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dc.rights.license© 2020. The American Astronomical Society. All rights reserved.-
dc.contributor.authorFeng, S.-
dc.contributor.authorLi, D.-
dc.contributor.authorCaselli, P.-
dc.contributor.authorDu, F.-
dc.contributor.authorLin, Y.-
dc.contributor.authorSipilä, O.-
dc.contributor.authorBeuther, H.-
dc.contributor.authorSanhueza, P.-
dc.contributor.authorTatematsu, K.-
dc.contributor.authorLiu, Y.-
dc.contributor.authorZhang, Q.-
dc.contributor.authorWang, Y.-
dc.contributor.authorHogge, T.-
dc.contributor.authorJiménez Serra, I.-
dc.contributor.authorLu, X.-
dc.contributor.authorLiu, T.-
dc.contributor.authorWang, K.-
dc.contributor.authorZhang, Y.-
dc.contributor.authorZahorecz, S.-
dc.contributor.authorLi, G.-
dc.contributor.authorLiu, H. B.-
dc.contributor.authorYuan, J.-
dc.contributor.otherUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737-
dc.date.accessioned2021-04-19T09:48:58Z-
dc.date.available2021-04-19T09:48:58Z-
dc.date.issued2020-10-01-
dc.identifier.citationThe Astrophysical Journal 901(2): 145(2020)es
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/414-
dc.description.abstractThe physical and chemical properties of cold and dense molecular clouds are key to understanding how stars form. Using the IRAM 30 m and NRO 45 m telescopes, we carried out a Multiwavelength line-Imaging survey of the 70 μm-dArk and bright clOuds (MIAO). At a linear resolution of 0.1–0.5 pc, this work presents a detailed study of parsec-scale CO depletion and HCO+ deuterium (D-) fractionation toward four sources (G11.38+0.81, G15.22–0.43, G14.49–0.13, and G34.74–0.12) included in our full sample. In each source with T < 20 K and nH ~ 104–105 cm−3, we compared pairs of neighboring 70 μm bright and dark clumps and found that (1) the H2 column density and dust temperature of each source show strong spatial anticorrelation; (2) the spatial distribution of CO isotopologue lines and dense gas tracers, such as 1–0 lines of H13CO+ and DCO+, are anticorrelated; (3) the abundance ratio between C18O and DCO+ shows a strong correlation with the source temperature; (4) both the C18O depletion factor and D-fraction of HCO+ show a robust decrease from younger clumps to more evolved clumps by a factor of more than 3; and (5) preliminary chemical modeling indicates that chemical ages of our sources are ~8 × 104 yr, which is comparable to their free-fall timescales and smaller than their contraction timescales, indicating that our sources are likely dynamically and chemically young.es
dc.description.sponsorshipS.F. acknowledges the support of National Natural Science Foundation of China No. 11988101, CAS International Partnership Program No. 114A11KYSB20160008, and the EACOA fellowship from the East Asia Core Observatories Association (EACOA). EACOA consists of the National Astronomical Observatory of China, the National Astronomical Observatory of Japan, the Academia Sinica Institute of Astronomy and Astrophysics, and the Korea Astronomy and Space Science Institute. P.C. acknowledges financial support from the Max Planck Society. H.B. and Y.W. acknowledge support from the European Research Council under the Horizon 2020 Framework Program via ERC Consolidator Grant CSF-648505. H.B. also acknowledges support from the Deutsche Forschungsgemeinschaft in the Collaborative Research Center (SFB 881) "The Milky Way System" (subproject B1). F.D. is supported by the One Hundred Person Project of the Chinese Academy of Sciences through grant 2017-089 and by NSFC grant No. 11873094. I.J.