J/ApJ/442/523ivo://CDS.VizieR/J/ApJ/442/523doi:10.26093/cds/vizier.14420523CDSEskridge P.B.Fabbiano G.Kim D.-W.1997-12-09T19:52:20Z1997-12-09T20:52:14ZCDS support team

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

cds-question@unistra.frgalaxiesvisible-astronomyinterstellar-mediumWe have conducted bivariate and multivariate statistical analysis of data measuring the integrated luminosity, shape, and potential depth of the Einstein sample of early-type galaxies (presented by Fabbiano et al. =1992ApJS...80..531F). We find significant correlations between the X-ray properties and the axial ratios (a/b) of our sample, such that the roundest systems tend to have the highest L_X and L_X/L_B. The most radio-loud objects are also the roundest. We confirm the assertion of Bender et al. (1989A&A...217...35B) that galaxies with high L_X are boxy (have negative a_4). Both a/b and a_4 are correlated with L_B, but not with IRAS 12 um and 100 um luminosities. There are strong correlations between L_X, Mg_2 and sigma_v in the sense that those systems with the deepest potential wells have the highest L_X and Mg_2. Thus the depth of the potential well appears to govern both the ability to retain an ISM at the present epoch and to retain the enriched ejecta of early star formation bursts. Both L_X/L_B and L_6 (the 6 cm radio luminosity) show threshold effects with sigma_v, exhibiting sharp increases at log(sigma_v) ~ 2.2. Finally, there is clearly an interrelationship between the various stellar and structural parameters: The scatter in the bivariate relationships between the shape parameters (a/b and a_4) and the depth parameter (sigma_v) is a function of abundance in the sense that, for a given a_4 or a/b, the systems with the highest sigma_v also have the highest Mg_2. Furthermore, for a constant sigma_v, disky galaxies tend to have higher Mg_2 than boxy ones. Alternatively, for a given abundance, boxy ellipticals tend to be more massive than disky ellipticals. One possibility is that early-type galaxies of a given mass, originating from mergers (boxy ellipticals), have lower abundances than "primordial" (disky) early-type galaxies. Another is that disky inner isophotes are due not to primordial dissipational collapse, but to either the self-gravitating inner disks of captured spirals or the dissipational collapse of new disk structures from the premerger ISM. The high measured nuclear Mg_2 values would thus be due to enrichment from secondary bursts of star formation triggered by the merging event.1995ApJ...442..523Ehttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/442/523CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/442/523https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/442/523http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/442/523https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/442/523https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/442/523http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/442/523GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/ApJ/442/523/tablea1aPartial Spearman Rank Analysis: Trends with Log(a/b), E+S0 SampleSizeNumber of objects in the samplemeta.numberintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPairTest pair, if blank, record is a continuationmeta.codecharHeldQuantities to be held constant in the testmeta.notecharSpearmanPartial Spearman rank statisticstat.fit.goodnessdoublel_ProbProbability limiting charactermeta.code.errorcharProbProbability that the test pair shows a correlation for this set of parametersstat.fit.goodnessfloatJ/ApJ/442/523/tablea1bPartial Spearman Rank Analysis: Trends with Log(a/b), Separate E and S0 SamplesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPairTest pair, if blank, record is a continuationmeta.codecharHeldQuantities to be held constant in the testmeta.notecharSampleSample designation, Es or S0smeta.id;meta.maincharSizeNumber of objects in the samplemeta.numberintSpearmanPartial Spearman rank statisticstat.fit.goodnessdoublel_ProbProbability limiting charactermeta.code.errorcharProbProbability that the test pair shows a correlation for this set of parametersstat.fit.goodnessfloatJ/ApJ/442/523/tablea2Partial Spearman Rank Analysis: Trends with Mg_2recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPairTest pair, if blank, record is a continuationmeta.codecharHeldQuantities to be held constant in the testmeta.notecharSizeNumber of objects in the samplemeta.numberintSpearmanPartial Spearman rank statisticstat.fit.goodnessdoublel_ProbProbability limiting charactermeta.code.errorcharProbProbability that the test pair shows a correlation for this set of parametersstat.fit.goodnessfloatJ/ApJ/442/523/tablea3Partial Spearman Rank Analysis: Trends with sigma_vrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPairTest pair, if blank, record is a continuationmeta.codecharHeldQuantities to be held constant in the testmeta.notecharSizeNumber of objects in the samplemeta.numberintSpearmanPartial Spearman rank statisticstat.fit.goodnessdoublel_ProbProbability limiting charactermeta.code.errorcharProbProbability that the test pair shows a correlation for this set of parametersstat.fit.goodnessfloatJ/ApJ/442/523/tablea4Partial Spearman Rank Analysis: Trends with a_4recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPairTest pair, if blank, record is a continuationmeta.codecharHeldQuantities to be held constant in the testmeta.notecharSizeNumber of objects in the samplemeta.numberintSpearmanPartial Spearman rank statisticstat.fit.goodnessdoublel_ProbProbability limiting charactermeta.code.errorcharProbProbability that the test pair shows a correlation for this set of parametersstat.fit.goodnessfloat