Angular momentum evolution of very low mass stars and brown dwarfs in the Orion Nebula Cluster: Spectroscopic determinations of masses and mass accretion rates.

Details Angular momentum evolution of very low mass stars and brown dwarfs in the Orion Nebula Cluster: Spectroscopic determinations of masses and mass accretion rates. Angular momentum evolution of very low mass stars and brown dwarfs in the Orion Nebula Cluster: Spectroscopic determinations of masses and mass accretion rates.

Aug 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008noao.prop..157r&link_type=abstract

NOAO Proposal ID #2008B-0157

Computer Science

Scientific paper

With the help of an extensive photometric monitoring program in the young (1 Myr) Orion Nebular Cluster (ONC, distance ~ 450pc) we derived rotational periods of nearly 500 objects, 120 of which are potential brown dwarfs (BDs) (M≲75M_jup). The faintest of these variable objects has I=20.7 and corresponds to a BD of only 15 M_jup in ONC if an average A_v=1.5 is assumed. This sample extends three magnitudes deeper in I than the one of Herbst et al. 2002. This is by far the most extensive and complete rotational periods data set in the very low mass (VLM) star and BD regime and it will represent the most important reference sample for all future angular momentum evolution study in this mass regime for many years to come. In order to exploit the great scientific potential of this sample we propose here medium resolution (R ~ 2200) multiobject spectroscopy with HYDRA to derive spectral types, A_v values, masses and mass accretion rates of these pre-main sequence (PMS) objects.

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