Ground-Based Capabilities for General Astrophysics and Exoplanets Science
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The Hunt for Exomoons with Kepler (Hek)
The Astrophysical Journal, 777:134 (17pp), 2013 November 10 doi:10.1088/0004-637X/777/2/134 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE HUNT FOR EXOMOONS WITH KEPLER (HEK). III. THE FIRST SEARCH FOR AN EXOMOON AROUND A HABITABLE-ZONE PLANET∗ D. M. Kipping1,6, D. Forgan2, J. Hartman3, D. Nesvorny´ 4,G.A.´ Bakos3, A. Schmitt7, and L. Buchhave5 1 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA; [email protected] 2 Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK 3 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 05844, USA 4 Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA 5 Niels Bohr Institute, Copenhagen University, Denmark Received 2013 June 4; accepted 2013 September 8; published 2013 October 22 ABSTRACT Kepler-22b is the first transiting planet to have been detected in the habitable zone of its host star. At 2.4 R⊕, Kepler-22b is too large to be considered an Earth analog, but should the planet host a moon large enough to maintain an atmosphere, then the Kepler-22 system may yet possess a telluric world. Aside from being within the habitable zone, the target is attractive due to the availability of previously measured precise radial velocities and low intrinsic photometric noise, which has also enabled asteroseismology studies of the star. For these reasons, Kepler-22b was selected as a target-of-opportunity by the “Hunt for Exomoons with Kepler” (HEK) project. In this work, we conduct a photodynamical search for an exomoon around Kepler-22b leveraging the transits, radial velocities, and asteroseismology plus several new tools developed by the HEK project to improve exomoon searches. -
2018 Workshop on Autonomy for Future NASA Science Missions
NOTE: This document was prepared by a team that participated in the 2018 Workshop on Autonomy for Future NASA Science Missions. It is for informational purposes to inform discussions regarding the use of autonomy in notional science missions and does not specify Agency plans or directives. 2018 Workshop on Autonomy for Future NASA Science Missions: Ocean Worlds Design Reference Mission Reports Table of Contents Introduction .................................................................................................................................... 2 The Ocean Worlds Design Reference Mission Report .................................................................... 3 Ocean Worlds Design Reference Mission Report Summary ........................................................ 20 1 NOTE: This document was prepared by a team that participated in the 2018 Workshop on Autonomy for Future NASA Science Missions. It is for informational purposes to inform discussions regarding the use of autonomy in notional science missions and does not specify Agency plans or directives. Introduction Autonomy is changing our world; commercial enterprises and academic institutions are developing and deploying drones, robots, self-driving vehicles and other autonomous capabilities to great effect here on Earth. Autonomous technologies will also play a critical and enabling role in future NASA science missions, and the Agency requires a specific strategy to leverage these advances and infuse them into its missions. To address this need, NASA sponsored the -
CARMENES Input Catalogue of M Dwarfs IV. New Rotation Periods from Photometric Time Series
Astronomy & Astrophysics manuscript no. pk30 c ESO 2018 October 9, 2018 CARMENES input catalogue of M dwarfs IV. New rotation periods from photometric time series E. D´ıezAlonso1;2;3, J. A. Caballero4, D. Montes1, F. J. de Cos Juez2, S. Dreizler5, F. Dubois6, S. V. Jeffers5, S. Lalitha5, R. Naves7, A. Reiners5, I. Ribas8;9, S. Vanaverbeke10;6, P. J. Amado11, V. J. S. B´ejar12;13, M. Cort´es-Contreras4, E. Herrero8;9, D. Hidalgo12;13;1, M. K¨urster14, L. Logie6, A. Quirrenbach15, S. Rau6, W. Seifert15, P. Sch¨ofer5, and L. Tal-Or5;16 1 Departamento de Astrof´ısicay Ciencias de la Atm´osfera, Facultad de Ciencias F´ısicas,Universidad Complutense de Madrid, E-280140 Madrid, Spain; e-mail: [email protected] 2 Departamento de Explotaci´ony Prospecci´onde Minas, Escuela de Minas, Energ´ıay Materiales, Universidad de Oviedo, E-33003 Oviedo, Asturias, Spain 3 Observatorio Astron´omicoCarda, Villaviciosa, Asturias, Spain (MPC Z76) 4 Centro de Astrobiolog´ıa(CSIC-INTA), Campus ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Ca~nada,Madrid, Spain 5 Institut f¨ur Astrophysik, Georg-August-Universit¨at G¨ottingen, Friedrich-Hund-Platz 1, D-37077 G¨ottingen, Germany 6 AstroLAB IRIS, Provinciaal Domein \De Palingbeek", Verbrandemolenstraat 5, B-8902 Zillebeke, Ieper, Belgium 7 Observatorio Astron´omicoNaves, Cabrils, Barcelona, Spain (MPC 213) 8 Institut de Ci`enciesde l'Espai (CSIC-IEEC), Campus UAB, c/ de Can Magrans s/n, E-08193 Bellaterra, Barcelona, Spain 9 Institut d'Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain 10 -
