DOCSLIB.ORG

Adaptive Optics for Directly Imaging Planetary Systems

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Adaptive Optics for Directly Imaging Planetary Systems Adaptive Optics for Directly Imaging Planetary Systems Item Type text; Electronic Dissertation Authors Bailey, Vanessa Perry Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 11/10/2021 02:38:53 Link to Item http://hdl.handle.net/10150/577514 ADAPTIVE OPTICS FOR DIRECTLY IMAGING PLANETARY SYSTEMS by Vanessa Perry Bailey A Dissertation Submitted to the Faculty of the DEPARTMENT OF ASTRONOMY In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College THE UNIVERSITY OF ARIZONA 2015 2 THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE As members of the Dissertation Committee, we certify that we have read the disserta- tion prepared by Vanessa Perry Bailey entitled Adaptive Optics for Directly Imaging Planetary Systems and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of Philosophy. Date: 26 May 2015 Philip Hinz Date: 26 May 2015 Daniel Apai Date: 26 May 2015 Laird Close Date: 26 May 2015 George Rieke Date: 26 May 2015 Kate Su Final approval and acceptance of this dissertation is contingent upon the candidate’s submission of the final copies of the dissertation to the Graduate College. I hereby certify that I have read this dissertation prepared under my direction and recommend that it be accepted as fulfilling the dissertation requirement. Date: 26 May 2015 Dissertation Director: Philip Hinz 3 STATEMENT BY AUTHOR This dissertation has been submitted in partial fulfillment of requirements for an advanced degree at the University of Arizona and is deposited in the University Library to be made available to borrowers under rules of the Library. Brief quotations from this dissertation are allowable without special permission, pro- vided that an accurate acknowledgment of the source is made. Requests for per- mission for extended quotation from or reproduction of this manuscript in whole or in part may be granted by the head of the major department or the Dean of the Graduate College when in his or her judgment the proposed use of the material is in the interests of scholarship. In all other instances, however, permission must be obtained from the author. SIGNED: Vanessa Perry Bailey 4 ACKNOWLEDGEMENTS I was drawn to this department with the promise of hands-on experience on some of the world’s largest telescopes, and I’ve not been disappointed. First and fore- most, I want to thank my advisor, Phil Hinz for giving me the opportunity to be a contributing member of an instrument commissioning team and for giving me the freedom and guidance to try, to fail in useful ways, and to learn from the experience. I owe thanks to many people for helping me reach this point, most especially to the following: Tiffany Meshkat for being an indispensable co-investigator on the Hole-y Debris Disks project. Matt Kenworthy, Kate Su, Laird Close, George Rieke, and Daniel Apai, who have each been instrumental in shaping me into the researcher I am today. You prodded me to dig a little deeper and push a little harder, and you gave me the resources to facilitate that journey. My work is better for it. Vidhya Vaitheeswaran for patience and mentorship as I learned to code for a live instrument. Alfio Puglisi for his tutelage, troubleshooting, and patience as I learned the AO software ropes. Jared Males for being a constant resource and for getting me out of more than one sticky situation at the telescope. Katie Morzinski, whose mentorship gave me the capability and confidence (and the connections) to move on to the next stage. My office neighbors Kate Follette and Jordan Stone for countless hours brainstorming and sanity checking. My officemate Brandon Swift for moral support and an endless supply of fantastic uses for everyday items. And, of course, to Don McCarthy and Astronomy Camp for reminding me why I got into this business in the first place. Thanks to all of the instrument teams and telescope crews who have made my thesis possible. I gratefully acknowledge the hard work and dedication of past and present members of the LBTI