TY - JOUR
T1 - Detection of a low-mass stellar companion to the accelerating A2IV star HR 1645
AU - de Rosa, Robert J.
AU - Nielsen, Eric L.
AU - Rameau, Julien
AU - Duchêne, Gaspard
AU - Greenbaum, Alexandra Z.
AU - Wang, Jason J.
AU - Mark Ammons, S.
AU - Bailey, Vanessa P.
AU - Barman, Travis
AU - Bulger, Joanna
AU - Chilcote, Jeffrey
AU - Cotten, Tara
AU - Doyon, Rene
AU - Esposito, Thomas M.
AU - Fitzgerald, Michael P.
AU - Follette, Katherine B.
AU - Gerard, Benjamin L.
AU - Goodsell, Stephen J.
AU - Graham, James R.
AU - Hibon, Pascale
AU - Hom, Justin
AU - Hung, Li Wei
AU - Ingraham, Patrick
AU - Kalas, Paul
AU - Konopacky, Quinn
AU - Larkin, James E.
AU - Macintosh, Bruce
AU - Maire, Jérôme
AU - Marchis, Franck
AU - Marley, Mark S.
AU - Marois, Christian
AU - Metchev, Stanimir
AU - Millar-Blanchaer, Maxwell A.
AU - Oppenheimer, Rebecca
AU - Palmer, David
AU - Patience, Jennifer
AU - Perrin, Marshall
AU - Poyneer, Lisa
AU - Pueyo, Laurent
AU - Rajan, Abhijith
AU - Rantakyrö, Fredrik T.
AU - Ren, Bin
AU - Ruffio, Jean Baptiste
AU - Savransky, Dmitry
AU - Schneider, Adam C.
AU - Sivaramakrishnan, Anand
AU - Song, Inseok
AU - Soummer, Remi
AU - Tallis, Melisa
AU - Thomas, Sandrine
AU - Kent Wallace, J.
AU - Ward-Duong, Kimberly
AU - Wiktorowicz, Sloane
AU - Wolff, Schuyler
N1 - Funding Information:
Supported by NSF grants AST-1411868 (R.D.R., E.L.N., K. B.F., B.M., and J.P.), AST-141378 (G.D.), AST-1518332 (R. D.R., J.J.W., T.M.E., J.R.G., P.G.K.), and AST1411868 (J.H., J.P.). Supported by NASA grants NNX14AJ80G (R.D.R., E.L. N., S.C.B., B.M., F.M., and M.P.), NNX15AC89G, and NNX15AD95G (R.D.R., B.M., J.E.W., T.M.E., G.D., J.R.G., P.G.K.). This work benefited from NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. J. R. is supported by the French National Research Agency in the framework of the Investissements dAvenir program (ANR-15IDEX-02), through the funding of the “Origin of Life” project of the University Grenoble-Alpes. Portions of this work were performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www. cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa. int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has made use of the SIMBAD database and the VizieR catalog access tool, both operated at the CDS, Strasbourg, France. This research has made use of the “Modern Mean Dwarf Stellar Color and Effective Temperature Sequence” available at http://www.pas.rochester.edu/ ~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt. This research has benefited from the SpeX Prism Library (and/or SpeX Prism Library Analysis Toolkit), maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism, the IRTF Spectral Library, maintained by Michael Cushing, the Brown Dwarfs in New York City database led by Jackie Faherty, Emily Rice, and Kelle Cruz, and the Montreal Brown Dwarf and Exoplanet Spectral Library, maintained by Jonathan Gagné.
Publisher Copyright:
© 2019. The American Astronomical Society. All rights reserved.
PY - 2019/12
Y1 - 2019/12
N2 - The ∼500 Myr A2IV star HR 1645 has one of the most significant low-amplitude accelerations of nearby early-type stars measured from a comparison of the Hipparcos and Gaia astrometric catalogs. This signal is consistent with either a stellar companion with a moderate mass ratio (q ∼ 0.5) on a short period (P < 1 yr), or a substellar companion at a separation wide enough to be resolved with ground-based high-contrast imaging instruments; long-period equal-mass ratio stellar companions that are also consistent with the measured acceleration are excluded with previous imaging observations. The small but significant amplitude of the acceleration made HR 1645 a promising candidate for targeted searches for brown dwarf and planetary-mass companions around nearby, young stars. In this paper we explore the origin of the astrometric acceleration by modeling the signal induced by a wide-orbit M8 companion discovered with the Gemini Planet Imager, as well as the effects of an inner short-period spectroscopic companion discovered a century ago but not since followed up. We present the first constraints on the orbit of the inner companion, and demonstrate that it is a plausible cause of the astrometric acceleration. This result demonstrates the importance of vetting of targets with measured astrometric acceleration for short-period stellar companions prior to conducting targeted direct imaging surveys for wide-orbit substellar companions.
AB - The ∼500 Myr A2IV star HR 1645 has one of the most significant low-amplitude accelerations of nearby early-type stars measured from a comparison of the Hipparcos and Gaia astrometric catalogs. This signal is consistent with either a stellar companion with a moderate mass ratio (q ∼ 0.5) on a short period (P < 1 yr), or a substellar companion at a separation wide enough to be resolved with ground-based high-contrast imaging instruments; long-period equal-mass ratio stellar companions that are also consistent with the measured acceleration are excluded with previous imaging observations. The small but significant amplitude of the acceleration made HR 1645 a promising candidate for targeted searches for brown dwarf and planetary-mass companions around nearby, young stars. In this paper we explore the origin of the astrometric acceleration by modeling the signal induced by a wide-orbit M8 companion discovered with the Gemini Planet Imager, as well as the effects of an inner short-period spectroscopic companion discovered a century ago but not since followed up. We present the first constraints on the orbit of the inner companion, and demonstrate that it is a plausible cause of the astrometric acceleration. This result demonstrates the importance of vetting of targets with measured astrometric acceleration for short-period stellar companions prior to conducting targeted direct imaging surveys for wide-orbit substellar companions.
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U2 - 10.3847/1538-3881/ab4ef7
DO - 10.3847/1538-3881/ab4ef7
M3 - Article
AN - SCOPUS:85085771228
SN - 0004-637X
VL - 158
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 6
M1 - ab4ef7
ER -