A Lucky Imaging Multiplicity Study of Exoplanet Host Stars – II
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. -
Homogeneous Spectroscopic Parameters for Bright Planet Host Stars from the Northern Hemisphere the Impact on Stellar and Planetary Mass (Research Note)
A&A 576, A94 (2015) Astronomy DOI: 10.1051/0004-6361/201425227 & c ESO 2015 Astrophysics Homogeneous spectroscopic parameters for bright planet host stars from the northern hemisphere The impact on stellar and planetary mass (Research Note) S. G. Sousa1,2,N.C.Santos1,2, A. Mortier1,3,M.Tsantaki1,2, V. Adibekyan1, E. Delgado Mena1,G.Israelian4,5, B. Rojas-Ayala1,andV.Neves6 1 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal 3 SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews KY16 9SS, UK 4 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain 5 Departamento de Astrofísica, Universidade de La Laguna, 38205 La Laguna, Tenerife, Spain 6 Departamento de Física, Universidade Federal do Rio Grande do Norte, Brazil Received 27 October 2014 / Accepted 19 February 2015 ABSTRACT Aims. In this work we derive new precise and homogeneous parameters for 37 stars with planets. For this purpose, we analyze high resolution spectra obtained by the NARVAL spectrograph for a sample composed of bright planet host stars in the northern hemisphere. The new parameters are included in the SWEET-Cat online catalogue. Methods. To ensure that the catalogue is homogeneous, we use our standard spectroscopic analysis procedure, ARES+MOOG, to derive effective temperatures, surface gravities, and metallicities. These spectroscopic stellar parameters are then used as input to compute the stellar mass and radius, which are fundamental for the derivation of the planetary mass and radius. -
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. -
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. -
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 -
121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S. -
RV Metric New Monday
A Science Metric for Direct Characterization of Known Radial-Velocity Exoplanets Robert A. Brown Space Telescope Science Institute [email protected] June 17, 2013 Abstract Known RV exoplanets are viewed as prime targets for a future high-contrast imaging mission, which may be able to detect and characterize these enigmatic objects in reflected starlight. To help define and differentiate the candidates for such a mission on the basis of scientific performance, and to help set realistic expectations, we develop a science metric, NRV, defined as the estimated number of planets that would be detected and characterized by such a mission. In this report, we estimate upper limits to NRV for missions with apertures in the range 1–2.4 m. We treat both star-shade and coronagraphic missions. 1. Introduction We define the science metric NRV to be the number of known RV exoplanets that satisfy four criteria: #1 permitted pointing: during observations, the angle between the host star and the sun (γ ) must be greater than the solar avoidance angle, γ > γ 1 and, for a star- shade mission, it must also be less than the angle at which the star shade appears illuminated, γ < γ 2 #2 systematic limit: the flux ratio of the planet to the host star, expressed in delta magnitudes ( Δmag ), must be better than the systematic limit in delta magnitudes ( Δmag0 ), i.e. Δmag < Δmag0 #3 wavelength: criteria #1–2 must be satisfied at all wavelengths deemed critical for planet detection and characterization, and particularly for the coronagraph, at the longest critical wavelength (λlc) #4 time: criteria #1–3 must be satisfied at some time during the mission for at least as long as the exposure time required for detection or characterization of a planet as faint as the systematic limit. -
The Study of Astronomical Transients in the Infrared
The Study of Astronomical Transients in the Infrared by Robert Strausbaugh A Dissertation Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy Approved May 2019 by the Graduate Supervisory Committee: Nathaniel Butler, Chair Rolf Jansen Phillip Mauskopf Rogier Windhorst ARIZONA STATE UNIVERSITY August 2019 ©2019 Robert Strausbaugh All Rights Reserved ABSTRACT Several key, open questions in astrophysics can be tackled by searching for and mining large datasets for transient phenomena. The evolution of massive stars and compact objects can be studied over cosmic time by identifying supernovae (SNe) and gamma-ray bursts (GRBs) in other galaxies and determining their redshifts. Modeling GRBs and their afterglows to probe the jets of GRBs can shed light on the emission mechanism, rate, and energetics of these events. In Chapter 1, I discuss the current state of astronomical transient study, including sources of interest, instrumentation, and data reduction techniques, with a focus on work in the infrared. In Chapter 2, I present original work published in the Proceedings of the Astronomical Society of the Pacific, testing InGaAs infrared detectors for astronomical use (Strausbaugh, Jackson, and Butler 2018); highlights of this work include observing the exoplanet transit of HD189773B, and detecting the nearby supernova SN2016adj with an InGaAs detector mounted on a small telescope at ASU. In Chapter 3, I discuss my work on GRB jets published in the Astrophysical Journal Letters, highlighting the interesting case of GRB 160625B (Strausbaugh et al. 2019), where I interpret a late-time bump in the GRB afterglow lightcurve as evidence for a bright-edged jet. -
SILICON and OXYGEN ABUNDANCES in PLANET-HOST STARS Erik Brugamyer, Sarah E
