DOCSLIB.ORG

Searching the Entirety of Kepler Data New Exoplanets and Occurrence Rate Estimates

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Searching the Entirety of Kepler Data New Exoplanets and Occurrence Rate Estimates Searching the Entirety of Kepler Data New Exoplanets and Occurrence Rate Estimates by Michelle Kunimoto B.Sc., The University of British Columbia, 2016 A THESIS SUBMITTED IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY in The Faculty of Graduate and Postdoctoral Studies (Astronomy) THE UNIVERSITY OF BRITISH COLUMBIA (Vancouver) April 2020 c Michelle Kunimoto 2020 The following individuals certify that they have read, and recommend to the Faculty of Graduate and Postdoctoral Studies for acceptance, a dissertation entitled: Searching the Entirety of Kepler Data: New Exoplanets and Occurrence Rate Estimates submitted by Michelle Kunimoto in partial fulfillment of the require- ments for the degree of Doctor of Philosophy in Astronomy Examining Committee: Jaymie Matthews, Physics and Astronomy Supervisor Aaron Boley, Physics and Astronomy Supervisory Committee Member Brett Gladman, Physics and Astronomy University Examiner Ronald Clowes, Earth, Ocean and Atmospheric Sciences University Examiner Additional Supervisory Committee Members: Vesna Sossi, Physics and Astronomy Supervisory Committee Member Catherine Johnson, Earth, Ocean and Atmospheric Sciences Supervisory Committee Member ii Abstract First, I present the results of an independent search of all ∼200,000 stars observed over the four-year Kepler mission for multiplanet systems, using a three-transit minimum detection criteria to search orbital periods up to hundreds of days. My search returned 17 planet candidates in addition to thousands of known Kepler Objects of Interest (KOIs), with a 98.8% recovery rate of already confirmed planets. I highlight the discovery of one candidate, KIC-7340288 b, that is both rocky (radius ≤ 1:6RL) and in the habitable zone (insolation between 0:25 and 2:2 times the Earth's insolation). Another candidate is an addition to the already known KOI-4509 system. I also present adaptive optics imaging follow-up for six of my new candidates, two of which reveal a line-of-sight stellar companion within 400. Using my planet catalogue, I then present exoplanet occurrence rates estimated with approximate Bayesian computation for planets with radii between 0:5 and 16 RL and orbital periods between 0:78 and 400 days, or- biting FGK dwarf stars. I characterize the efficiency of planet recovery by both my search and vetting pipelines using injection/recovery tests, and ac- count for both planet radius uncertainty and the estimated false positive rate due to transit-like noise signals in the data, unlike the majority of previous works. By analyzing my FGK occurrence rates as well as those computed after separating F-, G-, and K-type stars, I explore dependencies on stel- lar effective temperature, planet radius, and orbital period. I reveal new characteristics of the photoevaporation-driven \radius gap" between ∼1.5 and 2 RL, indicating that the significant bimodal distribution previously revealed for P < 100 days only exists over a much narrower range of orbital periods, above which sub-Neptunes dominate and below which super-Earths dominate. Finally, I provide several estimates of the \eta-Earth" value | iii the frequency of potentially habitable, rocky planets orbiting Sun-like stars. For planets with sizes 0:75 − 1:5 RL orbiting in a conservatively defined habitable zone (0.99 - 1.70 AU) around G-type stars, my calculations place an upper limit (84.1th percentile) of < 0:18 planets per star. iv Lay Summary The discovery of thousands of planets outside of the Solar System over the past decade has revolutionized our understanding of planet diversity. By analyzing results from missions dedicated to finding new planets, invaluable information about planet formation and evolution can be uncovered. This dissertation makes contributions on both fronts. First, I present the results of my own planet search. I found 17 new planet candidates, including a rare small planet in the habitable zone | where liquid water could potentially exist on a rocky planet's surface. Then, I analyze the search results to estimate the commonality of different kinds of planets, and explore what this can tell us about current theories. I estimate that there is likely less than one potentially habitable planet for every five Sun-like stars. Determining this is one of the major goals of astronomy, with implications for the search for life elsewhere in the Universe. v Preface Chapter 3, which details my full independent search of Kepler data and its results, was adapted from a first-author paper published in The Astro- nomical Journal: Kunimoto, M., Matthews, J., & Ngo, H. 2020, Searching the Entirety of Kepler Data. I. 17 New Planet Candidates Including 1 Habitable Zone World, AJ, 159, 124. I wrote the paper, with co-authors providing valuable feedback on the manuscript. The development of the full pipeline from start to finish, the downloading, reduction, and search of the light curves for planets, the vetting of surviving candidates, the follow-up analysis, and the interpretation of the