Abstract
The width of the 1.3 cm line of NH 3 in a dense core is related by simple power laws to the luminosity and mass of the most massive star associated with the core. These relations link the mass of the star to the initial conditions in the gas which formed the star. At the size scale ∼0.1 pc of NH 3 line observations, the effects of stellar winds on the core velocity dispersion are estimated from observations of cores with and without stars, and from the dependence of the wind momentum flux on stellar luminosity
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