Searching for Gas Giant Planets on Solar System Scales – a NACO/APP L-Band Survey of A- and F-Type Main-Sequence Stars
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Search for Associations Containing Young Stars (SACY). V. Is
Astronomy & Astrophysics manuscript no. sacy˙1˙accepted˙arxiv˙2 c ESO 2018 October 2, 2018 Search for associations containing young stars (SACY) V. Is multiplicity universal? Tight multiple systems?;??;??? P. Elliott1;2, A. Bayo1;3;4, C. H. F. Melo1, C. A. O. Torres5, M. Sterzik1, and G. R. Quast5 1 European Southern Observatory, Alonso de Cordova 3107, Vitacura Casilla 19001, Santiago 19, Chile e-mail: [email protected] 2 School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL 3 Max Planck Institut fur¨ Astronomie, Konigstuhl¨ 17, 69117, Heidelberg, Germany 4 Departamento de F´ısica y Astronom´ıa, Facultad de Ciencias, Universidad de Valpara´ıso, Av. Gran Bretana˜ 1111, 5030 Casilla, Valpara´ıso, Chile 5 Laboratorio´ Nacional de Astrof´ısica/ MCT, Rua Estados Unidos 154, 37504-364 Itajuba´ (MG), Brazil Received 21 March 2014 / Accepted 5 June 2014 ABSTRACT Context. Dynamically undisrupted, young populations of stars are crucial in studying the role of multiplicity in relation to star formation. Loose nearby associations provide us with a great sample of close (<150 pc) pre-main sequence (PMS) stars across the very important age range (≈5-70 Myr) to conduct such research. Aims. We characterize the short period multiplicity fraction of the search for associations containing young stars (SACY) sample, accounting for any identifiable bias in our techniques and present the role of multiplicity fractions of the SACY sample in the context of star formation. Methods. Using the cross-correlation technique we identified double-lined and triple-lined spectroscopic systems (SB2/SB3s), in addition to this we computed radial velocity (RV) values for our subsample of SACY targets using several epochs of fiber-fed extended range optical spectrograph (FEROS) and ultraviolet and visual echelle spectrograph (UVES) data. -
Search for Associations Containing Young Stars (SACY) VII
A&A 590, A13 (2016) Astronomy DOI: 10.1051/0004-6361/201628253 & c ESO 2016 Astrophysics Search for associations containing young stars (SACY) VII. New stellar and substellar candidate members in the young associations?,?? P. Elliott1; 2, A. Bayo3, C. H. F. Melo1, C. A. O. Torres4, M. F. Sterzik5, G. R. Quast4, D. Montes6, and R. Brahm7; 8 1 European Southern Observatory, Alonso de Cordova 3107, Vitacura Casilla 19001, Santiago 19, Chile e-mail: [email protected] 2 School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL 3 Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, 5030 Casilla, Valparaíso, Chile 4 Laboratório Nacional de Astrofísica/ MCT, Rua Estados Unidos 154, 37504-364 Itajubá (MG), Brazil 5 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 6 Departamento de Astrofísica y Ciencias de la Atmósfera, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain 7 Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile 8 Millennium Institute of Astrophysics, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile Received 4 February 2016 / Accepted 7 March 2016 ABSTRACT Context. The young associations offer us one of the best opportunities to study the properties of young stellar and substellar objects and to directly image planets thanks to their proximity (<200 pc) and age (≈5−150 Myr). However, many previous works have been limited to identifying the brighter, more active members (≈1 M ) owing to photometric survey sensitivities limiting the detections of lower mass objects. -
Searching for Gas Giant Planets on Solar System Scales-A NACO/APP
