Vol. 3 on Homogeneous Statistical Distributions Exoplanets for Their Dynamic Parameters
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Enabling Science with Gaia Observations of Naked-Eye Stars
Enabling science with Gaia observations of naked-eye stars J. Sahlmanna,b, J. Mart´ın-Fleitasb,c, A. Morab,c, A. Abreub,d, C. M. Crowleyb,e, E. Jolietb,f aEuropean Space Agency, STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA; bEuropean Space Agency, ESAC, P.O. Box 78, Villanueva de la Canada,˜ 28691 Madrid, Spain; cAurora Technology, Crown Business Centre, Heereweg 345, 2161 CA Lisse, The Netherlands; dElecnor Deimos Space, Ronda de Poniente 19, Ed. Fiteni VI, 28760 Tres Cantos, Madrid, Spain; eHE Space Operations BV, Huygensstraat 44, 2201 DK Noordwijk, The Netherlands; fCalifornia Institute of Technology, Pasadena, CA, 91125, USA ABSTRACT ESA’s Gaia space astrometry mission is performing an all-sky survey of stellar objects. At the beginning of the nominal mission in July 2014, an operation scheme was adopted that enabled Gaia to routinely acquire observations of all stars brighter than the original limit of G∼6, i.e. the naked-eye stars. Here, we describe the current status and extent of those observations and their on-ground processing. We present an overview of the data products generated for G<6 stars and the potential scientific applications. Finally, we discuss how the Gaia survey could be enhanced by further exploiting the techniques we developed. Keywords: Gaia, Astrometry, Proper motion, Parallax, Bright Stars, Extrasolar planets, CCD 1. INTRODUCTION There are about 6000 stars that can be observed with the unaided human eye. Greek astronomer Hipparchus used these stars to define the magnitude system still in use today, in which the faintest stars had an apparent visual magnitude of 6. -
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. -
Gaia Search for Stellar Companions of TESS Objects of Interest
Received 1 July 2020; Revised 29 August 2020; Accepted 18 September 2020 DOI: xxx/xxxx ARTICLE TYPE Gaia Search for stellar Companions of TESS Objects of Interest M. Mugrauer* | K.-U. Michel 1Astrophysikalisches Institut und Universitäts-Sternwarte Jena The first results of a new survey are reported, which explores the 2nd data release Correspondence of the ESA-Gaia mission, in order to search for stellar companions of (Community) M. Mugrauer, Astrophysikalisches Institut und Universitäts-Sternwarte Jena, TESS Objects of Interest and to characterize their properties. In total, 193 binary and Schillergäßchen 2, D-07745 Jena, Germany. 15 hierarchical triple star systems are presented, detected among 1391 target stars, Email: [email protected] which are located at distances closer than about 500 pc around the Sun. The com- panions and the targets are equidistant and share a common proper motion, as it is expected for gravitationally bound stellar systems, proven with their accurate Gaia astrometry. The companions exhibit masses in the range between about 0.08 M⊙ and 3 M⊙ and are most frequently found in the mass range between 0.13 and 0.6 M⊙. The companions are separated from the targets by about 40 up to 9900 au, and their frequency continually decreases with increasing separation. While most of the detected companions are late K to mid M dwarfs, also 5 white dwarf companions were identified in this survey, whose true nature is revealed by their photometric properties. KEYWORDS: binaries: visual, white dwarfs, stars: individual (TOI 249 C, TOI 1259 B, TOI 1624 B, TOI 1703 B, CTOI 53309262 B) 1 INTRODUCTION explored the 2nd data release of the European Space Agency (ESA) Gaia mission (Gaia DR2 from hereon, Gaia Collabora- A key aspect in the diversity of exoplanets is the multiplicity tion, Brown, Vallenari, et al., 2018), which provides manifold of their host stars. -
A Search for Planets Around Intermediate Mass Stars with the Hobby–Eberly Telescope
EPJ Web of Conferences 16, 02005 (2011) DOI: 10.1051/epjconf/20111602005 C Owned by the authors, published by EDP Sciences, 2011 A search for planets around intermediate Mass Stars with the Hobby–Eberly Telescope M. Adamów1,a, S. Gettel2,3, G. Nowak1,P. Zielinski´ 1, A. Niedzielski1 and A. Wolszczan2,3 1Torun´ Centre for Astronomy, Nicolaus Copernicus University, Torun,´ Poland 2Department for Astronomy and Astrophysics, Pennsylvania State University 3Center for Exoplanets and Habitable Worlds Abstract. We present the discovery of sub-stellar mass companions to three stars by the ongoing Penn State – Torun´ Planet Search (PTPS) conducted with the 9.2 m Hobby-Eberly Telescope. 