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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/2409
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dc.contributor.authorAnantharamaiah, K.R.-
dc.contributor.authorErickson, W.C.-
dc.contributor.authorRadhakrishnan, V.-
dc.date.accessioned2007-05-25T08:23:20Z-
dc.date.available2007-05-25T08:23:20Z-
dc.date.issued1985-06-20-
dc.identifier.citationNature, 1985, Vol.315, p647-649en
dc.identifier.issn0028-0836-
dc.identifier.issn1476-4687 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/2409-
dc.descriptionRestricted Access.en
dc.description.abstractThe absorption line at 26 MHz observed by Konovalenko and Sodin1 towards Cas A was interpreted by Blake et al. 2 as the 631alpha recombination line due to carbon or heavier elements. This was confirmed subsequently by Konovalenko and Sodin3, who detected the 640alpha line at the same optical depth as the 631alpha line, within error limits. These lines represent the highest excited states yet detected in interstellar gas and could provide4 a unique diagnostic of conditions in diffuse clouds if observed over a range of frequencies. We now report new observations of these lines carried out near 26, 38, 52 and 68 MHz using the National Radio Astronomy Observatory (NRAO) 91-m telescope at Green Bank. We detected absorption lines at all these frequencies, with a striking fourfold increase in width towards low frequencies due to collisional or radiation broadening. Assuming that these are recombination lines of carbon, the observed radial velocity corresponds well with that of the H I, OH, NH3 and H2CO absorption features that originate in the Perseus arm in the same direction5−8.en
dc.format.extent193437 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherNature Publishing Groupen
dc.relation.urihttp://dx.doi.org/10.1038/315647a0en
dc.rights1985 Nature Publishing Groupen
dc.titleObservation of highly excited radio recombination lines towards Cassiopeia Aen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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