results, was done by me. Henry Ngo was the PI for the adaptive optics (AO) observations. He also wrote the technical justification for our telescope proposal, while I co-wrote the scien- tific justification. The observations themselves were obtained by staff at the Gemini North telescope in Hawaii. Dr. Ngo also helped me write my own AO data reduction scripts. In terms of resources used to perform the research described in this chap- ter, all Kepler data was downloaded from the Mikulski Archive for Space Telescopes (http://archive.stsci.edu/). Some of the codes I used for the data reduction and transit search were written by Jason Rowe. These are all publicly available as part of the Kepler Transit Model Codebase (https://github.com/jasonfrowe/Kepler). Specifically, I used kfitsread to convert the data into a readable file format and combine each star's light curve into a single file, detrend5 to detrend the light curves, and transitfind2 to search through the data for transit signals. For the vet- ting pipeline, the code for my first uniqueness test was written by Kelsey Hoffman (private communication), while I used Jeffrey Coughlin's Model Shift package (https://github.com/JeffLCoughlin/Model-Shift) for the vi second uniqueness test, the shape metric, significant secondary test, and second odd-even depth test. For the follow-up analysis of planet candi- dates, I used emcee (https://github.com/dfm/emcee) to perform Markov Chain Monte Carlo fitting of transit models to the data. The transit models themselves were adapted from code available from Ian's Astro-Python Codes (http://www.lpl.arizona.edu/∼ianc/python/). I used isochrones (https://github.com/timothydmorton/isochrones) to produce posteri- ors for stellar parameters. I also analyzed each transit with vespa (https://github.com/timothydmorton), which is a probabilistic valida- tion tool for transiting exoplanets. All other code was written by me (e.g. code for other candidacy tests not mentioned here, scripts for automating the search and vetting pipeline to run on thousands of light curves, etc.). Lastly, due to the computational time required to search each star suffi- ciently, I performed the majority of my work on the Orcinus and Cedar computing clusters, provided by WestGrid (www.westgrid.ca) and Com- pute Canada (www.computecanada.ca). Chapter 4, which details the use of my independent search results for exoplanet occurrence rate estimates, was adapted from a first-author paper accepted for publication in The Astronomical Journal: Kunimoto, M. & Matthews, J. 2020, Searching the Entirety of Kepler Data. II. Occurrence Rate Estimates for FGK Stars. I wrote the paper, and performed the full occurrence rate estimates, analysis, and interpretation of the results. My co-author provided feedback on the manuscript. In terms of resources, I used cosmoabc (https:/github.com/ COINtoolbox/CosmoABC) to implement approximate Bayesian computation (ABC) in my occurrence rate estimates, and emcee to perform Markov Chain Monte Carlo fitting of power law-based functions to my occurrence rates as a function of orbital period. All other code was written by me (e.g. the exoplanet population simulator/forward model, scripts for automating the calculation of occurrence rates with different inputs, etc.). Lastly, due to the computational time required to compute ABC occurrence rates, I used the Graham Compute Canada cluster. Chapter 2 describes the motivation behind my research, and Chapter 5 vii concludes my results and summarizes their significance. These were each partially adapted from the Introduction and Conclusion sections of the two papers discussed previously. viii Table of Contents Abstract ................................. iii Lay Summary ..............................v Preface .................................. vi Table of Contents ............................ ix List of Tables .............................. xiii List of Figures .............................. xvi List of Symbols ............................. xxii List of Abbreviations .........................xxiii Acknowledgements ........................... xxiv 1 Introduction .............................1 1.1 Exoplanet Detection Techniques . .3 1.1.1 Pulsar Timing Variations . .3 1.1.2 Radial Velocity . .4 1.1.3 The Transit Method . .6 1.1.4 Microlensing . 10 1.1.5 Direct Imaging . 11 1.2 Confirmation of Transiting Exoplanets . 12 1.2.1 False Positives . 12 1.2.2 Follow-Up Observations and Validation . 16 ix 1.3 Exploring Exoplanet Populations . 19 1.3.1 Survey Selection Effects . 21 1.3.2 Occurrence Rate Methodologies . 22 1.4 The Habitable Zone . 28 2 Motivations for this Thesis .................... 31 2.1 An Independent Search of Kepler Data . 31 2.2 Occurrence Rate Estimates . 32 3 An Independent Search of Kepler Data ............ 36 3.1 Chapter Outline . 36 3.2 Planet Detection Pipeline . 36 3.2.1 Preparing the Light Curves . 36 3.2.2 Searching for Transiting Planets . 38 3.2.3 Initial Vetting and Identification of Transit Candi- dates . 39 3.3 Vetting Pipeline . 42 3.3.1 Choice of Candidacy Test Thresholds . 42 3.3.2 Transit Model Fitting . 43 3.3.3 Candidacy Tests Against Noise False Positives . 44 3.3.4 Candidacy Tests Against Eclipsing Binary False Pos- itives .
