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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. -
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. -
The NTT Provides the Deepest Look Into Space 6
The NTT Provides the Deepest Look Into Space 6. A. PETERSON, Mount Stromlo Observatory,Australian National University, Canberra S. D'ODORICO, M. TARENGHI and E. J. WAMPLER, ESO The ESO New Technology Telescope r on La Silla has again proven its extraor- - dinary abilities. It has now produced the "deepest" view into the distant regions of the Universe ever obtained with ground- or space-based telescopes. Figure 1 : This picture is a reproduction of a I.1 x 1.1 arcmin portion of a composite im- age of forty-one 10-minute exposures in the V band of a field at high galactic latitude in the constellation of Sextans (R.A. loh 45'7 Decl. -0' 143. The individual images were obtained with the EMMI imager/spectrograph at the Nas- myth focus of the ESO 3.5-m New Technolo- gy Telescope using a 1000 x 1000 pixel Thomson CCD. This combination gave a full field of 7.6 x 7.6 arcmin and a pixel size of 0.44 arcsec. The average seeing during these exposures was 1.0 arcsec. The telescope was offset between the indi- vidual exposures so that the sky background could be used to flat-field the frame. This procedure also removed the effects of cos- mic rays and blemishes in the CCD. More than 97% of the objects seen in this sub- field are galaxies. For the brighter galax- ies, there is good agreement between the galaxy counts of Tyson (1988, Astron. J., 96, 1) and the NTT counts for the brighter galax- ies. -
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, -
X-Ray Emission Processes in Stars and Their Immediate Environment
X-ray emission processes in stars and SPECIAL FEATURE their immediate environment Paola Testa1 Smithsonian Astrophysical Observatory, MS-58, 60 Garden Street, Cambridge, MA 02138 Edited by Harvey D. Tananbaum, Smithsonian Astrophysical Observatory, Cambridge, MA, and approved February 25, 2010 (received for review December 16, 2009) A decade of X-ray stellar observations with Chandra and XMM- cing significant unique insights, for instance providing precise Newton has led to significant advances in our understanding of temperature and abundance diagnostics, and, for the first time the physical processes at work in hot (magnetized) plasmas in stars in the X-ray range, diagnostics of density and optical depth. and their immediate environment, providing new perspectives and In the following I will attempt to provide an overview of our challenges, and in turn the need for improved models. The wealth current understanding of the X-ray emission mechanisms in mas- of high-quality stellar spectra has allowed us to investigate, in sive stars; of the progress in our knowledge of the X-ray activity in detail, the characteristics of the X-ray emission across the Hertz- solar-like stars; and of selected aspects of the X-ray physics of sprung-Russell (HR) diagram. Progress has been made in addressing stars in their early evolution stages in premain sequence. In fact, issues ranging from classical stellar activity in stars with solar-like X-ray stellar studies during this past decade have undergone a dynamos (such as flares, activity cycles, spatial and thermal struc- shift of focus toward the early phases of stellar evolution and turing of the X-ray emitting plasma, and evolution of X-ray activity the study of the interplay between circumstellar environment with age), to X-ray generating processes (e.g., accretion, jets, and X-ray activity. -
A Search for the Transit of HD 168443B: Improved Orbital
Submitted for publication in the Astrophysical Journal A Search for the Transit of HD 168443b: Improved Orbital Parameters and Photometry Genady Pilyavsky1, Suvrath Mahadevan1,2, Stephen R. Kane3, Andrew W. Howard4,5, David R. Ciardi3, Chris de Pree6, Diana Dragomir3,7, Debra Fischer8, Gregory W. Henry9, Eric L. N. Jensen10, Gregory Laughlin11, Hannah Marlowe6, Markus Rabus12, Kaspar von Braun3, Jason T. Wright1,2, Xuesong X. Wang1 [email protected] [email protected] ABSTRACT The discovery of transiting planets around bright stars holds the potential to greatly enhance our understanding of planetary atmospheres. In this work 1Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 2Center for Exoplanets & Habitable Worlds, Pennsylvania State University, 525 Davey Laboratory, Uni- versity Park, PA 16802 3NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125 4Department of Astronomy, University of California, Berkeley, CA 94720 5Space Sciences Laboratory, University of California, Berkeley, CA 94720 6Department of Physics and Astronomy, Agnes Scott College, 141 East College Avenue, Decatur, GA arXiv:1109.5166v1 [astro-ph.EP] 23 Sep 2011 30030, USA 7Department of Physics & Astronomy, University of British Columbia, Vancouver, BC V6T1Z1, Canada 8Department of Astronomy, Yale University, New Haven, CT 06511 9Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209 10Dept of Physics & Astronomy, Swarthmore College, Swarthmore, PA 19081 11UCO/Lick Observatory, University of California, Santa Cruz, CA 95064 12Departamento de Astonom´ıay Astrof´ısica, Pontificia Universidad Cat´olica de Chile, Casilla 306, Santiago 22, Chile –2– we present the search for transits of HD168443b, a massive planet orbiting the bright star HD 168443 (V =6.92) with a period of 58.11 days. -
A Review on Substellar Objects Below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs Or What?