1. INTRODUCTION Searches for planets around giant stars extend studies of planetary system formation and evolution to stars substantially more massive than 1 M (Hatzes et al. 2006; Sato et al. 2008; Niedzielski et al. 2009). Although searches for massive sub-stellar companions to early-type stars are possible (Galland 2005), it is much more efficient to utilize the power of the radial velocity (RV) method by exploiting the many narrow spectral lines of GK-giants, the descendants of the main sequence A-F type stars, sufficient to achieve a < 10 ms−1 RV measurement precision. The GK-giant surveys provide constraints on the efficiency of planet formation as a function of stellar mass and chemical composition. In fact, analyses by Johnson et al. (2007) and Lovis & Mayor (2007) extend to giants the correlation between planetary masses and primary mass that is observed for the lower-mass stars. This is most likely because massive stars tend to have more massive disks. -
The GAPS Programme with HARPS-N at TNG XII
A&A 599, A90 (2017) Astronomy DOI: 10.1051/0004-6361/201629484 & c ESO 2017 Astrophysics The GAPS Programme with HARPS-N at TNG XII. Characterization of the planetary system around HD 108874?,?? S. Benatti1, S. Desidera1, M. Damasso2, L. Malavolta3; 1, A. F. Lanza4, K. Biazzo4, A. S. Bonomo2, R. U. Claudi1, F. Marzari3, E. Poretti5, R. Gratton1, G. Micela6, I. Pagano4, G. Piotto3; 1, A. Sozzetti2, C. Boccato1, R. Cosentino7, E. Covino8, A. Maggio6, E. Molinari7, R. Smareglia9, L. Affer6, G. Andreuzzi7, A. Bignamini9, F. Borsa5, L. di Fabrizio7, M. Esposito8, A. Martinez Fiorenzano7, S. Messina4, P. Giacobbe2, A. Harutyunyan7, C. Knapic9, J. Maldonado6, S. Masiero1, V. Nascimbeni1, M. Pedani7, M. Rainer5, G. Scandariato4, and R. Silvotti2 1 INAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy e-mail: [email protected] 2 INAF–Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025 Pino Torinese, Italy 3 Dipartimento di Fisica e Astronomia Galileo Galilei – Università di Padova, via Francesco Marzolo, 8, Padova, Italy 4 INAF–Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy 5 INAF–Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy 6 INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento, 1, 90134 Palermo, Italy 7 Fundación Galileo Galilei – INAF, Rambla José Ana Fernandez Pérez 7, 38712 Breña Baja, TF, Spain 8 INAF–Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy 9 INAF–Osservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste, Italy Received 5 August 2016 / Accepted 21 November 2016 ABSTRACT In order to understand the observed physical and orbital diversity of extrasolar planetary systems, a full investigation of these objects and of their host stars is necessary. -
Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i, -
A Detailed Analysis of the Hd 73526 2:1 Resonant Planetary System∗
The Astrophysical Journal, 780:140 (9pp), 2014 January 10 doi:10.1088/0004-637X/780/2/140 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. A DETAILED ANALYSIS OF THE HD 73526 2:1 RESONANT PLANETARY SYSTEM∗ Robert A. Wittenmyer1,2,XianyuTan3,4, Man Hoi Lee3,5, Jonathan Horner1,2,C.G.Tinney1,2, R. P. Butler6, G. S. Salter1,2, B. D. Carter7,H.R.A.Jones8, S. J. O’Toole9, J. Bailey1,2, D. Wright1,2,J.D.Crane10, S. A. Schectman10, P. Arriagada6, I. Thompson10, D. Minniti11,12,andM.Diaz11 1 School of Physics, University of New South Wales, Sydney 2052, Australia; [email protected] 2 Australian Centre for Astrobiology, University of New South Wales, Sydney 2052, Australia 3 Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong 4 Department of Planetary Sciences and Lunar and Planetary Laboratory, The University of Arizona, 1629 University Boulevard, Tucson, AZ 85721, USA 5 Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong 6 Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington, DC 20015-1305, USA 7 Faculty of Sciences, University of Southern Queensland, Toowoomba, Queensland 4350, Australia 8 University of Hertfordshire, Centre for Astrophysics Research, Science and Technology Research Institute, College Lane, AL10 9AB, Hatfield, UK 9 Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia 10 The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA 11 Institute of Astrophysics, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22, Chile 12 Vatican Observatory, V00120 Vatican City State, Italy Received 2013 August 14; accepted 2013 November 26; published 2013 December 18 ABSTRACT We present six years of new radial velocity data from the Anglo-Australian and Magellan Telescopes on the HD 73526 2:1 resonant planetary system. -
Today in Astronomy 106: Exoplanets
