J/A+A/336/667ivo://CDS.VizieR/J/A+A/336/667doi:10.26093/cds/vizier.33360667CDSStasinska G.Richer M.G.Mc Call M.L.1999-08-07T09:58:18Z1999-08-07T09:58:08ZCDS support team

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

cds-question@unistra.frplanetary-nebulaechemical-abundancesstellar-atmospheric-opacityWe have collected photometric and spectroscopic data on planetary nebulae (PNe) in 5 galaxies: the Milky Way (bulge), M31 (bulge), M 32, the LMC and the SMC. We have computed the abundances of O, Ne and N and compared them from one galaxy to another. In each Galaxy, the distribution of oxygen abundances has a large dispersion. The average O/H ratio is larger in the M31 and the Galactic bulge PNe than in those in the Magellanic Clouds. In a given galaxy, it is also larger for PNe with [OIII] luminosities greater than 100L_{sun}_, which are likely to probe more recent epochs in the galaxy history. We find that the M31 and the Galactic bulge PNe extend the very tight Ne/H-O/H correlation observed in the Galactic disk and Magellanic Clouds PNe towards higher metallicities. We note that the anticorrelation between N/O and O/H that was known to occur in the Magellanic Clouds and in the disk PNe is also marginally found in the PNe of the Galactic bulge. Furthermore, we find that high N/O ratios are higher for less luminous PNe. In M 32, all PNe have a large N/O ratio, indicating that the stellar nitrogen abundance is enhanced in this galaxy. We have also compared the PN evolution in the different galactic systems by constructing diagrams that are independent of abundances, and have found strikingly different behaviours of the various samples. In order to help in the interpretation of these data, we have constructed a grid of expanding, PN photoionization models in which the central stars evolve according to the evolutionary tracks of Bloecker (1995A&A...299..755B). These models show that the apparent spectroscopic properties of PNe are extremely dependent, not only on the central stars, but also on the masses and expansion velocities of the nebular envelopes. The main conclusion of the confrontation of the observed samples with the model grids is that the PN populations are indeed not the same in the various parent galaxies. Both stars and nebulae are different. In particular, the central stars of the Magellanic Clouds PNe are shown to evolve differently from the hydrogen burning stellar evolutionary models of Bloecker (1995). In the Galactic bulge, on the other hand, the behaviour of the observed PNe is roughly compatible with the theoretical stellar evolutionary tracks. The case of M31 is not quite clear, and additional observations are necessary. It seems that the central star mass distribution is narrower for the M31 PNe than for the Galactic bulge PNe. We show that spectroscopy of complete samples of PNe down to a factor 100 below the maximum luminosity would help to better characterize the PN central star mass distribution.1998A&A...336..667Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/336/667CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/336/667https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/336/667http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/336/667https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/336/667https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/336/667http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/336/667GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/336/667/table1Reddening corrected line intensities on the scale I(H{beta})=100 and logarithms of [OIII] luminosities in solar unitsl_3727Limit flag on 3727meta.code.errorcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRegion[abcde] Region (1)meta.notecharObjectObject numbermeta.idintPNPN namemeta.id;meta.maincharRefReference (2)meta.refchar3727Reddening corrected line intensity at 3727AA (3)spect.line.intensity;arith.ratiofloatu_3727Uncertainty flag on 3727meta.code.errorchar3869Reddening corrected line intensity at 3869AA (3)spect.line.intensity;arith.ratiofloatu_3869Uncertainty flag on 3869meta.code.errorcharl_4363Limit flag on 4363meta.code.errorchar4363Reddening corrected line intensity at 4363AA (3)spect.line.intensity;arith.ratiofloatu_4363Uncertainty flag on 4363meta.code.errorcharl_4686Limit flag on 4686meta.code.errorchar4686Reddening corrected line intensity at 4686AA (3)spect.line.intensity;arith.ratiofloatu_4686Uncertainty flag on 4686meta.code.errorcharl_5007Limit flag on 5007meta.code.errorchar5007Reddening corrected line intensity at 5007AA (3)spect.line.intensity;arith.ratiofloatu_5007Uncertainty flag on 5007meta.code.errorcharl_5755Limit flag on 5755meta.code.errorchar5755Reddening corrected line intensity at 5755AA (3)spect.line.intensity;arith.ratiofloatu_5755Uncertainty flag on 5755meta.code.errorcharl_5876Limit flag on 5876meta.code.errorchar5876Reddening corrected line intensity at 5876AA (3)spect.line.intensity;arith.ratiofloatu_5876Uncertainty flag on 5876meta.code.errorcharl_6300Limit flag on 6300meta.code.errorchar6300Reddening corrected line intensity at 6300AA (3)spect.line.intensity;arith.ratiofloatu_6300Uncertainty flag on 6300meta.code.errorchar6563Reddening corrected line intensity at 6563AA (3)spect.line.intensity;arith.ratiofloatl_6583Limit flag on 6583meta.code.errorchar6583Reddening corrected line intensity at 6583AA (3)spect.line.intensity;arith.ratiofloatu_6583Uncertainty flag on 6583meta.code.errorcharl_6717Limit flag on 6717meta.code.errorchar6717Reddening corrected line intensity at 6717AA (3)spect.line.intensity;arith.ratiofloatu_6717Uncertainty flag on 6717meta.code.errorcharl_6731Limit flag on 6731meta.code.errorchar6731Reddening corrected line intensity at 6731AA (3)spect.line.intensity;arith.ratiofloatu_6731Uncertainty flag on 6731meta.code.errorchar7325Reddening corrected line intensity at 7325AA (3)spect.line.intensity;arith.ratiofloatu_7325Uncertainty flag on 7325meta.code.errorcharlogL5007? [OIII] luminositylog(Sun)phys.luminosityfloatnullableJ/A+A/336/667/modelsSummary of photoionization modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.intFileNameModel filename (in subdirectory "npgrid")charVexpExpansion velocitykm/sintMnebNebular masssolMassfloatMstarMass of the central starsolMassfloatZAbundance relative to the Sunlog(Sun)floatJ/A+A/336/667/table2Electron temperatures and densities, elemental and ionic abundancesT(O3)Electronic temperature deduced from [O III]4363/5007Kphys.temperature;phys.electronintT(N2)Electronic temperature deduced from [N II]5755/6584Kphys.temperature;phys.electronintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRegion[abcde] Regionmeta.notecharObjectObject numbermeta.idintPNNP namemeta.id;meta.maincharHe/HHe/H abundance ratiophys.abunddoubleN/HN/H abundance ratiophys.abunddoubleO/HO/H abundance ratiophys.abunddoubleNe/HNe/H abundance ratiophys.abunddoublene(SII)Electronic density deduced from [S II]6717/6730cm**-3phys.densitydoubleO+3727/HO^+^/H value deduced from [O II]3727/H{beta}phys.abunddoubleO+7325/HO^+^/H value deduced from [O II]7325/H{beta}phys.abunddoubleO++/HO^++/H abundance ratiophys.abunddoubleN+/HN^+/H abundance ratiophys.abunddoubleNe++/HNe^++^/H abundance ratiophys.abunddoubleHe+/HHe^+^/H abundance ratiophys.abunddoubleHe++/HHe^++^/H abundance ratiophys.abunddouble