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We present and discuss the results of the Herschel Gould Belt surveyobservations in a ~11 deg^2 area of the Aquila molecular cloud complex at d~260pc, imaged with the SPIRE/PACS cameras from 70 to 500 micron. We identify acomplete sample of starless dense cores and embedded protostars in this region,and analyze their global properties and spatial distributions. We find a totalof 651 starless cores, ~60% of which are gravitationally bound prestellarcores, and they will likely form stars in the future. We also detect 58protostellar cores. The core mass function (CMF) derived for the prestellarcores is very similar in shape to the stellar initial mass function (IMF),supporting the earlier view that there is a close physical link between the IMFand the CMF. The global shift in mass scale observed between the CMF and theIMF is consistent with a typical star formation efficiency of ~40%. Bycomparing the numbers of starless cores to the number of young stellar objects,we estimate that the lifetime of prestellar cores is ~1 Myr. We find a strongcorrelation between the spatial distribution of prestellar cores and thedensest filaments. About 90% of the Herschel-identified prestellar cores arelocated above a background column density corresponding to A_V~7, and ~75% ofthem lie within filamentary structures with supercritical masses per unitlength >~16 M_sun/pc. These findings support a picture wherein the cores makingup the peak of the CMF (and probably responsible for the base of the IMF)result primarily from the gravitational fragmentation of marginallysupercritical filaments. Given that filaments appear to dominate the massbudget of dense gas at A_V>7, our findings also suggest that the physics ofprestellar core formation within filaments is responsible for a characteristic"efficiency" SFR/M_dense ~5+-2 x 10^-8 yr^-1 for the star formation process indense gas.

A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey