Herschel far-infrared observations of the Carina Nebula complex I: Introduction and global cloud structure

TL;DR

This study uses Herschel far-infrared observations to analyze the complex, filamentary structure and temperature distribution of the Carina Nebula's clouds, revealing insights into their mass, composition, and star-forming potential.

Contribution

First comprehensive Herschel-based mapping of the Carina Nebula's cloud structure, temperature, and mass distribution, highlighting feedback effects and atomic versus molecular gas proportions.

Findings

Clouds exhibit complex filamentary structures dominated by stellar feedback.

Temperature gradient from 35-40 K centrally to <20 K at the edges.

Total cloud mass in the central region is approximately 656,000 solar masses.

Abstract

The Carina Nebula represents one of the most massive galactic star forming regions and displays a high level of massive star feedback. We used SPIRE and PACS onboard of Herschel to map the full spatial extent of the clouds in the Carina Nebula complex at wavelengths between 70 and 500 micrometer. We determine color temperatures and column densities of the clouds in the complex. Our Herschel maps show that the clouds have a very complex and filamentary structure that is dominated by the radiation and wind feedback from the massive stars. In most locations, the column density of the clouds is N_H < 2x10^22 cm^-2; denser cloud structures are restricted to just a few locations. We find a clear large scale temperature gradient from 35-40 K in the central region to <20 K at the periphery and in the densest parts of individual pillars. The total mass of the clouds seen by Herschel in the central (1 deg radius) region is ~656000 M_sun. A simple radiative transfer model for the global spectral energy distribution suggests that the total mass of all the gas (including a warmer component that is not well traced by Herschel) is <=890000 M_sun. Despite the strong feedback from numerous massive stars that is going on since several million years, there are still several 10000 M_sun of cool cloud material present at column-densities sufficient for further star formation. Comparison of our total gas mass estimates to molecular cloud masses derived from CO line mapping suggests that as much as about 75% of all the gas is in atomic rather than molecular form.