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Article: Radially inflowing molecular gas in NGC 1275 deposited by an x-ray cooling flow in the perseus cluster

TitleRadially inflowing molecular gas in NGC 1275 deposited by an x-ray cooling flow in the perseus cluster
Authors
KeywordsCooling Flows
Galaxies: Active
Galaxies: Individual (Perseus A, 3C 84)
Galaxies: Ism
Ism: Molecules
Radio Lines: Ism
Issue Date2008
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2008, v. 672 n. 1, p. 252-265 How to Cite?
AbstractWe have imaged in CO(2-1) the molecular gas in NGC 1275 (Perseus A), the cD galaxy at the center of the Perseus Cluster, at a spatial resolution of ∼1 kpc over a central region of radius ∼10 kpc. Per A is known to contain ∼1.3 × 10 10 M ⊙ of molecular gas, which has been proposed to be captured from mergers with or ram pressure stripping of gas-rich galaxies, or accreted from a X-ray cooling flow. The molecular gas detected in our image has a total mass of ∼4 × 10 9 M ⊙, and for the first time can be seen to be concentrated in three radial filaments with lengths ranging from at least 1.1 to 2.4 kpc, all lying in the east-west directions spanning the center of the galaxy to radii of ∼8 kpc. The eastern and outer western filaments exhibit larger blueshifted velocities with decreasing radii, whereas the inner western filament spans the systemic velocity of the galaxy. The molecular gas shows no signature of orbital motion, and is therefore unlikely to have been captured from gas-rich galaxies. Instead, we are able to reproduce the observed kinematics of the two outer filaments as free fall in the gravitational potential of Per A, as would be expected if they originate from a X-ray cooling flow. Indeed, all three filaments lie between two prominent X-ray cavities carved out by radio jets from Per A, and closely resemble the spatial distribution of the coolest X-ray gas in the cluster core. The inferred mass deposition rate into the two outermost filaments alone is roughly 75 M ⊙ yr -1. This cooling flow can provide a nearly continuous supply of molecular gas to fuel the active nucleus in Per A. © 2008. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175111
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorLim, Jen_US
dc.contributor.authorAo, Yen_US
dc.contributor.authorDinhVTrungen_US
dc.date.accessioned2012-11-26T08:49:16Z-
dc.date.available2012-11-26T08:49:16Z-
dc.date.issued2008en_US
dc.identifier.citationAstrophysical Journal Letters, 2008, v. 672 n. 1, p. 252-265en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175111-
dc.description.abstractWe have imaged in CO(2-1) the molecular gas in NGC 1275 (Perseus A), the cD galaxy at the center of the Perseus Cluster, at a spatial resolution of ∼1 kpc over a central region of radius ∼10 kpc. Per A is known to contain ∼1.3 × 10 10 M ⊙ of molecular gas, which has been proposed to be captured from mergers with or ram pressure stripping of gas-rich galaxies, or accreted from a X-ray cooling flow. The molecular gas detected in our image has a total mass of ∼4 × 10 9 M ⊙, and for the first time can be seen to be concentrated in three radial filaments with lengths ranging from at least 1.1 to 2.4 kpc, all lying in the east-west directions spanning the center of the galaxy to radii of ∼8 kpc. The eastern and outer western filaments exhibit larger blueshifted velocities with decreasing radii, whereas the inner western filament spans the systemic velocity of the galaxy. The molecular gas shows no signature of orbital motion, and is therefore unlikely to have been captured from gas-rich galaxies. Instead, we are able to reproduce the observed kinematics of the two outer filaments as free fall in the gravitational potential of Per A, as would be expected if they originate from a X-ray cooling flow. Indeed, all three filaments lie between two prominent X-ray cavities carved out by radio jets from Per A, and closely resemble the spatial distribution of the coolest X-ray gas in the cluster core. The inferred mass deposition rate into the two outermost filaments alone is roughly 75 M ⊙ yr -1. This cooling flow can provide a nearly continuous supply of molecular gas to fuel the active nucleus in Per A. © 2008. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectCooling Flowsen_US
dc.subjectGalaxies: Activeen_US
dc.subjectGalaxies: Individual (Perseus A, 3C 84)en_US
dc.subjectGalaxies: Ismen_US
dc.subjectIsm: Moleculesen_US
dc.subjectRadio Lines: Ismen_US
dc.titleRadially inflowing molecular gas in NGC 1275 deposited by an x-ray cooling flow in the perseus clusteren_US
dc.typeArticleen_US
dc.identifier.emailLim, J: jjlim@hku.hken_US
dc.identifier.authorityLim, J=rp00745en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/523664en_US
dc.identifier.scopuseid_2-s2.0-40249118305en_US
dc.identifier.volume672en_US
dc.identifier.issue1en_US
dc.identifier.spage252en_US
dc.identifier.epage265en_US
dc.identifier.eissn1538-4357-
dc.identifier.isiWOS:000253454000023-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridLim, J=7403453870en_US
dc.identifier.scopusauthoridAo, Y=7003967931en_US
dc.identifier.scopusauthoridDinhVTrung=6701469660en_US

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