-S. has received partial support from the Spanish FEDER (project No. ESP2017-86582-C4-1-R) and the State Research Agency (AEI; project number PID2019-105552RB-C41). P.S. was partially supported by Grant-in-Aid for Scientific Research (KAKENHI) No. 18H01259 of the Japan Society for the Promotion of Science (JSPS). K.W. acknowledges support by the National Key Research and Development Program of China (2017YFA0402702, 2019YFA0405100), the National Science Foundation of China (11973013, 11721303), and the starting grant at the Kavli Institute for Astronomy and Astrophysics, Peking University (7101502016). S.Z. acknowledges support by NAOJ ALMA Scientific Research grant No. 2016-03B. Part of this work was supported by the NAOJ Visiting Joint Research program (grant No. 1901-0403); With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).es
dc.language.isoenges
dc.publisherThe Institute of Physics (IOP)es
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2017-86582-C4-1-R/ES/CONTRIBUCION ESPAÑOLA A LAS MISIONES ESPACIALES CRIOGENICAS SPICA Y ATHENA, POST-OPERACIONES DE HERSCHEL Y EXPLOTACION CIENTIFICA MULTIFRECUENCIA/-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-105552RB-C41/ES/CONTRIBUCION DEL CAB A SPICA, DESARROLLO DE INSTRUMENTACION CRIOGENICA Y EXPLOTACION CIENTIFICA MULTILONGITUD DE ONDA/-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectInterstellar mediumes
dc.subjectInterstellar moleculeses
dc.subjectStar formationes
dc.subjectMassive starses
dc.subjectAstrochemistryes
dc.titleThe Chemical Structure of Young High-mass Star-forming Clumps. II. Parsec-scale CO Depletion and Deuterium Fraction of HCO+es
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidFeng, S. [0000-0002-4707-8409]-
dc.contributor.orcidLi, D. [0000-0003-3010-7661]-
dc.contributor.orcidCaselli, P. [0000-0003-1481-7911]-
dc.contributor.orcidDu, F. [0000-0002-7489-0179]-
dc.contributor.orcidLin, Y. [0000-0001-9299-5479-
dc.contributor.orcidSipilä, O. [0000-0002-9148-1625]-
dc.contributor.orcidBeuther, H. [0000-0002-1700-090X]-
dc.contributor.orcidSanhueza, P. [0000-0002-7125-7685]-
dc.contributor.orcidTatematsu, K. [0000-0002-8149-8546]-
dc.contributor.orcidLiu, S. Y. [0000-0003-4603-7119]-
dc.contributor.orcidZhang, Q. [0000-0003-2384-6589]-
dc.contributor.orcidWang, Y. [0000-0003-2226-4384]-
dc.contributor.orcidHogge, T. [0000-0002-7211-7078]-
dc.contributor.orcidJiménez Serra, I. [0000-0003-4493-8714]-
dc.contributor.orcidLu, X. [0000-0003-2619-9305]-
dc.contributor.orcidLiu, T. [0000-0002-5286-2564]-
dc.contributor.orcidWang, K. [0000-0002-7237-3856]-
dc.contributor.orcidZhang, Z. Y. [0000-0002-7299-2876]-
dc.contributor.orcidZahorecz, S. [0000-0001-6149-1278]-
dc.contributor.orcidLi, G. [0000-0003-3144-1952]-
dc.contributor.orcidLiu, H. B. [0000-0003-2300-2626]-
dc.contributor.orcidYuan, J. [0000-0001-8060-3538]-
dc.identifier.doi10.3847/1538-4357/abada3-
dc.identifier.e-issn1538-4357-
dc.contributor.funderNational Natural Science Foundation of China (NSFC)-
dc.contributor.funderMax-Planck-Gesellschaft (MPG)-
dc.contributor.funderEuropean Research Council (ERC)-
dc.contributor.funderChinese Academy of Sciences (CAS)-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
dc.contributor.funderJapan Society for the Promotion of Science (JSPS)-
dc.description.peerreviewedPeer reviewes
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001809-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004189-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100002367-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100011033-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001691-
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
dc.relation.projectIDinfo:eu-repo/grantAgreement/EC/H2020/648505-
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