J/ApJ/705/509ivo://CDS.VizieR/J/ApJ/705/509doi:10.26093/cds/vizier.17050509CDSOtsuka M.Hyung S.Lee S.-J.Izumiura H.Tajitsu A.2012-03-13T20:13:26Z2012-02-27T14:22:04ZCDS support team

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

cds-question@unistra.frplanetary-nebulaespectroscopyUsing the High Dispersion Spectrograph (HDS) at the Subaru Telescope, we secured the high-resolution line spectra in the 3600-7500{AA} wavelength range of the Galactic halo planetary nebula DdDm 1. We also analyzed the Hubble Space Telescope Faint Object Spectrograph data in the 1200-6730{AA} wavelength range. The diagnostic results indicate the electron temperatures of T_{epsilon}_~11000-14000K and the electron number densities of N_{epsilon}_~2000-10500cm^-3^. In spite of high gaseous temperatures, we have not detected high excitation lines, e.g., HeII. We derived abundance based on the ionic concentration of permitted and forbidden lines and the photoionization model. A comparison of the ionic concentrations from forbidden lines to recombination lines shows the abundance discrepancy between them. We tested various possibilities, e.g., temperature fluctuation and high-density blob components, to explain the discrepancy. The high-density components or density fluctuation might be partly responsible for the discrepancy. DdDm 1 shows a low carbon abundance that corresponds to metal-poor stars, [Fe/H]<=-1. Assuming a distance of 10kpc to DdDm 1, theoretical models suggest that the central star has T_eff_~39000K and L~2000-3000L_{sun}_. The relatively high gas temperatures appear to be caused by very low heavy elemental abundances or insufficient coolants in the shell gas. Its progenitor, born in an extremely carbon-poor environment as an initial mass of about 0.9M_{sun}_, had probably experienced only the first dredge-up.2009ApJ...705..509Ohttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/705/509CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/mk : Catalogue of Stellar Spectral Classifications (Skiff, 2010)B/hst : HST Archived Exposures Catalog (STScI, 2007)IV/24 : Catalogue of Galactic Planetary Nebulae (Kohoutek, 2001)V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992)J/PAZh/35/574 : He, C, N and O abundances in planetary nebulae (Milanova+,J/A+A/475/217 : Classification of planetary nebulae (Quireza+, 2007)J/MNRAS/349/793 : Galactic PNe abundances (Perinotto+, 2004)J/A+A/408/1029 : Coordinates of Galactic planetary nebulae (Kerber+, 2003)J/AZh/74/853 : Distances and physical parameters of PNe (Mal'kov, 1997)J/A+AS/94/399 : Absolute fluxes and distances of PN (Cahn+, 1992)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/705/509https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/705/509http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/705/509https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/705/509https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/705/509http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/705/509GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/ApJ/705/509/table4*Observed line intensities [F(H{beta})=100] and identificationsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlam(L)Laboratory wavelength in Angstroms0.1nmem.wlfloatIonThe ion of the most probable identificationmeta.id;phys.atmol.ionStagecharMultMultiplet numbermeta.id;meta.maincharlam(O)? Measured wavelength, {lambda}(obs), corrected for radial velocity0.1nmem.wlfloatnullablef_lam(O)[1,3]? 1= blue- or 2= red- shifted line components when they are separable; 3= second red-meta.codeintnullableFlux? Normalized line intensity, F({lambda}) (1)phot.fluxfloatnullablee_Flux? 1{sigma} error in Fluxstat.error;phot.fluxfloatnullableFtot? Normalized total line intensity when components were separatedphot.fluxfloatnullablee_Ftot? FTot uncertaintystat.errorfloatnullable