Exep Science Gap List 2021
Total Page:16
File Type:pdf, Size:1020Kb
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. -
2-6-NASA Exoplanet Archive
The NASA Exoplanet Archive Rachel Akeson NASA Exoplanet Science Ins5tute (NExScI) September 29, 2016 NASA Big Data Task Force Overview: Dat a NASA Exoplanet Archive supports both the exoplanet science community and NASA exoplanet missions (Kepler, K2, TESS, WFIRST) • Data • Confirmed exoplanets from the literature • Over 80,000 planetary and stellar parameter values for 3388 exoplanets • Updated weekly • Kepler stellar proper5es, planet candidate, data valida5on and occurrence rate products • MAST is archive for pixel and light curve data • Addi5onal space (CoRoT) and ground-based transit surveys (~20 million light curves) • Transit spectroscopy data • Auto-updated exoplanet plots and movies Big Data Task Force: Exoplanet Archive Overview: Tool s Example: Kepler 14 Time Series Viewer • Interac5ve tables and ploZng for data • Includes light curve normaliza5on • Periodogram calcula5ons • Searches for periodic signals in archive or user-supplied light curves • Transit predic5ons • Uses value from archive to predict future planet transits for observa5on and mission planning • URL-based queries Aliases • Calcula5on of observable proper5es Planet orbital period • Web-based service to collect follow-up observa5ons of planet candidates for Kepler, K2 and TESS (ExoFOP) Stellar ac5vity • Includes user-supplied data, file and notes Big Data Task Force: Exoplanet Archive Data Challenges and Technical Approach (1) • Challenges with Exoplanet Archive are not currently about data volume but about providing CPU resources and data complexity • CPU challenge -
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. -
Exep Science Plan Appendix (SPA) (This Document)
ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 1 of 61 Created By: David A. Breda Date Program TDEM System Engineer Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Nick Siegler Date Program Chief Technologist Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Concurred By: Dr. Gary Blackwood Date Program Manager Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology EXOPDr.LANET Douglas Hudgins E XPLORATION PROGRAMDate Program Scientist Exoplanet Exploration Program ScienceScience Plan Mission DirectorateAppendix NASA Headquarters Karl Stapelfeldt, Program Chief Scientist Eric Mamajek, Deputy Program Chief Scientist Exoplanet Exploration Program JPL CL#19-0790 JPL Document No: 1735632 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 2 of 61 Approved by: Dr. Gary Blackwood Date Program Manager, Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory Dr. Douglas Hudgins Date Program Scientist Exoplanet Exploration Program Science Mission Directorate NASA Headquarters Created by: Dr. Karl Stapelfeldt Chief Program Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Eric Mamajek Deputy Program Chief Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. © 2018 California Institute of Technology. Government sponsorship acknowledged. Exoplanet Exploration Program JPL CL#19-0790 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 3 of 61 Table of Contents 1. -
Pre-Vetted False Positives for TESS
Swarthmore College Works Physics & Astronomy Faculty Works Physics & Astronomy 11-1-2018 The KELT Follow-Up Network And Transit False-Positive Catalog: Pre-Vetted False Positives For TESS K. A. Collins K. I. Collins FJ.ollow Pepper this and additional works at: https://works.swarthmore.edu/fac-physics J. Labadie-Bar Part of the Astrtz ophysics and Astronomy Commons Let us know how access to these works benefits ouy K. G. Stassun See next page for additional authors Recommended Citation K. A. Collins, K. I. Collins, J. Pepper, J. Labadie-Bartz, K. G. Stassun, B. S. Gaudi, D. Bayliss, J. Bento, K. D. Colón, D. Feliz, D. James, M. C. Johnson, R. B. Kuhn, M. B. Lund, M. T. Penny, J. E. Rodriguez, R. J. Siverd, D. J. Stevens, X. Yao, G. Zhou, M. Akshay, G. F. Aldi, C. Ashcraft, S. Awiphan, Ö. Baştürk, D. Baker, T. G. Beatty, P. Benni, P. Berlind, G. B. Berriman, Z. Berta-Thompson, A. Bieryla, V. Bozza, S. C. Novati, M. L. Calkins, J. M. Cann, D. R. Ciardi, W. D. Cochran, David H. Cohen, D. Conti, J. R. Crepp, I. A. Curtis, G. D'Ago, K. A. Diazeguigure, C. D. Dressing, F. Dubois, E. Ellington, T. G. Ellis, G. A. Esquerdo, P. Evans, A. Friedli, A. Fukui, B. J. Fulton, E. J. Gonzales, J. C. Good, J. Gregorio, T. Gumusayak, D. A. Hancock, C. K. Harada, R. Hart, E. G. Hintz, H. Jang-Condell, E. J. Jeffery, Eric L.N. Jensen, E. Jofré, M. D. Joner, A. Kar, D. H. Kasper, B. Keten, J. -
