X-ray spectra of 4 cool starsJ/A+A/416/281ivo://CDS.VizieR/J/A+A/416/281doi:10.26093/cds/vizier.34160281CDSSanz-forcada J.Favata F.Micela G.2004-05-02T20:49:16Z2004-05-02T20:47:01ZCDS support team
CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France
cds-question@unistra.frlate-type-starsx-ray-sourcesspectroscopyThese tables include the observed fluxes of the lines identified in the X-ray spectra of four cool stars (Procyon, epsilon Eri, lambda And and V851 Cen). The spectra were taken using different configurations (Chandra/LETG, Chandra/HETG and XMM/RGS). The tables list the observed fluxes at Earth, and a comparison with the fluxes predicted for a given thermal coronal structure (the Emission Measure Distribution, EMD), the emissivities provided by the Astrophysical Plasma Emission Model (APED) and column density of absorbing material in the interstellar medium towards the star. A list of the most important (at least a 5% of the flux predicted for the line) blends that have been considered for each line is included.2004A&A...416..281Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/416/281CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/416/281https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/416/281http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/416/281https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/416/281https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/416/281http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/416/281GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapX-rayOpticaldefaultJ/A+A/416/281/table4Chandra/LETG line fluxes of Procyon (6/7-Nov-1999)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIonphys.atmol.ionizationcharlambdaWavelength of the line as identified in the model.0.1nmem.wldoublelogTmax? Maximum temperature of formation of the line (unweighted by the Emission Measure Distribution)log(K)spect.line.intensityfloatnullableFobsObserved line fluxmW.m**-2phot.fluxdoubleS/NSignal-to-noise ratiostat.snrfloatRatio? log(observed flux/predicted flux) (1)stat.fit.omcfloatnullableBlendsBlends to the main line amounting more than a 5% of the total flux (2)meta.notechar
J/A+A/416/281/table5Chandra/LETG line fluxes of epsilon Eri (7-Nov-1999)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIonphys.atmol.ionizationcharlambdaWavelength of the line as identified in the model.0.1nmem.wldoublelogTmax? Maximum temperature of formation of the line (unweighted by the Emission Measure Distribution)log(K)spect.line.intensityfloatnullableFobsObserved line fluxmW.m**-2phot.fluxdoubleS/NSignal-to-noise ratiostat.snrfloatRatio? log(observed flux/predicted flux) (1)stat.fit.omcfloatnullableBlendsBlends to the main line amounting more than a 5% of the total flux (2)meta.notechar
J/A+A/416/281/table6Chandra/HETG line fluxes of lambda And (21-Mar-2001)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIonphys.atmol.ionizationcharlambdaWavelength of the line as identified in the model.0.1nmem.wldoublelogTmax? Maximum temperature of formation of the line (unweighted by the Emission Measure Distribution)log(K)spect.line.intensityfloatnullableFobsObserved line fluxmW.m**-2phot.fluxdoubleS/NSignal-to-noise ratiostat.snrfloatRatio? log(observed flux/predicted flux) (1)stat.fit.omcfloatnullableBlendsBlends to the main line amounting more than a 5% of the total flux (2)meta.notechar
J/A+A/416/281/table7XMM/RGS line fluxes of V851 Cen (7-Mar-2003)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIonphys.atmol.ionizationcharlambdaWavelength of the line as identified in the model.0.1nmem.wldoublelogTmax? Maximum temperature of formation of the line (unweighted by the Emission Measure Distribution)log(K)spect.line.intensityfloatnullableFobsObserved line fluxmW.m**-2phot.fluxdoubleS/NSignal-to-noise ratiostat.snrfloatRatio? log(observed flux/predicted flux) (1)stat.fit.omcfloatnullableBlendsBlends to the main line amounting more than a 5% of the total flux (2)meta.notechar