team including: Phil Hinz, Paul Arbo, Hop Bailey, Teresa Bippert-Plymate, Denis Defrere, Elwood Downey, Oli Durney, Paul Grenz, William Hoffmann, Jarron Leisenring, Tom McMahon, Manny Montoya, Mitch Nash, T. J. Rodigas, Andy Skemer, Elliot Solheid, Eckhart Spalding, Vidhya Vaitheeswaran, and Amali Vaz. It’s been a pleasure working with you all. The LBTO staff and the Arcetri AO team built a lovely system and lent us their expertise on many occasions. Thanks in particular to John Hill, Doug Miller, Julian Christou, Juan Carlos Guerra, Guido Brusa, Simone Esposito, Enrico Pinna, and Marco Xom- pero. The MagAO team and Magellan Observatory staff carved out a niche in the AO world and let me jump in; thanks to Laird Close, Kate Follette, Jared Males, Katie Morzinski, Povilas Polunas and Dave Osip. Observations reported here were made at numerous observatories, including: MMT: a joint facility of the University of Arizona and the Smithsonian Institution; LBT Observatory: an international collaboration among institutions in the United 5 States, Italy and Germany. LBT Corporation partners are: The University of Ari- zona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University, and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota and University of Virginia; Magellan: located at Las Campanas Observatory, Chile; Gemini South: operated by the Association of Uni- versities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜ao (Brazil) and Ministerio de Ciencia, Tecnolog´ıa e Innovaci´on Productiva (Argentina); This work has made use of various archive services and surveys including: HST: data archive maintained by the Space Telescope Science Institute. STScI is oper- ated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. Spitzer Space Telescope: operated by the Jet Propulsion Lab- oratory, California Institute of Technology under a contract with NASA; Wide-field Infrared Survey Explorer: a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration; Two Micron All Sky Survey: a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation; NASA’s Astrophysics Data System; Simbad & Visier: database and catalogue access tools, administered by CDS, Strasbourg, France. The original description of the VizieR service was published in A&AS 143, 23. LBTI is funded by a NASA grant in support of the Exoplanet Exploration Pro- gram (NSF 0705296). My work was partially funded by: the University of Ari- zona’s College of Science Fellowship, the NSF Graduate Research Fellowship Pro- gram (DGE-1143953), and the aforementioned LBTI NASA grant. 6 DEDICATION To Peter: For being my partner in the true sense of the word. To Mom: For showing me that women have a place in science. To Dad: For tireless support. 7 TABLE OF CONTENTS LISTOFFIGURES ................................ 10 LISTOFTABLES ................................. 12 ABSTRACT .................................... 13 CHAPTER1 Introduction ............................ 15 1.1 ExoplanetsandTheirEnvironments. 17 1.1.1 Formation and Evolution of Giant Exoplanets . 17 1.1.2 Hole-y Debris Disks: A Potential Signpost for Giant Planets . 22 1.2 High-contrast Instrumentation & Techniques . .... 27 1.2.1 Science-Driven Performance Requirements for LBTIAO .... 27 1.2.2 Image Quality and Atmospheric Turbulence . 29 1.2.3 ComponentsofanAOSystem . 31 1.2.4 LBTIAO.............................. 34 CHAPTER 2 A Thermal Infrared Imaging Study of Very Low-Mass, Wide Sep- aration Brown Dwarf Companions to Upper Scorpius Stars: Constraining CircumstellarEnvironments . 39 2.1 Introduction................................ 40 2.2 Sample,ObservationsandDataReduction . 43 2.2.1 Sample............................... 43 2.2.2 Observations ........................... 46 2.2.3 ImageProcessing . 49 2.3 ResultsandAnalysis ........................... 51 2.3.1 GSC06214 ............................ 51 2.3.2 1RXS1609 ............................ 59 2.3.3 HIP78530............................. 62 2.4 Discussion................................. 66 2.4.1 GSC06214BDiskProperties . 66 2.4.2 HIP 78530B Spectral Type and Membership . 67 2.5 DisksasConstraintsonScatteringEvents . ... 68 2.6 SummaryandFutureWork . 70 8 TABLE OF CONTENTS – Continued CHAPTER 3 HD 106906 b: A Planetary-mass Companion outside a Massive DebrisDisk ................................... 74 3.1 Introduction................................ 75 3.2 ObservationsandDataReduction