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]. -
Observing Exoplanets
Observing Exoplanets Olivier Guyon University of Arizona Astrobiology Center, National Institutes for Natural Sciences (NINS) Subaru Telescope, National Astronomical Observatory of Japan, National Institutes for Natural Sciences (NINS) Nov 29, 2017 My Background Astronomer / Optical scientist at University of Arizona and Subaru Telescope (National Astronomical Observatory of Japan, Telescope located in Hawaii) I develop instrumentation to find and study exoplanet, for ground-based telescopes and space missions My interest is focused on habitable planets and search for life outside our solar system At Subaru Telescope, I lead the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument. 2 ALL known Planets until 1989 Approximately 10% of stars have a potentially habitable planet 200 billion stars in our galaxy → approximately 20 billion habitable planets Imagine 200 explorers, each spending 20s on each habitable planet, 24hr a day, 7 days a week. It would take >60yr to explore all habitable planets in our galaxy alone. x 100,000,000,000 galaxies in the observable universe Habitable planets Potentially habitable planet : – Planet mass sufficiently large to retain atmosphere, but sufficiently low to avoid becoming gaseous giant – Planet distance to star allows surface temperature suitable for liquid water (habitable zone) Habitable zone = zone within which Earth-like planet could harbor life Location of habitable zone is function of star luminosity L. For constant stellar flux, distance to star scales as L1/2 Examples: Sun → habitable zone is at ~1 AU Rigel (B type star) Proxima Centauri (M type star) Habitable planets Potentially habitable planet : – Planet mass sufficiently large to retain atmosphere, but sufficiently low to avoid becoming gaseous giant – Planet distance to star allows surface temperature suitable for liquid water (habitable zone) Habitable zone = zone within which Earth-like planet could harbor life Location of habitable zone is function of star luminosity L. -
Exoplanet Community Report
JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probeclass missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2 -
EXTENSIONS of REMARKS April 11, 1973
11958 EXTENSIONS OF REMARKS April 11, 1973 Yea-and-nay votes may occur on that ADJOURNMENT UNTIL 9:30 A.M. IN THE ARMY bill. It is possible, if consent is given, Mr. ROBERT C. BYRD. Mr. P resident, T he following-named officers to be placed that the measure would be temporarily on the retired list in grade indicated under if there be no further business to come the provisions of title 10, United States Code, laid aside from time to time and other before the Senate, I move, in accordance items on the Calendar could be taken section 3962: with the previous order, that the Senate To be lieutenant general up tomorrow and Friday—but only if stand in adjournment until 9:30 a.m. L t. Gen. Julian Johnson Ewell, xxx-xx-xxxx , unanimous consent is gotten. tomorrow. With respect to the bill to amend the A rm y of the U nited S tates (m ajor general, N ational Foundation on the A rts and T he m otion was agreed to; and at U.S. Army) . 5:53 p.m. the Senate adjourned until to- L t. Gen. William R aymond P eers, xxx-xx-x... Humanities A ct, I do not believe that xxx-x... A rmy of the United States (major gen- that bill will be taken up tomorrow. The morrow, Thursday, April 12, 1973, at 9:30 a.m. eral, U.S. Army) . distinguished author of the bill (M r. L t. G en. W illard P earson, xxx-xx-xxxx , PELL) has requested that the bill be taken A rm y of the U nited S tates (m ajor general, U.S. -
Tau Ceti Radius: 700,000 Km (109X Earth’S Radius)
Tau Ceti Radius: 700,000 km (109x Earth’s radius) Average surface temperature: 9,000,000° F Basic characteristics: A star somewhat similar to the Sun, Tau Ceti is about the same size and brightness as the Sun. Main elements: Hydrogen & Helium Boll Radius: 2,400 km (0.38x Earth’s radius) Distance from Tau Ceti (main star): 58,000,000 km (about 0.39x that of Earth) Average surface temperature: 527.1° F Basic characteristics: Rocky with an iron core. No atmosphere, Heavy cratering on the surface. Has no moons. Boll dominates its orbit. Main elements: Iron, Magnesium, Nickel, Oxygen, Silicon Bender Radius: 6,000 km (0.95x Earth’s radius) Distance from Tau Ceti (main star): 108,000,000 km (about 0.73x that of Earth) Average surface temperature: 862.3° F Basic characteristics: Rocky with an iron core. Has an extremely thick atmosphere made mostly of carbon dioxide and methane. This heavy atmosphere traps heat and makes it much hotter than it would be otherwise, There is cratering on the surface. Has no moons. Bender dominates its orbit. Main elements: Iron, Silicon, Magnesium, Oxygen, Silicon, Carbon Belior Radius: 1,700 km (0.27x Earth’s radius) Distance from Tau Ceti (main star): 108,000,000 km (about 0.73x that of Earth) Average surface temperature: 862.3° F Basic characteristics: Belior orbits the planet Bender. It is rocky with an iron core. Has no atmosphere. There is heavy cratering on the surface. Main elements: Iron, Silicon, Magnesium, Oxygen, Silicon, Carbon Pern Radius: 6,300 km (0.98x Earth’s radius) Distance from Tau Ceti (main star): 154,000,000 km (about 1.1x that of Earth) Average surface temperature: 58.2° F Basic characteristics: Rocky with an iron core. -
Exoplanet Exploration Collaboration Initiative TP Exoplanets Final Report
EXO Exoplanet Exploration Collaboration Initiative TP Exoplanets Final Report Ca Ca Ca H Ca Fe Fe Fe H Fe Mg Fe Na O2 H O2 The cover shows the transit of an Earth like planet passing in front of a Sun like star. When a planet transits its star in this way, it is possible to see through its thin layer of atmosphere and measure its spectrum. The lines at the bottom of the page show the absorption spectrum of the Earth in front of the Sun, the signature of life as we know it. Seeing our Earth as just one possibly habitable planet among many billions fundamentally changes the perception of our place among the stars. "The 2014 Space Studies Program of the International Space University was hosted by the École de technologie supérieure (ÉTS) and the École des Hautes études commerciales (HEC), Montréal, Québec, Canada." While all care has been taken in the preparation of this report, ISU does not take any responsibility for the accuracy of its content. Electronic copies of the Final Report and the Executive Summary can be downloaded from the ISU Library website at http://isulibrary.isunet.edu/ International Space University Strasbourg Central Campus Parc d’Innovation 1 rue Jean-Dominique Cassini 67400 Illkirch-Graffenstaden Tel +33 (0)3 88 65 54 30 Fax +33 (0)3 88 65 54 47 e-mail: [email protected] website: www.isunet.edu France Unless otherwise credited, figures and images were created by TP Exoplanets. Exoplanets Final Report Page i ACKNOWLEDGEMENTS The International Space University Summer Session Program 2014 and the work on the -
The HARPS Search for Earth-Like Planets in the Habitable Zone I
A&A 534, A58 (2011) Astronomy DOI: 10.1051/0004-6361/201117055 & c ESO 2011 Astrophysics The HARPS search for Earth-like planets in the habitable zone I. Very low-mass planets around HD 20794, HD 85512, and HD 192310, F. Pepe1,C.Lovis1, D. Ségransan1,W.Benz2, F. Bouchy3,4, X. Dumusque1, M. Mayor1,D.Queloz1, N. C. Santos5,6,andS.Udry1 1 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Versoix, Switzerland e-mail: [email protected] 2 Physikalisches Institut Universität Bern, Sidlerstrasse 5, 3012 Bern, Switzerland 3 Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis Bd Arago, 75014 Paris, France 4 Observatoire de Haute-Provence/CNRS, 04870 St. Michel l’Observatoire, France 5 Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 6 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal Received 8 April 2011 / Accepted 15 August 2011 ABSTRACT Context. In 2009 we started an intense radial-velocity monitoring of a few nearby, slowly-rotating and quiet solar-type stars within the dedicated HARPS-Upgrade GTO program. Aims. The goal of this campaign is to gather very-precise radial-velocity data with high cadence and continuity to detect tiny signatures of very-low-mass stars that are potentially present in the habitable zone of their parent stars. Methods. Ten stars were selected among the most stable stars of the original HARPS high-precision program that are uniformly spread in hour angle, such that three to four of them are observable at any time of the year.