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Massive Clumps in the NGC 6334 Star Forming Region

dc.contributor.authorMUNOZ, Diego J.
dc.contributor.authorMARDONES, Diego
dc.contributor.authorGARAY, Guido
dc.contributor.authorREBOLLEDO, David
dc.contributor.authorBROOKS, Kate
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire Hétérochimie Fondamentale et Appliquée [LHFA]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBONTEMPS, Sylvain
dc.date.created2007-06-20
dc.date.issued2007
dc.identifier.issn0004-637X
dc.description.abstractEnWe report observations of dust continuum emission at 1.2 mm toward the star forming region NGC 6334 made with the SEST SIMBA bolometer array. The observations cover an area of $\sim 2$ square degrees with approximately uniform noise. We detected 181 clumps spanning almost three orders of magnitude in mass (3\Msun$-6\times10^3$ \Msun) and with sizes in the range 0.1--1.0 pc. We find that the clump mass function $dN/d\log M$ is well fit with a power law of the mass with exponent -0.6 (or equivalently $dN/dM \propto M^{-1.6}$). The derived exponent is similar to those obtained from molecular line emission surveys and is significantly different from that of the stellar initial mass function. We investigated changes in the mass spectrum by changing the assumptions on the temperature distribution of the clumps and on the contribution of free-free emission to the 1.2 mm emission, and found little changes on the exponent. The Cumulative Mass Distribution Function is also analyzed giving consistent results in a mass range excluding the high-mass end where a power-law fit is no longer valid. The masses and sizes of the clumps observed in NGC 6334 indicate that they are not direct progenitors of stars and that the process of fragmentation determines the distribution of masses later on or occurs at smaller spatial scales. The spatial distribution of the clumps in NGC 6334 reveals clustering which is strikingly similar to that exhibited by young stars in other star forming regions. A power law fit to the surface density of companions gives $\Sigma\propto \theta^{-0.62}$.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subject.enstars: formation
dc.subject.enmolecular clouds: individual(NGC 6334)|stars: initial mass function
dc.title.enMassive Clumps in the NGC 6334 Star Forming Region
dc.typeArticle de revue
dc.identifier.doi10.1086/521206
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv0706.3035
bordeaux.journalThe Astrophysical Journal
bordeaux.page906-917
bordeaux.volume668
bordeaux.issue2
bordeaux.peerReviewedoui
hal.identifierhal-00177576
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00177576v1
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