The Astrophysical Journal, 738:97 (11pp), 2011 September 1 doi:10.1088/0004-637X/738/1/97 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. SILICON AND OXYGEN ABUNDANCES IN PLANET-HOST STARS Erik Brugamyer, Sarah E. Dodson-Robinson, William D. Cochran, and Christopher Sneden Department of Astronomy and McDonald Observatory, University of Texas at Austin, 1 University Station C1400, Austin, TX 78712, USA; [email protected] Received 2011 February 4; accepted 2011 June 22; published 2011 August 16 ABSTRACT The positive correlation between planet detection rate and host star iron abundance lends strong support to the core accretion theory of planet formation. However, iron is not the most significant mass contributor to the cores of giant planets. Since giant planet cores are thought to grow from silicate grains with icy mantles, the likelihood of gas giant formation should depend heavily on the oxygen and silicon abundance of the planet formation environment. Here we compare the silicon and oxygen abundances of a set of 76 planet hosts and a control sample of 80 metal-rich stars without any known giant planets. Our new, independent analysis was conducted using high resolution, high signal-to-noise data obtained at McDonald Observatory. Because we do not wish to simply reproduce the known planet–metallicity correlation, we have devised a statistical method for matching the underlying [Fe/H] distributions of our two sets of stars. We find a 99% probability that planet detection rate depends on the silicon abundance of the host star, over and above the observed planet–metallicity correlation. -
VEGA Science Review P
The CHARA Science Meeting 2021 VEGA Science Review P. Berio, L. Bigot, D. Bonneau, M. Challouf, O. Chesneau, J.M. Clausse, O. Creevey, O. Delaa, A. Domiciano, N. Jamialahmadi, R. Ligi, F. Millour, A. Meilland, F. Morand, D. Mourard, N. Nardetto, K. Perraut, E. Saldanha, A. Salsi, A. Spang, P. Stee, I. Tallon-Bosc on behalf the VEGA team VEGA Science Review 1 The CHARA Science Meeting 2021 VEGA in a few important dates 2005 - May: 1st email exchanges - November: 1st visit on the Mountain 2006 Green light after the Tucson 2-year CHARA Science Meeting 2007 - August: 8 boxes weighting about 1200 kg sent to Mt Wilson - September, 30th: 1st 2T fringes (after 3 weeks of integration) 2008 - October: 3T fringes 2009 - Summer: First remote operation 2010 - May: simultaneous CLIMB and VEGA operation - Oct, 12th: 4T fringes together with MIRC 2012 Upgraded detectors and group delay tracking VEGA Science Review 2 The CHARA Science Meeting 2021 VEGA niches Limiting magnitude Rmag = 8 @ R ~ 5000 Very high angular resolution Spectral resolution (λ/2B ~ 0.4 mas @ 330 m) (R ~ 5000, 30000) Accurate angular diameters Kinematics and environments [Mourard+2015] ] [Ligi+2016 Circumstellar disks, mass-loss, winds, chromospheric activity, spectro-imaging Fundamental parameters, Surface-Brightness Relations, parameters of multiple and hierarchic systems VEGA Science Review 3 The CHARA Science Meeting 2021 VEGA operation in a few figures 47 refereed papers • 509 nights with recorded data • 770 stars VEGA Publications 10 • 8500 observations 8 6 4 2 During these -
Download This Article in PDF Format
A&A 621, A87 (2019) Astronomy https://doi.org/10.1051/0004-6361/201833431 & © ESO 2019 Astrophysics Extrasolar planets and brown dwarfs around AF-type stars X. The SOPHIE sample: combining the SOPHIE and HARPS surveys to compute the close giant planet mass-period distribution around AF-type stars?,?? S. Borgniet1, A.-M. Lagrange1, N. Meunier1, F. Galland1, L. Arnold2, N. Astudillo-Defru3, J.-L. Beuzit1, I. Boisse4, X. Bonfils1, F. Bouchy4,5, K. Debondt1, M. Deleuil4, X. Delfosse1, M. Desort1, R. F. Díaz5, A. Eggenberger5, D. Ehrenreich5, T. Forveille1, G. Hébrard2,6, B. Loeillet6, C. Lovis5, G. Montagnier2,6, C. Moutou4,7, F. Pepe5, C. Perrier1, F. Pont5, D. Queloz5,8, A. Santerne4, N. C. Santos9,10, D. Ségransan5, R. da Silva11,12, J. P. Sivan2, S. Udry5, and A. Vidal-Madjar6 1 CNRS, IPAG, Université Grenoble Alpes, 38000 Grenoble, France e-mail: [email protected] 2 Observatoire de Haute-Provence, Institut Pythéas UMS 3470, CNRS, Aix-Marseille Université, 04870 St-Michel-l’Observatoire, France 3 Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile 4 LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, CNRS, Aix Marseille Université, 13388 Marseille, France 5 Observatoire Astronomique de l’Université de Genève, 51 Chemin des Maillettes, 1290 Versoix, Switzerland 6 Institut d’Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie, 98 bis Boulevard Arago, 75014 Paris, France 7 Canada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USA 8 Cavendish Laboratory, -
Determination of Stellar Parameters for M-Dwarf Stars: the NIR Approach
Determination of stellar parameters for M-dwarf stars: the NIR approach by Daniel Thaagaard Andreasen A thesis submitted in conformity with the requirements for the degree of Doctor of Philosophy Graduate Department of Departamento de Fisica e Astronomia University of Porto c Copyright 2017 by Daniel Thaagaard Andreasen Dedication To Linnea, Henriette, Rico, and Else For always supporting me ii Acknowledgements When doing a PhD it is important to remember it is more a team effort than the work of an individual. This is something I learned quickly during the last four years. Therefore there are several people I would like to thank. First and most importantly are my two supervisors, Sérgio and Nuno. They were after me in the beginning of my studies because I was too shy to ask for help; something that I quickly learned I needed to do. They always had their door open for me and all my small questions. It goes without saying that I am thankful for all their guidance during my studies. However, what I am most thankful for is the freedom I have had to explorer paths and ideas on my own, and with them safely on the sideline. This sometimes led to failures and dead ends, but it make me grow as a researcher both by learning from my mistake, but also by prioritising my time. When I thank Sérgio and Nuno, my official supervisors, I also have to thank Elisa. She has been my third unofficial supervisor almost from the first day. Although she did not have any experience with NIR spectroscopy, she was never afraid of giving her opinion and trying to help.