The Influence of Far-Ultraviolet Radiation on the Properties of Molecular Clouds in the 30 Dor Region of the Large Magellanic Cloud

TL;DR

This study maps molecular clouds in the Large Magellanic Cloud's 30 Dor region to understand how far-ultraviolet radiation affects their properties in a low-metallicity environment, revealing constant CO emission properties despite radiation variations.

Contribution

It provides the first complete CO map of the molecular ridge in the LMC and analyzes how FUV radiation influences molecular cloud characteristics in a low-metallicity setting.

Findings

CO-emitting clump properties do not vary with FUV radiation strength

CO-to-H2 conversion factor is about twice that of the outer Galaxy

Mass spectrum and scaling relations are similar to Galactic clouds

Abstract

We present a complete 12CO J = 1-0 map of the prominent molecular ridge in the Large Magellanic Cloud (LMC) obtained with the 22-m ATNF Mopra Telescope. The region stretches southward by ~2 degrees, (or 1.7kpc) from 30 Doradus, the most vigorous star-forming region in the Local Group. The location of this molecular ridge is unique insofar as it allows us to study the properties of molecular gas as a function of the ambient radiation field in a low-metallicity environment. We find that the physical properties of CO-emitting clumps within the molecular ridge do not vary with the strength of the far-ultraviolet (FUV) radiation field. Since the peak CO brightness of the clumps shows no correlation with the radiation field strength, the observed constant value for CO-to-H_2 conversion factor along the ridge seems to require an increase in the kinetic temperature of the molecular gas that is offset by a decrease in the angular filling factor of the CO emission. We find that the difference between the CO-to-H_2 conversion factor in the molecular ridge and the outer Milky Way is smaller than has been reported by previous studies of the CO emission: applying the same cloud identification and analysis methods to our CO observations of the LMC molecular ridge and CO data from the outer Galaxy survey by Dame et al. (2001), we find that the average CO-to-H_2 conversion factor in the molecular ridge is X_CO = (3.9+/-2.5)10^20 cm^-2 (K km s^-1)^-1, approximately twice the value that we determine for the outer Galaxy clouds. The mass spectrum and the scaling relations between the properties of the CO clumps in the molecular ridge are similar, but not identical, to those that have been established for Galactic molecular clouds.