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dc.contributor.authorBulak, M.en
dc.contributor.authorPaardekooper, D. M.en
dc.contributor.authorFedoseev, G.en
dc.contributor.authorLinnartz, H.en
dc.date.accessioned2022-05-12T08:19:17Z-
dc.date.available2022-05-12T08:19:17Z-
dc.date.issued2021-
dc.identifier.citationPhotolysis of Acetonitrile in a Water-rich Ice as a Source of Complex Organic Molecules: CH3CN and H2O:CH3CN Ices / M. Bulak, D. M. Paardekooper, G. Fedoseev et al. — DOI 10.1073/pnas.2100338118 // Astronomy and Astrophysics. — 2021. — Vol. 647. — A82.en
dc.identifier.issn0004-6361-
dc.identifier.otherAll Open Access, Bronze, Green3
dc.identifier.urihttp://elar.urfu.ru/handle/10995/111572-
dc.description.abstractContext. Many C-, O-, and H-containing complex organic molecules (COMs) have been observed in the interstellar medium (ISM) and their formation has been investigated in laboratory experiments. An increasing number of recent detections of large N-bearing COMs motivates our experimental investigation of their chemical origin. Aims. We investigate the potential role of acetonitrile (CH3CN) as a parent molecule to N-bearing COMs, motivated by its omnipresence in the ISM and structural similarity to another well-known precursor species, CH3OH. The aim of the present work is to characterize the chemical complexity that can result from vacuum UV photolysis of a pure CH3CN ice and a more realistic mixture of H2O:CH3CN. Methods. The CH3CN ice and H2O:CH3CN ice mixtures were UV irradiated at 20 K. Laser desorption post ionization time-of-flight mass spectrometry was used to detect the newly formed COMs in situ. We examined the role of water in the chemistry of interstellar ices through an analysis of two different ratios of H2O:CH3CN (1:1 and 20:1). Results. We find that CH3CN is an excellent precursor to the formation of larger nitrogen-containing COMs, including CH3CH2CN, NCCN/CNCN, and NCCH2CH2CN. During the UV photolysis of H2O:CH3CN ice, the water derivatives play a key role in the formation of molecules with functional groups of: imines, amines, amides, large nitriles, carboxylic acids, and alcohols. We discuss possible formation pathways for molecules recently detected in the ISM. © ESO 2021.en
dc.description.sponsorshipAcknowledgements. M.B. and H.L. acknowledge the European Union (EU) and Horizon 2020 funding awarded under the Marie Skłodowska-Curie action to the EUROPAH consortium (grant number 722346) as well as NOVA 5 funding. Additional funding has been realized through a NWO-VICI grant. This work has been supported by the Danish National Research Foundation through the Center of Excellence “InterCat” (Grant agreement no.: DNRF150). We thank N. F. W. Ligterink, A. G. G. M. Tielens, J. Terwischa van Scheltinga, J. Bouwman and T. Lamberts for helpful discussions.en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherEDP Sciencesen1
dc.publisherEDP Sciencesen
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceAstron. Astrophys.2
dc.sourceAstronomy and Astrophysicsen
dc.subjectASTROCHEMISTRYen
dc.subjectCIRCUMSTELLAR MATTERen
dc.subjectISM: MOLECULESen
dc.subjectMETHODS: LABORATORY: SOLID STATEen
dc.subjectMOLECULAR PROCESSESen
dc.subjectULTRAVIOLET: ISMen
dc.subjectACETONITRILEen
dc.subjectAMIDESen
dc.subjectAMINESen
dc.subjectCHEMICAL DETECTIONen
dc.subjectMASS SPECTROMETRYen
dc.subjectMIXTURESen
dc.subjectMOLECULESen
dc.subjectPHOTOLYSISen
dc.subjectULTRAVIOLET LASERSen
dc.subjectCHEMICAL COMPLEXITYen
dc.subjectCOMPLEX ORGANIC MOLECULESen
dc.subjectEXPERIMENTAL INVESTIGATIONSen
dc.subjectFORMATION PATHWAYSen
dc.subjectIN-LABORATORY EXPERIMENTSen
dc.subjectINTERSTELLAR ICEen
dc.subjectINTERSTELLAR MEDIUMSen
dc.subjectSTRUCTURAL SIMILARITYen
dc.subjectICEen
dc.titlePhotolysis of Acetonitrile in a Water-rich Ice as a Source of Complex Organic Molecules: CH3CN and H2O:CH3CN Icesen
dc.typeArticleen
dc.typeinfo:eu-repo/semantics/articleen
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.doi10.1051/0004-6361/202039695-
dc.identifier.scopus85102446354-
local.contributor.employeeBulak, M., Laboratory for Astrophysics, Leiden Observatory, Leiden University, PO Box 9513, Leiden, RA 2300, Netherlands; Paardekooper, D.M., Laboratory for Astrophysics, Leiden Observatory, Leiden University, PO Box 9513, Leiden, RA 2300, Netherlands; Fedoseev, G., Laboratory for Astrophysics, Leiden Observatory, Leiden University, PO Box 9513, Leiden, RA 2300, Netherlands, Research Laboratory for Astrochemistry, Ural Federal University, Kuibysheva St. 48, Ekaterinburg, 620026, Russian Federation; Linnartz, H., Laboratory for Astrophysics, Leiden Observatory, Leiden University, PO Box 9513, Leiden, RA 2300, Netherlandsen
local.volume647-
dc.identifier.wos000629649800001-
local.contributor.departmentLaboratory for Astrophysics, Leiden Observatory, Leiden University, PO Box 9513, Leiden, RA 2300, Netherlands; Research Laboratory for Astrochemistry, Ural Federal University, Kuibysheva St. 48, Ekaterinburg, 620026, Russian Federationen
local.identifier.pure21031875-
local.description.orderA82-
local.identifier.eid2-s2.0-85102446354-
local.fund.cordisH2020: 722346-
local.identifier.wosWOS:000629649800001-
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