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

hal.structure.identifierPhysikalisches Institut, Universität zu Köln
dc.contributor.authorMÜLLER, Holger S. P.
hal.structure.identifierMadrid
dc.contributor.authorGOICOECHEA, Javier R.
hal.structure.identifierMadrid
dc.contributor.authorCERNICHARO, José
hal.structure.identifierMadrid
dc.contributor.authorAGÚNDEZ, Marcelino
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
hal.structure.identifierInstrumentation et télédétection
hal.structure.identifierDynamique des milieux interstellaires et plasmas stellaires
dc.contributor.authorPETY, Jérôme
hal.structure.identifierMadrid
dc.contributor.authorCUADRADO, Sara
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
hal.structure.identifierInstrumentation et télédétection
hal.structure.identifierDynamique des milieux interstellaires et plasmas stellaires
dc.contributor.authorGERIN, Maryvonne
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorDUMAS, Gaëlle
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCHAPILLON, Edwige
dc.date.created2014-09-05
dc.date.issued2014
dc.identifier.issn0004-6361
dc.description.abstractEnHydrides represent the first steps of interstellar chemistry. Sulfanylium (SH<SUP> </SUP>), 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<SUP> </SUP> 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<SUP> </SUP>, we expected to detect emission of the two SH<SUP> </SUP> hyperfine structure (HFS) components of the N<SUB>J</SUB> = 1<SUB>0</SUB>-0<SUB>1</SUB> 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 ~15 MHz above the SH<SUP> </SUP> predictions and with relative intensities and HFS splitting expected for SH<SUP> </SUP>. The rest frequencies of the two newly detected lines are more compatible with the remainder of the SH<SUP> </SUP> laboratory data than the single line measured in the laboratory near 346 GHz and previously attributed to SH<SUP> </SUP>. Therefore, we assign these new features to the two SH<SUP> </SUP> HFS components of the N<SUB>J</SUB> = 1<SUB>0</SUB>-0<SUB>1</SUB> FS component and re-determine its spectroscopic parameters, which will be useful for future observations of SH<SUP> </SUP>, in particular if its lowest frequency FS components are studied. Our observations demonstrate the suitability of these lines for SH<SUP> </SUP> 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]/Astrophysique [astro-ph]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.L5
bordeaux.volume569
bordeaux.peerReviewedoui
hal.identifierhal-03730747
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-03730747v1
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