Today in Astronomy 106: exoplanets The successful search for extrasolar planets Prospects for determining the fraction of stars with planets, and the number of habitable planets per planetary system (fp and ne). T. Pyle, SSC/JPL/Caltech/NASA. 26 May 2011 Astronomy 106, Summer 2011 1 Observing exoplanets Stars are vastly brighter and more massive than planets, and most stars are far enough away that the planets are lost in the glare. So astronomers have had to be more clever and employ the motion of the orbiting planet. The methods they use (exoplanets detected thereby): Astrometry (0): tiny wobble in star’s motion across the sky. Radial velocity (399): tiny wobble in star’s motion along the line of sight by Doppler shift. Timing (9): tiny delay or advance in arrival of pulses from regularly-pulsating stars. Gravitational microlensing (10): brightening of very distant star as it passes behind a planet. 26 May 2011 Astronomy 106, Summer 2011 2 Observing exoplanets (continued) Transits (69): periodic eclipsing of star by planet, or vice versa. Very small effect, about like that of a bug flying in front of the headlight of a car 10 miles away. Imaging (11 but 6 are most likely to be faint stars): taking a picture of the planet, usually by blotting out the star. Of these by far the most useful so far has been the combination of radial-velocity and transit detection. Astrometry and gravitational microlensing of sufficient precision to detect lots of planets would need dedicated, specialized observatories in space. Imaging lots of planets will require 30-meter-diameter telescopes for visible and infrared wavelengths. -
Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55 -
HD45364, a Pair of Planets in a 3: 2 Mean Motion Resonance
Astronomy & Astrophysics manuscript no. 0774 c ESO 2018 November 11, 2018 The HARPS search for southern extra-solar planets⋆ XVI. HD 45364, a pair of planets in a 3:2 mean motion resonance A.C.M. Correia1, S. Udry2, M. Mayor2, W. Benz3, J.-L. Bertaux4, F. Bouchy5, J. Laskar6, C. Lovis2, C. Mordasini3, F. Pepe2, and D. Queloz2 1 Departamento de F´ısica, Universidade de Aveiro, Campus de Santiago, 3810-193 Aveiro, Portugal e-mail: [email protected] 2 Observatoire de Gen`eve, Universit´ede Gen`eve, 51 ch. des Maillettes, 1290 Sauverny, Switzerland e-mail: [email protected] 3 Physikalisches Institut, Universit¨at Bern, Silderstrasse 5, CH-3012 Bern, Switzerland 4 Service d’A´eronomie du CNRS/IPSL, Universit´ede Versailles Saint-Quentin, BP3, 91371 Verri`eres-le-Buisson, France 5 Institut d’Astrophysique de Paris, CNRS, Universit´ePierre et Marie Curie, 98bis Bd Arago, 75014 Paris, France 6 IMCCE, CNRS-UMR8028, Observatoire de Paris, UPMC, 77 avenue Denfert-Rochereau, 75014 Paris, France Received ; accepted To be inserted later ABSTRACT Precise radial-velocity measurements with the HARPS spectrograph reveal the presence of two planets orbiting the solar-type star HD 45364. The companion masses are m sin i = 0.187 MJup and 0.658 MJup, with semi-major axes of a = 0.681 AU and 0.897 AU, and eccentricities of e = 0.168 and 0.097, respectively. A dynamical analysis of the system further shows a 3:2 mean motion resonance between the two planets, which prevents close encounters and ensures the stability of the system over 5 Gyr. -
Precise Radial Velocities of Giant Stars
A&A 555, A87 (2013) Astronomy DOI: 10.1051/0004-6361/201321714 & c ESO 2013 Astrophysics Precise radial velocities of giant stars V. A brown dwarf and a planet orbiting the K giant stars τ Geminorum and 91 Aquarii, David S. Mitchell1,2,SabineReffert1, Trifon Trifonov1, Andreas Quirrenbach1, and Debra A. Fischer3 1 Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 2 Physics Department, California Polytechnic State University, San Luis Obispo, CA 93407, USA e-mail: [email protected] 3 Department of Astronomy, Yale University, New Haven, CT 06511, USA Received 16 April 2013 / Accepted 22 May 2013 ABSTRACT Aims. We aim to detect and characterize substellar companions to K giant stars to further our knowledge of planet formation and stellar evolution of intermediate-mass stars. Methods. For more than a decade we have used Doppler spectroscopy to acquire high-precision radial velocity measurements of K giant stars. All data for this survey were taken at Lick Observatory. Our survey includes 373 G and K giants. Radial velocity data showing periodic variations were fitted with Keplerian orbits using a χ2 minimization technique. Results. We report the presence of two substellar companions to the K giant stars τ Gem and 91 Aqr. The brown dwarf orbiting τ Gem has an orbital period of 305.5±0.1 days, a minimum mass of 20.6 MJ, and an eccentricity of 0.031±0.009. The planet orbiting 91 Aqr has an orbital period of 181.4 ± 0.1 days, a minimum mass of 3.2 MJ, and an eccentricity of 0.027 ± 0.026. -
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