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Gas phase Elemental abundances in Molecular cloudS (GEMS) I. The prototypical dark cloud TMC 1

dc.contributor.authorNAVARRO, D.
hal.structure.identifierINAF - Osservatorio Astrofisico di Arcetri [OAA]
dc.contributor.authorCASELLI, P.
hal.structure.identifierObservatoire de Paris
dc.contributor.authorGERIN, M.
dc.contributor.authorKRAMMER, C.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA (UMR_8112)]
dc.contributor.authorROUEFF, E.
hal.structure.identifierAMOR 2019
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierObservatorio Astronomico Nacional, Madrid
dc.contributor.authorALONSO-ALBI, T.
dc.contributor.authorBACHILLER, R.
hal.structure.identifierDépartement d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée [DAPNIA]
dc.contributor.authorCAZAUX, S.
hal.structure.identifierLaboratoire de Radioastronomie
dc.contributor.authorCOMMERÇON, B.
dc.contributor.authorFRIESEN, R.
hal.structure.identifierObservatorio Astronomico Nacional, Madrid
dc.contributor.authorGARCIA-BURILLO, S.
dc.contributor.authorGIULIANO, B. M.
hal.structure.identifierCentro de Astrobiologia [Madrid] [CAB]
dc.contributor.authorGOICOECHEA, J. R.
hal.structure.identifierAMOR 2019
dc.contributor.authorGRATIER, P.
dc.contributor.authorHACAR, A.
hal.structure.identifierQueen Mary University of London [QMUL]
dc.contributor.authorJIMENEZ-SERRA, I.
dc.contributor.authorKIRK, J.
dc.contributor.authorLATTANZI, V.
hal.structure.identifierInstitut des Sciences Moléculaires [ISM]
dc.contributor.authorLOISON, J. C.
dc.contributor.authorMALINEN, P. J.
hal.structure.identifierINAF - Osservatorio Astronomico di Bologna [OABO]
dc.contributor.authorMARCELINO, N.
dc.contributor.authorMARTÍN-DOMÉNECH, R.
dc.contributor.authorMUÑOZ-CARO, G.
hal.structure.identifierLaboratoire de Radiopathologie [LRP]
dc.contributor.authorPINEDA, J.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorTAFALLA, M.
hal.structure.identifierInstituto de Ciencia de Materiales de Madrid [ICMM]
dc.contributor.authorTERCERO, B.
hal.structure.identifierJeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston]
dc.contributor.authorWARD-THOMPSON, D.
hal.structure.identifierInstituto de Radio Astronomía Milimétrica
dc.contributor.authorTREVIÑO-MORALES, S.
hal.structure.identifierDepartamento de Astrofisica [Madrid]
dc.contributor.authorRIVIERE-MARICHALAR, P.
hal.structure.identifierConsejo Superior de Investigaciones Cientificas [España] = Spanish National Research Council [Spain] [CSIC]
dc.contributor.authorRONCERO, O.
hal.structure.identifierAMOR 2019
dc.contributor.authorVIDAL, Thomas
dc.date.issued2019
dc.identifier.issn0004-6361
dc.description.abstractEnThis is the first paper of the GEMS (Gas phase Elemental abundances in Molecular CloudS) project, dedicated to the study of the prototypical dark cloud TMC1. GEMS is an IRAM 30m Large Programme aimed to determine the S, C, N, O depletions and X(e-) as a function of visual extinction in a selected set of prototypical star forming regions. Extensive millimeter observations have been carried out with the IRAM 30m telescope (3mm and 2mm) and the 40m Yebes telescope (bands K and Q) to determine the abundances of CO, HCO$^+$, HCN, CS, SO, HCS$^+$ and N$_{2}$H$^+$ in three cuts across the TMC1 filament. These cuts intersect the dense filament at the well-known positions TMC1-CP, TMC1-NH3 and TMC1-C and cover a visual extinction range of $\sim$3 mag to $>$20 mag. Two phases with differentiated physical conditions and chemistry can be distinguished in TMC1: i) the translucent phase that is characterized by molecular hydrogen densities of 1-5x10$^{-3}$ cm$^{-3}$ and is located at visual extinctions of 3--7 mag; ii) the dense phase with molecular hydrogen densities of a few 10$^4$ cm$^{-3}$, located at A$_v$~$>$~10 mag. The transition between these two phases (from 7 to 10 mag) occurs in a spatial scale of $<$0.04 pc and it is not well sampled by our observations. We determine the S, C, N, O depletions through the comparison of our molecular abundance estimates with the Meudon PDR code. Our results show that carbon, oxygen and sulfur are significantly depleted in the CII/C/CO transition zone (Av~$\sim$~3-4~mag) with C/H~$\sim$~8x10$^{-5}$, C/O~$\sim$~1, and S/H~$\sim$~8x10$^{-7}$. The gas phase abundances of C and O decrease by an additional factor of $\sim$2 during the translucent phase until the beginning of the dense phase at $\sim$10 mag. During the translucent phase S/H remains constant within the uncertainty of our measurements (a factor of 2).
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enGas phase Elemental abundances in Molecular cloudS (GEMS) I. The prototypical dark cloud TMC 1
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201834654
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPhysique [physics]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv1809.04978
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.volume624
bordeaux.issueA105
bordeaux.peerReviewedoui
hal.identifierhal-01876896
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01876896v1
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