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A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey

dc.contributor.authorKONYVES, V.,
dc.contributor.authorANDRE, Ph.,
dc.contributor.authorMEN'SHCHIKOV, A.,
hal.structure.identifierDépartement d'Astrophysique (ex SAP) [DAP]
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorPALMEIRIM, P.,
hal.structure.identifierInstitut d'astrophysique spatiale [IAS]
dc.contributor.authorARZOUMANIAN, D.,
hal.structure.identifierLaboratory for Atmospheric and Space Physics [Boulder] [LASP]
dc.contributor.authorSCHNEIDER, N.
dc.contributor.authorROY, A.,
dc.contributor.authorDIDELON, P.,
hal.structure.identifierSan Pedro de Atacama Celestial Explorations [SPACE]
dc.contributor.authorMAURY, A.,
dc.contributor.authorSHIMAJIRI, Y.,
dc.contributor.authorDI FRANCESCO, J.,
hal.structure.identifierFORMATION STELLAIRE 2015
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierDépartement d'Astrophysique (ex SAP) [DAP]
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorPERETTO, N.,
dc.contributor.authorBENEDETTINI, M.,
dc.contributor.authorBERNARD, J.-Ph.,
dc.contributor.authorELIA, D.,
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorGRIFFIN, M. J.,
dc.contributor.authorHILL, T.,
dc.contributor.authorKIRK, J.,
dc.contributor.authorLADJELATE, B.,
hal.structure.identifierUniversity of California [Los Angeles] [UCLA]
dc.contributor.authorMARSH, K.,
hal.structure.identifierService des Photons, Atomes et Molécules [SPAM]
dc.contributor.authorMARTIN, P. G.,
hal.structure.identifierProcédés, Matériaux et Energie Solaire [PROMES]
dc.contributor.authorMOTTE, F.,
dc.contributor.authorNGUYEN LUONG, Q.,
dc.contributor.authorPEZZUTO, S.,
dc.contributor.authorROUSSEL, H.,
dc.contributor.authorRYGL, K. L. J.,
dc.contributor.authorSADAVOY, S. I.,
dc.contributor.authorSCHISANO, E.,
dc.contributor.authorSPINOGLIO, L.,
dc.contributor.authorWARD-THOMPSON, D.,
hal.structure.identifierSLAC National Accelerator Laboratory [SLAC]
dc.contributor.authorWHITE, G. J.,
dc.date.accessioned2021-07-07T16:12:51Z
dc.date.available2021-07-07T16:12:51Z
dc.date.issued2015-07
dc.identifier.issn0004-6361
dc.identifier.urihttps://oskar-bordeaux.fr/handle/20.500.12278/95957
dc.description.abstractEnWe present and discuss the results of the Herschel Gould Belt survey observations in a ~11 deg^2 area of the Aquila molecular cloud complex at d~260 pc, imaged with the SPIRE/PACS cameras from 70 to 500 micron. We identify a complete sample of starless dense cores and embedded protostars in this region, and analyze their global properties and spatial distributions. We find a total of 651 starless cores, ~60% of which are gravitationally bound prestellar cores, and they will likely form stars in the future. We also detect 58 protostellar cores. The core mass function (CMF) derived for the prestellar cores is very similar in shape to the stellar initial mass function (IMF), supporting the earlier view that there is a close physical link between the IMF and the CMF. The global shift in mass scale observed between the CMF and the IMF is consistent with a typical star formation efficiency of ~40%. By comparing the numbers of starless cores to the number of young stellar objects, we estimate that the lifetime of prestellar cores is ~1 Myr. We find a strong correlation between the spatial distribution of prestellar cores and the densest filaments. About 90% of the Herschel-identified prestellar cores are located above a background column density corresponding to A_V~7, and ~75% of them lie within filamentary structures with supercritical masses per unit length >~16 M_sun/pc. These findings support a picture wherein the cores making up the peak of the CMF (and probably responsible for the base of the IMF) result primarily from the gravitational fragmentation of marginally supercritical filaments. Given that filaments appear to dominate the mass budget of dense gas at A_V>7, our findings also suggest that the physics of prestellar core formation within filaments is responsible for a characteristic "efficiency" SFR/M_dense ~5+-2 x 10^-8 yr^-1 for the star formation process in dense gas.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enA census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey
dc.typeArticle de revue
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA&A 2015
bordeaux.hal.laboratoriesLaboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804*
bordeaux.institutionCNRS
bordeaux.institutionUniversité de Bordeaux
bordeaux.peerReviewedoui
hal.identifierhal-01179284
hal.version1
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01179284v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2015-07&rft.spage=A&A%202015&rft.epage=A&A%202015&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=KONYVES,%20V.,&ANDRE,%20Ph.,&MEN'SHCHIKOV,%20A.,&PALMEIRIM,%20P.,&ARZOUMANIAN,%20D.,&rft.genre=article


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