{"refrec":{"BRefID":303464,"RR":"<b>Keenan, F.P.; Aller, L.H.; Exter, K.M.; Hyung, S.; Pollacco, D.L.</b> (2003). Emission lines of [Cl II] in the optical spectra of gaseous nebulae. <i>Astrophys. J. 584(1)</i>: 385-389. <a href=\"https://dx.doi.org/10.1086/345542\" target=\"_blank\">https://dx.doi.org/10.1086/345542</a>","BEntID":295758,"PublicFlag":1,"CheckedFlag":0,"wosflag":1,"vabbflag":1,"RefStringPartII":". <i>Astrophys. J. 584(1)</i>: 385-389. <a href=\"https://dx.doi.org/10.1086/345542\" target=\"_blank\">https://dx.doi.org/10.1086/345542</a>","DocTypID":8,"DocType":"Journal article","MarineFlag":0,"FreshFlag":0,"BrackishFlag":0,"TerrestrialFlag":0,"Authorstring":"Keenan, F.P.; Aller, L.H.; Exter, K.M.; Hyung, S.; Pollacco, D.L.","OrigTitleTranslFlag":0,"Authorstringtrunc":"Keenan, F.P. <i>et al.</i>","Englishabstract":"Recent <b><i>R</i></b>-matrix calculations of electron impact excitation rates among the 3<i>s</i><sup>2</sup>3<i>p</i><sup>4</sup> levels of Cl <font size=\"-1\">II</font> are used to derive the nebular emission-line intensity ratios <i>R</i><sub>1</sub> = <i>I</i>(6161.8 Å)/<i>I</i>(8578.7 Å) and <i>R</i><sub>2</sub> = <i>I</i>(6161.8 Å)/<i>I</i>(9123.6 Å) as a function of electron temperature (<i>T</i><sub><i>e</i></sub>) and density (<i>N</i><sub><i>e</i></sub>). The ratios are found to be very sensitive to changes in <i>T</i><sub><i>e</i></sub> but not <i>N</i><sub><i>e</i></sub> for densities lower than 10<sup>5</sup> cm<sup>-3</sup>. Hence, they should, in principle, provide excellent optical <i>T</i><sub><i>e</i></sub> diagnostics for planetary nebulae. The observed values of <i>R</i><sub>1</sub> and <i>R</i><sub>2</sub> for the planetary nebulae NGC 6741 and IC 5117, measured from spectra obtained with the Hamilton echelle spectrograph on the 3 m Shane Telescope, imply temperatures in excellent agreement with those derived from other diagnostic lines formed in the same region of the nebula as [Cl <font size=\"-1\">II</font>]. This provides some observational support for the accuracy of the [Cl <font size=\"-1\">II</font>] line ratio calculations and hence the atomic data on which they are based. The [Cl <font size=\"-1\">II</font>] 8578.7 and 9123.6 Å lines are identified for the first time (to our knowledge) in 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. However, the 6161.8 Å feature is unfortunately too weak to be identified in the RR Telescopii observations, consistent with its predicted line strength.","AbstractOtherLang":null,"BibLvlCode":"AS","StandardTitle":"Emission lines of [Cl II] in the optical spectra of gaseous nebulae","OrigTitleLangCode":"en","OrigTitleLangCodeExtended":"eng","OrigTitleLangID":15,"DateLastModified":{"date":"2026-06-10 01:32:19.149114","timezone_type":1,"timezone":"+02:00"},"UserAccessRight":null,"UserAccID":null,"AuthorKeywords":null,"OtherDescriptors":null,"Notes":null,"AnaPub":2003,"MonPub":null,"DateUpdate":"2018-11-30","DateCreate":"2018-11-30","SecASFANote":null,"ConfID":null,"PeerRev":1,"VlizCoreFlag":1,"WoScode":"WOS:000180706000027","VABBcode":null,"OpenAcc":1,"DOI":"10.1086/345542"},"refs":null,"anarec":{"AnaID":303464,"PubliDate":2003,"Pagination":"385-389","XtraPublOfAnaID":null,"ISBN":null,"Volume":"584","Issue":"1","BRefMon":null,"BRefMonRR":null,"BRefXtra":null,"BRefXtraRR":null,"SerBRefID":239012,"SerRR":"The Astrophysical Journal. 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