2006A&A...446.1165J

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 in the ChaI star-forming cloud. Time-resolved high-resolution echelle spectra of ChaHα1-8 and ChaHα12 (M6-M8), B34 (M5), CHXR74 (M4.5), and Sz23 (M2.5) were taken with UVES at the VLT between 2000 and 2004. The precision achieved for the relative RVs range between 40 and 670m/s and is sufficient to detect Jupiter mass planets around the targets. This is the first RV survey of very young BDs. It 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 very low-mass stars (VLMSs, M≤0.12M_☉, spectral types M5-M8) has constant RVs on time scales of 40 days and less. For this group, estimates of upper limits for masses of hypothetical companions range between 0.1M_Jup and 1.5M_Jup for assumed orbital separations of 0.1AU. This hints at a rather small multiplicity fraction for very young BDs/VLMSs, for orbital separations of ≤0.1AU and orbital periods of ≤40 days. 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/VLMSs are suitable targets for RV surveys for planets. Three objects of the sample exhibit significant RV variations with peak-to-peak RV differences of 2-3km/s. For the highest mass object observed with UVES (Sz23, ∼0.3M_☉), the variations are on time scales of days, which might be explained by rotational modulation. On the other hand, the BD candidate ChaHα8 (M6.5) and the low-mass star CHXR74 (M4.5) both display significant RV variations on times scales of ≥150 days, while they are both RV constant or show only much smaller amplitude variations on time scales of days to weeks, i.e. of the rotation periods. A suggested explanation for the detected RV variations of CHXR74 and ChaHα8 is that they are caused by giant planets or very low-mass 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 (very) low-mass stars are possibly several months or longer, and that orbital separations are ≥0.2AU. This parameter range has not been covered for all targets yet, but will be probed by follow-up observations. Furthermore, we show that the scaled down equivalent to the BD desert found around solar-like stars would be a giant planet desert around BD and VLMS primaries, if formed by the same mechanism. The present data test its existence for the targets in the limited separation range of the survey. So far, no hints of companions in a ``giant planet desert'' have been found.