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Article: A molecular hydrogen nebula in the central cD galaxy of the perseus cluster

TitleA molecular hydrogen nebula in the central cD galaxy of the perseus cluster
Authors
Keywordsgalaxies: active
galaxies: clusters: intracluster medium
galaxies: individual (NGC 1275)
galaxies: ISM
infrared: ISM
ISM: molecules
Issue Date2012
PublisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
Astrophysical Journal, 2012, v. 744 n. 2 How to Cite?
AbstractWe report narrowband imaging of the 1-0 S(1) ro-vibrational transition of molecular hydrogen (H 2) from NGC1275, the central cD galaxy of the Perseus Cluster. We find that the H 2 gas has a spatial morphology identical to the optical emission-line nebula associated with this galaxy, a total luminosity in H 21-0S(1) only an order of magnitude less than in Hα, and if the line-emitting gas is thermalized a mass (at 2000K) that is over two orders of magnitude smaller than that of the optical emission-line nebula (at 10,000K). The ratio in H 21-0S(1) to Hα+[N II] line intensities spans a characteristic range of 0.02-0.08 throughout the nebula; the brighter inner nebula exhibits patches with (nearly) constant line ratios unrelated to individual filaments. Recent models proposed to explain the peculiar nebular spectrum from the optical to infrared invoke thermalized along with non-thermalized injection of energy from ionizing particles. The energy density of highly relativistic electrons inferred to cause inverse-Compton scattering of hard X-ray emission from the core of the Perseus Cluster decreases steeply beyond a central radius of 20kpc, yet we do not find any changes in the average or range spanned by the H 21-0S(1) to Hα+[N II] line ratio between the inner (≲20kpc) and outer (20-50kpc) nebulae. On the other hand, saturated conduction from the surrounding X-ray gas produces, in the absence of magnetic fields, a heat flux that is approximately constant throughout the nebula: the change in the line ratio with position would then reflect the ability of the X-ray gas to penetrate presumably magnetically threaded filaments at different locations. © 2012. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/145583
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
Funding AgencyGrant Number
National Science Council of Taiwan
Funding Information:

The work presented here is based on observations obtained with WIRCam, a joint project of the Canada-France-Hawaii Telescope (CFHT), Taiwan, Korea, Canada, and France. The CFHT is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. We acknowledge help from Ho I-Ting (then a graduate student at National Taiwan University and ASIAA) in the preliminary stages and Juan Wei-Chun (a summer student at the ASIAA) in the intermediate stages of the data analyses. We are immensely grateful to William Forman for providing us with the X-ray surface brightness radial profile of the Perseus Cluster. J. Lim performed a part of this work when he was a staff member at the ASIAA, and acknowledges support by a grant from the National Science Council of Taiwan during this time. Last but not least, we sincerely thank the anonymous referee for pointing out errors in our understanding of the literature, a careful reading, and constructive suggestions to improve the manuscript.

References

 

DC FieldValueLanguage
dc.contributor.authorLim, Jen_HK
dc.contributor.authorOhyama, Yen_HK
dc.contributor.authorChiHung, Yen_HK
dc.contributor.authorDinhVTrungen_HK
dc.contributor.authorShiangYu, Wen_HK
dc.date.accessioned2012-02-28T01:55:42Z-
dc.date.available2012-02-28T01:55:42Z-
dc.date.issued2012en_HK
dc.identifier.citationAstrophysical Journal, 2012, v. 744 n. 2en_HK
dc.identifier.issn0004-637Xen_HK
dc.identifier.urihttp://hdl.handle.net/10722/145583-
dc.description.abstractWe report narrowband imaging of the 1-0 S(1) ro-vibrational transition of molecular hydrogen (H 2) from NGC1275, the central cD galaxy of the Perseus Cluster. We find that the H 2 gas has a spatial morphology identical to the optical emission-line nebula associated with this galaxy, a total luminosity in H 21-0S(1) only an order of magnitude less than in Hα, and if the line-emitting gas is thermalized a mass (at 2000K) that is over two orders of magnitude smaller than that of the optical emission-line nebula (at 10,000K). The ratio in H 21-0S(1) to Hα+[N II] line intensities spans a characteristic range of 0.02-0.08 throughout the nebula; the brighter inner nebula exhibits patches with (nearly) constant line ratios unrelated to individual filaments. Recent models proposed to explain the peculiar nebular spectrum from the optical to infrared invoke thermalized along with non-thermalized injection of energy from ionizing particles. The energy density of highly relativistic electrons inferred to cause inverse-Compton scattering of hard X-ray emission from the core of the Perseus Cluster decreases steeply beyond a central radius of 20kpc, yet we do not find any changes in the average or range spanned by the H 21-0S(1) to Hα+[N II] line ratio between the inner (≲20kpc) and outer (20-50kpc) nebulae. On the other hand, saturated conduction from the surrounding X-ray gas produces, in the absence of magnetic fields, a heat flux that is approximately constant throughout the nebula: the change in the line ratio with position would then reflect the ability of the X-ray gas to penetrate presumably magnetically threaded filaments at different locations. © 2012. The American Astronomical Society. All rights reserved.en_HK
dc.languageengen_US
dc.publisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/en_HK
dc.relation.ispartofAstrophysical Journalen_HK
dc.rightsThe Astrophysical Journal. Copyright © Institute of Physics Publishing, Inc.-
dc.subjectgalaxies: activeen_HK
dc.subjectgalaxies: clusters: intracluster mediumen_HK
dc.subjectgalaxies: individual (NGC 1275)en_HK
dc.subjectgalaxies: ISMen_HK
dc.subjectinfrared: ISMen_HK
dc.subjectISM: moleculesen_HK
dc.titleA molecular hydrogen nebula in the central cD galaxy of the perseus clusteren_HK
dc.typeArticleen_HK
dc.identifier.emailLim, J: jjlim@hku.hken_HK
dc.identifier.authorityLim, J=rp00745en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1088/0004-637X/744/2/112en_HK
dc.identifier.scopuseid_2-s2.0-84555179092en_HK
dc.identifier.hkuros198795en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-84555179092&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume744en_HK
dc.identifier.issue2en_HK
dc.identifier.eissn1538-4357-
dc.identifier.isiWOS:000298666400032-
dc.publisher.placeUnited Statesen_HK
dc.identifier.scopusauthoridLim, J=7403453870en_HK
dc.identifier.scopusauthoridOhyama, Y=14825669800en_HK
dc.identifier.scopusauthoridChiHung, Y=54794762900en_HK
dc.identifier.scopusauthoridDinhVTrung=15520778600en_HK
dc.identifier.scopusauthoridShiangYu, W=54795789700en_HK
dc.identifier.citeulike10321493-

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