Shock-enhanced C+ emission and the detection of H2O from the Stephan’s Quintet group-wide shock using Herschel

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dc.contributor.authorAppleton, P N
dc.contributor.authorGuillard, P
dc.contributor.authorBoulanger, F
dc.contributor.authorCluver, M E
dc.contributor.authorOgle, P
dc.contributor.authorFalgarone, E
dc.contributor.authorPineau des Forêts, G
dc.contributor.authorO\'Sullivan, E
dc.contributor.authorDuc, P-A
dc.contributor.authorGallagher, S
dc.contributor.authorGao, Y
dc.contributor.authorJarrett, T
dc.contributor.authorKonstantopoulos, I
dc.contributor.authorLisenfeld, U
dc.contributor.authorLord, S
dc.contributor.authorLu, N
dc.contributor.authorPeterson, B W
dc.contributor.authorStruck, C
dc.contributor.authorSturm, E
dc.contributor.authorTuffs, R
dc.contributor.authorValchanov, I
dc.contributor.authorvan der Werf, P
dc.contributor.authorXu, K C
dc.date.accessioned2021-10-08T07:20:39Z
dc.date.available2021-10-08T07:20:39Z
dc.date.issued2013
dc.description.abstractWWe present the first Herschelspectroscopic detections of the [O i] 63 μm and [Cii] 158 μm fine-structure transitions, and a single para-H2O line from the 35 × 15 kpc2 shocked intergalactic filament in Stephan’s Quintet. The filament is believed to have been formed when a high-speed intruder to the group collided with a clumpy intergroup gas. Observations with the PACS spectrometer provide evidence for broad (>1000 km s−1) luminous [Cii] line profiles, as well as fainter [O i] 63 μm emission. SPIRE FTS observations reveal water emission from the p-H2O (111–000) transition at several positions in the filament, but no other molecular lines. The H2O line is narrow and may be associated with denser intermediate-velocity gas experiencing the strongest shock-heating. The [Cii]/PAHtot and [C ii]/FIR ratios are too large to be explained by normal photo-electric heating in photodissociation regions. H ii region excitation or X-ray/cosmic-ray heating can also be ruled out. The observations lead to the conclusion that a large fraction the molecular gas is diffuse and warm. We propose that the [Cii], [O i], and warm H2 line emission is powered by a turbulent cascade in which kinetic energy from the galaxy collision with the intergalactic medium is dissipated to small scales and low velocities, via shocks and turbulent eddies. Low-velocity magnetic shocks can help explain both the [Cii]/[O i] ratio, and the relatively high [C ii]/H2 ratios observed. The discovery that [Cii] emission can be enhanced, in large-scale turbulent regions in collisional environments, has implications for the interpretation of [C ii] emission in high-z galaxies.
