On the binary frequency of the lowest mass members of the pleiades with hubble space telescope wide field camera 3

E. V. Garcia; Trent J. Dupuy; Katelyn N. Allers; Michael C. Liu; Niall R. Deacon

doi:10.1088/0004-637X/804/1/65

On the binary frequency of the lowest mass members of the pleiades with hubble space telescope wide field camera 3

E. V. Garcia, Trent J. Dupuy, Katelyn N. Allers, Michael C. Liu, Niall R. Deacon

Centre for Astrophysics Research (CAR)

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Abstract

We present the results of a Hubble Space Telescope Wide Field Camera 3 (WFC3) imaging survey of 11 of the lowest mass brown dwarfs in the Pleiades known (25-40 M_Jup). These objects represent the predecessors to T dwarfs in the field. Using a semi-empirical binary point-spread function (PSF)-fitting technique, we are able to probe to 0.″ 03 (0.75 pixel), better than 2x the WFC3/UVIS diffraction limit. We did not find any companions to our targets. From extensive testing of our PSF-fitting method on simulated binaries, we compute detection limits which rule out companions to our targets with mass ratios of 0.7 and separations 4 AU. Thus, our survey is the first to attain the high angular resolution needed to resolve brown dwarf binaries in the Pleiades at separations that are most common in the field population. We constrain the binary frequency over this range of separation and mass ratio of 25-40 M_Jup Pleiades brown dwarfs to be

Original language	English
Article number	65
Number of pages	10
Journal	The Astrophysical Journal
Volume	804
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/804/1/65
Publication status	Published - 1 May 2015

Keywords

binaries: general
brown dwarfs
methods: observational
stars: low-mass
techniques: photometric

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10.1088/0004-637X/804/1/65

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title = "On the binary frequency of the lowest mass members of the pleiades with hubble space telescope wide field camera 3",

abstract = "We present the results of a Hubble Space Telescope Wide Field Camera 3 (WFC3) imaging survey of 11 of the lowest mass brown dwarfs in the Pleiades known (25-40 MJup). These objects represent the predecessors to T dwarfs in the field. Using a semi-empirical binary point-spread function (PSF)-fitting technique, we are able to probe to 0.″ 03 (0.75 pixel), better than 2x the WFC3/UVIS diffraction limit. We did not find any companions to our targets. From extensive testing of our PSF-fitting method on simulated binaries, we compute detection limits which rule out companions to our targets with mass ratios of 0.7 and separations 4 AU. Thus, our survey is the first to attain the high angular resolution needed to resolve brown dwarf binaries in the Pleiades at separations that are most common in the field population. We constrain the binary frequency over this range of separation and mass ratio of 25-40 MJup Pleiades brown dwarfs to be ",

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author = "Garcia, {E. V.} and Dupuy, {Trent J.} and Allers, {Katelyn N.} and Liu, {Michael C.} and Deacon, {Niall R.}",

note = "E. V. Garcia, et al., “On the Binary Frequency of the Lowest mass Members of the Pleiades with Hubble Space Telescope Wide Field Camera 3”, The Astrophysical Journal, Vol. 804(1), May 2015. {\textcopyright} 2015. The American Astronomical Society.",

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On the binary frequency of the lowest mass members of the pleiades with hubble space telescope wide field camera 3

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