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Title:
Low-Luminosity Companions to White Dwarfs
Authors:
Farihi, J.; Becklin, E. E.; Zuckerman, B.
Affiliation:
AA(Gemini Observatory, Northern Operations, 670 North A'ohoku Place, Hilo, HI 96720; .; Department of Physics and Astronomy, University of California, 430 Portola Plaza, Los Angeles, CA 90095), AB(Department of Physics and Astronomy, University of California, 430 Portola Plaza, Los Angeles, CA 90095; ), AC(Department of Physics and Astronomy, University of California, 430 Portola Plaza, Los Angeles, CA 90095; .)
Publication:
The Astrophysical Journal Supplement Series, Volume 161, Issue 2, pp. 394-428. (ApJS Homepage)
Publication Date:
12/2005
Origin:
UCP
ApJ Keywords:
Stars: Binaries: General, Stars: Evolution, Stars: Formation, Stars: Fundamental Parameters, Stars: Low-Mass, Brown Dwarfs, Stars: Luminosity Function, Mass Function, Stars: White Dwarfs
DOI:
10.1086/444362
Bibliographic Code:
2005ApJS..161..394F

Abstract

This paper presents results of a near-infrared imaging survey for low-mass stellar and substellar companions to white dwarfs. A wide-field proper-motion survey of 261 white dwarfs was capable of directly detecting companions at orbital separations between ~100 and 5000 AU with masses as low as 0.05 Msolar, while a deep near-field search of 86 white dwarfs was capable of directly detecting companions at separations between ~50 and 1100 AU with masses as low as 0.02 Msolar. Additionally, all white dwarf targets were examined for near-infrared excess emission, a technique capable of detecting companions at arbitrarily close separations down to masses of 0.05 Msolar. No brown dwarf candidates were detected, which implies a brown dwarf companion fraction of <0.5% for white dwarfs. In contrast, the stellar companion fraction of white dwarfs as measured by this survey is 22%, uncorrected for bias. Moreover, most of the known and suspected stellar companions to white dwarfs are low-mass stars whose masses are only slightly greater than the masses of brown dwarfs. Twenty previously unknown stellar companions were detected, five of which are confirmed or likely white dwarfs themselves, while 15 are confirmed or likely low-mass stars. Similar to the distribution of cool field dwarfs as a function of spectral type, the number of cool unevolved dwarf companions peaks at mid-M type. Based on the present work, relative to this peak, field L dwarfs appear to be roughly 2-3 times more abundant than companion L dwarfs. Additionally, there is no evidence that the initial companion masses have been altered by post-main-sequence binary interactions.

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