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Two Mass Distributions in the L 1641 Molecular Clouds: The Herschel connection of Dense Cores and Filaments in Orion A

dc.contributor.authorPOLYCHRONI, Danae
dc.contributor.authorSCHISANO, Eugenio
dc.contributor.authorELIA, Davide
dc.contributor.authorROY, Arnaud
dc.contributor.authorMOLINARI, Sergio
hal.structure.identifierEpilepsy Center Kork
dc.contributor.authorMARTIN, Peter
dc.contributor.authorANDRE, Philippe
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorTURRINI, Diego
dc.contributor.authorRYGL, Kazi
dc.contributor.authorBENEDETTINI, Milena
dc.contributor.authorBUSQUET, Gemma
dc.contributor.authorDI GIORGIO, Anna Maria
dc.contributor.authorPESTALOZZI, Michele
dc.contributor.authorPEZZUTO, Stefano
dc.contributor.authorARZOUMANIAN, Doris
hal.structure.identifierFORMATION STELLAIRE 2013
dc.contributor.authorBONTEMPS, Sylvain
dc.contributor.authorDI FRANCESCO, James
dc.contributor.authorHENNEMANN, Martin
dc.contributor.authorHILL, Tracy
dc.contributor.authorKONYVES, Vera
dc.contributor.authorMEN'SHCHIKOV, Alexander
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorMOTTE, Frederique
dc.contributor.authorNGUYEN-LUONG, Quang
hal.structure.identifierFORMATION STELLAIRE 2013
dc.contributor.authorSCHNEIDER, N.
dc.contributor.authorPERETTO, Nicolas
hal.structure.identifierSLAC National Accelerator Laboratory [SLAC]
dc.contributor.authorWHITE, Glenn
dc.date.conference2013
dc.description.abstractEnWe present the Herschel Gould Belt survey maps of the L 1641 molecular clouds in Orion A. We extracted both the filaments and dense cores in the region. We identified which of dense sources are proto- or pre-stellar, and studied their association with the identified filaments. We find that although most (71%) of the pre-stellar sources are located on filaments there is still a significant fraction of sources not associated with such structures. We find that these two populations (on and off the identified filaments) have distinctly different mass distributions. The mass distribution of the sources on the filaments is found to peak at 4 Solar Masses and drives the shape of the CMF at higher masses, which we fit with a power law of the form dN /dlogM ∝ M -1.4±0.4 . The mass distribution of the sources off the filaments, on the other hand, peaks at 0.8 Solar Masses and leads to a flattening of the CMF at masses lower than ˜4 Solar Masses. We postulate that this difference between the mass distributions is due to the higher proportion of gas that is available in the filaments, rather than in the diffuse cloud.
dc.language.isoen
dc.title.enTwo Mass Distributions in the L 1641 Molecular Clouds: The Herschel connection of Dense Cores and Filaments in Orion A
dc.typeCommunication dans un congrès
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
bordeaux.conference.titleProtostars and Planets VI, Heidelberg, July 15-20, 2013. Poster #1S044
bordeaux.countryDE
bordeaux.conference.cityHeidelberg
bordeaux.peerReviewedoui
hal.identifierhal-00880542
hal.version1
hal.invitednon
hal.proceedingsnon
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00880542v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.au=POLYCHRONI,%20Danae&SCHISANO,%20Eugenio&ELIA,%20Davide&ROY,%20Arnaud&MOLINARI,%20Sergio&rft.genre=unknown


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