J/A+A/664/A62ivo://CDS.VizieR/J/A+A/664/A62doi:10.26093/cds/vizier.36640062CDSGu L.Shah C.Mao J.Raassen A.J.J.de Plaa J.Pinto C.Akamatsu H.,Werner N.Simionescu A.Mernier F.Sawada M.Mohanty P.Amaro P.,Gu M.F.Porter F.S.Lopez-Urrutia J.R.C.Kaastra J.S.2022-12-16T22:20:29Z2022-08-09T08:47:12ZCDS support team

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

cds-question@unistra.fratomic-physicsThere has been a growing request from the X-ray astronomy community for a quantitative estimate of systematic uncertainties originating from the atomic data used in plasma codes. Though there have been several studies looking into atomic data uncertainties using theoretical calculations, in general, there is no commonly accepted solution for this task. We present a new approach for estimating uncertainties in the line emissivities for the current models of collisional plasma, mainly based upon a dedicated analysis of observed high resolution spectra of stellar coronae and galaxy clusters. We find that the systematic uncertainties of the observed lines consistently show an anticorrelation with the model line fluxes, after properly accounting for the additional uncertainties from the ion concentration calculation. The strong lines in the spectra are in general better reproduced, indicating that the atomic data and modeling of the main transitions are more accurate than those for the minor ones. This underlying anticorrelation is found to be roughly independent of source properties, line positions, ion species, and the line formation processes. We further applied our method to the simulated XRISM and Athena observations of collisional plasma sources and discuss the impact of uncertainties on the interpretation of these spectra. The typical uncertainties are 1-2% on temperature and 3-20% on abundances of O, Ne, Fe, Mg, and Ni.2022A&A...664A..62Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/664/A62CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/627/A51 : Levels and rate coefficients of the Fe-L (Gu+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/664/A62https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/664/A62http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/664/A62https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/664/A62https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/664/A62http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/664/A62GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/664/A62/tablea1Line informationrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIndexLine ID as given in Figures A1 and A2meta.idintlambdaLine wavelength0.1nmem.wldoubleZElementsrc.redshift;phys.atmol.elementintIonIsoelectronic sequence numberphys.atmol.ionStageintEXContribution of upper level population from direct excitationphys.atmolfloatCEXcontribution of upper level population from excitation followed by cascadephys.atmolfloatRRcontribution of upper level population from radiative recombinationphys.atmolfloatCRRcontribution of upper level population from radiative recombination followed by cascadephys.atmolfloatDRcontribution of upper level population from dielectronic recombinationphys.atmolfloatCDRcontribution of upper level population from dielectronic recombination followed by cascadephys.atmolfloatIcapCapella line emissivity from the best-fit models (model 1)ph.m**-2.s**-1phys.emissivityfloatUcapCapella fractional Gaussian contribution (model 2)phys.atmoldoubleIHRHR 1099 line emissivity from the best-fit models (model 1)ph.m**-2.s**-1phys.emissivityfloatUHR? HR 1099 fractional Gaussian contribution (model 2)phys.atmolfloatnullable