{"refrec":{"BRefID":303472,"RR":"<b>Keenan, F.P.; Aller, L.H.; Espey, B.R.; Exter, K.M.; Hyung, S.; Keenan, M.T.C.; Pollacco, D.L.; Ryans, R.S.I.</b> (2002). Emission lines of [K V] in the optical spectra of gaseous nebulae. <i>Proc. Natl. Acad. Sci. U.S.A. 99(7)</i>: 4152-4155. <a href=\"https://dx.doi.org/10.1073/pnas.062032299\" target=\"_blank\">https://dx.doi.org/10.1073/pnas.062032299</a>","BEntID":295766,"PublicFlag":1,"CheckedFlag":0,"wosflag":1,"vabbflag":1,"RefStringPartII":". <i>Proc. Natl. Acad. Sci. U.S.A. 99(7)</i>: 4152-4155. <a href=\"https://dx.doi.org/10.1073/pnas.062032299\" target=\"_blank\">https://dx.doi.org/10.1073/pnas.062032299</a>","DocTypID":8,"DocType":"Journal article","MarineFlag":0,"FreshFlag":0,"BrackishFlag":0,"TerrestrialFlag":0,"Authorstring":"Keenan, F.P.; Aller, L.H.; Espey, B.R.; Exter, K.M.; Hyung, S.; Keenan, M.T.C.; Pollacco, D.L.; Ryans, R.S.I.","OrigTitleTranslFlag":0,"Authorstringtrunc":"Keenan, F.P. <i>et al.</i>","Englishabstract":"Recent R-matrix calculations of electron impact excitation rates in K <span class=\"sc\">v</span> are used to derive the nebular emission line ratio <em>R</em> = <em>I</em>(4122.6 Å)/<em>I</em>(4163.3 Å) as a function of electron density (<em>N</em><sub>e</sub>). This ratio is found to be very sensitive to changes in <em>N</em><sub>e</sub> over the density range 10<sup>3</sup> to 10<sup>6</sup> cm<sup>−3</sup>, but does not vary significantly with electron temperature, and hence in principle should provide an excellent optical <em>N</em><sub>e</sub> diagnostic for the high-excitation zones of nebulae. The observed value of <em>R</em> for the planetary nebula NGC 7027, measured from a spectrum obtained with the Hamilton Echelle spectrograph on the 3-m Shane Telescope, implies a density in excellent agreement with that derived from [Ne <span class=\"sc\">iv</span>], formed in the same region of the nebula as [K <span class=\"sc\">v</span>]. This observation provides observational support for the accuracy of the theoretical [K <span class=\"sc\">v</span>] line ratios, and hence the atomic data on which they are based. However, the analysis of a high-resolution spectrum of the symbiotic star RR Telescopii, obtained with the University College London Echelle Spectrograph on the 3.9-m Anglo–Australian Telescope, reveals that the [K <span class=\"sc\">v</span>] 4122.6 Å line in this object is badly blended with Fe <span class=\"sc\">ii</span> 4122.6 Å. Hence, the [K <span class=\"sc\">v</span>] diagnostic may not be used for astrophysical sources that show a strong Fe <span class=\"sc\">ii</span> emission line spectrum.","AbstractOtherLang":null,"BibLvlCode":"AS","StandardTitle":"Emission lines of [K V] in the optical spectra of gaseous nebulae","OrigTitleLangCode":"en","OrigTitleLangCodeExtended":"eng","OrigTitleLangID":15,"DateLastModified":{"date":"2026-04-20 01:32:29.421087","timezone_type":1,"timezone":"+02:00"},"UserAccessRight":null,"UserAccID":null,"AuthorKeywords":null,"OtherDescriptors":null,"Notes":null,"AnaPub":2002,"MonPub":null,"DateUpdate":"2018-11-30","DateCreate":"2018-11-30","SecASFANote":null,"ConfID":null,"PeerRev":1,"VlizCoreFlag":1,"WoScode":"WOS:000174856000007","VABBcode":null,"OpenAcc":1,"DOI":"10.1073/pnas.062032299"},"refs":null,"anarec":{"AnaID":303472,"PubliDate":2002,"Pagination":"4152-4155","XtraPublOfAnaID":null,"ISBN":null,"Volume":"99","Issue":"7","BRefMon":null,"BRefMonRR":null,"BRefXtra":null,"BRefXtraRR":null,"SerBRefID":43690,"SerRR":"Proceedings of the National Academy of Sciences of the United States of America. 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