geosciences Review A Review on Substellar Objects below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs or What? José A. Caballero Centro de Astrobiología (CSIC-INTA), ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Madrid, Spain; [email protected] Received: 23 August 2018; Accepted: 10 September 2018; Published: 28 September 2018 Abstract: “Free-floating, non-deuterium-burning, substellar objects” are isolated bodies of a few Jupiter masses found in very young open clusters and associations, nearby young moving groups, and in the immediate vicinity of the Sun. They are neither brown dwarfs nor planets. In this paper, their nomenclature, history of discovery, sites of detection, formation mechanisms, and future directions of research are reviewed. Most free-floating, non-deuterium-burning, substellar objects share the same formation mechanism as low-mass stars and brown dwarfs, but there are still a few caveats, such as the value of the opacity mass limit, the minimum mass at which an isolated body can form via turbulent fragmentation from a cloud. The least massive free-floating substellar objects found to date have masses of about 0.004 Msol, but current and future surveys should aim at breaking this record. For that, we may need LSST, Euclid and WFIRST. Keywords: planetary systems; stars: brown dwarfs; stars: low mass; galaxy: solar neighborhood; galaxy: open clusters and associations 1. Introduction I can’t answer why (I’m not a gangstar) But I can tell you how (I’m not a flam star) We were born upside-down (I’m a star’s star) Born the wrong way ’round (I’m not a white star) I’m a blackstar, I’m not a gangstar I’m a blackstar, I’m a blackstar I’m not a pornstar, I’m not a wandering star I’m a blackstar, I’m a blackstar Blackstar, F (2016), David Bowie The tenth star of George van Biesbroeck’s catalogue of high, common, proper motion companions, vB 10, was from the end of the Second World War to the early 1980s, and had an entry on the least massive star known [1–3]. -
121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S. -
ON the INCLINATION DEPENDENCE of EXOPLANET PHASE SIGNATURES Stephen R
The Astrophysical Journal, 729:74 (6pp), 2011 March 1 doi:10.1088/0004-637X/729/1/74 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ON THE INCLINATION DEPENDENCE OF EXOPLANET PHASE SIGNATURES Stephen R. Kane and Dawn M. Gelino NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA; [email protected] Received 2011 December 2; accepted 2011 January 5; published 2011 February 10 ABSTRACT Improved photometric sensitivity from space-based telescopes has enabled the detection of phase variations for a small sample of hot Jupiters. However, exoplanets in highly eccentric orbits present unique opportunities to study the effects of drastically changing incident flux on the upper atmospheres of giant planets. Here we expand upon previous studies of phase functions for these planets at optical wavelengths by investigating the effects of orbital inclination on the flux ratio as it interacts with the other effects induced by orbital eccentricity. We determine optimal orbital inclinations for maximum flux ratios and combine these calculations with those of projected separation for application to coronagraphic observations. These are applied to several of the known exoplanets which may serve as potential targets in current and future coronagraph experiments. Key words: planetary systems – techniques: photometric 1. INTRODUCTION and inclination for a given eccentricity. We further calculate projected separations at apastron as a function of inclination The changing phases of an exoplanet as it orbits the host star and determine their correspondence with maximum flux ratio have long been considered as a means for their detection and locations. -
En Interaktiv Visualisering Av Data Och Upptäcktsmetoder Karin Reidarman
