Radial velocity survey for planets and brown dwarf companions to very young brown dwarfs and very low-mass stars in cha 1 with uves at the vlt - INSPIRE

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Radial velocity survey for planets and brown dwarf companions to very young brown dwarfs and very low-mass stars in cha 1 with uves at the vlt

Viki Joergens
(
- Leiden Observ. and
- Garching, Max Planck Inst., MPE
)

Sep, 2005

e-Print:

astro-ph/0509134 [astro-ph]

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Abstract: (arXiv)

We present results of a radial velocity (RV) survey for planets and brown dwarf (BD) companions to very young BDs and (very) low-mass stars (VLMSs) in ChaI. High-resolution echelle spectra of ChaHa1-8 and 12 (M6-M8), and B34, CHXR74, Sz23 (M2.5-M5) were taken with UVES / VLT between 2000 and 2004. The achieved precision (40 to 670 m/s) is sufficient to detect Jupiter mass planets around the targets. This first RV survey of very young BDs probes multiplicity which is a key parameter for formation in an as yet unexplored domain, in terms of age, mass, and orbital separation. We find that the subsample of ten BDs and VLMSs (M<0.12 Msun, M5-M8) has constant RVs on time scales of <40 days. For them, estimates of upper limits for masses of hypothetical companions are 0.1 to 1.5 MJup (assuming 0.1 AU). This hints at a rather small multiplicity fraction for very young BDs/VLMSs at <0.1 AU. Furthermore, the non-variable objects demonstrate the lack of any significant RV noise due to stellar activity down to the precision necessary to detect giant planets. Thus, very young BDs and VLMSs are suitable targets for RV surveys for planets. Three objects of the sample exhibit significant RV variations. For Sz23, they might be attributed to surface activity, while for ChaHa8 (M6.5) and CHXR74 (M4.5), the detected RV variations are on times scales of >150 days, which cannot be explained by rotational modulation. An alternative explanation are giant planets / BDs of at least a few Jupiter masses orbiting with periods of several months or longer. Thus, the presented RV data indicate that orbital periods of companions to very young BDs and (V)LMSs are possibly several months or longer, and that orbital separations are > 0.2 AU. This parameter range has not been covered for all targets yet, but will be probed by follow-up observations.

Note:

Submitted to Astron.Astrophys.

STARS LOW-MASS
STARS PRE-MAIN SEQUENCE
B 34
CHXR 74
SZ 23
BINARIES SPECTROSCOPIC
TECHNIQUES RADIAL VELOCITY
PLANETARY SYSTEM FORMATION

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