Clustered Low Mass Star Formation in the Ophiuchus Molecular Cloud

Details Clustered Low Mass Star Formation in the Ophiuchus Molecular Cloud Clustered Low Mass Star Formation in the Ophiuchus Molecular Cloud

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21332702f&link_type=abstract

American Astronomical Society, AAS Meeting #213, #327.02; Bulletin of the American Astronomical Society, Vol. 41, p.383

Astronomy and Astrophysics

Astronomy

Scientific paper

Stars form out of the gravitational collapse of centrally condensed cores of dense molecular gas. Recent years have seen leaps forward in our understanding of the structure and evolution of isolated, star forming cores. Most star formation, however, occurs in clustered environments. These regions are more complex, with complicated observed geometries, and contain cores which tend to have higher densities and more compact sizes than those found in isolation. Consequently, high resolution observations are key to probing their physical, chemical and dynamical structures.
In this detailed study, we present combined single-dish and interferometric observations of the dense gas tracers NH3 and N2H+ in three dense, fragmented filaments in the cluster-forming Ophiuchus molecular cloud. We find that, on average, the filaments are warmer and more turbulent on large scales than those in isolated regions. On small scales ( 1800 AU), we find poorer correspondence between N-based molecular line emission and thermal dust continuum emission than is seen in isolated cores. We attribute these discrepancies to abundance effects, which may be due to depletion in the densest regions of the filament.

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