LIU-ITN-TEK-A-018/045--SE Exoplaneter: En Interaktiv Visualisering av Data och Upptäcktsmetoder Karin Reidarman 2018-11-30 Department of Science and Technology Institutionen för teknik och naturvetenskap Linköping University Linköpings universitet nedewS ,gnipökrroN 47 106-ES 47 ,gnipökrroN nedewS 106 47 gnipökrroN LIU-ITN-TEK-A-018/045--SE Exoplaneter: En Interaktiv Visualisering av Data och Upptäcktsmetoder Examensarbete utfört i Medieteknik vid Tekniska högskolan vid Linköpings universitet Karin Reidarman Handledare Emil Axelsson Examinator Anders Ynnerman Norrköping 2018-11-30 Upphovsrätt Detta dokument hålls tillgängligt på Internet – eller dess framtida ersättare – under en längre tid från publiceringsdatum under förutsättning att inga extra- ordinära omständigheter uppstår. Tillgång till dokumentet innebär tillstånd för var och en att läsa, ladda ner, skriva ut enstaka kopior för enskilt bruk och att använda det oförändrat för ickekommersiell forskning och för undervisning. Överföring av upphovsrätten vid en senare tidpunkt kan inte upphäva detta tillstånd. All annan användning av dokumentet kräver upphovsmannens medgivande. För att garantera äktheten, säkerheten och tillgängligheten finns det lösningar av teknisk och administrativ art. Upphovsmannens ideella rätt innefattar rätt att bli nämnd som upphovsman i den omfattning som god sed kräver vid användning av dokumentet på ovan beskrivna sätt samt skydd mot att dokumentet ändras eller presenteras i sådan form eller i sådant sammanhang som är kränkande för upphovsmannens litterära eller konstnärliga anseende eller egenart. För ytterligare information om Linköping University Electronic Press se förlagets hemsida http://www.ep.liu.se/ Copyright The publishers will keep this document online on the Internet - or its possible replacement - for a considerable time from the date of publication barring exceptional circumstances. -
Downloaded From
Review HEAVY METAL RULES. I. EXOPLANET INCIDENCE AND METALLICITY Vardan Adibekyan1 ID 1 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal; [email protected] Academic Editor: name Received: date; Accepted: date; Published: date Abstract: Discovery of only handful of exoplanets required to establish a correlation between giant planet occurrence and metallicity of their host stars. More than 20 years have already passed from that discovery, however, many questions are still under lively debate: What is the origin of that relation? what is the exact functional form of the giant planet – metallicity relation (in the metal-poor regime)?, does such a relation exist for terrestrial planets? All these question are very important for our understanding of the formation and evolution of (exo)planets of different types around different types of stars and are subject of the present manuscript. Besides making a comprehensive literature review about the role of metallicity on the formation of exoplanets, I also revisited most of the planet – metallicity related correlations reported in the literature using a large and homogeneous data provided by the SWEET-Cat catalog. This study lead to several new results and conclusions, two of which I believe deserve to be highlighted in the abstract: i) The hosts of sub-Jupiter mass planets (∼0.6 – 0.9 M ) are systematically less metallic than the hosts of Jupiter-mass planets. This result might be relatedX to the longer disk lifetime and higher amount of planet building materials available at high metallicities, which allow a formation of more massive Jupiter-like planets. -
Near-Resonance in a System of Sub-Neptunes from TESS
Near-resonance in a System of Sub-Neptunes from TESS The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Quinn, Samuel N., et al.,"Near-resonance in a System of Sub- Neptunes from TESS." Astronomical Journal 158, 5 (November 2019): no. 177 doi 10.3847/1538-3881/AB3F2B ©2019 Author(s) As Published 10.3847/1538-3881/AB3F2B Publisher American Astronomical Society Version Final published version Citable link https://hdl.handle.net/1721.1/124708 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astronomical Journal, 158:177 (16pp), 2019 November https://doi.org/10.3847/1538-3881/ab3f2b © 2019. The American Astronomical Society. All rights reserved. Near-resonance in a System of Sub-Neptunes from TESS Samuel N. Quinn1 , Juliette C. Becker2 , Joseph E. Rodriguez1 , Sam Hadden1 , Chelsea X. Huang3,45 , Timothy D. Morton4 ,FredC.Adams2 , David Armstrong5,6 ,JasonD.Eastman1 , Jonathan Horner7 ,StephenR.Kane8 , Jack J. Lissauer9, Joseph D. Twicken10 , Andrew Vanderburg11,46 , Rob Wittenmyer7 ,GeorgeR.Ricker3, Roland K. Vanderspek3 , David W. Latham1 , Sara Seager3,12,13,JoshuaN.Winn14 , Jon M. Jenkins9 ,EricAgol15 , Khalid Barkaoui16,17, Charles A. Beichman18, François Bouchy19,L.G.Bouma14 , Artem Burdanov20, Jennifer Campbell47, Roberto Carlino21, Scott M. Cartwright22, David Charbonneau1 , Jessie L. Christiansen18 , David Ciardi18, Karen A. Collins1 , Kevin I. Collins23,DennisM.Conti24,IanJ.M.Crossfield3, Tansu Daylan3,48 , Jason Dittmann3 , John Doty25, Diana Dragomir3,49 , Elsa Ducrot17, Michael Gillon17 , Ana Glidden3,12 , Robert F.