| Issue |
A&A
Volume 483, Number 3, June I 2008
|
|
|---|---|---|
| Page(s) | 869 - 874 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:200809419 | |
| Published online | 26 March 2008 | |
A probable close brown dwarf companion to GJ 1046 (M 2.5V) *
1
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: This email address is being protected from spambots. You need JavaScript enabled to view it.
;This email address is being protected from spambots. You need JavaScript enabled to view it.
2
McDonald Observatory, University of Texas, Austin, TX 78712, USA e-mail: This email address is being protected from spambots. You need JavaScript enabled to view it.
3
Zentrum für Astronomie Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany e-mail: This email address is being protected from spambots. You need JavaScript enabled to view it.
Received:
18
January
2008
Accepted:
17
March
2008
Abstract
Context. Brown dwarf companions to stars at separations of a few AU or less are
rare objects, and none have been found so far around early-type M dwarfs
(M 0V-M 5V). With GJ 1046 (M 2.5V), a strong candidate for such a system
with a separation of 
is presented.
Aims. We aim at constraining the mass of the companion in order to decide whether it is a brown dwarf or a low-mass star.
Methods. We employed precision RV measurements to determine the orbital parameters and the minimum companion mass. We then derived an upper limit to the companion mass from the lack of disturbances of the RV measurements by a secondary spectrum. An even tighter upper limit is subsequently established by combining the RV-derived orbital parameters with the recent new version of the Hipparcos Intermediate Astrometric Data.
Results. For the mass of the companion, we derive
from the RV data.
Based on the RV data alone, the
probability that the companion exceeds the stellar mass threshold is
just 
.
The absence of effects from the secondary spectrum lets us constrain
the companion mass to 
.
The combination of RV and Hipparcos data yields a 
upper mass limit to the companion mass of 
with a formal optimum value at 
.
From the combination of RV and astrometric data, the chance probability
that the companion is a star is 
.
Conclusions. We have found a low-mass, close companion to an early-type M dwarf. While the most likely interpretation of this object is that it is a brown dwarf, a low-mass stellar companion is not fully excluded.
Key words: stars: low-mass, brown dwarfs / stars: binaries: spectroscopic / stars: individual: GJ 1046 / astrometry
Based on observations collected at the European Southern Observatory, Paranal, Chile, programmes 173.C-0606 and 078.C-0829.
© ESO, 2008
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