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Sodium and Potassium Signatures Of
Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets Apurva Oza, Robert Johnson, Emmanuel Lellouch, Carl Schmidt, Nick Schneider, Chenliang Huang, Diana Gamborino, Andrea Gebek, Aurelien Wyttenbach, Brice-Olivier Demory, et al. To cite this version: Apurva Oza, Robert Johnson, Emmanuel Lellouch, Carl Schmidt, Nick Schneider, et al.. Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets. The Astro- physical Journal, American Astronomical Society, 2019, 885 (2), pp.168. 10.3847/1538-4357/ab40cc. hal-02417964 HAL Id: hal-02417964 https://hal.sorbonne-universite.fr/hal-02417964 Submitted on 18 Dec 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. The Astrophysical Journal, 885:168 (19pp), 2019 November 10 https://doi.org/10.3847/1538-4357/ab40cc © 2019. The American Astronomical Society. Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets Apurva V. Oza1 , Robert E. Johnson2,3 , Emmanuel Lellouch4 , Carl Schmidt5 , Nick Schneider6 , Chenliang Huang7 , Diana Gamborino1 , Andrea Gebek1,8 , Aurelien Wyttenbach9 , Brice-Olivier Demory10 , Christoph Mordasini1 , Prabal Saxena11, David Dubois12 , Arielle Moullet12, and Nicolas Thomas1 1 Physikalisches Institut, Universität Bern, Bern, Switzerland; [email protected] 2 Engineering Physics, University of Virginia, Charlottesville, VA 22903, USA 3 Physics, New York University, 4 Washington Place, New York, NY 10003, USA 4 LESIA–Observatoire de Paris, CNRS, UPMC Univ. -
Downloads/ Astero2007.Pdf) and by Aerts Et Al (2010)
This work is protected by copyright and other intellectual property rights and duplication or sale of all or part is not permitted, except that material may be duplicated by you for research, private study, criticism/review or educational purposes. Electronic or print copies are for your own personal, non- commercial use and shall not be passed to any other individual. No quotation may be published without proper acknowledgement. For any other use, or to quote extensively from the work, permission must be obtained from the copyright holder/s. i Fundamental Properties of Solar-Type Eclipsing Binary Stars, and Kinematic Biases of Exoplanet Host Stars Richard J. Hutcheon Submitted in accordance with the requirements for the degree of Doctor of Philosophy. Research Institute: School of Environmental and Physical Sciences and Applied Mathematics. University of Keele June 2015 ii iii Abstract This thesis is in three parts: 1) a kinematical study of exoplanet host stars, 2) a study of the detached eclipsing binary V1094 Tau and 3) and observations of other eclipsing binaries. Part I investigates kinematical biases between two methods of detecting exoplanets; the ground based transit and radial velocity methods. Distances of the host stars from each method lie in almost non-overlapping groups. Samples of host stars from each group are selected. They are compared by means of matching comparison samples of stars not known to have exoplanets. The detection methods are found to introduce a negligible bias into the metallicities of the host stars but the ground based transit method introduces a median age bias of about -2 Gyr. -
Arxiv:0908.2624V1 [Astro-Ph.SR] 18 Aug 2009
Astronomy & Astrophysics Review manuscript No. (will be inserted by the editor) Accurate masses and radii of normal stars: Modern results and applications G. Torres · J. Andersen · A. Gim´enez Received: date / Accepted: date Abstract This paper presents and discusses a critical compilation of accurate, fun- damental determinations of stellar masses and radii. We have identified 95 detached binary systems containing 190 stars (94 eclipsing systems, and α Centauri) that satisfy our criterion that the mass and radius of both stars be known to ±3% or better. All are non-interacting systems, so the stars should have evolved as if they were single. This sample more than doubles that of the earlier similar review by Andersen (1991), extends the mass range at both ends and, for the first time, includes an extragalactic binary. In every case, we have examined the original data and recomputed the stellar parameters with a consistent set of assumptions and physical constants. To these we add interstellar reddening, effective temperature, metal abundance, rotational velocity and apsidal motion determinations when available, and we compute a number of other physical parameters, notably luminosity and distance. These accurate physical parameters reveal the effects of stellar evolution with un- precedented clarity, and we discuss the use of the data in observational tests of stellar evolution models in some detail. Earlier findings of significant structural differences between moderately fast-rotating, mildly active stars and single stars, ascribed to the presence of strong magnetic and spot activity, are confirmed beyond doubt. We also show how the best data can be used to test prescriptions for the subtle interplay be- tween convection, diffusion, and other non-classical effects in stellar models. -
