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We present Herschel SPIRE and PACS maps of the Cepheus Flare clouds L1157,L1172, L1228, L1241, and L1251, observed by the Herschel Gould Belt Survey(HGBS) of nearby star-forming molecular clouds. Through modified blackbody fitsto the SPIRE and PACS data, we determine typical cloud column densities of0.5-1.0 $\times$ 10$^{21}$ cm$^{-2}$ and typical cloud temperatures of 14-15 K.Using the getsources identification algorithm, we extract 832 dense cores fromthe SPIRE and PACS data at 160-500 $\mu$m. From placement in a mass vs. sizediagram, we consider 303 to be candidate prestellar cores, and 178 of these tobe "robust" prestellar cores. From an independent extraction of sources at 70$\mu$m, we consider 25 of the 832 dense cores to be protostellar. Thedistribution of background column densities coincident with candidateprestellar cores peaks at 2-4 $\times$ 10$^{21}$ cm$^{-2}$. About half of thecandidate prestellar cores in Cepheus may have formed due to the widespreadfragmentation expected to occur within filaments of "transcritical" line mass.The lognormal robust prestellar core mass function (CMF) drawn from all fiveCepheus clouds peaks at 0.56 M$_{\odot}$ and has a width of $\sim$0.5 dex,similar to that of Aquila's CMF. Indeed, the width of Cepheus' aggregate CMF issimilar to the stellar system Initial Mass Function (IMF). The similarity ofCMF widths in different clouds and the system IMF suggests a common, possiblyturbulent origin for seeding the fluctuations that evolve into prestellar coresand stars.

Herschel Gould Belt Survey Observations of Dense Cores in the Cepheus Flare Clouds