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

hal.structure.identifierEuropean Space Astronomy Centre [ESAC]
dc.contributor.authorALVES DE OLIVEIRA, Catarina,
hal.structure.identifierFORMATION STELLAIRE 2015
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierHerschel Science Center [Madrid]
dc.contributor.authorMERÍN, Bruno,
hal.structure.identifierResearch and Scientific Support Department, ESTEC [RSSD]
dc.contributor.authorPRUSTI, Timo,
dc.contributor.authorRIBAS, Álvaro,
hal.structure.identifierInstituut voor Sterrenkunde [Leuven]
dc.contributor.authorCOX, Nick,
hal.structure.identifierHerschel Science Center [Madrid]
dc.contributor.authorVAVREK, Roland,
dc.contributor.authorKÖNYVES, Vera,
hal.structure.identifierInstitut d'astrophysique spatiale [IAS]
dc.contributor.authorARZOUMANIAN, Doris,
dc.contributor.authorPUGA, Elena,
hal.structure.identifierResearch and Scientific Support Department, ESTEC [RSSD]
dc.contributor.authorPILBRATT, Göran,
dc.contributor.authorKÓSPAL, Ágnes,
dc.contributor.authorANDRÉ, Philippe,
dc.contributor.authorDIDELON, Pierre,
dc.contributor.authorMEN'SHCHIKOV, Alexander,
hal.structure.identifierLeosphere, 76 rue Monceau, 75008 Paris, France
dc.contributor.authorROYER, Pierre,
hal.structure.identifierInstituut voor Sterrenkunde [Leuven]
dc.contributor.authorWAELKENS, Christoffel,
hal.structure.identifierFORMATION STELLAIRE 2015
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierResearch and Scientific Support Department, ESTEC [RSSD]
dc.contributor.authorWINSTON, Elaine,
dc.date.issued2015-08
dc.date.conference2015-01-04
dc.description.abstractEnThe 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.
dc.language.isoen
dc.title.enHerschel view of the large-scale structure in the Chamaeleon dark clouds
dc.typeCommunication dans un congrès
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
bordeaux.page52675
bordeaux.volume22
bordeaux.countryUS
bordeaux.conference.citySeattle
bordeaux.peerReviewedoui
hal.identifierhal-01197438
hal.version1
hal.invitednon
hal.proceedingsnon
hal.conference.end2015-01-08
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01197438v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.date=2015-08&rft.volume=22&rft.spage=52675&rft.epage=52675&rft.au=ALVES%20DE%20OLIVEIRA,%20Catarina,&SCHNEIDER,%20N.&MER%C3%8DN,%20Bruno,&PRUSTI,%20Timo,&RIBAS,%20%C3%81lvaro,&rft.genre=unknown


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