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]
  • KEPLER-21B: a 1.6 Rearth PLANET TRANSITING the BRIGHT OSCILLATING F SUBGIANT STAR HD 179070 Steve B
    The Astrophysical Journal, 746:123 (18pp), 2012 February 20 doi:10.1088/0004-637X/746/2/123 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ∗ KEPLER-21b: A 1.6 REarth PLANET TRANSITING THE BRIGHT OSCILLATING F SUBGIANT STAR HD 179070 Steve B. Howell1,2,36, Jason F. Rowe2,3,36, Stephen T. Bryson2, Samuel N. Quinn4, Geoffrey W. Marcy5, Howard Isaacson5, David R. Ciardi6, William J. Chaplin7, Travis S. Metcalfe8, Mario J. P. F. G. Monteiro9, Thierry Appourchaux10, Sarbani Basu11, Orlagh L. Creevey12,13, Ronald L. Gilliland14, Pierre-Olivier Quirion15, Denis Stello16, Hans Kjeldsen17,Jorgen¨ Christensen-Dalsgaard17, Yvonne Elsworth7, Rafael A. Garc´ıa18, Gunter¨ Houdek19, Christoffer Karoff7, Joanna Molenda-Zakowicz˙ 20, Michael J. Thompson8, Graham A. Verner7,21, Guillermo Torres4, Francois Fressin4, Justin R. Crepp23, Elisabeth Adams4, Andrea Dupree4, Dimitar D. Sasselov4, Courtney D. Dressing4, William J. Borucki2, David G. Koch2, Jack J. Lissauer2, David W. Latham4, Lars A. Buchhave22,35, Thomas N. Gautier III24, Mark Everett1, Elliott Horch25, Natalie M. Batalha26, Edward W. Dunham27, Paula Szkody28,36, David R. Silva1,36, Ken Mighell1,36, Jay Holberg29,36,Jeromeˆ Ballot30, Timothy R. Bedding16, Hans Bruntt12, Tiago L. Campante9,17, Rasmus Handberg17, Saskia Hekker7, Daniel Huber16, Savita Mathur8, Benoit Mosser31, Clara Regulo´ 12,13, Timothy R. White16, Jessie L. Christiansen3, Christopher K. Middour32, Michael R. Haas2, Jennifer R. Hall32,JonM.Jenkins3, Sean McCaulif32, Michael N. Fanelli33, Craig
    [Show full text]
  • The New Generation Planetary Population Synthesis (NGPPS). II
    Astronomy & Astrophysics manuscript no. pop c ESO 2020 July 14, 2020 The New Generation Planetary Population Synthesis (NGPPS) II. Planetary population of solar-like stars and overview of statistical results? Alexandre Emsenhuber1; 2, Christoph Mordasini2, Remo Burn2, Yann Alibert2, Willy Benz2, and Erik Asphaug1 1 Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA e-mail: [email protected] 2 Physikalisches Institut, Universität Bern, Gesselschaftsstrasse 6, 3012 Bern, Switzerland Received DD MMM YYYY / Accepted DD MMM YYYY ABSTRACT Context. Planetary formation and evolution is a combination of multiple processes that are interlinked. These processes are not known in detail and many uncertainties remain. Constraining the formation and evolution mechanisms observationally requires statistical comparison to a large diversity of planetary systems. Aims. We want to understand the global observable consequences of different physical processes (accretion, migration, and interac- tions) and initial properties (such as disc masses and metallicities) on the demographics of the planetary population. We also want to study the convergence of our scheme with respect to one initial condition, the initial number of planetary embryo in each disc. Methods. We select distributions of initial conditions that are representative of known protoplanetary discs. Then, we use the Gener- ation III Bern model to perform planetary population synthesis. We synthesise five populations with each a different initial number of Moon-mass embryos per disc: 1, 10, 20, 50, and 100. The last is our nominal planetary population consisting of 1000 stars (systems) that we use to provide an extensive statistical analysis of the planetary systems around 1 M stars.
