Empirical mass determination for very low-mass stars and brown dwarfs in NGC 2516

Details Empirical mass determination for very low-mass stars and brown dwarfs in NGC 2516 Empirical mass determination for very low-mass stars and brown dwarfs in NGC 2516

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006noao.prop..115h&link_type=abstract

NOAO Proposal ID #2006A-0115

Physics

Scientific paper

We have begun a large-scale program of time-resolved wide-field photometry on nearby young open clusters and star-forming regions (SFRs) with known age and metallicity, to search for low-mass eclipsing binary and planet systems (the Monitor project). We propose to use the CTIO- 4m+Mosaic to obtain photometry for NGC 2516, a nearby intermediate-age (~ 150 Myr, distance modulus 7.7) open cluster, where we will measure ~ 1400 primaries with masses M < 0.4 M_&sun; over ~ 1 sq.deg with sufficient precision to find eclipses. The goals of this project are (1) to make empirical mass determinations of very low-mass (VLM) pre-main-sequence (PMS) stars and brown dwarfs (BDs) at known age, to calibrate the mass-luminosity-radius relation and stellar models at the bottom of the main sequence and into the BD regime, (2) to detect the first planets orbiting stars younger than 200 Myr, and measure their periods, masses (with radial velocity follow-up observations) and radii to place constraints on planet formation and evolution scenarios, and (3) to obtain rotation periods for members of a sample of open clusters, and examine the evolution of stellar rotation, up to an age of 200 Myr.

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