J/A+A/624/A108ivo://CDS.VizieR/J/A+A/624/A108doi:10.26093/cds/vizier.36240108CDSLaas J.C.Caselli P.2019-05-06T15:31:16Z2019-04-23T08:39:38ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmolecular-cloudsastronomical-modelsThe elemental depletion of interstellar sulfur from the gas phase has been a recurring challenge for astrochemical models. Observations show that sulfur remains relatively non-depleted with respect to its cosmic value throughout the diffuse and translucent stages of an interstellar molecular cloud, but its atomic and molecular gas-phase constituents cannot account for this cosmic value toward lines of sight containing higher-density environments. We have attempted to address this issue by modeling the evolution of an interstellar cloud from its pristine state as a diffuse atomic cloud to a molecular environment of much higher density, using a gas-grain astrochemical code and an enhanced sulfur reaction network. A common gas-grain astrochemical reaction network has been systematically updated and greatly extended based on previous literature and previous sulfur models, with a focus on the grain chemistry and processes. A simple astrochemical model was used to benchmark the resulting network updates, and the results of the model were compared to typical astronomical observations sourced from the literature. Our new gas-grain astrochemical model is able to reproduce the elemental depletion of sulfur, whereby sulfur can be depleted from the gas-phase by two orders of magnitude, and that this process may occur under dark cloud conditions if the cloud has a chemical age of at least 106 years. The resulting mix of sulfur-bearing species on the grain ranges across all the most common chemical elements (H/C/N/O), not dissimilar to the molecules observed in cometary environments. Notably, this mixture is not dominated simply by H2S, unlike all other current astrochemical models. Despite our relatively simple physical model, most of the known gas-phase S-bearing molecular abundances are accurately reproduced under dense conditions, however they are not expected to be the primary molecular sinks of sulfur. Our model predicts that most of the "missing" sulfur is in the form of organo-sulfur species that are trapped on grains.2019A&A...624A.108Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/624/A108CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/624/A108https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/624/A108http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/624/A108https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/624/A108https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/624/A108http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/624/A108GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/624/A108/tableb4New sulfur reactionsrtypeReaction type (1)meta.noteintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintReactionFull chemical reactionmeta.notecharalpha{alpha} reaction coefficientphys.atmoldoublebeta{beta} reaction coefficientphys.atmolfloatgamma{gamma} reaction coefficientphys.atmolfloatRemarksRemark/reference about tabulated values (2)meta.notecharJ/A+A/624/A108/tablea1Thermochemistry for all grain speciesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGrain surface molecular speciesmeta.idcharEbindGrain surface binding energyKphys.energyintdelH_f? Heat of formationkcal.mol**-1phys.mol.formationHeatfloatnullableRemarksRemark/reference about tabulated values (1)meta.notechar