    [Show full text]
  • Space News Update – May 2019
    Space News Update – May 2019 By Pat Williams IN THIS EDITION: • India aims to be 1st country to land rover on Moon's south pole. • Jeff Bezos says Blue Origin will land humans on moon by 2024. • China's Chang'e-4 probe resumes work for sixth lunar day. • NASA awards Artemis contract for lunar gateway power. • From airport to spaceport as UK targets horizontal spaceflight. • Russian space sector plagued by astronomical corruption. • Links to other space and astronomy news published in May 2019. Disclaimer - I claim no authorship for the printed material; except where noted (PW). INDIA AIMS TO BE 1ST COUNTRY TO LAND ROVER ON MOON'S SOUTH POLE India will become the first country to land a rover on the Moon's the south pole if the country's space agency "Indian Space Research Organisation (ISRO)" successfully achieves the feat during the country's second Moon mission "Chandrayaan-2" later this year. "This is a place where nobody has gone. All the ISRO missions till now to the Moon have landed near the Moon's equator. Chandrayaan-2, India’s second lunar mission, has three modules namely Orbiter, Lander (Vikram) & Rover (Pragyan). The Orbiter and Lander modules will be interfaced mechanically and stacked together as an integrated module and accommodated inside the GSLV MK-III launch vehicle. The Rover is housed inside the Lander. After launch into earth bound orbit by GSLV MK-III, the integrated module will reach Moon orbit using Orbiter propulsion module. Subsequently, Lander will separate from the Orbiter and soft land at the predetermined site close to lunar South Pole.
    [Show full text]
  • Sized Exoplanet Thomas Barclay1,2, Jason F
    A sub-Mercury-sized exoplanet Thomas Barclay1,2, Jason F. Rowe1,3, Jack J. Lissauer1, Daniel Huber1,4, François Fressin5, Steve B. Howell1, Stephen T. Bryson1, William J. Chaplin6, Jean-Michel Désert5, Eric D. Lopez7, Geoffrey W. Marcy8, Fergal Mullally1,3, Darin Ragozzine5,9, Guillermo Torres5, Elisabeth R. Adams5, Eric Agol10, David Barrado11,12, Sarbani Basu13, Timothy R. Bedding14, Lars A. Buchhave15,16, David Charbonneau5, Jessie L. Christiansen1,3, Jørgen Christensen-Dalsgaard17, David Ciardi18, William D. Cochran19, Andrea K. Dupree5, Yvonne Elsworth6, Mark Everett20, Debra A. Fischer13, Eric B. Ford9, Jonathan J. Fortney7, John C. Geary5, Michael R. Haas1, Rasmus Handberg17, Saskia Hekker6,21, Christopher E. Henze1, Elliott Horch22, Andrew W. Howard23, Roger C. Hunter1, Howard Isaacson8, Jon M. Jenkins1,3, Christoffer Karoff17, Steven D. Kawaler24, Hans Kjeldsen17, Todd C. Klaus25, David W. Latham5, Jie Li1,3, Jorge Lillo-Box12, Mikkel N. Lund17, Mia Lundkvist17, Travis S. Metcalfe26, Andrea Miglio6, Robert L. Morris1,3, Elisa V. Quintana1,3, Dennis Stello14, Jeffrey C. Smith1,3, Martin Still1,2, & Susan E. Thompson1,3 1 NASA Ames Research Center, Moffett Field, CA 94035, USA 2 Bay Area Environmental Research Institute, 596 First St West, Sonoma, CA 95476, USA 3 SETI Institute, 189 Bernardo Ave, Mountain View, CA 94043, USA 4 NASA Postdoctoral Program Fellow 5 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 6 School of Physics and Astronomy, University of Birmingham, Edgbaston, B15 2TT, UK 7 Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA 8 Department of Astronomy, UC Berkeley, Berkeley, CA 94720, USA 9 Astronomy Department, University of Florida, 211 Bryant Space Sciences Center, Gainesville, FL 32111, USA 10 Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA 11 Calar Alto Observatory, Centro Astronómico Hispano Alemán, C/ Jesús Durbán Remón, E- 04004 Almería, Spain 12 Depto.
