We describe a search for new pre-main-sequence stars in a sample of faint 60 micrometers sources identified by the Infrared Astronomical Satallite in the Taurus-Auriga molecular cloud. Most of these sources appear to be galaxies based on near-infrared imaging, optical spectroscopy, and their spatial locations relative to dense molecular gas. However, nine objects are probably pre-main-sequence stars, and at least one of these appears to be an embedded protostar. Our results suggest the population of protostars in Taurus-Auriga is essentially complete for L greater than or equal to 0.1 solar luminosity. We combined published data with our results to construct a new luminosity function for Taurus-Auriga embedded sources. As in previous studies, the luminosity function has a roughly Gaussian shape and a distinct peak at approximately 1 solar luminosity. This peak lies a factor of 10-50 below predictions of steady, spherical infall models, but it can be explained if cloud material falls into a circumstellar disk instead of radially onto the central star.
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Kenyon et al. (1994) studied this question.