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dc.contributor.authorMcDonald, Michael A.
dc.contributor.authorWei, Lisa H.
dc.contributor.authorVeilleux, Sylvain
dc.date.accessioned2015-02-19T21:22:44Z
dc.date.available2015-02-19T21:22:44Z
dc.date.issued2012-08
dc.date.submitted2012-01
dc.identifier.issn2041-8205
dc.identifier.issn2041-8213
dc.identifier.urihttp://hdl.handle.net/1721.1/95429
dc.description.abstractWe present the results of interferometric observations of the cool core of A1795 at CO(1-0) using the Combined Array for Research in Millimeter-wave Astronomy. In agreement with previous work, we detect a significant amount of cold molecular gas (3.9 ± 0.4 × 10[superscript 9] M ☉) in the central ~10 kpc. We report the discovery of a substantial clump of cold molecular gas at clustercentric radius of 30 kpc (2.9 ± 0.4 × 10[superscript 9] M ☉), coincident in both position and velocity with the warm, ionized filaments. We also place an upper limit on the H2 mass at the outer edge of the star-forming filament, corresponding to a distance of 60 kpc (<0.9 × 10[superscript 9] M ☉). We measure a strong gradient in the Hα/H2 ratio as a function of radius, suggesting different ionization mechanisms in the nucleus and filaments of A1795. The total mass of cold molecular gas (~7 × 10[superscript 9] M ☉) is roughly 30% of the classical cooling estimate at the same position, assuming a cooling time of 10[superscript 9] yr. Combining the cold molecular gas mass with the UV-derived star formation rate and the warm, ionized gas mass, the spectroscopically derived X-ray cooling rate is fully accounted for and in good agreement with the cooling byproducts over timescales of ~10[superscript 9] yr. The overall agreement between the cooling rate of the hot intracluster medium and the mass of the cool gas reservoir suggests that, at least in this system, the cooling flow problem stems from a lack of observable cooling in the more diffuse regions at large radii.en_US
dc.description.sponsorshipUnited States. National Aeronautics and Space Administration (NASA contract 2834-MIT-SAO-4018)en_US
dc.description.sponsorshipChandra X-ray Center (U.S.) (contract NAS8-03060)en_US
dc.description.sponsorshipNational Science Foundation (U.S.) (NSF contract AST-0606932)
dc.description.sponsorshipNational Science Foundation (U.S.) (NSF contract AST-100958)
dc.language.isoen_US
dc.publisherInstitute of Physics/American Astronomical Societyen_US
dc.relation.isversionofhttp://dx.doi.org/10.1088/2041-8205/755/2/l24en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourceAmerican Astronomical Societyen_US
dc.titleCOLD MOLECULAR GAS ALONG THE COOLING X-RAY FILAMENT IN A1795en_US
dc.typeArticleen_US
dc.identifier.citationMcDonald, Michael, Lisa H. Wei, and Sylvain Veilleux. “COLD MOLECULAR GAS ALONG THE COOLING X-RAY FILAMENT IN A1795.” The Astrophysical Journal 755, no. 2 (July 30, 2012): L24. © 2012 American Meteorological Society.en_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.contributor.mitauthorMcDonald, Michael A.en_US
dc.relation.journalAstrophysical Journalen_US
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsMcDonald, Michael; Wei, Lisa H.; Veilleux, Sylvainen_US
mit.licensePUBLISHER_POLICYen_US


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