    [Show full text]
  • Determining the True Mass of Radial-Velocity Exoplanets with Gaia F
    Determining the true mass of radial-velocity exoplanets with Gaia F. Kiefer, G. Hébrard, A. Lecavelier Des Etangs, E. Martioli, S. Dalal, A. Vidal-Madjar To cite this version: F. Kiefer, G. Hébrard, A. Lecavelier Des Etangs, E. Martioli, S. Dalal, et al.. Determining the true mass of radial-velocity exoplanets with Gaia: Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets. Astronomy and Astrophysics - A&A, EDP Sciences, 2021, 645, pp.A7. 10.1051/0004-6361/202039168. hal-03085694 HAL Id: hal-03085694 https://hal.archives-ouvertes.fr/hal-03085694 Submitted on 21 Dec 2020 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. A&A 645, A7 (2021) Astronomy https://doi.org/10.1051/0004-6361/202039168 & © F. Kiefer et al. 2020 Astrophysics Determining the true mass of radial-velocity exoplanets with Gaia Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets? F. Kiefer1,2, G. Hébrard1,3, A. Lecavelier des Etangs1, E. Martioli1,4, S. Dalal1, and A. Vidal-Madjar1 1 Institut d’Astrophysique de Paris, Sorbonne
    [Show full text]
  • Exoplanet Demographics Conference November 9-13, 2020 Tuesday Talk Abstracts
    Exoplanet Demographics Conference November 9-13, 2020 Tuesday Talk Abstracts Small Planets Low-mass Exoplanet Demographics - Daniel Jontof-Hutter (Univ. of the Pacific) Exoplanet science is advancing rapidly on many fronts following the detection of thousands of planets, particularly from transit surveys. Precise stellar characterization has revealed the bimodal planetary size distribution, and has enabled precise planetary mass measurements with radial velocities and transit timing. Over 120 exoplanets less massive than 30 Earths have measured masses and radii (Jontof-Hutter, 2019, AREPS, 47, 141), and a remarkably diverse range of bulk densities among these exoplanets has been revealed. Planetary mass and radius characterization has also entered the terrestrial regime- over 30 exoplanets smaller than 1.6 Earth-radii have detected masses, and planets as small as Mars now populate the mass-radius diagram. In this review, we summarize the progress that has been made in characterizing this diverse population: where planet sizes and incident fluxes inform on bulk planet properties, where compositions by volume are dominated by volatiles and where bulk planet properties within individuals systems differ substantially. To some extent, however, detection biases prevent individual characterizations from revealing underlying planet demographics. We review progress to correct for these biases in determining distributions of planet properties. Looking forward, planetary system demographics will require observations to probe system architectures beyond the compact configurations that have been detected close to stellar hosts. A small number of compact multi-transiting systems show evidence of additional planets from radial velocities, and observing campaigns to detect non-transiting planets that orbit beyond the known planets have begun.