Load more

Recommended publications
  • 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]
  • Curriculum Vitae - 24 March 2020
    Dr. Eric E. Mamajek Curriculum Vitae - 24 March 2020 Jet Propulsion Laboratory Phone: (818) 354-2153 4800 Oak Grove Drive FAX: (818) 393-4950 MS 321-162 [email protected] Pasadena, CA 91109-8099 https://science.jpl.nasa.gov/people/Mamajek/ Positions 2020- Discipline Program Manager - Exoplanets, Astro. & Physics Directorate, JPL/Caltech 2016- Deputy Program Chief Scientist, NASA Exoplanet Exploration Program, JPL/Caltech 2017- Professor of Physics & Astronomy (Research), University of Rochester 2016-2017 Visiting Professor, Physics & Astronomy, University of Rochester 2016 Professor, Physics & Astronomy, University of Rochester 2013-2016 Associate Professor, Physics & Astronomy, University of Rochester 2011-2012 Associate Astronomer, NOAO, Cerro Tololo Inter-American Observatory 2008-2013 Assistant Professor, Physics & Astronomy, University of Rochester (on leave 2011-2012) 2004-2008 Clay Postdoctoral Fellow, Harvard-Smithsonian Center for Astrophysics 2000-2004 Graduate Research Assistant, University of Arizona, Astronomy 1999-2000 Graduate Teaching Assistant, University of Arizona, Astronomy 1998-1999 J. William Fulbright Fellow, Australia, ADFA/UNSW School of Physics Languages English (native), Spanish (advanced) Education 2004 Ph.D. The University of Arizona, Astronomy 2001 M.S. The University of Arizona, Astronomy 2000 M.Sc. The University of New South Wales, ADFA, Physics 1998 B.S. The Pennsylvania State University, Astronomy & Astrophysics, Physics 1993 H.S. Bethel Park High School Research Interests Formation and Evolution
    [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]
  • Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
    Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i,
    [Show full text]
  • Marta L. Bryan
    Marta L. Bryan 501 Campbell Hall #3411 Email: [email protected] University of California at Berkeley Homepage: w.astro.berkeley.edu/∼martalbryan Berkeley, CA 94720-3411 Appointments NASA Hubble Fellowship Program Sagan Fellow, UC Berkeley Astronomy Fall 2021 - present Department 51 Pegasi b Postdoctoral Fellow, UC Berkeley Astronomy Department 2018 - Fall 2021 Education PhD in Astrophysics, California Institute of Technology May 2018 Advisor: Prof. Heather Knutson Thesis: Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation MS in Astrophysics, California Institute of Technology June 2014 BA cum laude with High Honors in Astrophysics, Harvard University June 2012 Undergraduate Thesis Advisor: Prof. David Latham Thesis: Characterizing Qatar-2b: A Hot Jupiter Orbiting a K Dwarf Research Interests Exploring the formation, evolution, and architectures of planetary systems Characterizing exoplanet rotation rates and atmospheres using high-resolution spectroscopy High-contrast AO imaging of exoplanets and brown dwarfs Constraining the frequencies of gas giants in systems hosting different populations of terrestrial and ice giant planets Bridging the gap between radial velocity and direct imaging survey sensitivities to planets using radial velocity trends Awards and Honors NASA Hubble Fellowship Program Sagan Fellowship 2021 51 Pegasi b Postdoctoral Fellowship 2018 NASA Hubble Fellowship Program Sagan Fellowship (declined) 2018 David and Barbara Groce Grant to attend the Exoplanets I meeting in Davos 2016 Switzerland, California Institute of Technology AAS 2015 International Travel Grant 2015 National Science Foundation Graduate Research Fellowship Honorable Mention 2014, 2013 Chambliss Astronomy Achievement Student Award Honorable Mention, AAS 2014 Moffet Fellowship, California Institute of Technology 2012-2013 Origins of Life Research Grant, Harvard University 2011-2012 Leo Goldberg Prize for outstanding undergraduate thesis work, Harvard University 2011 U.S.
