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WISEP J061135.13-041024.0AB: A J-Band Flux Reversal Binary at the L/T Transition

Gelino, Christopher R. and Smart, R. L. and Marocco, Federico and Kirkpatrick, J. Davy and Cushing, Michael C. and Mace, Gregory and Mendez, Rene A. and Tinney, C. G. and Jones, Hugh R. A. (2014) WISEP J061135.13-041024.0AB: A J-Band Flux Reversal Binary at the L/T Transition. Astronomical Journal, 148 (1). Art. No. 6. ISSN 0004-6256.

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We present Keck II laser guide star adaptive optics observations of the brown dwarf WISEP J061135.13–041024.0 showing it is a binary with a component separation of 0.''4. This system is one of the six known resolved binaries in which the magnitude differences between the components show a reversal in sign between the Y/J band and the H/K bands. Deconvolution of the composite spectrum results in a best-fit binary solution with L9 and T1.5 components. We also present a preliminary parallax placing the system at a distance of 21.2 ± 1.3 pc. Using the distance and resolved magnitudes we are able to place WISEP J061135.13–041024.0 AB on a color-absolute magnitude diagram, showing that this system contributes to the well-known "J-band bump" and the components' properties appear similar to other late-type L and early-type T dwarfs. Fitting our data to a set of cloudy atmosphere models suggests the system has an age >1 Gyr with WISE 0611–0410 A having an effective temperature (T_(eff)) of 1275-1325 K and mass of 64-65 M_(Jup), and WISE 0611–0410 B having T_(eff) = 1075-1115 K and mass 40-65 M_(Jup).

Item Type:Article
Related URLs:
URLURL TypeDescription
Smart, R. L.0000-0002-4424-4766
Marocco, Federico0000-0001-7519-1700
Kirkpatrick, J. Davy0000-0003-4269-260X
Cushing, Michael C.0000-0001-7780-3352
Mace, Gregory0000-0001-7875-6391
Tinney, C. G.0000-0002-7595-0970
Additional Information:© 2014 American Astronomical Society. Received 2013 July 26; accepted 2014 April 20; published 2014 May 28. The authors acknowledge telescope operators Heather Hershley, Carolyn Jordan, Julie Renaud-Kim, and Cynthia Wilburn and instrument specialists Scott Dahm, Marc Kassis, and Luca Rizzi for their assistance during the Keck observations. We would also like to thank Chas Beichman for obtaining images of WISE 0611−0410 on 2012 November 29 and 2013 September 21, Mark Marley and Didier Saumon for providing the models, Mike Read for help in mining the UKIDSS database and useful discussions, and the anonymous referee for useful comments. Based partially on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile program 186.C-0756. R.L.S., H.R.A.J., and F.M. would like to acknowledge the Marie Curie 7th European Community Framework Programme grant no. 247593 Interpretation and Parameterization of Extremely Red COOL dwarfs (IPERCOOL) International Research Staff Exchange Scheme. R.A.M. acknowledges partial support from project PFB-06 CATA and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Iniciativa Cientifica Milenio del Ministerio de Economa, Fomento y Turismo de Chile.C.G.T. acknowledges the support of ARC grants DP0774000 and DP130102695. This publication makes use of data products from 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology (Caltech), funded by the National Aeronautics and Space Administration (NASA) and the National Science Foundation. This publication makes use of data products from the Wide-field Infrared Survey Explorer (WISE), which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL)/Caltech, and NEOWISE, which is a project of JPL/Caltech. WISE and NEOWISE are funded by NASA. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to NASA through the agency’s scientific partnership with the Caltech and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Facilities: Keck:II (NIRC2, LGS-AO), NTT (SofI)
Funding AgencyGrant Number
Marie Curie 7th European Community Framework Programme247593
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:binaries: general; brown dwarfs; stars: fundamental parameters; stars: individual (WISEP J061135.13–041024.0); stars: low-mass
Issue or Number:1
Record Number:CaltechAUTHORS:20140807-153129124
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Official Citation:WISEP J061135.13–041024.0 AB: A J-band Flux Reversal Binary at the L/T Transition Christopher R. Gelino et al. 2014 The Astronomical Journal 148 6
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:48208
Deposited By: Ruth Sustaita
Deposited On:07 Aug 2014 22:51
Last Modified:09 Mar 2020 13:19

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