    [Show full text]
  • School of Physics and Astronomy – Yearbook 2020
    Credit: SohebCredit: Mandhai, Physics PhD Student * SCHOOL OF PHYSICS AND ASTRONOMY – YEARBOOK 2020 Introduction Table of Contents research, and some have wandered the socially-distanced corridors with a heavy heart, missing the noise, chaos, and Introduction ....................................................... 2 energy of previous years. Many living within the city School Events & Activities ................................... 4 boundaries have been under some sort of restrictions ever since. Each of us has had to adapt, to try to find our own paths Science News .................................................... 20 through the COVID-19 pandemic, and to hold onto the certainty that better times are in front of us. From the Archive .............................................. 34 But despite the Earth-shattering events of the past year, Space Park Leicester News ................................ 37 compiling this 2020 yearbook has been remarkable, eye- Physicists Away from the Department (Socially opening, and inspiring. In the pages that follow, we hope that Distanced Edition*) .......................................... 44 you’ll be proud of the flexibility and resilience shown in the Physics and Astronomy community – the pages are Celebrating Success .......................................... 48 overflowing with School events; stories of successes in our student, research, and academic communities; highlights Meeting Members of the School ....................... 51 from our public engagement across the UK; momentous changes in our teaching through the Ignite programme; and Physics Special Topics: Editors Pick ................... 68 new leaps forward for our world-leading research. Our Comings and Goings ......................................... 70 Directors of Teaching have done a phenomenal job, working non-stop to support teaching staff who have worked tirelessly Twelve months ago, as the Leicester Physics News Team were to prepare blended courses suitable for the virtual world.
    [Show full text]
  • The Discovery of WASP-151B, WASP-153B, WASP-156B: Insights on Giant Planet Migration and the Upper Boundary of the Neptunian Desert', Astronomy and Astrophysics, Vol
    University of Birmingham The discovery of WASP-151b, WASP-153b, WASP- 156b Demangeon, Olivier D. S.; Faedi, F.; Hébrard, G.; Brown, D. J. A.; Barros, S. C. C.; Doyle, A. P.; Maxted, P. F. L.; Cameron, A. Collier; Hay, K. L.; Alikakos, J.; Anderson, D. R.; Armstrong, D. J.; Boumis, P.; Bonomo, A. S.; Bouchy, F.; Haswell, C. A.; Hellier, C.; Kiefer, F.; Lam, K. W. F.; Mancini, L. DOI: 10.1051/0004-6361/201731735 License: None: All rights reserved Document Version Publisher's PDF, also known as Version of record Citation for published version (Harvard): Demangeon, ODS, Faedi, F, Hébrard, G, Brown, DJA, Barros, SCC, Doyle, AP, Maxted, PFL, Cameron, AC, Hay, KL, Alikakos, J, Anderson, DR, Armstrong, DJ, Boumis, P, Bonomo, AS, Bouchy, F, Haswell, CA, Hellier, C, Kiefer, F, Lam, KWF, Mancini, L, McCormac, J, Norton, AJ, Osborn, HP, Palle, E, Pepe, F, Pollacco, DL, Prieto-Arranz, J, Queloz, D, Ségransan, D, Smalley, B, Triaud, AHMJ, Udry, S, West, R & Wheatley, PJ 2018, 'The discovery of WASP-151b, WASP-153b, WASP-156b: Insights on giant planet migration and the upper boundary of the Neptunian desert', Astronomy and Astrophysics, vol. 610, A63. https://doi.org/10.1051/0004- 6361/201731735 Link to publication on Research at Birmingham portal Publisher Rights Statement: Checked for eligibility: 12/07/2019 This document appears in its final form in [JournalTitle], copyright © ESO 2018. The final Version of Record can be found at: https://doi.org/10.1051/0004-6361/201731735 General rights Unless a licence is specified above, all rights (including copyright and moral rights) in this document are retained by the authors and/or the copyright holders.
