Young Stars and Their Companions in NGC 2362

Details Young Stars and Their Companions in NGC 2362 Young Stars and Their Companions in NGC 2362

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.3101w&link_type=abstract

American Astronomical Society, ESS meeting #2, #31.01

Astronomy and Astrophysics

Astronomy

Scientific paper

The mass-radius relation of young, low-mass (M < M&sun;) stars is poorly understood due to a dearth of observations. Better measurements of the masses and radii of these stars would enable a fuller understanding of how low-mass stars form and better characterization of planets orbiting such stars. We investigate velocities of 116 cool (K-type and later), small (0.1 < M/M&sun; < 1.2) stars with magnitude 14 < I < 19 in the ˜ 5 Myr open cluster NGC 2362 with the aims of:
(1) Identifying cluster members by finding the velocity and velocity dispersion of the cluster.
(2) Constraining the masses and radii of candidate occulting systems by examining their radial velocities at multiple epochs.
We obtained time-series photometry of 1180 candidate cluster members at the CTIO 4-m Blanco telescope with the Mosaic-II detector between January and December 2006. Multi- epoch spectra of 116 stars were obtained from the ESO/VLT using the GIRAFFE/FLAMES multi-fibre spectrograph in December 2007. We measured radial velocities of 93 cluster can- didates, 81 of which are within 3σ of the cluster velocity (39.7±1.58 km/s). One M dwarf displays eclipse depths of 5%, although the double-lined spectrum of this object suggest that it is an M dwarf binary. We calculate upper and lower limits on the masses and radii of the primary star and its companion: 0.34 < M1/M&sun; < 0.53; 1.0 < R1/R&sun; < 1.25; 0.035 < M2/M&sun; < 0.34; 0.28 < R2/R&sun; < 1.0. This system is ideal for follow-up with high cadence photometry and high resolution spectroscopy at quadrature. These measurements would allow the solution of the primary and secondary masses and radii and adding to the sparse existing measurements of the masses and radii of young, low-mass stars.

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