The Carina Nebula and Gum 31 molecular complex: I. Molecular gas distribution, column densities and dust temperatures

TL;DR

This study provides high-resolution molecular gas, dust temperature, and column density maps of the Carina Nebula and Gum 31, revealing detailed gas distribution and star formation indicators through combined CO and infrared observations.

Contribution

It offers the first high-resolution CO and dust temperature mapping of the Carina-Gum 31 complex, analyzing gas distribution, column densities, and their relation to star formation activity.

Findings

Gas column densities range from 6.3×10^{20} to 1.4×10^{23} cm^{-2}.

Dust temperatures vary from 17 to 43 K.

Gas column density distribution shows a log-normal shape with a high-density tail.

Abstract

We report high resolution observations of the $^{12}$CO$(1\rightarrow0)$ and $^{13}$CO$(1\rightarrow0)$ molecular lines in the Carina Nebula and the Gum 31 region obtained with the 22-m Mopra telescope as part of the The Mopra Southern Galactic Plane CO Survey. We cover 8 deg$^2$ from $l = 285^{\circ}$ to 290$^{\circ}$, and from $b = -1.5^{\circ}$ to +0.5$^{\circ}$. The molecular gas column density distributions from both tracers have a similar range of values. By fitting a grey-body function to the observed infrared spectral energy distribution from Herschel maps, we derive gas column densities and dust temperatures. The gas column density has values in the range from $6.3\times\ 10^{20}$ to $1.4\times 10^{23}$ cm$^{-2}$, while the dust temperature has values in the range from 17 to 43 K. The gas column density derived from the dust emission is approximately described by a log-normal function for a limited range of column densities. A high-column density tail is clearly evident for the gas column density distribution, which appears to be a common feature in regions with active star formation. There are regional variations in the fraction of the mass recovered by the CO emission lines with respect to the total mass traced by the dust emission. These variations may be related to changes in the radiation field strength, variation of the atomic to molecular gas fraction across the observed region, differences in the CO molecule abundance with respect to H$_{2}$, and evolutionary stage differences of the molecular clouds that compose the Carina Nebula-Gum 31 complex.