J/A+A/530/A18ivo://CDS.VizieR/J/A+A/530/A18doi:10.26093/cds/vizier.35300018CDSFang X.Storey P.J.Liu X.-W.2017-07-12T07:00:02Z2011-04-29T12:33:34ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fratomic-physicsIn nebular astrophysics, there has been a long-standing dichotomy in plasma diagnostics between abundance determinations using the traditional method based on collisionally excited lines (CELs), on the one, hand and (optical) recombination lines/continuum, on the other. A number of mechanisms have been proposed to explain the dichotomy. Deep spectroscopy and recombination line analysis of emission line nebulae (planetary nebulae and HII regions) in the past decade have pointed to the existence of another previously unknown component of cold, H-deficient material as the culprit. Better constraints are needed on the physical conditions (electron temperature and density), chemical composition, mass, and spatial distribution of the postulated H-deficient inclusions in order to unravel their astrophysical origins. This requires knowledge of the relevant atomic parameters, most importantly the effective recombination coefficients of abundant heavy element ions such as CII, OII, NII, and NeII, appropriate for the physical conditions prevailing in those cold inclusions (e.g. Te<=1000K ).2011A&A...530A..18Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/530/A18CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/387/1135 : NII effective recombination coefficients (Kisielius+, 2002)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/530/A18https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/530/A18http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/530/A18https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/530/A18https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/530/A18http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/530/A18GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/530/A18/recombCase B effective recombination coefficients for electron densities between 10^2^ and 10^5^cm^-3^recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogNeElectron density (values 2, 3, 4, 5 in log)log(cm**-3)phys.densityintnullableTrGeneral transition term (multiplet)phys.atmol.term;phys.atmol.transitioncharlambdaTransition wavelength {lambda}(0.1nm)em.wl;phys.atmol.transitiondoublen_lambda[*] experimentally known energies (1)meta.notecharERC1Effective recombination coefficient {alpha}_eff_({lambda}) for Te=125K (2)1e-15cm**3.s**-1phys.recombination.coeffdoubleERC2Effective recombination coefficient {alpha}_eff_({lambda}) for Te=500K (2)1e-15cm**3.s**-1phys.recombination.coeffdoubleERC3Effective recombination coefficient {alpha}_eff_({lambda}) for Te=1000K (2)1e-15cm**3.s**-1phys.recombination.coeffdoubleERC4Effective recombination coefficient {alpha}_eff_({lambda}) for Te=5000K (2)1e-15cm**3.s**-1phys.recombination.coeffdoubleERC5Effective recombination coefficient {alpha}_eff_({lambda}) for Te=10000K (2)1e-15cm**3.s**-1phys.recombination.coeffdoubleERC6Effective recombination coefficient {alpha}_eff_({lambda}) for Te=15000K (2)1e-15cm**3.s**-1phys.recombination.coeffdoubleERC7Effective recombination coefficient {alpha}_eff_({lambda}) for Te=20000K (2)1e-15cm**3.s**-1phys.recombination.coeffdoubleTransDetailed transitionphys.atmol.transProb;phys.atmol.transitioncharJ/A+A/530/A18/fitBCombined table from original tablesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMultMultipletphys.atmol.levelcharlambdaWavelength of transition {lambda}(0.1nm)em.wl;phys.atmol.transitionfloataa coefficient (1)physdoublebb coefficient (1)stat.fit.paramdoublecc coefficient (1)stat.fit.paramdoubledd coefficient (1)stat.fit.paramdoubleee coefficient (1)stat.fit.paramdoubleff coefficient (1)stat.fit.paramdoublegg coefficient (1)stat.fit.paramdoublehh coefficient (1)stat.fit.paramdoubledelAverage deviation of the fit (delta)%stat.stdevfloatDelMaximum deviation of the fit {Delta}%stat.stdevfloatlogNeElectron density (values 2, 3, 4, 5 in log)log(cm**-3)phys.densityintnullableTransTransitionmeta.id;phys.atmol.transitioncharJ/A+A/530/A18/fitACombined table from original tablesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMultMultipletphys.atmol.levelcharlambdaWavelength of transition {lambda}(0.1nm)em.wl;phys.atmol.transitionfloataa coefficient (1)physdoublebb coefficient (1)stat.fit.paramdoublecc coefficient (1)stat.fit.paramdoubledd coefficient (1)stat.fit.paramdoubleee coefficient (1)stat.fit.paramdoubleff coefficient (1)stat.fit.paramdoublegg coefficient (1)stat.fit.paramdoublehh coefficient (1)stat.fit.paramdoubledelAverage deviation of the fit (delta)%stat.stdevfloatDelMaximum deviation of the fit {Delta}%stat.stdevfloatlogNeElectron density (values 2, 3, 4, 5 in log)log(cm**-3)phys.densityintnullableTransTransitionmeta.id;phys.atmol.transitioncharJ/A+A/530/A18/table15*Comparison of our direct recombination coefficients to states of N^+^ with those of Kisielius & Storey (2002, Cat. J/A+A/387/1135) and of Nahar (1995ApJS..101..423N)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStateState (1)physcharDRCN3? Nahar (1995ApJS..101..423N) direct recombination coefficient for Te=1000Kcm**3.s**-1phys.recombination.coeffdoublenullableDRCK3? Kisielius & Storey (J/A+A/387/1135) direct recombination coefficient for Te=1000Kcm**3.s**-1phys.recombination.coeffdoublenullableDRCP3Present work direct recombination coefficient for Te=1000Kcm**3.s**-1phys.recombination.coeffdoubleDRCN4? Nahar (1995ApJS..101..423N) direct recombination coefficient for Te=10000Kcm**3.s**-1phys.recombination.coeffdoublenullableDRCK4? Kisielius & Storey (J/A+A/387/1135) direct recombination coefficient for Te=10000Kcm**3.s**-1phys.recombination.coeffdoublenullableDRCP4Present work direct recombination coefficient for Te=10000Kcm**3.s**-1phys.recombination.coeffdouble