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 ........................................................................................ -
Optical Interferometry in Astronomy
Home Search Collections Journals About Contact us My IOPscience Optical interferometry in astronomy This article has been downloaded from IOPscience. Please scroll down to see the full text article. 2003 Rep. Prog. Phys. 66 789 (http://iopscience.iop.org/0034-4885/66/5/203) View the table of contents for this issue, or go to the journal homepage for more Download details: IP Address: 128.196.208.1 The article was downloaded on 18/08/2010 at 17:12 Please note that terms and conditions apply. INSTITUTE OF PHYSICS PUBLISHING REPORTS ON PROGRESS IN PHYSICS Rep. Prog. Phys. 66 (2003) 789–857 PII: S0034-4885(03)90003-0 Optical interferometry in astronomy John D Monnier University of Michigan Astronomy Department, 941 Dennison Building, 500 Church Street, Ann Arbor, MI 48109, USA E-mail: [email protected] Received 22 January 2003, in final form 24 March 2003 Published 25 April 2003 Online at stacks.iop.org/RoPP/66/789 Abstract Here I review the current state of the field of optical stellar interferometry, concentrating on ground-based work although a brief report of space interferometry missions is included. We pause both to reflect on decades of immense progress in the field as well as to prepare for a new generation of large interferometers just now being commissioned (most notably, the CHARA, Keck and VLT Interferometers). First, this review summarizes the basic principles behind stellar interferometry needed by the lay-physicist and general astronomer to understand the scientific potential as well as technical challenges of interferometry. Next, the basic design principles of practical interferometers are discussed, using the experience of past and existing facilities to illustrate important points. -
Dr. Gerard T. Van Belle Curriculum Vitae
Lowell Observatory Dr. Gerard T. van Belle 1400 W Mars Hill Rd Flagstaff, AZ 86001 Curriculum Vitae +1 928 233 3207 [email protected] http://www.lowell.edu/~gerard Experience: Lowell Observatory, Flagstaff, Arizona. Astronomer, 2011-present. On staff with the observatory with a principal interest in astronomical interferometry with the Navy Prototype Optical Interferometer (NPOI), and high-resolution imaging with the Discovery Channel Telescope (DCT). European Southern Observatory, Garching bei München, Germany. PRIMA Instrument Scientist, 2007-2011. Responsible for the scientific development and use of the PRIMA (Phase-Referenced Imaging and Microarcsecond Astrometry) facility of ESO’s Very Large Telescope Interferometer, including instrument implementation and commissioning. MATISSE Instrument Scientist, 2011. Responsible for the instrument development progress, including development of institutional agreements for budgets and deliverables. Member of the Astronomy faculty at the Associate Astronomer level. Michelson Science Center, California Institute of Technology, Pasadena, California. Science Community Development Lead, 2002-2007. Responsible for administration of the Michelson Program at the MSC and coordination of scientific use of NASA time of the Keck telescopes. Additional activities include oversight of the Michelson Summer Workshop, MSC web page management, and independent scientific research. The Jet Propulsion Laboratory, Pasadena, California. Senior Optical Engineer, Interferometry Technology Group, 1996-2002. Beginning with designing the basic optical layout of the Keck Interferometer, duties with KI included delay line and transport optic design, heavy construction of the interferometer facility, ensuing instrument installation, and scientific utilization of the interferometer. Additionally, scientific observations with the Palomar Testbed Interferometer included size and shape characterizations of nearby stars. Saint Mary's College of Maryland, Saint Mary's City, Maryland. -
Arxiv:0709.4613V2 [Astro-Ph] 16 Apr 2008 .Quirrenbach A
