J/AJ/144/64 Solar neighborhood. XXVIII. Substellar companions (Dieterich+, 2012)
The solar neighborhood.
XXVIII. The multiplicity fraction of nearby stars from 5 to 70 AU and the brown
dwarf desert around M dwarfs.
Dieterich S.B., Henry T.J., Golimowski D.A., Krist J.E., Tanner A.M.
<Astron. J., 144, 64 (2012)>
=2012AJ....144...64D 2012AJ....144...64D
ADC_Keywords: Stars, nearby ; Stars, double and multiple ; Stars, dwarfs ;
Stars, M-type ; Photometry, infrared
Keywords: binaries: close - brown dwarfs - infrared: stars -
solar neighborhood - stars: low-mass - stars: statistics
Abstract:
We report on our analysis of Hubble Space Telescope/NICMOS snapshot
high-resolution images of 255 stars in 201 systems within ∼10 pc of
the Sun. Photometry was obtained through filters F110W, F180M, F207M,
and F222M using NICMOS Camera 2. These filters were selected to permit
clear identification of cool brown dwarfs through methane contrast
imaging. With a plate scale of 76mas/pixel, NICMOS can easily resolve
binaries with subarcsecond separations in the 19.5"x19".5 field of
view. We previously reported five companions to nearby M and L dwarfs
from this search. No new companions were discovered during the second
phase of data analysis presented here, confirming that
stellar/substellar binaries are rare. We establish magnitude and
separation limits for which companions can be ruled out for each star
in the sample, and then perform a comprehensive sensitivity and
completeness analysis for the subsample of 138 M dwarfs in 126
systems. We calculate a multiplicity fraction of 0.0+3.5-0.0% for
L companions to M dwarfs in the separation range of 5-70 AU, and
2.3+5.0-0.7% for L and T companions to M dwarfs in the separation
range of 10-70AU. We also discuss trends in the color-magnitude
diagrams using various color combinations and present astrometry for
19 multiple systems in our sample. Considering these results and
results from several other studies, we argue that the so-called brown
dwarf desert extends to binary systems with low-mass primaries and is
largely independent of primary mass, mass ratio, and separations.
While focusing on companion properties, we discuss how the qualitative
agreement between observed companion mass functions and initial mass
functions suggests that the paucity of brown dwarfs in either
population may be due to a common cause and not due to binary
formation mechanisms.
Description:
We obtained direct images of each target using NICMOS Camera 2 NIC2
through four near-infrared filters during cycles 7 (1997-1998) and 11
(2002-2003). Targets were imaged through the F110W, F180M, F207M, and
F222M filters, centered at 1.10µm, 1.80µm, 2.07µm, and
2.22µm, respectively.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 104 231 Sensitivity to companions: faintest detectable
absolute magnitudes for putative companions
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See also:
V/130 : Geneva-Copenhagen Survey of Solar neighbourhood III (Holmberg+, 2009)
V/70 : Nearby Stars, Preliminary 3rd Version (Gliese+ 1991)
J/ApJ/736/89 : Companions around nearby massive stars (Janson+, 2011)
J/AJ/142/92 : New proper motion stars with pm≥0.18"/yr (Boyd+, 2011)
J/AJ/142/10 : New proper motion stars 0.40"/yr>pm≥0.18"/yr (Boyd+, 2011)
J/AJ/141/21 : CCD distance estimates of SCR targets (Winters+, 2011)
J/AJ/133/971 : Companions of low-mass stars and brown dwarfs (Allen+, 2007)
J/AJ/133/439 : Luminosity function of M7-L8 ultracool dwarfs (Cruz+, 2007)
J/AJ/134/252 : New nearby white dwarf systems (Subasavage+, 2007)
J/AJ/133/2898 : New proper-motion stars (-90<DE< -47) (Finch+, 2007)
J/ApJ/640/1051 : 25pc sample of Sun-like stars (Grether+, 2006)
J/AJ/132/866 : New M dwarfs in solar neighborhood (Riaz+, 2006)
J/MNRAS/360/1345 : F- and G-type stars in solar neighbourhood (Karatas+, 2005)
J/AJ/129/413 : New high proper motion stars (-90<DE< -47) (Subasavage+, 2005)
J/ApJS/161/394 : Low-luminosity companions to white dwarfs (Farihi+, 2005)
J/AJ/130/1658 : New high proper motion stars (-47<δ< -00)
(Subasavage+, 2005)
J/AJ/125/3302 : HST binary very low mass stars and brown dwarfs (Gizis+, 2003)
J/A+A/327/1039 : Structure and evolution of low-mass stars (Chabrier+ 1997)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Source Source name
18- 22 A5 --- Res Resolved system point-spread function (PSF)
detected in field of view (1)
24- 31 A8 --- SpT Spectral type
33- 36 F4.1 pc Dist Heliocentric distance
38- 48 A11 "Y:M:D" Date Date of the observation
50- 54 F5.2 mag F180 ? HST/NICMOS F180M band magnitude
56- 59 F4.1 mag M0.2 ? Companion magnitude limit at 0.2"
(absolute F180M band magnitude)
61- 64 F4.1 mag M0.4 ? Companion magnitude limit at 0.4"
(absolute F180M band magnitude)
66- 69 F4.1 mag M0.6 ? Companion magnitude limit at 0.6"
(absolute F180M band magnitude)
71- 74 F4.1 mag M0.8 ? Companion magnitude limit at 0.8"
(absolute F180M band magnitude)
76- 79 F4.1 mag M1.0 Companion magnitude limit at 1.0"
(absolute F180M band magnitude)
81- 84 F4.1 mag M2.0 Companion magnitude limit at 2.0"
(absolute F180M band magnitude)
86- 89 F4.1 mag M3.0 ? Companion magnitude limit at 3.0"
(absolute F180M band magnitude)
91- 94 F4.1 mag M4.0 ? Companion magnitude limit at 4.0"
(absolute F180M band magnitude)
96-104 A9 --- Note Additional note(s) (2)
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Note (1): A/B denotes that components A and B are resolved. AB denotes an
unresolved known multiple.
Note (2): Note as follows:
a = No PSF subtraction;
b = Known multiple system, excluding planets;
c = Sensitivity measured around unresolved or very close binary;
d = 2MASS H magnitude for primary;
e = Off-center by more than 5";
f = Sensitivity measured around brighter component only;
g = Beyond 10pc;
h = Sensitivity measurements exclude 30° between components;
i = Saturated core.
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History:
From electronic version of the journal
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(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 14-Oct-2013