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We present the results of our investigation of the star-forming potential inthe Perseus star-forming complex. We build on previous starless core,protostellar core, and young stellar object (YSO) catalogs from Spitzer,Herschel, and SCUBA observations in the literature. We place the cores and YSOswithin seven star-forming clumps based on column densities greater than 5x10^21cm^-2. We calculate the mean density and free-fall time for 69 starless coresas 5.55x10^-19 gcm^-3 and 0.1 Myr,respectively, and we estimate the starformation rate for the near future as 150 Msun Myr^-1. According to BonnorEbert stability analysis, we find that majority of starless cores in Perseusare unstable. Broadly, these cores can collapse to form the next generation ofstars. We found a relation between starless cores and YSOs, where the numbersof young protostars (Class 0 + Class I) are similar to the numbers of starlesscores. This similarity, which shows a one-to-one relation, suggests that thesestarless cores may form the next generation of stars with approximately thesame formation rate as the current generation, as identified by the Class 0 andClass I protostars. It follows that if such a relation between starless coresand any YSO stage exists, the SFR values of these two populations must benearly constant. In brief, we propose that this one-to-one relation is animportant factor in better understanding the star formation process within acloud.

An Estimation of the Star Formation Rate in the Perseus Complex