Astronomy and Astrophysics Review manuscript No. (will be inserted by the editor) M. S. Cunha · C. Aerts · J. Christensen-Dalsgaard · A. Baglin · L. Bigot · T. M. Brown · C. Catala · O. L. Creevey · A. Domiciano de Souza · P. Eggenberger · P. J. V. Garcia · F. Grundahl · P. Kervella · D. W. Kurtz · P. Mathias · A. Miglio · M. J. P. F. G. Monteiro · G. Perrin · F. P. Pijpers · D. Pourbaix · A. Quirrenbach · K. Rousselet-Perraut · T. C. Teixeira · F. Th´evenin · M. J. Thompson Asteroseismology and interferometry Received: date M. S. Cunha and T. C. Teixeira Centro de Astrof´ısica da Universidade do Porto, Rua das Estrelas, 4150-762, Porto, Portugal. E-mail: [email protected] C. Aerts Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium; Afdeling Sterrenkunde, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands. J. Christensen-Dalsgaard and F. Grundahl Institut for Fysik og Astronomi, Aarhus Universitet, Aarhus, Denmark. A. Baglin and C. Catala and P. Kervella and G. Perrin LESIA, UMR CNRS 8109, Observatoire de Paris, France. L. Bigot and F. Th´evenin Observatoire de la Cˆote d’Azur, UMR 6202, BP 4229, F-06304, Nice Cedex 4, France. T. M. Brown Las Cumbres Observatory Inc., Goleta, CA 93117, USA. arXiv:0709.4613v2 [astro-ph] 16 Apr 2008 O. L. Creevey High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO 80301, USA; Instituto de Astrofsica de Canarias, Tenerife, E-38200, Spain. A. Domiciano de Souza Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, 53121 Bonn, Ger- many. P. Eggenberger Observatoire de Gen`eve, 51 chemin des Maillettes, 1290 Sauverny, Switzerland; In- stitut d’Astrophysique et de G´eophysique de l’Universit´e de Li`ege All´ee du 6 Aoˆut, 17 B-4000 Li`ege, Belgium. -
The Transiting Dust Clumps in the Evolved Disk of the Sun-Like Uxor
The transiting dust clumps in the evolved disk of the Sun-like UXor RZ Psc rsos.royalsocietypublishing.org 1 Grant M. Kennedy , Matthew A. 2 3 Kenworthy , Joshua Pepper , Joseph E. Research 4 5 6 Rodriguez , , Robert J. Siverd , Keivan G. 5 7 1 Stassun , , & Mark C. Wyatt Article submitted to journal 1 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 2 Subject Areas: Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Netherlands astrophysics, extrasolar planets, stars 3 Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA Keywords: 4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, variable stars, protoplanetary disks, MS-78, Cambridge, MA 02138, USA 5 debris disks, circumstellar matter Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN 37235, USA 6 Las Cumbres Observatory Global Telescope Network, 6740 Author for correspondence: Cortona Dr., Suite 102, Santa Barbara, CA 93117, USA 7 Grant M. Kennedy Department of Physics, Fisk University, 1000 17th Avenue North, Nashville, TN 37208, USA e-mail: [email protected] RZ Psc is a young Sun-like star, long associated with the UXor class of variable stars, which is partially or wholly dimmed by dust clumps several times each year. The system has a bright and variable infrared excess, which has been interpreted as evidence that the dimming events are the passage of asteroidal fragments in front of the host star. Here, we present a decade of optical photometry of RZ Psc and take a critical look at the asteroid belt interpretation. -
Détection Et Caractérisation De Planètes Extrasolaires Par Photométrie Visible Et Interférométrie Infrarouge À Très Haute Précision Pascal Bordé
Détection et caractérisation de planètes extrasolaires par photométrie visible et interférométrie infrarouge à très haute précision Pascal Bordé To cite this version: Pascal Bordé. Détection et caractérisation de planètes extrasolaires par photométrie visible et in- terférométrie infrarouge à très haute précision. Astrophysique [astro-ph]. Université Pierre et Marie Curie - Paris VI, 2003. Français. tel-00004349 HAL Id: tel-00004349 https://tel.archives-ouvertes.fr/tel-00004349 Submitted on 27 Jan 2004 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Universit´ePierre & Marie Curie – Paris VI Ecole´ doctorale Astronomie & Astrophysique d’ˆIle-de-France Observatoire de Paris D´etection et caract´erisation de plan`etes extrasolaires par photom´etrie visible et interf´erom´etrie infrarouge `atr`es haute pr´ecision THESE` pr´esent´ee et soutenue publiquement le 27 octobre 2003 pour l’obtention du Doctorat de l’universit´ePierre & Marie Curie – Paris VI (sp´ecialit´eastrophysique et instrumentations associ´ees) par Pascal Borde´ Composition du jury Pr´esident : Pr. Pierre Encrenaz Directeurs de th`ese : Dr. Vincent Coud´edu Foresto Pr. Pierre L´ena Rapporteurs : Dr. Pierre Barge Dr. Didier Queloz Examinateur : Dr. Alain L´eger Laboratoire d’Etudes´ Spatiales et d’Instrumentation en Astrophysique — UMR 8109 Mis en page avec la classe thloria. -
Compact Binaries Frank Verbunt
