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Quantitative inference of the H2 column densities from 3 mm molecular emission: case study towards Orion B

hal.structure.identifierFORMATION STELLAIRE 2020
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorGRATIER, Pierre
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres [LERMA]
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorPETY, Jérôme
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres [LERMA]
dc.contributor.authorBRON, Emeric
hal.structure.identifierPhyTI [PhyTI]
hal.structure.identifierInstitut FRESNEL [FRESNEL]
dc.contributor.authorROUEFF, Antoine
hal.structure.identifierChalmers University of Technology [Gothenburg, Sweden]
dc.contributor.authorORKISZ, Jan
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres [LERMA]
dc.contributor.authorGERIN, Maryvonne
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorDE SOUZA MAGALHAES, Victor
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres [LERMA]
dc.contributor.authorGAUDEL, Mathilde
hal.structure.identifierSignal et Communications [IRIT-SC]
dc.contributor.authorVONO, Maxime
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorBARDEAU, Sébastien
hal.structure.identifierGIPSA - Signal Images Physique [GIPSA-SIGMAPHY]
hal.structure.identifierApprentissage de modèles à partir de données massives [Thoth]
dc.contributor.authorCHANUSSOT, Jocelyn
hal.structure.identifierCentre de Recherche en Informatique, Signal et Automatique de Lille - UMR 9189 [CRIStAL]
dc.contributor.authorCHAINAIS, Pierre
hal.structure.identifierInstituto de Física Fundamental [Madrid] [IFF]
dc.contributor.authorGOICOECHEA, Javier
hal.structure.identifierPontificia Universidad Católica de Chile [UC]
dc.contributor.authorGUZMÁN, Viviana
hal.structure.identifierInstitut de recherche en astrophysique et planétologie [IRAP]
dc.contributor.authorHUGHES, Annie
hal.structure.identifierChalmers University of Technology [Gothenburg, Sweden]
dc.contributor.authorKAINULAINEN, Jouni
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres [LERMA]
dc.contributor.authorLANGUIGNON, David
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres [LERMA]
dc.contributor.authorLE BOURLOT, Jacques
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres [LERMA]
dc.contributor.authorLE PETIT, Franck
hal.structure.identifierAstrophysique
dc.contributor.authorLEVRIER, François
hal.structure.identifierNational Radio Astronomy Observatory [Charlottesville] [NRAO]
dc.contributor.authorLISZT, Harvey
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorPERETTO, Nicolas
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres [LERMA]
dc.contributor.authorROUEFF, Evelyne
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorSIEVERS, Albrecht
dc.date.issued2021-01
dc.identifier.issn0004-6361
dc.description.abstractEnContext. Based on the finding that molecular hydrogen is unobservable in cold molecular clouds, the column density measurements of molecular gas currently rely either on dust emission observation in the far-infrared, which requires space telescopes, or on star counting, which is limited in angular resolution by the stellar density. The (sub)millimeter observations of numerous trace molecules can be effective using ground-based telescopes, but the relationship between the emission of one molecular line and the H2 column density is non-linear and sensitive to excitation conditions, optical depths, and abundance variations due to the underlying physico- chemistry.Aims. We aim to use multi-molecule line emission to infer the H2 molecular column density from radio observations.Methods. We propose a data-driven approach to determine the H2 gas column densities from radio molecular line observations. We use supervised machine-learning methods (random forest) on wide-field hyperspectral IRAM-30m observations of the Orion B molecular cloud to train a predictor of the H2 column density, using a limited set of molecular lines between 72 and 116 GHz as input, and the Herschel-based dust-derived column densities as “ground truth” output.Results. For conditions similar to those of the Orion B molecular cloud, we obtained predictions of the H2 column density within a typical factor of 1.2 from the Herschel-based column density estimates. A global analysis of the contributions of the different lines to the predictions show that the most important lines are 13CO(1–0), 12CO(1–0), C18O(1–0), and HCO+(1–0). A detailed analysis distinguishing between diffuse, translucent, filamentary, and dense core conditions show that the importance of these four lines depends on the regime, and that it is recommended that the N2H+(1–0) and CH3OH(20–10) lines be added for the prediction of the H2 column density in dense core conditions.Conclusions. This article opens a promising avenue for advancing direct inferencing of important physical parameters from the molecular line emission in the millimeter domain. The next step will be to attempt to infer several parameters simultaneously (e.g., the column density and far-UV illumination field) to further test the method.
dc.description.sponsorshipMIAI @ Grenoble Alpes - ANR-19-P3IA-0003
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/
dc.subject.enmethods: statistical
dc.subject.enISM: clouds
dc.subject.enISM: molecules
dc.title.enQuantitative inference of the H2 column densities from 3 mm molecular emission: case study towards Orion B
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202037871
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.subject.halInformatique [cs]
dc.identifier.arxiv2008.13417
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA27
bordeaux.volume645
bordeaux.peerReviewedoui
hal.identifierhal-03017404
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-03017404v1
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