    [Show full text]
  • The VAST Survey – IV. a Wide Brown Dwarf Companion to the A3V Star Ζ Delphini
    MNRAS 445, 3694–3705 (2014) doi:10.1093/mnras/stu2018 The VAST Survey – IV. A wide brown dwarf companion to the A3V star ζ Delphini R. J. De Rosa,1,2† J. Patience,1 K. Ward-Duong,1 A. Vigan,3 C. Marois,4 I. Song,5 B. Macintosh,6,7 J. R. Graham,8 R. Doyon,9 M. S. Bessell,10 O. Lai,11,12 D. W. McCarthy13 and C. Kulesa13 1School of Earth and Space Exploration, Arizona State University, PO Box 871404, Tempe, AZ 85287, USA 2School of Physics, College of Engineering, Mathematics and Physical Sciences, University of Exeter, Stocker Road, Exeter EX4 4QL, UK 3Aix Marseille Universite,´ CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, F-13388 Marseille, France 4NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 5Physics and Astronomy, University of Georgia, 240 Physics, Athens, GA 30602, USA Downloaded from 6Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 7Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, 7000 East Ave, Livermore, CA 94550, USA 8Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720, USA 9Dept´ de Physique, Universite´ de Montreal,´ C.P. 6128, Succ. Centre-Ville, Montreal,´ QC H3C 3J7, Canada 10Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, ACT 2611, Australia 11Gemini Observatory, 670 N. A’ohoku Place, Hilo, HI 96720, USA http://mnras.oxfordjournals.org/ 12National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720, USA 13Steward Observatory, University of Arizona, 933 N.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
    exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55
    [Show full text]
  • Exoplanet Meteorology: Characterizing the Atmospheres Of
    Exoplanet Meteorology: Characterizing the Atmospheres of Directly Imaged Sub-Stellar Objects by Abhijith Rajan A Dissertation Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy Approved April 2017 by the Graduate Supervisory Committee: Jennifer Patience, Co-Chair Patrick Young, Co-Chair Paul Scowen Nathaniel Butler Evgenya Shkolnik ARIZONA STATE UNIVERSITY May 2017 ©2017 Abhijith Rajan All Rights Reserved ABSTRACT The field of exoplanet science has matured over the past two decades with over 3500 confirmed exoplanets. However, many fundamental questions regarding the composition, and formation mechanism remain unanswered. Atmospheres are a window into the properties of a planet, and spectroscopic studies can help resolve many of these questions. For the first part of my dissertation, I participated in two studies of the atmospheres of brown dwarfs to search for weather variations. To understand the evolution of weather on brown dwarfs we conducted a multi- epoch study monitoring four cool brown dwarfs to search for photometric variability. These cool brown dwarfs are predicted to have salt and sulfide clouds condensing in their upper atmosphere and we detected one high amplitude variable. Combining observations for all T5 and later brown dwarfs we note a possible correlation between variability and cloud opacity. For the second half of my thesis, I focused on characterizing the atmospheres of directly imaged exoplanets. In the first study Hubble Space Telescope data on HR8799, in wavelengths unobservable from the ground, provide constraints on the presence of clouds in the outer planets. Next, I present research done in collaboration with the Gemini Planet Imager Exoplanet Survey (GPIES) team including an exploration of the instrument contrast against environmental parameters, and an examination of the environment of the planet in the HD 106906 system.
