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dc.contributor.authorAgúndez, Marcelino-
dc.contributor.authorCernicharo, José-
dc.contributor.authorVicente, P. de-
dc.contributor.authorMarcelino, Nuria-
dc.contributor.authorRoueff, E.-
dc.contributor.authorFuente, A.-
dc.contributor.authorGerin, M.-
dc.contributor.authorGuélin, M.-
dc.contributor.authorAlbo, C.-
dc.contributor.authorBarcia, A.-
dc.contributor.authorBarbas, L.-
dc.contributor.authorBolaño, R.-
dc.contributor.authorColomer, F.-
dc.contributor.authorDiez, M. C.-
dc.contributor.authorGallego, J. D.-
dc.contributor.authorGómez-González, J.-
dc.contributor.authorLópez-Fernández, I.-
dc.contributor.authorLópez-Fernández, J. A.-
dc.contributor.authorLópez-Pérez, J. A.-
dc.contributor.authorMalo, I.-
dc.contributor.authorSerna, J. M.-
dc.contributor.authorTercero, F.-
dc.date.accessioned2019-05-31T09:38:38Z-
dc.date.available2019-05-31T09:38:38Z-
dc.date.issued2015-07-15-
dc.identifierdoi: 10.1051/0004-6361/201526650-
dc.identifiere-issn: 1432-0746-
dc.identifierissn: 0004-6361-
dc.identifier.citationAstronomy and Astrophysics 579: L10 (2015)-
dc.identifier.urihttp://hdl.handle.net/10261/183013-
dc.description.abstractCyanogen (NCCN) is the simplest member of the series of dicyanopolyynes. It has been hypothesized that this family of molecules can be important constituents of interstellar and circumstellar media, although the lack of a permanent electric dipole moment prevents its detection through radioastronomical techniques. Here we present the first solid evidence of the presence of cyanogen in interstellar clouds by detection of its protonated form toward the cold dark clouds TMC-1 and L483. Protonated cyanogen (NCCNH+) has been identified through the J = 5−4 and J = 10−9 rotational transitions using the 40 m radiotelescope of Yebes and the IRAM 30 m telescope. We derive beam-averaged column densities for NCCNH+ of (8.6 ± 4.4) × 1010 cm-2 in TMC-1 and (3.9 ± 1.8) × 1010 cm-2 in L483, which translate into fairly low fractional abundances relative to H2, in the range (1–10) × 10-12. The chemistry of protonated molecules in dark clouds is discussed, and it is found that, in general terms, the abundance ratio between the protonated and non-protonated forms of a molecule increases with increasing proton affinity. Our chemical model predicts an abundance ratio NCCNH+/NCCN of ~10-4, which implies that the abundance of cyanogen in dark clouds could be as high as (1–10) × 10-8 relative to H2, i.e., comparable to that of other abundant nitriles such as HCN, HNC, and HC3N.-
dc.description.sponsorshipM.A. and J.C. acknowledge funding support from the European Research Council (ERC Grant 610256: NANOCOSMOS) and from Spanish MINECO through grants CSD2009-00038, AYA2009-07304, and AYA2012-32032. Authors from Yebes Observatory acknowledge funding by MINECO through grant FIS2012-32096. E.R. and M.G. acknowledge funding support from the CNRS program “Physique et Chimie du Milieu Interstellaire” (PCMI).-
dc.publisherEDP Sciences-
dc.relationinfo:eu-repo/grantAgreement/EC/FP7/610256-
dc.rightsclosedAccess-
dc.subjectLine: identification-
dc.subjectRadio lines: ISM-
dc.subjectISM: molecules-
dc.subjectISM: clouds-
dc.subjectAstrochemistry-
dc.titleProbing non-polar interstellar molecules through their protonated form: Detection of protonated cyanogen (NCCNH+)-
dc.typeartículo-
dc.identifier.doi10.1051/0004-6361/201526650-
dc.relation.publisherversionhttps://doi.org/10.1051/0004-6361/201526650-
dc.date.updated2019-05-31T09:38:38Z-
dc.description.versionPeer Reviewed-
dc.language.rfc3066eng-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderMinisterio de Ciencia e Innovación (España)-
dc.contributor.funderEuropean Research Council-
dc.contributor.funderCentre National de la Recherche Scientifique (France)-
dc.relation.csic-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004837es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004794es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781es_ES
dc.identifier.pmid26543239-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501es_ES
item.openairetypeartículo-
item.cerifentitytypePublications-
item.grantfulltextnone-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.fulltextNo Fulltext-
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