The Mass Distribution and Lifetime of Prestellar Cores in Perseus, Serpens, and Ophiuchus

TL;DR

This study provides an unbiased census of starless cores in three molecular clouds, analyzing their properties, lifetimes, and implications for star formation, revealing that prestellar core characteristics are linked to the initial mass function.

Contribution

It offers the first comprehensive comparison of starless and protostellar cores across multiple clouds, linking core properties to star formation outcomes and core evolution.

Findings

Prestellar cores in Perseus are larger and less dense than protostellar cores.

The prestellar core mass distribution slope is consistent with the stellar initial mass function.

Prestellar core lifetime is approximately 4.5x10^5 years, indicating dynamic evolution.

Abstract

We present an unbiased census of starless cores in Perseus, Serpens, and Ophiuchus, assembled by comparing large-scale Bolocam 1.1 mm continuum emission maps with Spitzer c2d surveys. We use the c2d catalogs to separate 108 starless from 92 protostellar cores in the 1.1 mm core samples from Enoch et al. (2006), Young et al. (2006), and Enoch et al. (2007). A comparison of these populations reveals the initial conditions of the starless cores. Starless cores in Perseus have similar masses but larger sizes and lower densities on average than protostellar cores, with sizes that suggest density profiles substantially flatter than r^-2. By contrast, starless cores in Serpens are compact and have lower masses than protostellar cores; future star formation will likely result in lower mass objects than the currently forming protostars. Comparison to dynamical masses estimated from the NH_3 survey of Perseus cores by Rosolowsky et al. (2007) suggests that most of the starless cores are likely to be gravitationally bound, and thus prestellar. The combined prestellar core mass distribution includes 108 cores and has a slope of -2.3+/-0.4 for M>0.8 Msun. This slope is consistent with recent measurements of the stellar initial mass function, providing further evidence that stellar masses are directly linked to the core formation process. We place a lower limit on the core-to-star efficiency of 25%. There are approximately equal numbers of prestellar and protostellar cores in each cloud, thus the dense prestellar core lifetime must be similar to the lifetime of embedded protostars, or 4.5x10^5 years, with a total uncertainty of a factor of two. Such a short lifetime suggests a dynamic, rather than quasi-static, core evolution scenario, at least at the relatively high mean densities (n>2x10^4 cm^-3) to which we are sensitive.