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First detection of the [CII] 158 µm line in the intermediate-velocity cloud Draco

hal.structure.identifierI. Physikalisches Institut [Köln]
dc.contributor.authorSCHNEIDER, Nicola
dc.contributor.authorOSSENKOPF-OKADA, Volker
dc.contributor.authorKEILMANN, Eduard
hal.structure.identifierGoethe-Universität Frankfurt am Main
dc.contributor.authorRÖLLIG, Markus
dc.contributor.authorKABANOVIC, Slawa
hal.structure.identifierStratospheric Observatory for Infrared Astronomy [SOFIA]
dc.contributor.authorBONNE, Lars
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCSENGERI, Timea
dc.contributor.authorKLEIN, Bernd
dc.contributor.authorSIMON, Robert
hal.structure.identifierEuropean Southern Observatory [ESO]
dc.contributor.authorCOMERÓN, Fernando
dc.date.accessioned2024-11-22T03:11:12Z
dc.date.available2024-11-22T03:11:12Z
dc.date.issued2024-06-04
dc.identifier.issn0004-6361
dc.identifier.urihttps://oskar-bordeaux.fr/handle/20.500.12278/203418
dc.description.abstractEnHigh-latitude intermediate-velocity clouds (IVCs) are part of the Milky Way’s H I halo and originate from either a galactic fountain process or extragalactic gas infall. They are partly molecular and can most of the time be identified in CO. Some of these regions also exhibit high-velocity cloud gas, which is mostly atomic, and gas at local velocities (LVCs), which is partly atomic and partly molecular. We conducted a study on the IVCs Draco and Spider, both were exposed to a very weak UV field, using the spectroscopic receiver upGREAT on the Stratospheric Observatory for Infrared Astronomy (SOFIA). The 158 µm fine-structure line of ionized carbon ([C II ]) was observed, and the results are as follows: In Draco, the [C II ] line was detected at intermediate velocities (but not at local or high velocities) in four out of five positions. No [C II ] emission was found at any velocity in the two observed positions in Spider. To understand the excitation conditions of the gas in Draco, we analyzed complementary CO and H I data as well as dust column density and temperature maps from Herschel . The observed [C II ] intensities suggest the presence of shocks in Draco that heat the gas and subsequently emit in the [C II ] cooling line. These shocks are likely caused by the fast cloud’s motion toward the Galactic plane that is accompanied by collisions between H I clouds. The nondetection of [C II ] in the Spider IVC and LVC as well as in other low-density clouds at local velocities that we present in this paper (Polaris and Musca) supports the idea that highly dynamic processes are necessary for [C II ] excitation in UV-faint low-density regions.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enFirst detection of the [CII] 158 µm line in the intermediate-velocity cloud Draco
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202348349
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA109
bordeaux.volume686
bordeaux.hal.laboratoriesLaboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804*
bordeaux.institutionUniversité de Bordeaux
bordeaux.institutionCNRS
bordeaux.peerReviewedoui
hal.identifierhal-04795636
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04795636v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2024-06-04&rft.volume=686&rft.spage=A109&rft.epage=A109&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=SCHNEIDER,%20Nicola&OSSENKOPF-OKADA,%20Volker&KEILMANN,%20Eduard&R%C3%96LLIG,%20Markus&KABANOVIC,%20Slawa&rft.genre=article


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