    [Show full text]
  • Direct Imaging of Exoplanets in the Habitable Zone with Adaptive Optics
    Direct imaging of exoplanets in the habitable zone with adaptive optics Jared R. Malesa,*, Laird M. Closea, Olivier Guyona, Katie Morzinskia,*, Alfio Puglisib, Philip Hinza, Katherine B. Follettea, John D. Monnierc, Volker Tollsd, Timothy J. Rodigase, Alycia Weinbergere, Alan Bosse, Derek Koponf, Ya-lin Wua, Simone Espositob, Armando Riccardib, Marco Xomperob, Runa Brigugliob, Enrico Pinnab aSteward Observatory, University of Arizona, Tucson, AZ, USA; bInstituto Nazionale di Astrofisica, Osservatorio Astrofisico di Arcetri, Firenze, Italy; cAstronomy Department, University of Michigan; dHarvard-Smithsonian, CfA, Boston, MA, USA; eCarnegie Institution DTM, Washington, DC, USA; fMPiA Heidelberg, Germany; *NASA Sagan Fellow ABSTRACT One of the primary goals of exoplanet science is to find and characterize habitable planets, and direct imaging will play a key role in this effort. Though imaging a true Earth analog is likely out of reach from the ground, the coming generation of giant telescopes will find and characterize many planets in and near the habitable zones (HZs) of nearby stars. Radial velocity and transit searches indicate that such planets are common, but imaging them will require achieving extreme contrasts at very small angular separations, posing many challenges for adaptive optics (AO) system design. Giant planets in the HZ may even be within reach with the latest generation of high-contrast imagers for a handful of very nearby stars. Here we will review the definition of the HZ, and the characteristics of detectable planets there. We then review some of the ways that direct imaging in the HZ will be different from the typical exoplanet imaging survey today. Finally, we present preliminary results from our observations of the HZ of α Centauri A with the Magellan AO system’s VisAO and Clio2 cameras.
    [Show full text]
  • DIRECT IMAGING DISCOVERY of a “SUPER-JUPITER” AROUND the LATE B-TYPE STAR Κ And∗
    The Astrophysical Journal Letters, 763:L32 (6pp), 2013 February 1 doi:10.1088/2041-8205/763/2/L32 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DIRECT IMAGING DISCOVERY OF A “SUPER-JUPITER” AROUND THE LATE B-TYPE STAR κ And∗ J. Carson1,2, C. Thalmann2,3,M.Janson4, T. Kozakis1, M. Bonnefoy2, B. Biller2, J. Schlieder2,T.Currie5, M. McElwain5, M. Goto6, T. Henning2, W. Brandner2, M. Feldt2, R. Kandori7, M. Kuzuhara7,8, L. Stevens1,P.Wong1, K. Gainey1, M. Fukagawa9, Y. Kuwada9, T. Brandt4, J. Kwon7,L.Abe10,S.Egner11, C. Grady5,O.Guyon11, J. Hashimoto7, Y. Hayano11, M. Hayashi7, S. Hayashi11, K. Hodapp12,M.Ishii11,M.Iye7, G. Knapp4,T.Kudo11, N. Kusakabe7,T.Matsuo13,S.Miyama14,J.Morino7, A. Moro-Martin15, T. Nishimura11,T.Pyo11, E. Serabyn16, H. Suto7, R. Suzuki7, M. Takami17, N. Takato11, H. Terada11, D. Tomono11, E. Turner4,18, M. Watanabe19, J. Wisniewski20, T. Yamada21, H. Takami7,T.Usuda11, and M. Tamura7 1 Department of Physics & Astronomy, College of Charleston, 58 Coming Street, Charleston, SC 29424, USA 2 Max-Planck-Institut fur¨ Astronomie, Konigstuhl¨ 17, D-69117 Heidelberg, Germany 3 Astronomical Institute “Anton Pannekoek,” University of Amsterdam, Science Park 904, 1098-XH Amsterdam, The Netherlands 4 Department of Astrophysical Sciences, Princeton University, NJ 08544, USA 5 ExoPlanets and Stellar Astrophysics Laboratory, Code 667, Goddard Space Flight Center, Greenbelt, MD 20771, USA 6 Young Stars and Star Formation Universitats-Sternwarte¨ Munchen,¨ Ludwig-Maximilians-Universitat,¨ D-81679
