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We summarize the first results from the Gould Belt survey, obtained towardthe Aquila Rift and Polaris Flare regions during the 'science demonstrationphase' of Herschel. Our 70-500 micron images taken in parallel mode with theSPIRE and PACS cameras reveal a wealth of filamentary structure, as well asnumerous dense cores embedded in the filaments. Between ~ 350 and 500prestellar cores and ~ 45-60 Class 0 protostars can be identified in the Aquilafield, while ~ unbound starless cores and no protostars are observed in thePolaris field. The prestellar core mass function (CMF) derived for the Aquilaregion bears a strong resemblance to the stellar initial mass function (IMF),already confirming the close connection between the CMF and the IMF with muchbetter statistics than earlier studies. Comparing and contrasting our Herschelresults in Aquila and Polaris, we propose an observationally-driven scenariofor core formation according to which complex networks of long, thin filamentsform first within molecular clouds, and then the densest filaments fragmentinto a number of prestellar cores via gravitational instability.

From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt survey