Mon. Not. R. Astron. Soc. 000, 1–8 (2015) Printed 2 June 2021 (MN LATEX style file v2.2) Searching for gas giant planets on Solar System scales - A NACO/APP L′-band survey of A- and F-type Main Sequence stars T. Meshkat,1⋆ M. A. Kenworthy,1 M. Reggiani,2 S. P. Quanz,2 E. E. Mamajek,3 M. R. Meyer2 1Leiden Observatory, P.O. Box 9513, Niels Bohrweg 2, 2300 RA Leiden, The Netherlands 2Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland 3Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627-0171, USA 2015 March 17 ABSTRACT We report the results of a direct imaging survey of A- and F-type main sequence stars search- ing for giant planets. A/F stars are often the targets of surveys, as they are thought to have more massive giant planets relative to solar-type stars. However, most imaging is only sensi- tive to orbital separations > 30 AU, where it has been demonstrated that giant planets are rare. In this survey, we take advantage of the high-contrast capabilities of the Apodizing Phase Plate coronagraph on NACO at the Very Large Telescope. Combined with optimized princi- pal component analysis post-processing, we are sensitive to planetary-mass companions (2 ′ to 12 MJup) at Solar System scales (630 AU). We obtained data on 13 stars in L -band and detected one new companion as part of this survey: an M6.0 ± 0.5 dwarf companion around HD 984. We re-detect low-mass companions around HD 12894 and HD 20385, both reported shortly after the completion of this survey. -
Extrasolar Planets and Brown Dwarfs Around A–F Type Stars VI
A&A 495, 335–352 (2009) Astronomy DOI: 10.1051/0004-6361:200810105 & c ESO 2009 Astrophysics Extrasolar planets and brown dwarfs around A–F type stars VI. High precision RV survey of early type dwarfs with HARPS A.-M. Lagrange1, M. Desort1,F.Galland1,S.Udry2, and M. Mayor2 1 Laboratoire d’Astrophysique de l’Observatoire de Grenoble, Université Joseph Fourier, BP 53, 38041 Grenoble, France e-mail: [email protected] 2 Observatoire de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland Received 30 April 2008 / Accepted 10 October 2008 ABSTRACT Aims. Systematic surveys to search for exoplanets have been mostly dedicated to solar-type stars sofar. We developed in 2004 a method to extend such searches to earlier A−F type dwarfs and started spectroscopic surveys to search for planets and quantify the detection limit achievable when taking the stars properties (Spectral Type, v sin i) and their actual levels of intrinsic variations into account. We give here the first results of our southern survey with HARPS. Methods. We observed 185 A–F (B − V in the range [−0.1; 0.6]) stars with HARPS and analysed them with our dedicated software. We used several criteria to probe different origins for the radial-velocity variations – stellar activity (spots, pulsations) or companions: bisector shape, radial-velocity variations amplitudes, and timescales. Results. 1) Sixty-four percent of the 170 stars with enough data points are found to be variable. Twenty are found to be binaries or candidate binaries (with stars or brown dwarfs). More than 80% of the latest type stars (once binaries are removed), are intrinsically variable at a 2 m s−1precision level. -
Banyan. Ix. the Initial Mass Function and Planetary-Mass Object Space Density of the Tw Hya Association
To appear in ApJS. Preprint typeset using LATEX style AASTeX6 v. 1.0 BANYAN. IX. THE INITIAL MASS FUNCTION AND PLANETARY-MASS OBJECT SPACE DENSITY OF THE TW HYA ASSOCIATION Jonathan Gagne´1,2, Jacqueline K. Faherty1,3, Eric E. Mamajek4,5, Lison Malo6,7, Rene´ Doyon7, Joseph C. Filippazzo8, Alycia J. Weinberger1, Jessica K. Donaldson1,Sebastien´ Lepine´ 9, David Lafreniere` 7, Etienne´ Artigau7, Adam J. Burgasser10, Dagny Looper11, Anne Boucher7, Yuri Beletsky12, Sara Camnasio13, Charles Brunette7, Genevieve` Arboit7 1 Carnegie Institution of Washington DTM, 5241 Broad Branch Road NW, Washington, DC 20015, USA; [email protected] 2 NASA Sagan Fellow 3 NASA Hubble Fellow 4 Department of Physics & Astronomy, University of Rochester, Rochester, NY 14627, USA 5Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 6 Canada-France-Hawaii Telescope, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USA 7 Institute for Research on Exoplanets, Universit´ede Montr´eal,D´epartement