Interferometric Observations of Protostellar Binary Systems

Details Interferometric Observations of Protostellar Binary Systems Interferometric Observations of Protostellar Binary Systems

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21333001c&link_type=abstract

American Astronomical Society, AAS Meeting #213, #330.01; Bulletin of the American Astronomical Society, Vol. 41, p.386

Astronomy and Astrophysics

Astronomy

Scientific paper

Binary and higher-order multiple stellar systems represent the preferred outcome of the star formation process, but at present we do not understand well how this occurs. Our current knowledge on binary star formation mostly relies on observations of main sequence and pre-main sequence stars and the constraints they put on the theoretical models. Direct observations of the earliest, embedded phase of binary star formation were long limited by the low angular resolution of single-dish telescopes. Only the recent advance of large (sub-)millimeter interferometers has enabled us to directly observe the formation phase of binary stars, although the number of known and well-studied systems is still very small. To search for protostellar binary systems and to derive their kinematic properties, we have started a systematic program to observe, at high angular resolution, a number of low-mass protostellar cores. The initial survey was conducted at the OVRO mm array, and is now continued with the ATCA, IRAM-PdBI, and SMA arrays. The observations were mainly carried out at mm dust continuum and in the N2H+ and CO molecular lines. With the mm dust continuum images, we identified several protobinary candidates and derived their circumstellar mass distribution, density profiles, and mass ratios. Based on the molecular lines data, we could, for the first time, derive the velocity fields and the distribution of specific angular momentum of the protobinary systems, and kinematically study the fragmentation process. In this talk we present the main results of this program.

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