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dc.contributor.authorGRATIER, P.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorBRON, Emeric
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorGERIN, Maryvonne
dc.contributor.authorPETY, Jérôme
dc.contributor.authorGUZMAN, Viviana V.
hal.structure.identifierUniversité Grenoble Alpes [2016-2019] [UGA [2016-2019]]
dc.contributor.authorORKISZ, Jan
dc.contributor.authorBARDEAU, Sébastien
dc.contributor.authorGOICOECHEA, Javier
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorLE PETIT, Franck
dc.contributor.authorLISZT, Harvey
dc.contributor.authorÖBERG, Karin
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorPERETTO, Nicolas
dc.contributor.authorROUEFF, Evelyne
dc.contributor.authorSIEVERS, Albrech
hal.structure.identifierMaison de la Simulation [MDLS]
dc.contributor.authorTREMBLIN, Pascal
dc.date.issued2017
dc.identifier.issn0004-6361
dc.description.abstractEnContext. The combination of wideband receivers and spectrometers currently available in (sub-)millimeter observatories deliver wide-field hyperspectral imaging of the interstellar medium. Tens of spectral lines can be observed over degree wide fields in about 50 h. This wealth of data calls for restating the physical questions about the interstellar medium in statistical terms.Aims. We aim to gain information on the physical structure of the interstellar medium from a statistical analysis of many lines from different species over a large field of view, without requiring detailed radiative transfer or astrochemical modeling.Methods. We coupled a non-linear rescaling of the data with one of the simplest multivariate analysis methods, namely the principal component analysis, to decompose the observed signal into components that we interpret first qualitatively and then quantitatively based on our deep knowledge of the observed region and of the astrochemistry at play.Results. We identify three principal components, linear compositions of line brightness temperatures, that are correlated at various levels with the column density, the volume density and the UV radiation field.Conclusions. When sampling a sufficiently diverse mixture of physical parameters, it is possible to decompose the molecular emission in order to gain physical insight on the observed interstellar medium. This opens a new avenue for future studies of the interstellar medium.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.subject.enISM: molecules
dc.subject.enISM: clouds
dc.subject.enphoton-dominated region (PDR)
dc.subject.enISM: individual objects: Orion B
dc.subject.enmethods: statistical
dc.title.enDissecting the molecular structure of the Orion B cloud: insight from principal component analysis
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201629847
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv1701.04205
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA100
bordeaux.volume599
bordeaux.peerReviewedoui
hal.identifierhal-01438758
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01438758v1
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