High Resolution IR Spectroscopy: Another Way to Study Star Formation in Clusters

Details High Resolution IR Spectroscopy: Another Way to Study Star Formation in Clusters High Resolution IR Spectroscopy: Another Way to Study Star Formation in Clusters

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.prop..335j&link_type=abstract

NOAO Proposal ID #2000A-0335

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Scientific paper

Current models of protostellar evolution may be correct but do not yet have a strong underpinning of observational support. The most critical missing data are measured masses for objects with different surface temperatures and luminosities. As with main sequence and post main sequence stars, these masses must come from orbital determinations for binaries. To date, very little has been done to get such data because the measurements must be obtained on large telescopes with high resolution IR spectrographs and such instruments are rare. We are beginning a program at McDonald that takes advantage of our new instrument, NIRSHELL, to find protostellar and YSO spectroscopic binaries and to determine their orbital parameters. Our orbit determination technique, however, requires us to obtain single-epoch spectra of our target stars at high S/N. We propose here to take such spectra with Phoenix on the 4m. The nature of our long-term effort means that the data we take at KPNO will be highly leveraged by the data taken at many other epochs at McDonald. The Phoenix data alone will give us valuable information about young objects embedded in the ρOph molecular cloud. The stellar velocities, when compared to the well defined cloud velocity, will give us a crude estimate of the binary frequency at separations of <=1-3 AU.

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