Volume 554, June 2013
|Number of page(s)||16|
|Section||Interstellar and circumstellar matter|
|Published online||28 May 2013|
III. Detailed cloud structure and feedback effects
Received: 11 January 2013
Accepted: 19 March 2013
Context. The star formation process in large clusters/associations can be strongly influenced by the feedback from high-mass stars. Whether the resulting net effect of the feedback is predominantly negative (cloud dispersal) or positive (triggering of star formation due to cloud compression) is still an open question.
Aims. The Carina Nebula complex (CNC) represents one of the most massive star-forming regions in our Galaxy. We use our Herschel far-infrared observations to study the properties of the clouds over the entire area of the CNC (with a diameter of ≈3.2°, which corresponds to ≈125 pc at a distance of 2.3 kpc). The good angular resolution (10′′−36′′) of the Herschel maps corresponds to physical scales of 0.1–0.4 pc, and allows us to analyze the small-scale (i.e., clump-size) structures of the clouds.
Methods. The full extent of the CNC was mapped with PACS and SPIRE in the 70, 160, 250, 350, and 500 μm bands. We determined temperatures and column densities at each point in these maps by modeling the observed far-infrared spectral energy distributions. We also derived a map showing the strength of the UV radiation field. We investigated the relation between the cloud properties and the spatial distribution of the high-mass stars and computed total cloud masses for different density thresholds.
Results. Our Herschel maps resolve for the first time the small-scale structure of the dense clouds over the entire spatial extent of the CNC. Several particularly interesting regions, including the prominent pillars south of η Car, are analyzed in detail. We compare the cloud masses derived from the Herschel data with previous mass estimates based on sub-mm and molecular line data. Our maps also reveal a peculiar wave-like pattern in the northern part of the Carina Nebula. Finally, we characterize two prominent cloud complexes at the periphery of our Herschel maps, which are probably molecular clouds in the Galactic background.
Conclusions. We find that the density and temperature structure of the clouds in most parts of the CNC is dominated by the strong feedback from the numerous massive stars, and not by random turbulence. Comparing the cloud mass and the star formation rate derived for the CNC with other Galactic star-forming regions suggests that the CNC is forming stars in a particularly efficient way. We suggest this to be a consequence of triggered star formation by radiative cloud compression.
Key words: ISM: clouds / ISM: structure / stars: formation / ISM: general
The Herschel data described in this paper have been obtained in the open time project OT1_tpreibis_1 (PI: Preibisch). Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
Appendix A is available in electronic form at http://www.aanda.org
© ESO, 2013
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