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Revised spectroscopic parameters of SH$^+$ from ALMA and IRAM 30 m observations

dc.contributor.authorMÜLLER, Holger S. P.
dc.contributor.authorGOICOECHEA, Javier
hal.structure.identifierDepartamento de Astrofísica Molecular e Infrarroja [DAMIR]
dc.contributor.authorCERNICHARO, José
dc.contributor.authorAGÚNDEZ, M.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorPETY, Jérôme
dc.contributor.authorCUADRADO, Sara
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorGERIN, Maryvonne
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorDUMAS, Gaelle
hal.structure.identifierAMOR 2014
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorCHAPILLON, E.
dc.date.accessioned2021-07-07T16:16:07Z
dc.date.available2021-07-07T16:16:07Z
dc.date.created2014-09-05
dc.date.issued2014
dc.identifier.issn0004-6361
dc.identifier.urihttps://oskar-bordeaux.fr/handle/20.500.12278/96085
dc.description.abstractEnHydrides represent the first steps of interstellar chemistry. Sulfanylium (SH$^+$), in particular, is a key tracer of energetic processes. We used ALMA and the IRAM 30 m telescope to search for the lowest frequency rotational lines of SH$^+$ toward the Orion Bar, the prototypical photo-dissociation region illuminated by a strong UV radiation field. On the basis of previous $Herschel$/HIFI observations of SH$^+$, we expected to detect emission of the two SH$^+$ hyperfine structure (HFS) components of the $N_J = 1_0 - 0_1$ fine structure (FS) component near 346 GHz. While we did not observe any lines at the frequencies predicted from laboratory data, we detected two emission lines, each $\sim$15 MHz above the SH$^+$ predictions and with relative intensities and HFS splitting expected for SH$^+$. The rest frequencies of the two newly detected lines are more compatible with the remainder of the SH$^+$ laboratory data than the single line measured in the laboratory near 346 GHz and previously attributed to SH$^+$. Therefore, we assign these new features to the two SH$^+$ HFS components of the $N_J = 1_0 - 0_1$ FS component and re-determine its spectroscopic parameters, which will be useful for future observations of SH$^+$, in particular if its lowest frequency FS components are studied. Our observations demonstrate the suitability of these lines for SH$^+$ searches at frequencies easily accessible from the ground.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enRevised spectroscopic parameters of SH$^+$ from ALMA and IRAM 30 m observations
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201424756
dc.subject.halPhysique [physics]/Physique [physics]/Agrégats Moléculaires et Atomiques [physics.atm-clus]
dc.identifier.arxiv1409.1807
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.L5
bordeaux.volume569
bordeaux.hal.laboratoriesLaboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804*
bordeaux.institutionCNRS
bordeaux.institutionUniversité de Bordeaux
bordeaux.peerReviewedoui
hal.identifierhal-01062001
hal.version1
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01062001v1
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=2014&rft.volume=569&rft.spage=id.L5&rft.epage=id.L5&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=M%C3%9CLLER,%20Holger%20S.%20P.&GOICOECHEA,%20Javier&CERNICHARO,%20Jos%C3%A9&AG%C3%9ANDEZ,%20M.&PETY,%20J%C3%A9r%C3%B4me&rft.genre=article


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