017-ben ............................................................................ 262 Szabó M. Gyula: Az ELTE Gothard Asztrofi zikai Obszervatórium
    [Show full text]
  • 10. Scientific Programme 10.1
    10. SCIENTIFIC PROGRAMME 10.1. OVERVIEW (a) Invited Discourses Plenary Hall B 18:00-19:30 ID1 “The Zoo of Galaxies” Karen Masters, University of Portsmouth, UK Monday, 20 August ID2 “Supernovae, the Accelerating Cosmos, and Dark Energy” Brian Schmidt, ANU, Australia Wednesday, 22 August ID3 “The Herschel View of Star Formation” Philippe André, CEA Saclay, France Wednesday, 29 August ID4 “Past, Present and Future of Chinese Astronomy” Cheng Fang, Nanjing University, China Nanjing Thursday, 30 August (b) Plenary Symposium Review Talks Plenary Hall B (B) 8:30-10:00 Or Rooms 309A+B (3) IAUS 288 Astrophysics from Antarctica John Storey (3) Mon. 20 IAUS 289 The Cosmic Distance Scale: Past, Present and Future Wendy Freedman (3) Mon. 27 IAUS 290 Probing General Relativity using Accreting Black Holes Andy Fabian (B) Wed. 22 IAUS 291 Pulsars are Cool – seriously Scott Ransom (3) Thu. 23 Magnetars: neutron stars with magnetic storms Nanda Rea (3) Thu. 23 Probing Gravitation with Pulsars Michael Kremer (3) Thu. 23 IAUS 292 From Gas to Stars over Cosmic Time Mordacai-Mark Mac Low (B) Tue. 21 IAUS 293 The Kepler Mission: NASA’s ExoEarth Census Natalie Batalha (3) Tue. 28 IAUS 294 The Origin and Evolution of Cosmic Magnetism Bryan Gaensler (B) Wed. 29 IAUS 295 Black Holes in Galaxies John Kormendy (B) Thu. 30 (c) Symposia - Week 1 IAUS 288 Astrophysics from Antartica IAUS 290 Accretion on all scales IAUS 291 Neutron Stars and Pulsars IAUS 292 Molecular gas, Dust, and Star Formation in Galaxies (d) Symposia –Week 2 IAUS 289 Advancing the Physics of Cosmic
    [Show full text]
  • Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
    Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis,
    [Show full text]
  • FY13 High-Level Deliverables
    National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2013 (1 October 2012 – 30 September 2013) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 13 December 2013 Revised 18 September 2014 Contents NOAO MISSION PROFILE .................................................................................................... 1 1 EXECUTIVE SUMMARY ................................................................................................ 2 2 NOAO ACCOMPLISHMENTS ....................................................................................... 4 2.1 Achievements ..................................................................................................... 4 2.2 Status of Vision and Goals ................................................................................. 5 2.2.1 Status of FY13 High-Level Deliverables ............................................ 5 2.2.2 FY13 Planned vs. Actual Spending and Revenues .............................. 8 2.3 Challenges and Their Impacts ............................................................................ 9 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 11 3.1 Cerro Tololo Inter-American Observatory ....................................................... 11 3.2 Kitt Peak National Observatory ....................................................................... 14 3.3 Gemini Observatory ........................................................................................
    [Show full text]
  • Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 Through 2009
    Vol. 6 No. 3 July 1, 2010 Journal of Double Star Observations Page 180 Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 through 2009 Rainer Anton Altenholz/Kiel, Germany e-mail: rainer.anton”at”ki.comcity.de Abstract: Using a 10” Newtonian and a fast CCD camera, recordings of double and multiple stars were made at high frame rates with a notebook computer. From superpositions of “lucky images”, measurements of 139 systems were obtained and compared with literature data. B/w and color images of some noteworthy systems are also presented. mented double stars, as will be described in the next Introduction section. Generally, I used a red filter to cope with By using the technique of “lucky imaging”, seeing chromatic aberration of the Barlow lens, as well as to effects can strongly be reduced, and not only the reso- reduce the atmospheric spectrum. For systems with lution of a given telescope can be pushed to its limits, pronounced color contrast, I also made recordings but also the accuracy of position measurements can be with near-IR, green and blue filters in order to pro- better than this by about one order of magnitude. This duce composite images. This setup was the same as I has already been demonstrated in earlier papers in used with telescopes under the southern sky, and as I this journal [1-3]. Standard deviations of separation have described previously [1-3]. Exposure times varied measurements of less than +/- 0.05 msec were rou- between 0.5 msec and 100 msec, depending on the tinely obtained with telescopes of 40 or 50 cm aper- star brightness, and on the seeing.
    [Show full text]