Compact Binaries Part I Frank Verbunt this version: March 13, 2015 these lecture notes will be extended and adapted as the course proceeds. please check the date above to see whether your download is the most recent one. Astronomical and physical constants Physical constants are constant, but the values we assign to them improve with the quality of measuring apparatus. That is why the date must be given at which the value one uses is taken. The National Institute of Standards and Technology in Maryland, U.S.A., keeps track of new measurements of physical constants, and every few years updates the list of recommended values. The information is collected on a website: http://physics.nist.gov/cuu/Constants This site also gives the paper in which the (updates of) the constants are described. From the December 2007 preprint of this paper we copy Table XLIX below, which is based on the 2006 adjustment. based on the 2006 adjustment. Relative std. Quantity Symbol Numerical value Unit uncert. ur 1 speed of light in vacuum c, c0 299 792 458 m s− (exact) 7 2 magnetic constant µ0 4π 10− N A− × 7 2 = 12.566 370 614... 10− N A− (exact) 2 × 12 1 electric constant 1/µ0c ǫ0 8.854 187 817... 10− F m− (exact) Newtonian constant × 11 3 1 2 4 of gravitation G 6.674 28(67) 10− m kg− s− 1.0 10− × × 34 8 Planck constant h 6.626 068 96(33) 10− J s 5.0 10− × 34 × 8 h/2π ¯h 1.054 571 628(53) 10− J s 5.0 10− × 19 × 8 elementary charge e 1.602 176 487(40) 10− C 2.5 10− × 15 × 8 magnetic flux quantum h/2e Φ0 2.067 833 667(52) 10− Wb 2.5 10− 2 × 5 × 10 conductance quantum -
Michael Shao
Michael Shao Address: Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, MS 301-520, Pasadena, CA 91109 Phone: 818-354-7834, FAX: 818-393-0068, Email address: [email protected] Citizenship: USA Positions Project Scientist, SIM Project, Jet Propulsion Laboratory 1997-Present Project Scientist, Keck Interferometer Project, Jet Propulsion Laboratory 1997-2007 Spatial Interferometry Group Supervisor, Jet Propulsion Laboratory 1989-1996 Astrophysicist, Smithsonian Astrophysical Observatory 1984-1989 Astrophysicist, Naval Research Laboratory 1981-1984 Education Ph.D., Astronomy, Massachusetts Institute of Technology, Cambridge, MA 1978 B.S., Physics, Massachusetts Institute of Technology, Cambridge, MA 1971 Memberships American Astronomical Society 1981-present Fellow, Optical Society of America 1991-present Co-Chair Space Interferometry Mission Science Working Group (SIMSWSG) 1996-2003 Ex-officio, Keck Interferometer Science Steering Group (KISSG) 1997-2007 Terrestrial Planet Finder Science Working Group 1999-2007 SIM Science Team Chair 2003-2007 Selected Publications 1. Discovery and Characterization of a Faint Stellar Companion to the A3V Star ζ Virginis, S. Hinkley, B. R. Oppenheimer, D. Brenner, N. Zimmerman, L. C. Roberts, I. R. Parry, R. Soummer, A. Sivaramakrishnan, M. Simon, M. D. Perrin, D. King, J. Lloyd, A. Bouchez, J. Roberts, R. Dekany, C. Beichman, L. Hillenbrand, R. Burruss, M. Shao, G. Vasisht, The Astrophysical Journal, Vol. 712, p. 421 (2010). 2. Sub-Microarcsecond Astrometry with SIM-Lite: A Testbed-based Performance, M. Shao, B. Nemati, PASP, Vol. 121, p. 41 (2009). 3. “Galileo Galilei” (GG) a small satellite to test the equivalence principle of Galileo, Newton and Einstein, A. M. Nobili, G. L. Comandi, S. -
Dark and Quiet Skies for Science and Society
On-line Workshop Dark and Quiet Skies for Science and Society Report and recommendations Cover picture: Jupiter and Saturn photographed over the “Tre Cime di Lavaredo” (The three peaks of La- varedo), a famous dolomitic group. The picture symbolically joins two UNESCO World Heritage items, the terrestrial Dolomites and the celestial starry sky. Courtesy of Giorgia Hofer, Photographer Dark and Quiet Skies for Science and Society «Zwei Dinge erfüllen das Gemüt mit immer neuer und zuneh- mender Bewunderung und Ehrfurcht, je öfter und anhaltender sich das Nachdenken damit beschäftigt: Der bestirnte Himmel über mir, und das moralische Gesetz in mir.» I. Kant - Kritik der praktischen Vernunft «Two things fill the mind with ever new and increasing admira- tion and awe, the more often and longer the reflection occupies itself with it: the starry sky above me, and the moral law within me.» I. Kant - Critique of Practical Reason Dark and Quiet Skies for Science and Society Table of Contents About the Authors .....................................................................................................7 1. Introduction ........................................................................................................12 2. Executive summary .............................................................................................14 2.1. General executive summary ............................................................................... 14 2.2. Dark Sky Oases executive summary ..................................................................