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