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Integral Field Spectroscopy of the Low-Mass Companion HD 984 B with the Gemini Planet Imager

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Integral Field Spectroscopy of the Low-Mass Companion HD 984 B with the Gemini Planet Imager UCLA UCLA Previously Published Works Title Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager Permalink https://escholarship.org/uc/item/0z30b9nr Journal Astronomical Journal, 153(4) ISSN 0004-6256 Authors Johnson-Groh, M Marois, C De Rosa, RJ et al. Publication Date 2017-04-01 DOI 10.3847/1538-3881/aa6480 Peer reviewed eScholarship.org Powered by the California Digital Library University of California The Astronomical Journal, 153:190 (13pp), 2017 April https://doi.org/10.3847/1538-3881/aa6480 © 2017. The American Astronomical Society. All rights reserved. Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager Mara Johnson-Groh1, Christian Marois1,2, Robert J. De Rosa3, Eric L. Nielsen4,5, Julien Rameau6, Sarah Blunt4,5,7, Jeffrey Vargas3, S. Mark Ammons8, Vanessa P. Bailey5, Travis S. Barman9, Joanna Bulger10, Jeffrey K. Chilcote11, Tara Cotten12, René Doyon6, Gaspard Duchêne3,13, Michael P. Fitzgerald14, Kate B. Follette5, Stephen Goodsell15,16, James R. Graham3, Alexandra Z. Greenbaum17, Pascale Hibon18, Li-Wei Hung14, Patrick Ingraham19, Paul Kalas3, Quinn M. Konopacky20, James E. Larkin14, Bruce Macintosh5, Jérôme Maire11, Franck Marchis4, Mark S. Marley21, Stanimir Metchev22,23, Maxwell A. Millar-Blanchaer11,24, Rebecca Oppenheimer25, David W. Palmer8, Jenny Patience26, Marshall Perrin27, Lisa A. Poyneer8, Laurent Pueyo27, Abhijith Rajan26, Fredrik T. Rantakyrö15, Dmitry Savransky28, Adam C. Schneider26, Anand Sivaramakrishnan27, Inseok Song12, Remi Soummer27, Sandrine Thomas29, David Vega4, J. Kent Wallace30, Jason J. Wang3, Kimberly Ward-Duong26, Sloane J. Wiktorowicz31, and Schuyler G. Wolff17 1 Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Victoria, BC V8P 5C2, Canada 2 Herzberg Astronomy & Astrophysics, National Research Council of Canada, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 3 Department of Astronomy, UC Berkeley, Berkeley CA, 94720, USA 4 SETI Institute, Carl Sagan Center, 189 Bernardo Avenue, Mountain View, CA 94043, USA 5 Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 6 Institut de Recherche sur les Exoplanètes, Départment de Physique, Université de Montréal, Montréal QC H3C 3J7, Canada 7 Department of Physics, Brown University, Providence, RI 02912, USA 8 Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA, 94550, USA 9 Lunar and Planetary Lab, University of Arizona, Tucson, AZ 85721, USA 10 Subaru Telescope, NAOJ, 650 North A’ohoku Place, Hilo, HI 96720, USA 11 Dunlap Institute for Astronomy & Astrophysics, University of Toronto, 50 St. George Street, Toronto ON M5S 3H4, Canada 12 Department of Physics and Astronomy, University of Georgia, Athens, GA, USA 13 Université Grenoble Alpes/CNRS, Institut de Planétologie et d’Astrophysique de Grenoble, F-38000 Grenoble, France 14 Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095, USA 15 Department of Physics, Durham University, Stockton Road, Durham DH1, UK 16 Gemini Observatory, Casilla 603, La Serena, Chile 17 Physics and Astronomy Department, Johns Hopkins University, Baltimore MD 21218, USA 18 European Southern Observatory, Casilla 19001-Santiago 19, Chile 19 Large Synoptic Survey Telescope, 950 N Cherry Avenue, Tucson AZ 85719, USA 20 Center for Astrophysics and Space Sciences, University of California, San Diego, La Jolla, CA 92093, USA 21 Space Science Division, NASA Ames Research Center, Mail Stop 245-3, Moffett Field CA 94035, USA 22 Department of Physics and Astronomy, Centre for Planetary Science and Exploration, The University of Western Ontario, London, ON N6A 3K7, Canada 23 Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA 24 Department of Astronomy & Astrophysics, University of Toronto, Toronto ON M5S 3H4, Canada 25 American Museum of Natural History, Department of Astrophysics, Central Park West at 79th Street, New York, NY 10024, USA 26 School of Earth and Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287, USA 27 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218, USA 28 Sibley School of Mechanical and Aerospace Engineering, Cornell University, Ithaca, NY 14853, USA 29 Large Synoptic Survey Telescope, 950 N Cherry Avenue, Tucson AZ, 85719, USA 30 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 31 The Aerospace Corporation, 2310 E. El Segundo Boulevard, El Segundo, CA 90245, USA Received 2016 August 12; revised 2017 February 25; accepted 2017 March 1; published 2017 March 31 Abstract We present new observations of the low-mass companion to HD 984 taken with the Gemini Planet Imager (GPI) as a part of the GPI Exoplanet Survey campaign. Images of HD 984 B were obtained in the J (1.12–1.3 μm) and H (1.50–1.80 μm) bands. Combined with archival epochs from 2012 and 2014, we fitthefirst orbit to the companion to find an 18 au (70-year) orbit with a 68% confidence interval between 14 and 28 au, an eccentricity of 0.18 with a 68% confidence interval between 0.05 and 0.47, and an inclination of 119°with a 68% confidence interval between 114°and 125°. To address the considerable spectral covariance in both spectra, we present a method of splitting the spectra into low and high frequencies to analyze the spectral structure at different spatial frequencies with the proper spectral noise correlation. Using the split spectra, we compare them to known spectral types using field brown dwarf and low-mass star spectra and find a best-fit match of a field gravity ± +120 M6.5 1.5 spectral type with a corresponding temperature of 2730-180 K. Photometry of the companion yields a luminosity of log(Lbol/L☉) =-2.88 0.07 dex with DUSTY models. Mass estimates, again from DUSTY models, find an age-dependent mass of 34±1to95±4MJup.Theseresultsareconsistent with previous measurements of the object. Key words: planetary systems – stars: individual (HD 984) 1 The Astronomical Journal, 153:190 (13pp), 2017 April Johnson-Groh et al. 1. Introduction exoplanets, which would provide insight into planet formation in binary systems. The search for exoplanets through direct imaging has led to The star HD 984 was observed as one of the targets of the many serendipitous detections of brown dwarfs and low-mass Gemini Planet Imager Exoplanet Survey (GPIES, Macintosh stellar companions (e.g., Chauvin et al. 2005; Biller et al. 2010; ) ) et al. 2014b . This is an ongoing survey of over 600 nearby Nielsen et al. 2012; Mawet et al. 2015; Konopacky et al. 2016 . young stars with nearly 900 hr dedicated time on the 8 m These surveys tend to target young bright stars whose potential ( ( Gemini South Telescope using the Gemini Planet Imager GPI, companions would still be warm and bright in the infrared e.g., Macintosh et al. 2014a), which is a coronagraphic adaptive ) Burrows et al. 1997 . Brown dwarfs, having higher tempera- optics integral field spectrograph and imaging polarimeter. tures than planetary-mass companions of the same age, are Using near-infrared imaging spectroscopy (0.9–2.4 μm) and fi signi cantly brighter and therefore easier to detect. While advanced imaging and post-processing techniques, GPI detects brown dwarf companions are not the primary focus of direct thermal emission from exoplanets and brown dwarfs at angular imaging searches, they are useful in their own right for a better separations of 0 2–1 0 from their parent star. understanding of substellar atmospheres and for comparing We present new spectroscopic observations of HD 984 B at J competing formation models (e.g., Boley & Durisen 2010; (1.12–1.35 μm, R∼34) and H (1.50–1.80 μm, R∼45) bands Perets & Kouwenhoven 2012; Bodenheimer et al. 2013). with GPI, from which we derive the first orbit estimate and Meshkat et al. (2015) reports the discovery of a bound low- update luminosity, magnitude, and mass measurements. In mass companion to HD 984, a bright nearby (47.1 ± 1.4 pc) Section 2 we describe the GPI observations. Basic reductions F7V star of mass ∼1.2 M☉ (van Leeuwen 2007; Meshkat are explained in Section 3. Section 4 details the point-spread et al. 2015) and a temperature of 6315±89 K (White function (PSF) subtraction technique. Astrometry is discussed et al. 2007; Casagrande et al. 2011). With an age estimate of in Section 5, orbital fitting in Section 6, and spectral and 30–200 Myr (115 ± 85 Myr at a 95% confidence level) derived photometric analyses are presented in Section 7. Finally, we from isochronal age, X-ray emission, and rotation (Meshkat conclude in Section 8. et al. 2015) that is consistent with previous age estimates ( ) Wright et al. 2004; Torres et al. 2008 , HD 984 is ideal for 2. Observations direct imaging campaigns to search for young substellar objects. The star HD 984 was observed with the GPI integral field The results presented in Meshkat et al. (2015) find HD 984 B spectrograph (IFS, Chilcote et al. 2012; Larkin et al. 2014) on at a separation of 0 19±0 02 (9.0 ± 1.0 au) based on the L¢ 2015 August 30 UT during the GPIES campaign (program observations with NaCo (Lenzen et al. 2003; Rousset GPIES-2015B-01, Gemini observation ID: GS-2015B-Q-500- et al. 2003) in 2012 July and the H+K band observations 982) at Gemini South. The GPI IFS has a field of view (FOV) of 2 with SINFONI (Eisenhauer et al. 2003; Bonnet et al. 2004) in 2.8×2.8 arcsec with a plate scale of 14.166±0.007 mili- / − ° ± ° 2014 September. These two instruments are both mounted on arcseconds pixel and a position angle offset of 0.10 0.13 ( ) UT4 on the Very Large Telescope at Cerro Paranal, Chile. Macintosh et al.
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