dc.identifier.apacitationAppleton, P. N., Guillard, P., Boulanger, F., Cluver, M. E., Ogle, P., Falgarone, E., ... Xu, K. C. (2013). Shock-enhanced C+ emission and the detection of H2O from the Stephan’s Quintet group-wide shock using Herschel. <i>The Astrophysical Journal</i>, 777(1), 66 - 177. http://hdl.handle.net/11427/34974en_ZA
dc.identifier.chicagocitationAppleton, P N, P Guillard, F Boulanger, M E Cluver, P Ogle, E Falgarone, G Pineau des Forêts, et al "Shock-enhanced C+ emission and the detection of H2O from the Stephan’s Quintet group-wide shock using Herschel." <i>The Astrophysical Journal</i> 777, 1. (2013): 66 - 177. http://hdl.handle.net/11427/34974en_ZA
dc.identifier.citationAppleton, P.N., Guillard, P., Boulanger, F., Cluver, M.E., Ogle, P., Falgarone, E., Pineau des Forêts, G. & et al. 2013. Shock-enhanced C+ emission and the detection of H2O from the Stephan’s Quintet group-wide shock using Herschel. <i>The Astrophysical Journal.</i> 777(1):66 - 177. http://hdl.handle.net/11427/34974en_ZA
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.ris TY - Journal Article AU - Appleton, P N AU - Guillard, P AU - Boulanger, F AU - Cluver, M E AU - Ogle, P AU - Falgarone, E AU - Pineau des Forêts, G AU - O\'Sullivan, E AU - Duc, P-A AU - Gallagher, S AU - Gao, Y AU - Jarrett, T AU - Konstantopoulos, I AU - Lisenfeld, U AU - Lord, S AU - Lu, N AU - Peterson, B W AU - Struck, C AU - Sturm, E AU - Tuffs, R AU - Valchanov, I AU - van der Werf, P AU - Xu, K C AB - WWe present the first Herschelspectroscopic detections of the [O i] 63 μm and [Cii] 158 μm fine-structure transitions, and a single para-H2O line from the 35 × 15 kpc2 shocked intergalactic filament in Stephan’s Quintet. The filament is believed to have been formed when a high-speed intruder to the group collided with a clumpy intergroup gas. Observations with the PACS spectrometer provide evidence for broad (>1000 km s−1) luminous [Cii] line profiles, as well as fainter [O i] 63 μm emission. SPIRE FTS observations reveal water emission from the p-H2O (111–000) transition at several positions in the filament, but no other molecular lines. The H2O line is narrow and may be associated with denser intermediate-velocity gas experiencing the strongest shock-heating. The [Cii]/PAHtot and [C ii]/FIR ratios are too large to be explained by normal photo-electric heating in photodissociation regions. H ii region excitation or X-ray/cosmic-ray heating can also be ruled out. The observations lead to the conclusion that a large fraction the molecular gas is diffuse and warm. We propose that the [Cii], [O i], and warm H2 line emission is powered by a turbulent cascade in which kinetic energy from the galaxy collision with the intergalactic medium is dissipated to small scales and low velocities, via shocks and turbulent eddies. Low-velocity magnetic shocks can help explain both the [Cii]/[O i] ratio, and the relatively high [C ii]/H2 ratios observed. The discovery that [Cii] emission can be enhanced, in large-scale turbulent regions in collisional environments, has implications for the interpretation of [C ii] emission in high-z galaxies. DA - 2013 DB - OpenUCT DP - University of Cape Town IS - 1 J1 - The Astrophysical Journal LK - https://open.uct.ac.za PY - 2013 SM - 0004-637X SM - 1538-4357 T1 - Shock-enhanced C+ emission and the detection of H2O from the Stephan’s Quintet group-wide shock using Herschel TI - Shock-enhanced C+ emission and the detection of H2O from the Stephan’s Quintet group-wide shock using Herschel UR - http://hdl.handle.net/11427/34974 ER - en_ZA
dc.identifier.urihttp://hdl.handle.net/11427/34974
dc.identifier.vancouvercitationAppleton PN, Guillard P, Boulanger F, Cluver ME, Ogle P, Falgarone E, et al. Shock-enhanced C+ emission and the detection of H2O from the Stephan’s Quintet group-wide shock using Herschel. The Astrophysical Journal. 2013;777(1):66 - 177. http://hdl.handle.net/11427/34974.en_ZA
dc.language.isoeng
dc.publisher.departmentDepartment of Astronomy
dc.publisher.facultyFaculty of Science
dc.sourceThe Astrophysical Journal
dc.source.journalissue1
dc.source.journalvolume777
dc.source.pagination66 - 177
dc.source.urihttps://dx.doi.org/10.1088/0004-637X/777/1/66
dc.subject.othergalaxies: groups: individual (Stephan's Quintet)
dc.subject.otherinfrared: galaxies
dc.titleShock-enhanced C+ emission and the detection of H2O from the Stephan’s Quintet group-wide shock using Herschel
dc.typeJournal Article
uct.type.publicationResearch
uct.type.resourceJournal Article
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