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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/1632
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dc.contributor.authorMohan, Niruj R.-
dc.contributor.authorGoss, W.M.-
dc.contributor.authorAnantharamaiah, K.R.-
dc.date.accessioned2006-12-29T10:56:48Z-
dc.date.available2006-12-29T10:56:48Z-
dc.date.issued2005-03-
dc.identifier.citationAstronomy and Astrophysics, 2005, Vol.432, p1-14en
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/2289/1633-
dc.description.abstractWe have imaged the H92α (8.3 GHz), H75α (15 GHz), and H166α (1.4 GHz) Radio Recombination Lines (RRLs) from NGC 253 at resolutions of 4.5 pc (0.4'') , 2.5 pc (0.2'') and 53 pc (4.5'') respectively. The H92α line arises from individual compact sources, most of which possess radio continuum counterparts. The line widths range from ~200 km s-1 for the sources near the radio nucleus to 70-100 km s-1 for the extranuclear ones. These lines are emitted by gas at a density ~104 cm-3. The remainder of the cm-wave RRLs arise in lower density gas (~500 cm-3) with a higher area filling factor and with ten times higher mass. A third component of higher density gas (〉104 cm-3) is required to explain the mm-wave RRLs. Appendix A is only available in electronic form at http://www.edpsciences.orgen
dc.format.extent761946 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherEDP Sciencesen
dc.relation.urihttp://arxiv.org/abs/astro-ph/0410676en
dc.relation.urihttp://dx.doi.org/10.1051/0004-6361:20041488en
dc.rights(2005) by the European Southern Observatory (ESO).en
dc.subjectgalaxies: individual: NGC 253en
dc.subjectgalaxies: ISMen
dc.subjectgalaxies: starbursten
dc.subjectradio lines: galaxiesen
dc.subjectradio lines: ISMen
dc.titleMulti-density model of the ionised gas in NGC 253 using radio recombination linesen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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