    [Show full text]
  • Why Do Hydrogen and Helium Migrate from Some Planets and Smaller
    Why do Hydrogen and Helium Migrate from Some Planets and Smaller Objects? Author Weitter Duckss Independent Researcher, Zadar, Croatia mail: [email protected] Project: https://www.svemir-ipaksevrti.com/ Abstract This article analyzes the processes through measuring the material incoming from the outer space onto Earth, through migrating of hydrogen and helium from our atmosphere and from other objects and through inability to detect the radioactive effects on stars and objects with melted interiorities. Habitable periods on such objects are determined through the processes. 1. Introduction The goal of the article is to give arguments, based on the existing data bases, that a constant growth of space objects, as well as their rotation and tidal forces, cause their warming up and radiation emissions, therefore making radioactive processes of fission and fusion – which are not detected on stars and other objects anyway – unnecessary. The article gives evidence of hydrogen and helium migrating towards the objects that have more mass and of temperature levels of stars being directly related to their chemical compositions and the objects in their orbits. The argumentation to support a habitable period will be derived from the natural processes of constant growth and matter gathering. 2. Why there is no radioactive emission, derived from the processes of fission and fusion, inside stars? All data bases indicate that astronomic research (or, evidence) support the existence of a constant (monotonous), omnipresent, slow gathering of matter. The processes are "more accelerated" in such part of the Universe where there is more matter gathered (in the form of nebulae, molecular clouds, etc.) during a long period of time, but gathering takes place constantly in the whole volume of the Universe as well.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 Star Distance Star Name Star Mass
    exoplanet.eu_catalog star_distance star_name star_mass Planet name mass 1.3 Proxima Centauri 0.120 Proxima Cen b 0.004 1.3 alpha Cen B 0.934 alf Cen B b 0.004 2.3 WISE 0855-0714 WISE 0855-0714 6.000 2.6 Lalande 21185 0.460 Lalande 21185 b 0.012 3.2 eps Eridani 0.830 eps Eridani b 3.090 3.4 Ross 128 0.168 Ross 128 b 0.004 3.6 GJ 15 A 0.375 GJ 15 A b 0.017 3.6 YZ Cet 0.130 YZ Cet d 0.004 3.6 YZ Cet 0.130 YZ Cet c 0.003 3.6 YZ Cet 0.130 YZ Cet b 0.002 3.6 eps Ind A 0.762 eps Ind A b 2.710 3.7 tau Cet 0.783 tau Cet e 0.012 3.7 tau Cet 0.783 tau Cet f 0.012 3.7 tau Cet 0.783 tau Cet h 0.006 3.7 tau Cet 0.783 tau Cet g 0.006 3.8 GJ 273 0.290 GJ 273 b 0.009 3.8 GJ 273 0.290 GJ 273 c 0.004 3.9 Kapteyn's 0.281 Kapteyn's c 0.022 3.9 Kapteyn's 0.281 Kapteyn's b 0.015 4.3 Wolf 1061 0.250 Wolf 1061 d 0.024 4.3 Wolf 1061 0.250 Wolf 1061 c 0.011 4.3 Wolf 1061 0.250 Wolf 1061 b 0.006 4.5 GJ 687 0.413 GJ 687 b 0.058 4.5 GJ 674 0.350 GJ 674 b 0.040 4.7 GJ 876 0.334 GJ 876 b 1.938 4.7 GJ 876 0.334 GJ 876 c 0.856 4.7 GJ 876 0.334 GJ 876 e 0.045 4.7 GJ 876 0.334 GJ 876 d 0.022 4.9 GJ 832 0.450 GJ 832 b 0.689 4.9 GJ 832 0.450 GJ 832 c 0.016 5.9 GJ 570 ABC 0.802 GJ 570 D 42.500 6.0 SIMP0136+0933 SIMP0136+0933 12.700 6.1 HD 20794 0.813 HD 20794 e 0.015 6.1 HD 20794 0.813 HD 20794 d 0.011 6.1 HD 20794 0.813 HD 20794 b 0.009 6.2 GJ 581 0.310 GJ 581 b 0.050 6.2 GJ 581 0.310 GJ 581 c 0.017 6.2 GJ 581 0.310 GJ 581 e 0.006 6.5 GJ 625 0.300 GJ 625 b 0.010 6.6 HD 219134 HD 219134 h 0.280 6.6 HD 219134 HD 219134 e 0.200 6.6 HD 219134 HD 219134 d 0.067 6.6 HD 219134 HD
    [Show full text]