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dc.contributor.authorTanarro, Isabeles_ES
dc.contributor.authorAlemán, B.es_ES
dc.contributor.authorPardo Carrión, Juan Ramónes_ES
dc.contributor.authorSantoro, Gonzaloes_ES
dc.contributor.authorLauwaet, Koenes_ES
dc.contributor.authorMoreno, E.es_ES
dc.contributor.authorAgúndez, Marcelinoes_ES
dc.contributor.authorGoicoechea, Javier R.es_ES
dc.contributor.authorSobrado, Jesús Manueles_ES
dc.contributor.authorMartínez-Orellana, Lidiaes_ES
dc.contributor.authorDoménech, José Luises_ES
dc.contributor.authorHerrero, Víctor J.es_ES
dc.contributor.authorPeláez, Ramón J.es_ES
dc.contributor.authorCastellanos, M.es_ES
dc.contributor.authorMartín-Gago, José A.es_ES
dc.contributor.authorCernicharo, Josées_ES
dc.date.accessioned2018-02-12T11:33:12Z-
dc.date.available2018-02-12T11:33:12Z-
dc.date.issued2017-12-22-
dc.identifier.citationAstronomy & Astrophysics 609: A15 (2018)es_ES
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10261/160485-
dc.descriptionI. Tanarro et al. -- 16 pags., 18 figs., app.-
dc.description.abstractWe present a proof of concept on the coupling of radio astronomical receivers and spectrometers with chemical reactors and the performances of the resulting setup for spectroscopy and chemical simulations in laboratory astrophysics. Several experiments including cold plasma generation and UV photochemistry were performed in a 40 cm long gas cell placed in the beam path of the Aries 40 m radio telescope receivers operating in the 41–49 GHz frequency range interfaced with fast Fourier transform spectrometers providing 2 GHz bandwidth and 38 kHz resolution. The impedance matching of the cell windows has been studied using di erent materials. The choice of the material and its thickness was critical to obtain a sensitivity identical to that of standard radio astronomical observations. Spectroscopic signals arising from very low partial pressures of CH3OH, CH3CH2OH, HCOOH, OCS, CS, SO2 (<103 mbar) were detected in a few seconds. Fast data acquisition was achieved allowing for kinetic measurements in fragmentation experiments using electron impact or UV irradiation. Time evolution of chemical reactions involving OCS, O2 and CS2 was also observed demonstrating that reactive species, such as CS, can be maintained with high abundance in the gas phase during these experimentses_ES
dc.description.sponsorshipThe research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC-SyG-2013 Grant Agreement No. 610256 NANOCOSMOS and from spanish MINECO CSD2009-00038 (ASTROMOL) under the Consolider-Ingenio Program. We also thank spanish MINECO for funding under grants AYA2012-32032, AYA2016-75066-C2-1-P, FIS2013-48087-C2-1-P, FIS2016-77726-C3-1-P, FIS2016-77578-R, MAT2014- 54231-C4-1-P.es_ES
dc.language.isoenges_ES
dc.publisherEDP Scienceses_ES
dc.relationinfo:eu-repo/grantAgreement/EC/FP7/610256es_ES
dc.relationMINECO/ICTI2013-2016/AYA2016-75066-C2-1-Pes_ES
dc.relationMINECO/ICTI2013-2016/FIS2013-48087-C2-1-Pes_ES
dc.relationMINECO/ICTI2013-2016/FIS2016-77726-C3-1-Pes_ES
dc.relationMINECO/ICTI2013-2016/FIS2016-77578-Res_ES
dc.relationMINECO/ICTI2013-2016/MAT2014-54231-C4-1-Pes_ES
dc.relation.isversionofPublisher's versiones_ES
dc.rightsopenAccesses_ES
dc.subjectMethods: laboratory: moleculares_ES
dc.subjectInstrumentation: spectrographses_ES
dc.subjectAstrochemistryes_ES
dc.subjectMolecular dataes_ES
dc.titleUsing radio astronomical receivers for molecular spectroscopic characterization in astrochemical laboratory simulations: A proof of conceptes_ES
dc.typeartículoes_ES
dc.identifier.doi10.1051/0004-6361/201730969-
dc.description.peerreviewedPeer reviewedes_ES
dc.relation.publisherversionhttp://doi.org/10.1051/0004-6361/201730969-
dc.identifier.e-issn1432-0746-
dc.contributor.funderEuropean Research Counciles_ES
dc.contributor.funderEuropean Commissiones_ES
dc.contributor.funderMinisterio de Economía y Competitividad (España)es_ES
dc.relation.csices_ES
oprm.item.hasRevisionno ko 0 false*
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
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