Breakthrough Propulsion Study Assessing Interstellar Flight Challenges and Prospects
Breakthrough Propulsion Study Assessing Interstellar Flight Challenges and Prospects NASA Grant No. NNX17AE81G First Year Report Prepared by: Marc G. Millis, Jeff Greason, Rhonda Stevenson Tau Zero Foundation Business Office: 1053 East Third Avenue Broomfield, CO 80020 Prepared for: NASA Headquarters, Space Technology Mission Directorate (STMD) and NASA Innovative Advanced Concepts (NIAC) Washington, DC 20546 June 2018 Millis 2018 Grant NNX17AE81G_for_CR.docx pg 1 of 69 ABSTRACT Progress toward developing an evaluation process for interstellar propulsion and power options is described. The goal is to contrast the challenges, mission choices, and emerging prospects for propulsion and power, to identify which prospects might be more advantageous and under what circumstances, and to identify which technology details might have greater impacts. Unlike prior studies, the infrastructure expenses and prospects for breakthrough advances are included. This first year's focus is on determining the key questions to enable the analysis. Accordingly, a work breakdown structure to organize the information and associated list of variables is offered. A flow diagram of the basic analysis is presented, as well as more detailed methods to convert the performance measures of disparate propulsion methods into common measures of energy, mass, time, and power. Other methods for equitable comparisons include evaluating the prospects under the same assumptions of payload, mission trajectory, and available energy. Missions are divided into three eras of readiness (precursors, era of infrastructure, and era of breakthroughs) as a first step before proceeding to include comparisons of technology advancement rates. Final evaluation "figures of merit" are offered. Preliminary lists of mission architectures and propulsion prospects are provided. -
Alien Maps of an Ocean-Bearing World
Alien Maps of an Ocean-Bearing World The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Cowan, Nicolas B., Eric Agol, Victoria S. Meadows, Tyler Robinson, Timothy A. Livengood, Drake Deming, Carey M. Lisse, et al. 2009. Alien maps of an ocean-bearing world. Astrophysical Journal 700(2): 915-923. Published Version doi: 10.1088/0004-637X/700/2/915 Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:4341699 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Open Access Policy Articles, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#OAP Accepted for publication in ApJ A Preprint typeset using LTEX style emulateapj v. 10/09/06 ALIEN MAPS OF AN OCEAN-BEARING WORLD Nicolas B. Cowan1, Eric Agol, Victoria S. Meadows2, Tyler Robinson2, Astronomy Department and Astrobiology Program, University of Washington, Box 351580, Seattle, WA 98195 Timothy A. Livengood3, Drake Deming2, NASA Goddard Space Flight Center, Greenbelt, MD 20771 Carey M. Lisse, Johns Hopkins University Applied Physics Laboratory, SD/SRE, MP3-E167, 11100 Johns Hopkins Road, Laurel, MD 20723 Michael F. A’Hearn, Dennis D. Wellnitz, Department of Astronomy, University of Maryland, College Park MD 20742 Sara Seager, Department of Earth, Atmospheric, and Planetary Sciences, Dept of Physics, Massachusetts Institute of Technology, 77 Massachusetts Ave. 54-1626, MA 02139 David Charbonneau, Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 and the EPOXI Team Accepted for publication in ApJ ABSTRACT When Earth-mass extrasolar planets first become detectable, one challenge will be to determine which of these worlds harbor liquid water, a widely used criterion for habitability. -
100 Closest Stars Designation R.A
100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79, -
The Solar Neighborhood VI: New Southern Stars Identified by Optical
