We have completed a 1.1 mm continuum survey of 7.5 deg ^ { 2 } of the Perseus Molecular Cloud using Bolocam at the Caltech Submillimeter Observatory .
This represents the largest millimeter or submillimeter continuum map of Perseus to date .
Our map covers more than 30,000 31 \arcsec ( FWHM ) resolution elements to a 1 \sigma RMS of 15 mJy/beam .
We detect a total of 122 cores above a 5 \sigma point source mass detection limit of 0.18 M _ { \sun } , assuming a dust temperature of T _ { D } = 10 K , 60 of which are new millimeter or submillimeter detections .
The 1.1 mm mass function is consistent with a broken power law of slope \alpha _ { 1 } = 1.3 ~ { } ( 0.5 M _ { \sun } < M < 2.5 M _ { \sun } ) and \alpha _ { 2 } = 2.6 ~ { } ( M > 2.5 M _ { \sun } ) , similar to the local initial mass function slope ( \alpha _ { 1 } = 1.6 ~ { } M < 1 M _ { \sun } , \alpha _ { 2 } = 2.7 ~ { } M > 1 M _ { \sun } ) .
No more than 5 % of the total cloud mass is contained in discrete 1.1 mm cores , which account for a total mass of 285 M _ { \sun } .
We suggest an extinction threshold for millimeter cores of A _ { V } \sim 5 mag , based on our calculation of the probability of finding a 1.1 mm core as a function of A _ { V } .
Much of the cloud is devoid of compact millimeter emission ; despite the significantly greater area covered compared to previous surveys , only 5 - 10 of the newly identified sources lie outside previously observed areas .
The two-point correlation function confirms that dense cores in the cloud are highly structured , with significant clustering on scales as large as 2 \times 10 ^ { 5 } AU .
Our 1.1 mm emission survey reveals considerably denser , more compact material than maps in other column density tracers such as ^ { 13 } CO and A _ { V } , although the general morphologies are roughly consistent .
These 1.1 mm results , especially when combined with recently acquired c2d Spitzer Legacy data , will provide a census of dense cores and protostars in Perseus and improve our understanding of the earliest stages of star formation in molecular clouds .