First Detection of Interstellar S2H
We present the first detection of gas-phase S2H in the Horsehead, a moderately UV-irradiated nebula. This confirms the presence of doubly sulfuretted species in the interstellar medium and opens a new challenge for sulfur chemistry. The observed S2H abundance is ∼5 × 10−11, only a factor of 4-6 lowe...
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| Veröffentlicht in: | Astrophysical journal. Letters 2017-12, Vol.851 (2) |
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| creator | Fuente, Asunción Goicoechea, Javier R. Pety, Jérôme Le Gal, Romane Martín-Doménech, Rafael Gratier, Pierre Guzmán, Viviana Roueff, Evelyne Loison, Jean Christophe Muñoz Caro, Guillermo M. Wakelam, Valentine Gerin, Maryvonne Riviere-Marichalar, Pablo Vidal, Thomas |
| description | We present the first detection of gas-phase S2H in the Horsehead, a moderately UV-irradiated nebula. This confirms the presence of doubly sulfuretted species in the interstellar medium and opens a new challenge for sulfur chemistry. The observed S2H abundance is ∼5 × 10−11, only a factor of 4-6 lower than that of the widespread H2S molecule. H2S and S2H are efficiently formed on the UV-irradiated icy grain mantles. We performed ice irradiation experiments to determine the H2S and S2H photodesorption yields. The obtained values are ∼1.2 × 10−3 and |
| doi_str_mv | 10.3847/2041-8213/aaa01b |
| format | Article |
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This confirms the presence of doubly sulfuretted species in the interstellar medium and opens a new challenge for sulfur chemistry. The observed S2H abundance is ∼5 × 10−11, only a factor of 4-6 lower than that of the widespread H2S molecule. H2S and S2H are efficiently formed on the UV-irradiated icy grain mantles. We performed ice irradiation experiments to determine the H2S and S2H photodesorption yields. The obtained values are ∼1.2 × 10−3 and <1 × 10−5 molecules per incident photon for H2S and S2H, respectively. Our upper limit to the S2H photodesorption yield suggests that photodesorption is not a competitive mechanism to release the S2H molecules to the gas phase. Other desorption mechanisms such as chemical desorption, cosmic-ray desorption, and grain shattering can increase the gaseous S2H abundance to some extent. Alternatively, S2H can be formed via gas-phase reactions involving gaseous H2S and the abundant ions S+ and SH+. The detection of S2H in this nebula therefore could be the result of the coexistence of an active grain-surface chemistry and gaseous photochemistry.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/aaa01b</identifier><identifier>PMID: 29862006</identifier><language>eng</language><publisher>Austin: The American Astronomical Society</publisher><subject>Abundance ; astrochemistry ; Astrophysics ; Atmospheric chemistry ; Cosmic rays ; Desorption ; Galactic Astrophysics ; Hydrogen sulfide ; Interstellar chemistry ; Interstellar gas ; Interstellar matter ; Interstellar medium ; Irradiation ; ISM: abundances ; ISM: individual objects (Horsehead) ; ISM: molecules ; methods: laboratory: solid state ; Nebulae ; Organic chemistry ; Photochemistry ; photon-dominated region (PDR) ; Sciences of the Universe ; Sulfur ; Surface chemistry ; Vapor phases</subject><ispartof>Astrophysical journal. Letters, 2017-12, Vol.851 (2)</ispartof><rights>2017. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Dec 20, 2017</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><orcidid>0000-0001-8063-8685 ; 0000-0003-3061-6546 ; 0000-0003-1837-3772 ; 0000-0001-9676-2605 ; 0000-0002-2418-7952 ; 0000-0001-6317-6343 ; 0000-0002-6636-4304</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/2041-8213/aaa01b/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,776,780,881,27901,27902,38845,38867,53815,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/2041-8213/aaa01b$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://hal.science/hal-01661652$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Fuente, Asunción</creatorcontrib><creatorcontrib>Goicoechea, Javier R.</creatorcontrib><creatorcontrib>Pety, Jérôme</creatorcontrib><creatorcontrib>Le Gal, Romane</creatorcontrib><creatorcontrib>Martín-Doménech, Rafael</creatorcontrib><creatorcontrib>Gratier, Pierre</creatorcontrib><creatorcontrib>Guzmán, Viviana</creatorcontrib><creatorcontrib>Roueff, Evelyne</creatorcontrib><creatorcontrib>Loison, Jean Christophe</creatorcontrib><creatorcontrib>Muñoz Caro, Guillermo M.