Testing envelope models of young stellar objects with submillimeter continuum and molecular-line observation

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Abstract
This paper examines the density and velocity structure of envelopes around young stellar objects through submillimeter continuum imaging of four objects in Taurus and previously obtained molecular-line data. Observations carried out with the SCUBA on the JCMT at 850 and 450 micron of L1489 IRS, L1535 IRS, L1527 IRS, and TMC 1 reveal ~2000 AU elongated structures embedded in extended envelopes. The density distribution in these envelopes is equally well fit by a radial power-law of index p=1.0-2.0 or with a collapse model such as that of Shu (1997: ApJ, 214, 488). This inside-out collapse model predicts 13CO, C18O, HCO+, and H13CO+ line profiles which closely match observed spectra toward three of our four sources. This shows that the inside-out collapse model offers a good description of YSO envelopes, but also that reliable constraints on its parameters require independent measurements of the density and the velocity structure, e.g., through continuum and line observations. For the remaining source, L1489 IRS, we find that a model consisting of a 2000 AU radius, rotating, disk-like structure better describes the data. Possibly, this source is in transition between the embedded Class I and the optically revealed T Tauri phases. Two apparently starless cores are found at ~10,000 AU from L1489 IRS and L1535 IRS. They are cold, 10-15 K, contain 0.5-3.0 M_sol, and have flat density distributions characterized by a Gaussian of ~10,000 AU FWHM. The proximity of these cores shows that star formation in truly isolated cores is rare even in Taurus.

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