To appear in the April 2002 issue of the Astronomical Journal The Solar Neighborhood VI: New Southern Nearby Stars Identified by Optical Spectroscopy Todd J. Henry1 Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30303 Lucianne M. Walkowicz Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 Todd C. Barto1 Lockheed Martin Aeronautics Company, Boulder, CO 80306 and David A. Golimowski Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 ABSTRACT Broadband optical spectra are presented for 34 known and candidate nearby stars in the southern sky. Spectral types are determined using a new method that compares the entire spectrum with spectra of more than 100 standard stars. We estimate distances to 13 candidate nearby stars using our spectra and new or published photometry. Six of these stars are probably within 25 pc, and two are likely to be within the RECONS horizon of 10 pc. arXiv:astro-ph/0112496v1 20 Dec 2001 Subject headings: stars: distances — stars: low mass, brown dwarfs — white dwarfs — surveys 1. Introduction The nearest stars have received renewed scrutiny because of their importance to fundamental astrophysics (e.g., stellar atmospheres, the mass content of the Galaxy) and because of their poten- tial for harboring planetary systems and life (e.g., the NASA Origins and Astrobiology initiatives). 1Visiting Astronomer, Cerro Tololo Inter-American Observatory. CTIO is operated by AURA, Inc. under contract to the National Science Foundation. – 2 – The smallest stars, the M dwarfs, account for at least 70% of all stars in the solar neighborhood and make up nearly half of the Galaxy’s total stellar mass (Henry et al. -
The Transfiguration in the Theology of Gregory Palamas And
Duquesne University Duquesne Scholarship Collection Electronic Theses and Dissertations Spring 2015 Deus in se et Deus pro nobis: The rT ansfiguration in the Theology of Gregory Palamas and Its Importance for Catholic Theology Cory Hayes Follow this and additional works at: https://dsc.duq.edu/etd Recommended Citation Hayes, C. (2015). Deus in se et Deus pro nobis: The rT ansfiguration in the Theology of Gregory Palamas and Its Importance for Catholic Theology (Doctoral dissertation, Duquesne University). Retrieved from https://dsc.duq.edu/etd/640 This Immediate Access is brought to you for free and open access by Duquesne Scholarship Collection. It has been accepted for inclusion in Electronic Theses and Dissertations by an authorized administrator of Duquesne Scholarship Collection. For more information, please contact [email protected]. DEUS IN SE ET DEUS PRO NOBIS: THE TRANSFIGURATION IN THE THEOLOGY OF GREGORY PALAMAS AND ITS IMPORTANCE FOR CATHOLIC THEOLOGY A Dissertation Submitted to the McAnulty Graduate School of Liberal Arts Duquesne University In partial fulfillment of the requirements for the degree of Doctor of Philosophy By Cory J. Hayes May 2015 Copyright by Cory J. Hayes 2015 DEUS IN SE ET DEUS PRO NOBIS: THE TRANSFIGURATION IN THE THEOLOGY OF GREGORY PALAMAS AND ITS IMPORTANCE FOR CATHOLIC THEOLOGY By Cory J. Hayes Approved March 31, 2015 _______________________________ ______________________________ Dr. Bogdan Bucur Dr. Radu Bordeianu Associate Professor of Theology Associate Professor of Theology (Committee Chair) (Committee Member) _______________________________ Dr. Christiaan Kappes Professor of Liturgy and Patristics Saints Cyril and Methodius Byzantine Catholic Seminary (Committee Member) ________________________________ ______________________________ Dr. James Swindal Dr. -
Useful Constants
Appendix A Useful Constants A.1 Physical Constants Table A.1 Physical constants in SI units Symbol Constant Value c Speed of light 2.997925 × 108 m/s −19 e Elementary charge 1.602191 × 10 C −12 2 2 3 ε0 Permittivity 8.854 × 10 C s / kgm −7 2 μ0 Permeability 4π × 10 kgm/C −27 mH Atomic mass unit 1.660531 × 10 kg −31 me Electron mass 9.109558 × 10 kg −27 mp Proton mass 1.672614 × 10 kg −27 mn Neutron mass 1.674920 × 10 kg h Planck constant 6.626196 × 10−34 Js h¯ Planck constant 1.054591 × 10−34 Js R Gas constant 8.314510 × 103 J/(kgK) −23 k Boltzmann constant 1.380622 × 10 J/K −8 2 4 σ Stefan–Boltzmann constant 5.66961 × 10 W/ m K G Gravitational constant 6.6732 × 10−11 m3/ kgs2 M. Benacquista, An Introduction to the Evolution of Single and Binary Stars, 223 Undergraduate Lecture Notes in Physics, DOI 10.1007/978-1-4419-9991-7, © Springer Science+Business Media New York 2013 224 A Useful Constants Table A.2 Useful combinations and alternate units Symbol Constant Value 2 mHc Atomic mass unit 931.50MeV 2 mec Electron rest mass energy 511.00keV 2 mpc Proton rest mass energy 938.28MeV 2 mnc Neutron rest mass energy 939.57MeV h Planck constant 4.136 × 10−15 eVs h¯ Planck constant 6.582 × 10−16 eVs k Boltzmann constant 8.617 × 10−5 eV/K hc 1,240eVnm hc¯ 197.3eVnm 2 e /(4πε0) 1.440eVnm A.2 Astronomical Constants Table A.3 Astronomical units Symbol Constant Value AU Astronomical unit 1.4959787066 × 1011 m ly Light year 9.460730472 × 1015 m pc Parsec 2.0624806 × 105 AU 3.2615638ly 3.0856776 × 1016 m d Sidereal day 23h 56m 04.0905309s 8.61640905309 -
Open Batalha-Dissertation.Pdf