de Physique, C.P. 6128 Succ. Centre-ville, Montr´eal,QC H3C 3J7, Canada 8 Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA 9 Department of Physics and Astronomy, Georgia State University, 25 Park Place, Atlanta, GA 30302, USA 10 Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Dr., Mail Code 0424, La Jolla, CA 92093, USA 11 New York University Tisch School of the Arts, 721 Broadway, 10th floor, New York, NY 10003, USA 12 Las Campanas Observatory, Carnegie Institution of Washington, Colina el Pino, Casilla 601 La Serena, Chile 13 Department of Physics and Astronomy, Hunter College, City University of New York, NY 10065, USA ABSTRACT A determination of the initial mass function (IMF) of the current, incomplete census of the 10 Myr- old TW Hya association (TWA) is presented. -
Search for Associations Containing Young Stars (SACY). VII. New Stellar
Astronomy & Astrophysics manuscript no. new˙members˙language˙corrected˙upload c ESO 2016 April 14, 2016 Search for associations containing young stars (SACY) VII. New stellar and substellar candidate members in the young associations?;?? P. Elliott1;2, A. Bayo3, C. H. F. Melo1, C. A. O. Torres4, M. F. Sterzik5, G. R. Quast4, D. Montes6, and R. Brahm7;8 1 European Southern Observatory, Alonso de Cordova 3107, Vitacura Casilla 19001, Santiago 19, Chile e-mail: [email protected] 2 School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL 3 Departamento de F´ısica y Astronom´ıa, Facultad de Ciencias, Universidad de Valpara´ıso, Av. Gran Bretana˜ 1111, 5030 Casilla, Valpara´ıso, Chile 4 Laboratorio´ Nacional de Astrof´ısica/ MCT, Rua Estados Unidos 154, 37504-364 Itajuba´ (MG), Brazil 5 European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany 6 Departamento de Astrof´ısica y Ciencias de la Atmosfera,´ Facultad de Ciencias F´ısicas, Universidad Complutense de Madrid, 28040 Madrid, Spain 7 Instituto de Astrof´ısica, Facultad de F´ısica, Pontificia Universidad Catolica´ de Chile, Av. Vicuna˜ Mackenna 4860, 7820436 Macul, Santiago, Chile 8 Millennium Institute of Astrophysics, Av. Vicuna˜ Mackenna 4860, 7820436 Macul, Santiago, Chile Received 4 February 2016; accepted 7 March 2016 ABSTRACT Context. The young associations offer us one of the best opportunities to study the properties of young stellar and substellar objects and to directly image planets thanks to their proximity (<200 pc) and age (≈5-150 Myr). However, many previous works have been limited to identifying the brighter, more active members (≈1 M ) owing to photometric survey sensitivities limiting the detections of lower mass objects. -
Kappa Crateris
Kappa Crateris Kappa Crateris has a visual companion: a magnitude 13.0 star located at an angular separation of 24.6 arc seconds along a position angle of 343°, as of 2000.[10]. References. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653â“664, arXiv:0708.1752 , Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. Psi Crateris (Psi Crateris) is a star in the constellation of Crater. The star can be located at the coordinates of Declination (-18d 29` 59.3) and Right Ascension(11h 12m 30.38) Based on the spectral type (A0V), the star is a blue main sequence dwarf star. Psi Crateris is a blue main sequence dwarf star that can be located in the constellation of Crater. The description is based on the spectral class. Psi Crateris is not part of the constellation but is within the borders of the constellation. Kappa Crateris. Quite the same Wikipedia. Just better. Kappa Crateris (κ Crt) is the Bayer designation for a star in the southern constellation of Crater. It has an apparent visual magnitude of 5.94,[2] which, according to the Bortle scale, can be seen with the naked eye under dark suburban skies. The distance to this star, as determined from an annual parallax shift of 14.27 mas,[1] is around 229 light years. Kappa Crateris has a visual companion: a magnitude 13.0 star located at an angular separation of 24.6 arc seconds along a position angle of 343°, as of 2000.[10].