J/A+A/658/A82ivo://CDS.VizieR/J/A+A/658/A82doi:10.26093/cds/vizier.36580082CDSRynkun P.Banerjee S.Gaigalas G.Tanaka M.Radziute L.Kato D.2022-05-18T14:31:58Z2022-02-03T08:23:10ZCDS support team

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

cds-question@unistra.fratomic-physicsWe present extensive energy level and transition data for the Ce IV spectrum. By providing accurate atomic data, we evaluate the impact of atomic data on the opacity in the neutron star merger ejecta. We performed energy spectra and transition data calculations using the GRASP2018 package, which is based on the multiconfiguration Dirac-Hartree-Fock and relativistic configuration interaction methods, and the HULLAC code, which is based on a parametric potential method. We present energy spectra calculated for the 225 levels for the Ce^3+^ ion. Energy levels are compared with recommended values from the NIST Atomic Spectra Database and other available works. The root-mean-square (rms) deviations obtained for the GRASP2018 energy levels of the 5p^6^nl configurations from the NIST data are 1270cm^-1^. The rms deviations for the HULLAC results from the NIST data are 5780cm^-1^. Furthermore, electric dipole (E1) transition data, line strengths, weighted oscillator strengths, and transition rates are computed between the above levels. The computed transition rates are compared with other theoretical computations. We also evaluate the accuracy of the wave functions and transition parameters by analyzing the dependencies of the line strength S on the gauge parameter G. The gauge dependency method also allows us to determine the transitions for which the ratio between the Babushkin and Coulomb gauges shows real agreement between forms and the transitions for which the agreement between both gauges is random. Using the GRASP2018 and HULLAC data, the opacities in the neutron star merger ejecta are also calculated. We find that the opacity of CeIV is higher than that presented by previous works, which is because of the higher completeness of our atomic data. Although the differences in the energy levels and transition probabilities cause different features in the opacity spectrum, the Planck mean opacities of both data sets agree within 20%.2022A&A...658A..82Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/658/A82CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/658/A82https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/658/A82http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/658/A82https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/658/A82https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/658/A82http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/658/A82GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/658/A82/table6Transition data of E1 transitions for the CeIVrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNuNumber of upper level as in Table A.1.meta.idintJuJ of upper levelmeta.notecharpuParity of upper levelphys.atmol.paritycharustateLabel of upper levelphys.energy;phys.atmol.levelcharNlNumber of lower level as in Table A.1.meta.idintJlJ of lower levelmeta.notecharplParity of lower levelphys.atmol.paritycharlstateLabel of lower levelphys.energy;phys.atmol.levelchardeltaETransition energycm**-1phys.energy;phys.atmol.transitionintlambdaWavelength of transition (Angstroem)0.1nmem.wl;phys.atmol.transitiondoubleARadiative transition probability in the Babushkin gauges**-1phys.atmol.transProbdoublegfWeighted oscillator strength in the Babushkin gaugephys.atmol.oscStrengthdoubleSBLine strength in the Babushkin gaugespect.line.intensitydoubleSCLine strength in the Coulomb gaugespect.line.intensitydoubledTParameter defined in (Ekman et al., 2014A&A...564A..24E), which shows the relative difference between the Babushkin and Coulomb gauges of the computed transition ratesphys.atmolfloatG(S=0)The minimum of the parabola, which shows the accuracy of the wave functionsphys.atmoldoubleAccAccuracy classes match the NIST ASD (Kramida et al., 2020, NIST Atomic Spectra Database (ver. 5.8)) terminology (1)meta.codechar