    [Show full text]
  • An Earth-Sized Planet in the Habitable Zone of a Cool Star Authors: Elisa V
    Title: An Earth-sized Planet in the Habitable Zone of a Cool Star Authors: Elisa V. Quintana1,2*, Thomas Barclay2,3, Sean N. Raymond4,5, Jason F. Rowe1,2, Emeline Bolmont4,5, Douglas A. Caldwell1,2, Steve B. Howell2, Stephen R. Kane6, Daniel Huber1,2, Justin R. Crepp7, Jack J. Lissauer2, David R. Ciardi8, Jeffrey L. Coughlin1,2, Mark E. Everett9, Christopher E. Henze2, Elliott Horch10, Howard Isaacson11, Eric B. Ford12,13, Fred C. Adams14,15, Martin Still3, Roger C. Hunter2, Billy Quarles2, Franck Selsis4,5 Affiliations: 1SETI Institute, 189 Bernardo Ave, Suite 100, Mountain View, CA 94043, USA. 2NASA Ames Research Center, Moffett Field, CA 94035, USA. 3Bay Area Environmental Research Institute, 596 1st St West Sonoma, CA 95476, USA. 4Univ. Bordeaux, Laboratoire d'Astrophysique de Bordeaux, UMR 5804, F-33270, Floirac, France. 5CNRS, Laboratoire d'Astrophysique de Bordeaux, UMR 5804, F-33270, Floirac, France. 6San Francisco State University, 1600 Holloway Avenue, San Francisco, CA 94132, USA. 7University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556, USA. 8NASA Exoplanet Science Institute, California Institute of Technology, 770 South Wilson Avenue Pasadena, CA 91125, USA. 9National Optical Astronomy Observatory, 950 N. Cherry Ave, Tucson, AZ 85719 10Southern Connecticut State University, New Haven, CT 06515 11University of California, Berkeley, CA, 94720, USA. 12Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA, 16802, USA 13Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA 14Michigan Center for Theoretical Physics, Physics Department, University of Michigan, Ann Arbor, MI 48109, USA 15Astronomy Department, University of Michigan, Ann Arbor, MI 48109, USA *Correspondence to: [email protected] ! ! ! ! ! ! ! Abstract: The quest for Earth-like planets represents a major focus of current exoplanet research.
    [Show full text]
  • Pos(BASH2015)007
    Precision Stellar Astrophysics in the Kepler Era PoS(BASH2015)007 Daniel Huber∗ Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia E-mail: [email protected] The study of fundamental properties (such as temperatures, radii, masses, and ages) and interior processes (such as convection and angular momentum transport) of stars has implications on var- ious topics in astrophysics, ranging from the evolution of galaxies to understanding exoplanets. In this contribution I will review the basic principles of two key observational methods for con- straining fundamental and interior properties of single field stars: the study stellar oscillations (asteroseismology) and optical long-baseline interferometry. I will highlight recent breakthrough discoveries in asteroseismology such as the measurement of core rotation rates in red giants and the characterization of exoplanet systems. I will furthermore comment on the reliability of inter- ferometry as a tool to calibrate indirect methods to estimate fundamental properties, and present a new angular diameter measurement for the exoplanet host star HD 219134 which demonstrates that diameters for stars which are relatively well resolved (& 1 mas for the K band) are consistent across different instruments. Finally I will discuss the synergy between asteroseismology and interferometry to test asteroseismic scaling relations, and give a brief outlook on the expected impact of space-based missions such as K2, TESS and Gaia. Frank N. Bash Symposium 2015 18-20 October The University of Texas at Austin, USA ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0).
    [Show full text]
  • Determining the True Mass of Radial-Velocity Exoplanets with Gaia 9 Planet Candidates in the Brown-Dwarf/Stellar Regime and 27 Confirmed Planets
    Astronomy & Astrophysics manuscript no. exoplanet_mass_gaia c ESO 2020 September 30, 2020 Determining the true mass of radial-velocity exoplanets with Gaia 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets F. Kiefer1; 2, G. Hébrard1; 3, A. Lecavelier des Etangs1, E. Martioli1; 4, S. Dalal1, and A. Vidal-Madjar1 1 Institut d’Astrophysique de Paris, Sorbonne Université, CNRS, UMR 7095, 98 bis bd Arago, 75014 Paris, France 2 LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, France? 3 Observatoire de Haute-Provence, CNRS, Universiteé d’Aix-Marseille, 04870 Saint-Michel-l’Observatoire, France 4 Laboratório Nacional de Astrofísica, Rua Estados Unidos 154, 37504-364, Itajubá - MG, Brazil Submitted on 2020/08/20 ; Accepted for publication on 2020/09/24 ABSTRACT Mass is one of the most important parameters for determining the true nature of an astronomical object. Yet, many published exoplan- ets lack a measurement of their true mass, in particular those detected thanks to radial velocity (RV) variations of their host star. For those, only the minimum mass, or m sin i, is known, owing to the insensitivity of RVs to the inclination of the detected orbit compared to the plane-of-the-sky. The mass that is given in database is generally that of an assumed edge-on system (∼90◦), but many other inclinations are possible, even extreme values closer to 0◦ (face-on). In such case, the mass of the published object could be strongly underestimated by up to two orders of magnitude.
    [Show full text]