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Fragmentation and filaments at the onset of star and cluster formation: SABOCA 350 $\mu$m view of ATLASGAL selected massive clumps

dc.contributor.authorLIN, Yuxin
hal.structure.identifierFORMATION STELLAIRE 2019
dc.contributor.authorCSENGERI, Timea
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, Friedrich
dc.contributor.authorURQUHART, James S.
hal.structure.identifierLaboratoire de Physique des Lasers [LPL]
dc.contributor.authorSCHULLER, Frédéric
hal.structure.identifierMillimeter and Submillimeter Astronomy
dc.contributor.authorWEISS, Axel
hal.structure.identifierMillimeter and Submillimeter Astronomy
dc.contributor.authorMENTEN, Karl M.
dc.date.issued2019
dc.identifier.issn0004-6361
dc.description.abstractEnThe structure formation of the dense interstellar material and the fragmentation of clumps into cores is a fundamental step to understand how stars and stellar clusters form. We aim to establish a statistical view of clump fragmentation at sub-parsec scales based on a large sample of massive clumps selected from the ATLASGAL survey. We used the APEX/SABOCA camera at 350 $\mu$m to image clumps at a resolution of 8.$''$5. The majority of the sample consists of massive clumps that are weak or in absorption at 24 $\mu$m. We resolve rich filamentary structures and identify the population of compact sources. We use association with mid-infrared 22-24 $\mu$m and 70 $\mu$m point sources to pin down the star formation activity of the cores. We then statistically assess their physical properties, and the fragmentation characteristics of massive clumps. We find a moderate correlation between the clump fragmentation levels with the clump gas density and the predicted number of fragments with pure Jeans fragmentation scenario; we find a strong correlation between the mass of the most massive fragment and the total clump mass, suggesting that the self-gravity may play an important role in the clumps' small scale structure formation. We identify 27 massive quiescent cores with $M_{\rm core}>100$ M$_{\odot}$ within 5 kpc; these are massive enough to be self-gravitating but do not yet show any sign of star-formation. This sample comprises, therefore, promising candidates of massive pre-stellar cores, or deeply embedded high-mass protostars.
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.title.enFragmentation and filaments at the onset of star and cluster formation: SABOCA 350 $\mu$m view of ATLASGAL selected massive clumps
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201935410
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A72
bordeaux.volume631
bordeaux.peerReviewedoui
hal.identifierhal-02281652
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02281652v1
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