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Article: Multiple radial cool molecular filaments in NGC 1275

TitleMultiple radial cool molecular filaments in NGC 1275
Authors
KeywordsCooling Flows
Galaxies: Active
Galaxies: Individual (Ngc 1275, Perseus A)
Galaxies: Ism
Ism: Molecules
Radio Lines: Ism
Issue Date2009
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2009, v. 698 n. 2, p. 1191-1206 How to Cite?
AbstractWe have extended our previous observation of NGC 1275 (Perseus A (Per A), the central giant elliptical galaxy in the Perseus Cluster) covering a central radius of 10 kpc to the entire main body of cool molecular gas spanning 14 kpc east and west of the center. We find no new features beyond the region previously mapped, and show that all six spatially resolved features on both the eastern and western sides (three on each side) comprise radially aligned filaments. Such radial filaments can be most naturally explained by a model in which gas deposited "upstream" in localized regions experiencing a X-ray cooling flow subsequently free falls along the gravitational potential of Per A, as we previously showed can explain the observed kinematics of the two longest filaments. All the detected filaments coincide with locally bright Hα features, and have a ratio of CO(2-1) to Hα luminosity of 10 -3; we show that these filaments have lower star formation efficiencies than the nearly constant value found for molecular gas in nearby normal spiral galaxies. On the other hand, some at least equally luminous Hα features, including a previously identified giant HII region, show no detectable cool molecular gas with a corresponding ratio at least a factor of 5 lower; in the giant HII region, essentially all the pre-existing molecular gas may have been converted to stars. We demonstrate that all the cool molecular filaments are gravitationally bound, and without any means of support beyond thermal pressure should collapse on timescales ≲106 yr. By comparison, as we showed previously, the two longest filaments have much longer dynamical ages of 107 yr. Tidal shear may help delay their collapse, but more likely turbulent velocities of at least a few tens of km s-1 or magnetic fields with strengths of at least several 10 μG are required to support these filaments. © 2009. The American Astronomical Society.
Persistent Identifierhttp://hdl.handle.net/10722/175161
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorHo, ITen_US
dc.contributor.authorLim, Jen_US
dc.contributor.authorDinhTrung, Ven_US
dc.date.accessioned2012-11-26T08:49:29Z-
dc.date.available2012-11-26T08:49:29Z-
dc.date.issued2009en_US
dc.identifier.citationAstrophysical Journal Letters, 2009, v. 698 n. 2, p. 1191-1206en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175161-
dc.description.abstractWe have extended our previous observation of NGC 1275 (Perseus A (Per A), the central giant elliptical galaxy in the Perseus Cluster) covering a central radius of 10 kpc to the entire main body of cool molecular gas spanning 14 kpc east and west of the center. We find no new features beyond the region previously mapped, and show that all six spatially resolved features on both the eastern and western sides (three on each side) comprise radially aligned filaments. Such radial filaments can be most naturally explained by a model in which gas deposited "upstream" in localized regions experiencing a X-ray cooling flow subsequently free falls along the gravitational potential of Per A, as we previously showed can explain the observed kinematics of the two longest filaments. All the detected filaments coincide with locally bright Hα features, and have a ratio of CO(2-1) to Hα luminosity of 10 -3; we show that these filaments have lower star formation efficiencies than the nearly constant value found for molecular gas in nearby normal spiral galaxies. On the other hand, some at least equally luminous Hα features, including a previously identified giant HII region, show no detectable cool molecular gas with a corresponding ratio at least a factor of 5 lower; in the giant HII region, essentially all the pre-existing molecular gas may have been converted to stars. We demonstrate that all the cool molecular filaments are gravitationally bound, and without any means of support beyond thermal pressure should collapse on timescales ≲106 yr. By comparison, as we showed previously, the two longest filaments have much longer dynamical ages of 107 yr. Tidal shear may help delay their collapse, but more likely turbulent velocities of at least a few tens of km s-1 or magnetic fields with strengths of at least several 10 μG are required to support these filaments. © 2009. The American Astronomical Society.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 (Ngc 1275, Perseus A)en_US
dc.subjectGalaxies: Ismen_US
dc.subjectIsm: Moleculesen_US
dc.subjectRadio Lines: Ismen_US
dc.titleMultiple radial cool molecular filaments in NGC 1275en_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.doi10.1088/0004-637X/698/2/1191en_US
dc.identifier.scopuseid_2-s2.0-66649132846en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-66649132846&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume698en_US
dc.identifier.issue2en_US
dc.identifier.spage1191en_US
dc.identifier.epage1206en_US
dc.identifier.eissn1538-4357-
dc.identifier.isiWOS:000266782400019-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridHo, IT=26642525300en_US
dc.identifier.scopusauthoridLim, J=7403453870en_US
dc.identifier.scopusauthoridDinhTrung, V=26642297200en_US

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