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The $Herschel$ view of the dense core population in the Ophiuchus molecular cloud

hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorLADJELATE, B.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorANDRÉ, Ph.
hal.structure.identifierJeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston]
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorKÖNYVES, V.
hal.structure.identifierJeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston]
dc.contributor.authorWARD-THOMPSON, D.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorMEN’SHCHIKOV, A.
hal.structure.identifierAstrophysique
dc.contributor.authorBRACCO, A.
hal.structure.identifierInstituto de Astrofísica e Ciências do Espaço [IASTRO]
dc.contributor.authorPALMEIRIM, P.
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorROY, A.
hal.structure.identifierKagoshima University
hal.structure.identifierNational Astronomical Observatory of Japan [NAOJ]
dc.contributor.authorSHIMAJIRI, Y.
hal.structure.identifierJeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston]
dc.contributor.authorKIRK, J. M.
hal.structure.identifierInstituto de Astrofísica e Ciências do Espaço [IASTRO]
dc.contributor.authorARZOUMANIAN, D.
hal.structure.identifierIstituto di Astrofisica e Planetologia Spaziali - INAF [IAPS]
dc.contributor.authorBENEDETTINI, M.
hal.structure.identifierNational Research Council of Canada [NRC]
dc.contributor.authorDI FRANCESCO, J.
hal.structure.identifierEuropean Southern Observatory [ESO]
hal.structure.identifierIstituto di Astrofisica e Planetologia Spaziali - INAF [IAPS]
hal.structure.identifierUniversità degli Studi di Roma Tor Vergata [Roma, Italia] = University of Rome Tor Vergata [Rome, Italy] = Université de Rome Tor Vergata [Rome, Italie]
dc.contributor.authorFIORELLINO, E.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierNational Astronomical Observatory of Japan [NAOJ]
dc.contributor.authorPEZZUTO, S.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorMOTTE, F.
dc.date.issued2020
dc.identifier.issn0004-6361
dc.description.abstractEnContext. $Herschel$ observations of nearby clouds in the Gould Belt support a paradigm for low-mass star formation, starting with the generation of molecular filaments, followed by filament fragmentation, and the concentration of mass into self-gravitating prestellar cores. In the case of the Ophiuchus molecular complex, a rich star formation activity has been documented for many years inside the clumps of L1688, the main and densest cloud of the complex, and in the more quiescent twin cloud L1689 thanks to extensive surveys at infrared and other wavelengths.Aims. With the unique far-infrared and submillimeter continuum imaging capabilities of the $Herschel$ Space observatory, the closeby ($d$ = 139 pc) Ophiuchus cloud was extensively mapped at five wavelengths from 70 to 500 $\mu$m with the aim of providing a complete census of dense cores in this region, including unbound starless cores, bound prestellar cores, and protostellar cores.Methods. Taking full advantage of the high dynamic range and multi-wavelength nature of the $Herschel$ data, we used the multi-scale decomposition algorithms $getsources$ and $getfilaments$ to identify an essentially complete sample of dense cores and filaments in the cloud and study their properties.Results. The densest clouds of the Ophiuchus complex, L1688 and L1689, which thus far are only indirectly described as filamentary regions owing to the spatial distribution of their young stellar objects, are now confirmed to be dominated by filamentary structures. The tight correlation observed between prestellar cores and filamentary structures in L1688 and L1689 supports the view that solar-type star formation occurs primarily in dense filaments. While the sub clouds of the complex show some disparities, L1689 being apparently less efficient than L1688 at forming stars when considering their total mass budgets, both sub clouds share almost the same prestellar core formation efficiency in dense molecular gas. We also find evidence in the $Herschel$ data for a remarkable concentric geometrical configuration in L1688 which is dominated by up to three arc-like compression fronts and has presumably been created by shockwave events emanating from the Sco OB2 association, including the neighboring massive (O9V) star $\sigma$ Sco.Conclusions. Our $Herschel$ study of the well-documented Ophiuchus region has allowed us to further analyze the influence of several early-type (OB) stars surrounding the complex, thus providing positive feedback and enhancing star formation activity in the dense central part of the region, L1688.
dc.description.sponsorshipVers une vision unifiée de la formation stellaire dans les galaxies : Origine de la structure filamentaire du milieu interstellaire, des cœurs pré-stellaires et des amas protostellaires vus avec Herschel - ANR-11-BS56-0010
dc.description.sponsorshipGENeration et Evolution des Structures du milieu InterStellaire - ANR-16-CE92-0035
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enstars: formation
dc.subject.enISM: clouds
dc.subject.enISM: structure
dc.subject.enISM: individual objects: Ophiuchus Complex
dc.subject.ensubmillimeter: ISM
dc.title.enThe $Herschel$ view of the dense core population in the Ophiuchus molecular cloud
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201936442
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.description.sponsorshipEuropeToward a Complete View of Star Formation: The Origin of Molecular Clouds, Prestellar Cores, and Star Clusters
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA74
bordeaux.volume638
bordeaux.peerReviewedoui
hal.identifiercea-02870754
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//cea-02870754v1
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=2020&rft.volume=638&rft.spage=A74&rft.epage=A74&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=LADJELATE,%20B.&ANDR%C3%89,%20Ph.&K%C3%96NYVES,%20V.&WARD-THOMPSON,%20D.&MEN%E2%80%99SHCHIKOV,%20A.&rft.genre=article


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