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WISEP J004701.06+680352.1: An Intermediate Surface Gravity, Dusty Brown Dwarf in the AB Dor Moving Group

Gizis, John E. and Allers, Katelyn N. and Liu, Michael C. and Harris, Hugh C. and Faherty, Jacqueline K. and Burgasser, Adam J. and Kirkpatrick, J. Davy (2015) WISEP J004701.06+680352.1: An Intermediate Surface Gravity, Dusty Brown Dwarf in the AB Dor Moving Group. Astrophysical Journal, 799 (2). Art. No. 203. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20150306-144833368

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Abstract

We present spectroscopy, astrometry, and photometry of the brown dwarf WISEP J004701.06+680352.1 (W0047+68), an unusually red field L dwarf at a distance of 12.2 ± 0.4 pc. The three-dimensional space motion identifies it as a member of the AB Dor Moving Group, an identification supported by our classification of W0047+68 as intermediate surface gravity (INT-G) using the Allers & Liu near-infrared classification system. This moving group membership implies near-solar metallicity, age ~100-125 Myr, M ≈ 0.018 M_☉, and log g ≈ 4.5; the thick condensate clouds needed to explain the infrared spectrum are, therefore, a result of surface gravity that is lower than that of ordinary field brown dwarfs. From the observed luminosity and evolutionary model radius, we find T_(eff) ≈ 1300 K, a temperature normally associated with early T dwarfs. Thick clouds are also used to explain the spectral properties of directly imaged giant planets, and we discuss the successes and challenges for such substellar models in matching the observed optical and infrared spectra. W0047+68 shows that cloud thickness is more sensitive to intermediate surface gravity than in most models. We also present a trigonometric parallax of the dusty L6 dwarf 2MASS J21481628+4003593. It lies at 8.060 ± 0.036 parsecs; its astrometry is consistent with the view that it is older and metal-rich.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/799/2/203DOIArticle
http://iopscience.iop.org/0004-637X/799/2/203PublisherArticle
http://arxiv.org/abs/1412.1856arXivDiscussion Paper
ORCID:
AuthorORCID
Gizis, John E.0000-0002-8916-1972
Allers, Katelyn N.0000-0003-0580-7244
Liu, Michael C.0000-0003-2232-7664
Faherty, Jacqueline K.0000-0001-6251-0573
Burgasser, Adam J.0000-0002-6523-9536
Kirkpatrick, J. Davy0000-0003-4269-260X
Additional Information:© 2015 American Astronomical Society. Received 2014 March 9; accepted 2014 December 4; published 2015 January 30. We are grateful to the USNO CCD parallax team for allowing us to use the preliminary parallax measurements.We thank Eric Mamajek for discussions of local associations; Kimberly Aller for examining Pan-STARRS data; Denise Stephens, Satoko Sorohana, and Dagny Looper for providing electronic copies of their data; and France Allard and Adam Burrows for sharing their grids of synthetic spectra. This research has benefitted from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism. Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. MMT telescope time was granted by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The Pan-STARRS1 surveys have been made possible by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the institutions of the Pan-STARRS1 Science Consortium (http://www.ps1sc.org), NSF, and NASA. This research has made use of NASA’s Astrophysics Data System, the VizieR catalogue access tool, CDS, Strasbourg, France, and the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NSFUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:brown dwarfs; infrared: stars; stars: individual (WISEP J004701.06+680352.1, 2MASS J21481628+4003593)
Issue or Number:2
Record Number:CaltechAUTHORS:20150306-144833368
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20150306-144833368
Official Citation:WISEP J004701.06+680352.1: An Intermediate Surface Gravity, Dusty Brown Dwarf in the AB Dor Moving Group John E. Gizis et al. 2015 ApJ 799 203
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:55617
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:06 Mar 2015 23:33
Last Modified:09 Mar 2020 13:18

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