</creatorcontrib><creatorcontrib>Wakelam, Valentine</creatorcontrib><creatorcontrib>Gerin, Maryvonne</creatorcontrib><creatorcontrib>Riviere-Marichalar, Pablo</creatorcontrib><creatorcontrib>Vidal, Thomas</creatorcontrib><title>First Detection of Interstellar S2H</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>We present the first detection of gas-phase S2H in the Horsehead, a moderately UV-irradiated nebula. This confirms the presence of doubly sulfuretted species in the interstellar medium and opens a new challenge for sulfur chemistry. The observed S2H abundance is ∼5 × 10−11, only a factor of 4-6 lower than that of the widespread H2S molecule. H2S and S2H are efficiently formed on the UV-irradiated icy grain mantles. We performed ice irradiation experiments to determine the H2S and S2H photodesorption yields. The obtained values are ∼1.2 × 10−3 and <1 × 10−5 molecules per incident photon for H2S and S2H, respectively. Our upper limit to the S2H photodesorption yield suggests that photodesorption is not a competitive mechanism to release the S2H molecules to the gas phase. Other desorption mechanisms such as chemical desorption, cosmic-ray desorption, and grain shattering can increase the gaseous S2H abundance to some extent. Alternatively, S2H can be formed via gas-phase reactions involving gaseous H2S and the abundant ions S+ and SH+. 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Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Fuente, Asunción</au><au>Goicoechea, Javier R.</au><au>Pety, Jérôme</au><au>Le Gal, Romane</au><au>Martín-Doménech, Rafael</au><au>Gratier, Pierre</au><au>Guzmán, Viviana</au><au>Roueff, Evelyne</au><au>Loison, Jean Christophe</au><au>Muñoz Caro, Guillermo M.</au><au>Wakelam, Valentine</au><au>Gerin, Maryvonne</au><au>Riviere-Marichalar, Pablo</au><au>Vidal, Thomas</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>First Detection of Interstellar S2H</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2017-12-20</date><risdate>2017</risdate><volume>851</volume><issue>2</issue><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>We present the first detection of gas-phase S2H in the Horsehead, a moderately UV-irradiated nebula. This confirms the presence of doubly sulfuretted species in the interstellar medium and opens a new challenge for sulfur chemistry. The observed S2H abundance is ∼5 × 10−11, only a factor of 4-6 lower than that of the widespread H2S molecule. H2S and S2H are efficiently formed on the UV-irradiated icy grain mantles. We performed ice irradiation experiments to determine the H2S and S2H photodesorption yields. The obtained values are ∼1.2 × 10−3 and <1 × 10−5 molecules per incident photon for H2S and S2H, respectively. Our upper limit to the S2H photodesorption yield suggests that photodesorption is not a competitive mechanism to release the S2H molecules to the gas phase. Other desorption mechanisms such as chemical desorption, cosmic-ray desorption, and grain shattering can increase the gaseous S2H abundance to some extent. Alternatively, S2H can be formed via gas-phase reactions involving gaseous H2S and the abundant ions S+ and SH+. The detection of S2H in this nebula therefore could be the result of the coexistence of an active grain-surface chemistry and gaseous photochemistry.</abstract><cop>Austin</cop><pub>The American Astronomical Society</pub><pmid>29862006</pmid><doi>10.3847/2041-8213/aaa01b</doi><tpages>6</tpages><orcidid>https://orcid.org/0000-0001-8063-8685</orcidid><orcidid>https://orcid.org/0000-0003-3061-6546</orcidid><orcidid>https://orcid.org/0000-0003-1837-3772</orcidid><orcidid>https://orcid.org/0000-0001-9676-2605</orcidid><orcidid>https://orcid.org/0000-0002-2418-7952</orcidid><orcidid>https://orcid.org/0000-0001-6317-6343</orcidid><orcidid>https://orcid.org/0000-0002-6636-4304</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Abundance astrochemistry Astrophysics Atmospheric chemistry Cosmic rays Desorption Galactic Astrophysics Hydrogen sulfide Interstellar chemistry Interstellar gas Interstellar matter Interstellar medium Irradiation ISM: abundances ISM: individual objects (Horsehead) ISM: molecules methods: laboratory: solid state Nebulae Organic chemistry Photochemistry photon-dominated region (PDR) Sciences of the Universe Sulfur Surface chemistry Vapor phases |
| title | First Detection of Interstellar S2H |
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