An unbiased search for the signatures of protostars in the rho Ophiuchi Molecular Cloud. II. Millimetre continuum observations

TL;DR

This study conducted a millimetre continuum survey of the rho Ophiuchi cloud, discovering new cores and analyzing their distribution, mass function, and orientations, revealing insights into star formation processes in a turbulent environment.

Contribution

First comprehensive millimetre survey of rho Oph cloud revealing core properties, distribution, and their relation to turbulence and star formation.

Findings

Core mass function resembles stellar initial mass function.

Inner regions have more compact cores due to higher pressure.

Core orientations suggest turbulence-driven formation.

Abstract

We have performed a 1 square degree 1.2mm dust continuum survey in the rho Oph molecular cloud. We detect a number of previously unknown sources, ranging from extended cores over compact, starless cores to envelopes surrounding young stellar objects of Class 0, Class I, and Class II type. We analyse the mass distribution, spatial distribution and the potential equilibrium of the cores. For the inner regions, the survey results are consistent with the findings of previous narrower surveys. The core mass function resembles the stellar initial mass function, with the core mass function shifted by a factor of two to higher masses (for the chosen opacity and temperature). In addition, we find no statistical variation in the core mass function between the crowded inner regions and those in more isolated fields except for the absence of the most massive cores in the extended cloud. The inner region contains compacter cores. This is interpreted as due to a medium of higher mean pressure although strong pressure variations are evident in each region. The cores display a hierarchical spatial distribution with no preferred separation scale length. However, the frequency distribution of nearest neighbours displays two peaks, one of which at 5000AU can be the result of core fragmentation. The orientations of the major axes of cores are consistent with an isotropic distribution. In contrast, the relative orientations of core pairs are preferentially in the NW-SE direction on all separation scales. These results are consistent with core production and evolution in a turbulent environment. We report a new low-mass Class 0 object and its CO outflow.