Astrophys. J., 638, 293-313 (2006/February-2)
Bolocam survey for 1.1mm dust continuum emission in the c2d Legacy clouds. I. Perseus.
ENOCH M.L., YOUNG K.E., GLENN J., EVANS II N.J., GOLWALA S., SARGENT A.I., HARVEY P., AGUIRRE J., GOLDIN A., HAIG D., HUARD T.L., LANGE A., LAURENT G., MALONEY P., MAUSKOPF P., ROSSINOT P. and SAYERS J.
Abstract (from CDS):
We have completed a 1.1 mm continuum survey of 7.5 deg2 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" (FWHM) resolution elements to a 1 σ rms of 15 mJy/beam. We detect a total of 122 cores above a 5 σ point-source mass detection limit of 0.18 M☉, assuming a dust temperature of TD=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 α1=1.3 (0.5 M☉<M<2.5 M☉) and α2=2.6 (M>2.5 M☉), similar to the local initial mass function slope (α1=1.6, M<1 M☉; α2=2.7, M>1 M☉). 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☉. We suggest an extinction threshold for millimeter cores of AV∼5 mag, based on our calculation of the probability of finding a 1.1 mm core as a function of AV. 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 2x105 AU. Our 1.1 mm emission survey reveals considerably denser, more compact material than maps in other column density tracers such as 13CO and AV, 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.
ISM: Clouds - ISM: Individual: Name: Perseus - Stars: Formation
VizieR on-line data:
<Available at CDS (J/ApJ/638/293): table1.dat table2.dat>
Table 1: [EYG2006] Bolo NNN (Nos 1-122).
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