The Pennsylvania State University The Graduate School Eberly College of Science A SYNERGISTIC APPROACH TO INTERPRETING PLANETARY ATMOSPHERES A Dissertation in Astronomy and Astrophysics by Natasha E. Batalha © 2017 Natasha E. Batalha Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy August 2017 The dissertation of Natasha E. Batalha was reviewed and approved∗ by the following: Steinn Sigurdsson Professor of Astronomy and Astrophysics Dissertation Co-Advisor, Co-Chair of Committee James Kasting Professor of Geosciences Dissertation Co-Advisor, Co-Chair of Committee Jason Wright Professor of Astronomy and Astrophysics Eric Ford Professor of Astronomy and Astrophysics Chris Forest Professor of Meteorology Avi Mandell NASA Goddard Space Flight Center, Research Scientist Special Signatory Michael Eracleous Professor of Astronomy and Astrophysics Graduate Program Chair ∗Signatures are on file in the Graduate School. ii Abstract We will soon have the technological capability to measure the atmospheric compo- sition of temperate Earth-sized planets orbiting nearby stars. Interpreting these atmospheric signals poses a new challenge to planetary science. In contrast to jovian-like atmospheres, whose bulk compositions consist of hydrogen and helium, terrestrial planet atmospheres are likely comprised of high mean molecular weight secondary atmospheres, which have gone through a high degree of evolution. For example, present-day Mars has a frozen surface with a thin tenuous atmosphere, but 4 billion years ago it may have been warmed by a thick greenhouse atmosphere. Several processes contribute to a planet’s atmospheric evolution: stellar evolution, geological processes, atmospheric escape, biology, etc. Each of these individual processes affects the planetary system as a whole and therefore they all must be considered in the modeling of terrestrial planets. -
AD Leonis: Flares Observed by XMM-Newton and Chandra
A&A 411, 587–593 (2003) Astronomy DOI: 10.1051/0004-6361:20031398 & c ESO 2003 Astrophysics AD Leonis: Flares observed by XMM-Newton and Chandra E. J. M. van den Besselaar1;2, A. J. J. Raassen1;3,R.Mewe1,R.L.J.vanderMeer1,M.G¨udel4, and M. Audard5 1 SRON National Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands e-mail: [email protected];[email protected];[email protected] 2 Department of Astrophysics, University of Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands 3 Astronomical Institute “Anton Pannekoek”, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands 4 Paul Scherrer Institut, W¨urenlingen & Villigen, 5232 Villigen PSI, Switzerland e-mail: [email protected] 5 Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027, USA e-mail: [email protected] Received 3 February 2003 / Accepted 2 September 2003 Abstract. The M-dwarf AD Leonis has been observed with the Reflection Grating Spectrometers and the European Photon Imaging Camera aboard XMM-Newton and also with the Low Energy Transmission Grating Spectrometer aboard the Chandra X-ray Observatory. In the observation taken with XMM-Newton five large flares produced by AD Leo were identified and only one in the observation taken with Chandra. A quiescent level to the lightcurves is difficult to define, since several smaller flares mutually overlap each other. However, we defined a quasi-steady state outside of obvious flares or flare decays. The spectra from the flare state and the quasi-steady state are analysed separately. -
RECONS Discoveries Within 10 Parsecs
The Astronomical Journal, 155:265 (23pp), 2018 June https://doi.org/10.3847/1538-3881/aac262 © 2018. The American Astronomical Society. All rights reserved. The Solar Neighborhood XLIV: RECONS Discoveries within 10 parsecs Todd J. Henry1,8, Wei-Chun Jao2,8 , Jennifer G. Winters3,8 , Sergio B. Dieterich4,8, Charlie T. Finch5,8, Philip A. Ianna1,8, Adric R. Riedel6,8 , Michele L. Silverstein2,8 , John P. Subasavage7,8 , and Eliot Halley Vrijmoet2 1 RECONS Institute, Chambersburg, PA 17201, USA; [email protected], [email protected] 2 Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30302, USA; [email protected], [email protected], [email protected] 3 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA; [email protected] 4 Department of Terrestrial Magnetism, Carnegie Institution for Science, Washington, DC 20015, USA; [email protected] 5 Astrometry Department, U.S. Naval Observatory, Washington, DC 20392, USA; charlie.fi[email protected] 6 Space Telescope Science Institute, Baltimore, MD 21218, USA; [email protected] 7 United States Naval Observatory, Flagstaff, AZ 86001, USA; [email protected] Received 2018 April 12; revised 2018 April 27; accepted 2018 May 1; published 2018 June 4 Abstract We describe the 44 systems discovered to be within 10 pc of the Sun by the RECONS team, primarily via the long- term astrometry program at the CTIO/SMARTS 0.9 m that began in 1999. The systems—including 41 with red dwarf primaries, 2 white dwarfs, and 1 brown dwarf—have trigonometric parallaxes greater than 100 mas, with errors of 0.4–2.4 mas in all but one case.