The Chamaeleon II low-mass star-forming region: radial velocities, elemental abundances, and accretion properties

Context. Knowledge of radial velocities, elemental abundances, and accretion properties of members of star-forming regions is important for our understanding of stellar and planetary formation. While infrared observations reveal the evolutionary status of the disk, optical spectroscopy is fundamental to acquire information on the properties of the central star and on the accretion characteristics. Aims. Existing 2MASS archive data and the Spitzer c2d survey of the Chamaeleon II dark cloud have provided disk properties of a large number of young stars. We complement these data with optical spectroscopy with the aim of providing physical stellar parameters and accretion properties. Methods. We use FLAMES/UVES and FLAMES/GIRAFFE spectroscopic observations of 40 members of the Chamaeleon II star-forming region to measure radial velocities through cross-correlation technique, lithium abundances by means of curves of growth, and for a suitable star elemental abundances of Fe, Al, Si, Ca, Ti, and Ni using the code MOOG. From the equivalent widths of the H alpha, H beta, and the He I lambda 5876, lambda 6678, lambda 7065 angstrom emission lines, we estimate the mass accretion rates, (M) over dot(acc), for all the objects. Results. We derive a radial velocity distribution for the Chamaeleon II stars, which is peaked at < V-rad > = 11.4 +/- 2.0 km s(-1). We find dependencies of (M) over dot(acc) proportional to M-star(1.3) and of (M) over dot(acc) proportional to Age(-0.82) in the similar to 0.1-1.0 M-circle dot mass regime, as well as a mean mass accretion rate for Chamaeleon II of (M) over dot(acc) similar to 7(-5)(+26-) x 10(-10) M-circle dot yr(-1). We also establish a relationship between the He I lambda 7065 angstrom line emission and the accretion luminosity. Conclusions. The radial velocity distributions of stars and gas in Chamaeleon II are consistent. The spread in (M) over dot(acc) at a given stellar mass is about one order of magnitude and can not be ascribed entirely to short timescale variability. Analyzing the relation between (M) over dot(acc) and the colors in Spitzer c2d and 2MASS bands, we find indications that the inner disk changes from optically thick to optically thin at (M) over dot(acc) x 10(-1)0 M-circle dot yr(-1). Finally, the disk fraction is consistent with the age of Chamaeleon II.