Dense cores in the Pipe Nebula: An improved core mass function

TL;DR

This study refines the core mass function of the Pipe Nebula by combining extinction and molecular-line data, revealing a shape similar to the stellar initial mass function scaled by star formation efficiency.

Contribution

It introduces a more accurate core sample and CMF for the Pipe Nebula using velocity data to distinguish physical cores from line-of-sight overlaps.

Findings

CMF departs from a single power-law with a break at ~2.7 Msun

CMF shape is similar to the stellar IMF but scaled by ~4.5

Star formation efficiency estimated at 22%

Abstract

In this paper we derive an improved core mass function (CMF) for the Pipe Nebula from a detailed comparison between measurements of visual extinction and molecular-line emission. We have compiled a refined sample of 201 dense cores toward the Pipe Nebula using a 2-dimensional threshold identification algorithm informed by recent simulations of dense core populations. Measurements of radial velocities using complimentary C18O (1-0) observations enable us to cull out from this sample those 43 extinction peaks that are either not associated with dense gas or are not physically associated with the Pipe Nebula. Moreover, we use the derived C18O, central velocities to differentiate between single cores with internal structure and blends of two or more physically distinct cores, superposed along the same line-of-sight. We then are able to produce a more robust dense core sample for future follow-up studies and a more reliable CMF than was possible previously. We confirm earlier indications that the CMF for the Pipe Nebula departs from a single power-law like form with a break or knee at M ~ 2.7 +/- 1.3 Msun. Moreover, we also confirm that the CMF exhibits a similar shape to the stellar IMF, but is scaled to higher masses by a factor of ~4.5. We interpret this difference in scaling to be a measure of the star formation efficiency (22 +/- 8%). This supports earlier suggestions that the stellar IMF may originate more or less directly from the CMF.