Protostars and Planets VI, Heidelberg, July 15-20, 2013

Poster 1G001

Determining Protostar Masses: L1527 IRS in Taurus

Terebey, Susan (California State University, Los Angeles)
Isella, Andrea (California Institute of Technology)
De Vries, Christopher (California State University, Stanislaus)

Protostar masses have been difficult to determine, in part due to the complex nature of protostar environments. We report on a pilot study to determine the mass of the L1527 protostar using CARMA interferometer data. The velocity channel maps are compared with a model that incorporates 1) LVG radiative transfer, 2) TSC collapse envelope and outflow cavity, and 3) a CARMA interferometer simulation. The models are able to reproduce observed C18O(2-1) channel maps quite well, and are sensitive to the gravity field of the infalling gas. The best-fit mass is 0.24 +/- 0.04 Mo for the L1527 protostar plus disk. The models indicate that line-width is a sensitive and robust indicator of mass. We conclude that this method of comparing millimeter interferometer data with infall models incorporating radiative transfer shows promise for determining a fundamental but poorly known quantity, the protostar mass.

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