Abstract
Our stellar formation scenario has changed considerably during the last two decades. The very detection of interstellar ammonia in 1968 revealed the existence of a denser cloud population immersed in the dilute HI medium known from extensive observations of the 21 cm hydrogen line. Since then some 80 interstellar molecules have been indentified. These trace molecules are not only curiosities in space. They are our major probes of the physical conditions and processes inside the dense star formation regions. Moreover, the molecular lines provide the cooling necessary for cloud evolution towards stellar formation.
Our current knowledge of the small and large scale structure of molecular clouds as well as their large scale distribution in galaxies is reviewed with emphasis on the initial conditions for stellar formation. we also discuss cloud formation processes, support against gravitaional collapse as well as bipolar outflows indicating extensive mass loss during early stellar evolution.
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Hjalmarson, Å., Friberg, P. (1988). Radio and (Sub)Millimeter Observations of the Initial Conditions for Star Formation. In: Dupree, A.K., Lago, M.T.V.T. (eds) Formation and Evolution of Low Mass Stars. NATO ASI Series, vol 241. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3037-7_4
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