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dc.contributorVirginia Techen
dc.contributor.authorSpoon, H. W. W.en
dc.contributor.authorFarrah, D.en
dc.contributor.authorLebouteiller, V.en
dc.contributor.authorGonzalez-Alfonso, E.en
dc.contributor.authorBernard-Salas, J.en
dc.contributor.authorUrrutia, T.en
dc.contributor.authorRigopoulou, D.en
dc.contributor.authorWestmoquette, M. S.en
dc.contributor.authorSmith, H. A.en
dc.contributor.authorAfonso, J.en
dc.contributor.authorPearson, C.en
dc.contributor.authorCormier, D.en
dc.contributor.authorEfstathiou, A.en
dc.contributor.authorBorys, C.en
dc.contributor.authorVerma, A.en
dc.contributor.authorEtxaluze, M.en
dc.contributor.authorClements, D. L.en
dc.date.accessioned2014-02-25T13:57:05Zen
dc.date.available2014-02-25T13:57:05Zen
dc.date.issued2013-10en
dc.identifier.citationH. W. W. Spoon et al. 2013. "Diagnostics of AGN-driven molecular outflows in ULIRGs from Herschel-PACS observations of OH at 119 μm," ApJ 775 127 doi:10.1088/0004-637X/775/2/127en
dc.identifier.issn0004-637Xen
dc.identifier.urihttp://hdl.handle.net/10919/25555en
dc.description.abstractWe report on our observations of the 79 and 119 mu m doublet transitions of OH for 24 local (z < 0.262) ULIRGs observed with Herschel-PACS as part of the Herschel ULIRG Survey (HERUS). Some OH 119 mu m profiles display a clear P-Cygni shape and therefore imply outflowing OH gas, while other profiles are predominantly in absorption or are completely in emission. We find that the relative strength of the OH emission component decreases as the silicate absorption increases. This result locates the OH outflows inside the obscured nuclei. The maximum outflow velocities for our sources range from less than 100 to similar to 2000 km s(-1), with 15/24 (10/24) sources showing OH absorption at velocities exceeding 700 km s(-1) (1000 km s(-1)). Three sources show maximum OH outflow velocities exceeding that of Mrk231. Since outflow velocities above 500-700 km s(-1) are thought to require an active galactic nucleus (AGN) to drive them, about two-thirds of our ULIRG sample may host AGN-driven molecular outflows. This finding is supported by the correlation we find between the maximum OH outflow velocity and the IR-derived bolometric AGN luminosity. No such correlation is found with the IR-derived star formation rate. The highest outflow velocities are found among sources that are still deeply embedded. We speculate that the molecular outflows in these sources may be in an early phase of disrupting the nuclear dust veil before these sources evolve into less-obscured AGNs. Four of our sources show high-velocity wings in their [C II] fine-structure line profiles, implying neutral gas outflow masses of at least (2-4.5) x 10(8) M-circle dot.en
dc.description.sponsorshipCEA/Marie Curie Eurotalents fellowshipen
dc.description.sponsorshipSpanish Ministerio de Economia y Competitividad AYA2010-21697-C05-0, FIS2012-39162-C06-01en
dc.description.sponsorshipScience and Technology Foundation (FCT, Portugal) PTDC/CTE-AST/105287/2008, PEst-OE/FIS/UI2751/2011, PTDC/FIS-AST/2194/2012en
dc.description.sponsorshipASTROMADRID S2009ESP-1496en
dc.description.sponsorshipSpanish MINECO AYA2009-07304en
dc.description.sponsorshipASTROMOL CSD2009-00038en
dc.description.sponsorshipNASA through JPL/Caltechen
dc.language.isoen_USen
dc.publisherIOP Publishing Ltd.en
dc.rightsIn Copyrighten
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en
dc.subjectinfrared: galaxiesen
dc.subjectism: jets and outflowsen
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: ismen
dc.subjectquasars: absorption linesen
dc.subjectactive galactic nucleien
dc.subjectultraluminous infrared galaxiesen
dc.subjectstar-formationen
dc.subjectblack-holesen
dc.subjectquasar feedbacken
dc.subjectemission-lineen
dc.subjectbright galaxiesen
dc.subjectscaleen
dc.subjectoutflowsen
dc.subjectlocal ulirgsen
dc.subjectspectroscopyen
dc.titleDiagnostics of AGN-driven molecular outflows in ULIRGs from Herschel-PACS observations of OH at 119 μmen
dc.typeArticle - Refereeden
dc.contributor.departmentPhysicsen
dc.identifier.urlhttp://iopscience.iop.org/0004-637X/775/2/127/pdf/0004-637X_775_2_127.pdfen
dc.date.accessed2014-02-05en
dc.title.serialAstrophysical Journalen
dc.identifier.doihttps://doi.org/10.1088/0004-637x/775/2/127en


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