Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12666/191
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dc.rights.licenseCopyright © 2020, Oxford University Press-
dc.contributor.authorZeng, S.-
dc.contributor.authorZhang, Q.-
dc.contributor.authorJiménez Serra, I.-
dc.contributor.authorTercero, B.-
dc.contributor.authorLu, X.-
dc.contributor.authorMartín Pintado, J.-
dc.contributor.authorDe Vicente, P.-
dc.contributor.authorRivilla, V. M.-
dc.contributor.authorLi, S.-
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.accessioned2021-04-09T10:32:06Z-
dc.date.available2021-04-09T10:32:06Z-
dc.date.issued2020-07-29-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 497(4): 4896–4909(2020)es
dc.identifier.issn1365-2966-
dc.identifier.otherhttps://academic.oup.com/mnras/article-abstract/497/4/4896/5877919-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/191-
dc.descriptionCloud–cloud collision as drivers of the chemical complexity in Galactic Centre molecular clouds - 24 Hours accesses
dc.description.abstractG+0.693-0.03 is a quiescent molecular cloud located within the Sagittarius B2 (Sgr B2) star-forming complex. Recent spectral surveys have shown that it represents one of the most prolific repositories of complex organic species in the Galaxy. The origin of such chemical complexity, along with the small-scale physical structure and properties of G+0.693-0.03, remains a mystery. In this paper, we report the study of multiple molecules with interferometric observations in combination with single-dish data in G+0.693-0.03. Despite the lack of detection of continuum source, we find small-scale (0.2 pc) structures within this cloud. The analysis of the molecular emission of typical shock tracers such as SiO, HNCO, and CH3OH unveiled two molecular components, peaking at velocities of 57 and 75 km s(-1). They are found to be interconnected in both space and velocity. The position-velocity diagrams show features that match with the observational signatures of a cloud-cloud collision. Additionally, we detect three series of class I methanol masers known to appear in shocked gas, supporting the cloud-cloud collision scenario. From the maser emission we provide constraints on the gas kinetic temperatures (similar to 30-150 K) and H-2 densities (10(4)-10(5) cm(-2)). These properties are similar to those found for the starburst galaxy NGC 253 also using class I methanol masers, suggested to be associated with a cloud-cloud collision. We conclude that shocks driven by the possible cloud-cloud collision is likely the most important mechanism responsible for the high level of chemical complexity observed in G+0.693-0.03.es
dc.description.sponsorshipWe wish to thank the anonymous referee for his/her very useful comments that helped to improve this article. We would like to thank Adam Ginsburg (University of Florida) for providing the ALMA image. Based on observations with the 40m radio telescope of the National Geographic Institute of Spain (IGN) at Yebes Observatory (project number 20A008). Yebes Observatory acknowledges the ERC for funding support under grant ERC-2013-Syg-610256-NANOCOSMOS. SZ acknowledges support through a Principal's studentship funded by Queen Mary University of London, the visiting student program funded by Harvard-Smithsonian Center for Astrophysics. IJS and JMP have received partial support from the Spanish FEDER under project number ESP2017-86582-C4-1-R. VMRhas received funding from the European Union'sHorizon 2020 research and innovation programme under the Marie SklodowskaCurie grant agreement No 664931. XL was financially supported by JSPS KAKENHI grants No. 18K13589 & 20K14528; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).es
dc.language.isoenges
dc.publisherOxford Academics: Blackwell Publishinges
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.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectISM: cloudses
dc.subjectKinematics and dynamicses
dc.subjectISM: moleculeses
dc.subjectGalaxy: centrees
dc.titleCloud–cloud collision as drivers of the chemical complexity in Galactic Centre molecular clouds.es
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidDe Vicente, P. [0000-0002-5902-5005]-
dc.contributor.orcidRivilla, V. M. [0000-0002-2887-5859]-
dc.contributor.orcidLi, S. [0000-0003-1275-5251]-
dc.identifier.doi10.1093/mnras/staa2187-
dc.identifier.e-issn0035-8711-
dc.contributor.funderEuropean Research Council (ERC)-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
dc.contributor.funderEuropean Commission (EC)-
dc.contributor.funderJapan Society for the Promotion of Science (KAKENHI)-
dc.description.peerreviewedPeer reviewes
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/FP7/610256-
dc.relation.projectIDinfo:eu-repo/grantAgreement/EC/H2020/664931-
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