![]() Result primarily from the gravitational fragmentation of marginally Up the peak of the CMF (and probably responsible for the base of the IMF) These findings support a picture wherein the cores making Them lie within filamentary structures with supercritical masses per unit Located above a background column density corresponding to A_V~7, and ~75% of About 90% of the Herschel-identified prestellar cores are We find a strongĬorrelation between the spatial distribution of prestellar cores and theĭensest filaments. ![]() We estimate that the lifetime of prestellar cores is ~1 Myr. ByĬomparing the numbers of starless cores to the number of young stellar objects, IMF is consistent with a typical star formation efficiency of ~40%. The global shift in mass scale observed between the CMF and the Supporting the earlier view that there is a close physical link between the IMFĪnd the CMF. The core mass function (CMF) derived for the prestellarĬores is very similar in shape to the stellar initial mass function (IMF), Of 651 starless cores, ~60% of which are gravitationally bound prestellarĬores, and they will likely form stars in the future. ![]() ![]() We identify aĬomplete sample of starless dense cores and embedded protostars in this region,Īnd analyze their global properties and spatial distributions. Pc, imaged with the SPIRE/PACS cameras from 70 to 500 micron. Observations in a ~11 deg^2 area of the Aquila molecular cloud complex at d~260 We present and discuss the results of the Herschel Gould Belt survey
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