G048.66-0.29: Physical State of an Isolated Site of Massive Star Formation

TL;DR

This study uses multi-wavelength observations to analyze the physical state, structure, and star formation potential of the isolated infrared dark cloud G48.66-0.29, revealing its collapse dynamics and core evolution.

Contribution

It provides detailed temperature, density, and molecular composition maps of G48, demonstrating its collapse and fragmentation in the absence of external feedback, and identifying potential high-mass star-forming cores.

Findings

G48 has a simple, isolated structure suitable for studying filament collapse.

Two cores are likely to form high-mass stars (>8 Msun).

The filament is collapsing, with molecular depletion indicating freeze-out processes.

Abstract

We present continuum observations of the infrared dark cloud (IRDC) G48.66-0.22 (G48) obtained with Herschel, Spitzer, and APEX, in addition to several molecular line observations. The Herschel maps are used to derive temperature and column density maps of G48 using a model based on a modified blackbody. We find that G48 has a relatively simple structure and is relatively isolated; thus this IRDC provides an excellent target to study the collapse and fragmentation of a filamentary structure in the absence of complicating factors such as strong external feedback. The derived temperature structure of G48 is clearly non-isothermal from cloud to core scale. The column density peaks are spatially coincident with the lowest temperatures (~ 17.5 K) in G48. A total cloud mass of ~390Msun is derived from the column density maps. By comparing the luminosity-to-mass ratio of 13 point sources detected in the Herschel/PACS bands to evolutionary models, we find that two cores are likely to evolve into high-mass stars (M>8 Msun). The derived mean projected separation of point sources is smaller than in other IRDCs but in good agreement with theoretical predications for cylindrical collapse. We detect several molecular species such as CO, HCO+, HCN, HNC and N2H+. CO is depleted by a factor of ~3.5 compared to the expected interstellar abundance, from which we conclude that CO freezes out in the central region. Furthermore, the molecular clumps, associated with the sub-millimeter peaks in G48, appear to be gravitationally unbound or just pressure confined. The analysis of critical line masses in G48 show that the entire filament is collapsing, overcoming any internal support.