Near-Infrared Spectroscopy of New Very Low Mass Young Stars and the Lower End of the IMF in Chamaeleon I: From Stellar to Sub-Stellar Objects

Details Near-Infrared Spectroscopy of New Very Low Mass Young Stars and the Lower End of the IMF in Chamaeleon I: From Stellar to Sub-Stellar Objects Near-Infrared Spectroscopy of New Very Low Mass Young Stars and the Lower End of the IMF in Chamaeleon I: From Stellar to Sub-Stellar Objects

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop..199m&link_type=abstract

NOAO Proposal ID #1999A-0199

Physics

Scientific paper

We propose to obtain near-infrared 4-m cross dispersed IRS spectra of ~ 100 CIRIM very low mass young stellar object candidates (some of them likely young brown dwarfs) of the Chamaeleon I cloud to derive physical properties of the stellar photospheres - such as T_eff, surface gravity, and reddening -. Optical spectra for the candidates with counterparts on the DSS plates (~10% of the sample) and for all known visible members of the cloud will be obtained somewhere else. The spectral types of all these sources, together with stellar luminosities will allow us to construct the HR diagram of the cloud. Adopting recent pre-main sequence evolutionary tracks we will determine masses and ages for the individual sources. We will use this information to estimate the IMF (particularly toward and in the sub- stellar regime), evaluate the overall star-formation efficiency and test the concept of a coeval star-formation process in the cloud. Surface gravities and reddenings for the individual sources will provide additional checks on their evolutionary status.

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