Herschel view of the large-scale structure in the Chamaeleon dark clouds

Catarina, Alves de Oliveira 1 N. Schneider 2 Bruno, Merín 3 Timo, Prusti 4 Álvaro, Ribas Nick, Cox 5 Roland, Vavrek 3 Vera, Könyves Doris, Arzoumanian 6 Elena, Puga Göran, Pilbratt 4 Ágnes, Kóspal Philippe, André Pierre, Didelon Alexander, Men'Shchikov Pierre, Royer 7 Christoffel, Waelkens 8 Sylvain Bontemps 2 Elaine, Winston 4
1 ESAC - European Space Astronomy Center
2 FORMATION STELLAIRE 2015
LAB - Laboratoire d'Astrophysique de Bordeaux [Pessac], UB - Université de Bordeaux, INSU - CNRS - Institut national des sciences de l'Univers , CNRS - Centre National de la Recherche Scientifique
3 Herschel Science Center [Madrid]
4 RSSD - Research and Scientific Support Department, ESTEC
5 INSTITUUT VOOR STERRENKUNDE - Instituut voor Sterrenkunde
6 IAS - Institut d'astrophysique spatiale
7 Leosphere, 76 rue Monceau, 75008 Paris, France
8 Instituut voor Sterrenkunde
Abstract : The Chamaeleon molecular cloud complex is one of the nearest star-forming sites and encompasses three molecular clouds (Cha I, II, and III) that have a different star-formation history, from quiescent (Cha III) to actively forming stars (Cha II), and one that reaches the end of star-formation (Cha I). In this contribution we will present the analysis of the column density and temperature maps derived from PACS and SPIRE observations from the Herschel Gould Belt Survey. We find that the column density maps reveal a different morphological appearance for each of the three clouds, with a ridge-like structure for Cha I, a clump-dominated regime for Cha II, and an intricate filamentary network for Cha III. The filament width is measured to be about 0.12±0.04 pc in the three clouds, and the filaments are found to be gravitationally unstable in Cha I and II, but mostly subcritical in Cha III. Faint filaments (striations) are prominent in Cha I and are mostly aligned with the large-scale magnetic field. The PDFs of all regions show a lognormal distribution at low column densities. For higher densities, the PDF of Cha I shows a turnover indicative of an extended higher density component and culminates in a power-law tail. Cha II shows a power-law tail with a slope characteristic of gravity. The PDF of Cha III can be best fit by a single lognormal. The turbulence properties of the three regions are found to be similar, pointing towards a scenario where the clouds are impacted by large-scale processes.
Type de document :
Communication dans un congrès
2015IAUGA.2252675A - IAU General Assembly, Meeting #29, #2252675 - held 4-8 January 2015 in Seattle, USA, Jan 2015, Seattle, United States. 22, pp.52675, 2015
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https://hal.archives-ouvertes.fr/hal-01197438
Contributeur : Marie-Paule Pomies <>
Soumis le : vendredi 11 septembre 2015 - 16:28:42
Dernière modification le : mardi 29 mai 2018 - 12:51:08

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L3AB | INSU | UNIV-PARIS-SACLAY

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Catarina, Alves de Oliveira, N. Schneider, Bruno, Merín, Timo, Prusti, Álvaro, Ribas, et al.. Herschel view of the large-scale structure in the Chamaeleon dark clouds. 2015IAUGA.2252675A - IAU General Assembly, Meeting #29, #2252675 - held 4-8 January 2015 in Seattle, USA, Jan 2015, Seattle, United States. 22, pp.52675, 2015. 〈hal-01197438〉

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