J/ApJS/218/25ivo://CDS.VizieR/J/ApJS/218/25doi:10.26093/cds/vizier.22180025CDSSterling N.C.Porter R.L.Dinerstein H.L.2017-07-06T06:25:56Z2015-09-08T07:33:11ZCDS support team

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

cds-question@unistra.frchemical-abundancesatomic-physicsplanetary-nebulaeThe detection of neutron(n)-capture elements in several planetary nebulae (PNe) has provided a new means of investigating s-process nucleosynthesis in low-mass stars. However, a lack of atomic data has inhibited accurate trans-iron element abundance determinations in astrophysical nebulae. Recently, photoionization (PI) and recombination data were determined for Se and Kr, the two most widely detected n-capture elements in nebular spectra. We have incorporated these new data into the photoionization code Cloudy (Ferland et al. 2013RMxAA..49..137F). To test the atomic data, numerical models were computed for 15 PNe that exhibit emission lines from multiple Kr ions. We found systematic discrepancies between the predicted and observed emission lines that are most likely caused by inaccurate PI and recombination data. These discrepancies were removed by adjusting the Kr^+^-Kr^3+^ PI cross sections within their cited uncertainties and the dielectronic recombination rate coefficients by slightly larger amounts. From grids of models spanning the physical conditions encountered in PNe, we derive new, broadly applicable ionization correction factor (ICF) formulae for calculating Se and Kr elemental abundances. The ICFs were applied to our previous survey of near-infrared [KrIII] and [SeIV] emission lines in 120 PNe. The revised Se and Kr abundances are 0.1-0.3dex lower than former estimates, with average values of [Se/(O,Ar)]=0.12+/-0.27 and [Kr/(O,Ar)]=0.82+/-0.29, but correlations previously found between their abundances and other nebular and stellar properties are unaffected. We also find a tendency for high-velocity PNe that can be associated with the Galactic thick disk to exhibit larger s-process enrichments than low-velocity PNe belonging to the thin-disk population.2015ApJS..218...25Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/218/25CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toVI/64 : Recombination line intensities for hydrogenic ions (Storey+ 1995)J/A+A/562/A71 : Abundances of solar neighbourhood dwarfs (Bensby+, 2014)J/ApJ/778/149 : Abundances for 3 stars in Sgr dSph (McWilliam+, 2013)J/ApJ/771/67 : Abundances for 97 metal-poor stars. II. (Ishigaki+, 2013)J/A+A/552/A128 : Abundances of neutron-capture elements (Mishenina+, 2013)J/MNRAS/428/3443 : PNe and HII regions plasma diagnostics (McNabb+, 2013)J/A+A/538/A54 : Spectroscopy of 12 planetary nebulae (Garcia-Rojas+, 2012)J/A+A/535/A117 : Low-charge ions charge transfer rate coeff. (Sterling+, 2011)J/A+A/535/A107 : Spectrosc. survey of 479 thick disc stars (Kordopatis+, 2011)J/A+A/533/A62 : Atomic Data for Neutron-Capture Elements. II (Sterling, 2011)J/MNRAS/415/181 : Deep spectroscopy of NGC 7009 (Fang+, 2011)J/A+A/530/A138 : Geneva-Copenhagen survey re-analysis (Casagrande+, 2011)J/A+A/529/A147 : Photoionization cross sections of Selenium (Sterling+, 2011)J/ApJ/724/975 : Heavy elements abundance of metal-poor stars (Roederer+, 2010)J/ApJ/724/748 : Galactic anticenter PNe and oxygen abundance (Henry+, 2010)J/ApJ/723/658 : Abundances of the halo PN BoBn 1 (Otsuka+, 2010)J/ApJ/714/1096 : Galactic planetary nebulae (Stanghellini+, 2010)J/A+A/500/1089 : Abundances in planetary nebulae (Gorny+, 2009)J/ApJ/696/797 : Evolution and yields of low-mass AGB stars (Cristallo+, 2009)J/ApJ/659/1265 : Emission lines in 4 planetary nebulae (Sharpee+, 2007)J/A+A/465/271 : Oxygen abundances in nearby stars (Ramirez+, 2007)J/A+A/463/265 : Chemical compositions of WR planetary nebulae (Girard+, 2007)J/MNRAS/367/1329 : Elemental abundances for 176 stars (Reddy+, 2006)J/A+A/442/249 : Integrated spectrum of NGC 7027 (Zhang+, 2005)J/A+A/427/231 : Abundances in planetary nebulae (Gorny+, 2004)J/A+A/423/199 : Chemical abundances of planetary nebulae (Costa+, 2004)J/MNRAS/349/793 : Galactic PNe abundances (Perinotto+, 2004)J/A+A/415/155 : Oxygen abundances in the Galactic disk (Bensby+, 2004)J/A+A/410/527 : Abundances in the Galactic disk (Bensby+, 2003)J/A+AS/147/111 : Iron Project. XLIV. Fe VI. (Chen+, 2000)J/ApJS/124/195 : PN medium-resolution spectra (Hora+, 1999)J/A+A/332/721 : Planetary nebulae abundances (Perinotto+ 1998)J/A+AS/126/297 : PN abundances (Ratag+ 1997)J/A+A/318/256 : Planetary nebulae properties (Gorny+ 1997)J/A+A/307/215 : Spectrophotomety of planetary nebulae (Cuisinier+, 1996)J/A+A/303/893 : Planetary nebulae with WR-type nuclei (Gorny+, 1995)J/PASP/105/1279 : The Spectrum of NGC 6567 (Hyung+ 1993)http://fruity.oa-teramo.inaf.it/ : Full-Network Repository of Updatedhttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/218/25https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJS/218/25http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJS/218/25https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJS/218/25https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJS/218/25http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJS/218/25GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJS/218/25/table14 (Se and Kr abundances relative to H, O, and Ar)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJS/218/25/table14?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJS/218/25/table14?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJS/218/25/table14?GETtext/xml+votable180.050000true293.688467830.51637310.005555555555555556Cone search capability for table J/ApJS/218/25/pne (Observational data references, model input parameters and comparison of modeled Se and Kr abundances for the 15 PNe exhibiting emission lines from multiple Kr ions)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJS/218/25/pne?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJS/218/25/pne?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJS/218/25/pne?GETtext/xml+votable180.050000true81.8675156-12.69729580.0055555555555555566/1244 1399 1552 1562 2883 2979 2993 3152 3332 3353 3365 3637 3819 6146 9233 9461 11605 12222 12812 12852 12857 12907 12960 12971 12992 13055 13676 13968 13995 14005 14118 14214 14279 14282 14402 14429 14443 14596 14602 14642 14796 14827 14853 15172 15384 15437 15472 15481 15639 20816 20826 21215 21315 21600 21609 22137 22166 23389 23816 23949 24361 28772 28825 28844 28871 28881 28906 28917 28922 28923 28963 28975 29057 29086 29092 29094 29096 29130 29146 29160 29168 29182 29213 29254 29266 29267 29286 29317 29451 29472 29520 29523 29540 29718 29852 29886 30288 30308 30340 30431 30472 30491 30527 30615 30656 30684 30686 31670 31775 31847 32193 32571 37354 39935 40279 40621 41574 41617 42446 44416 48032 48951https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJS/218/25?format=asciidefaultJ/ApJS/218/25/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefCode referencemeta.ref;pos.framecharBibCodeBibcodemeta.bib.bibcodecharAutFirst author's name(s)meta.bib.authorcharCommCommentmeta.notecharJ/ApJS/218/25/table4Predicted vs. observed diagnostics and line intensitiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDPlanetary nebula identifiermeta.id;meta.maincharIonIon or diagnostic identifier (1)phys.atmol.ionStagecharlam_um[2.1/57]? Wavelength in micronsumem.wlfloatnullablePred[0/2180]? Predicted line intensity (2)spect.line.intensity;arith.ratiodoublenullablef_Pred[ab] peculiar line ratio (3)meta.codecharObs[0.003/1720]? Observed line intensity (2)spect.line.intensity;arith.ratiodoublenullableJ/ApJS/218/25/table14Se and Kr abundances relative to H, O, and ArSimbadNameSimbad column added by the CDSmeta.idcharIDObject namemeta.id;meta.mainchare_[Se/H][0.08/0.7]? [Se/H] uncertaintylog(Sun)stat.error;phys.abundfloatnullablel_[Kr/Ar]Limit flag on [Kr/Ar]meta.code.errorcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNNumber of Se and Kr abundances determinations for this PNmeta.numberintnullablef_ID[f] Abundances may be not reliable (1)meta.codecharl_[Kr/H]Limit flag on [Kr/H]meta.code.error;phys.abundchar[Kr/H][-0.4/2.1]? Kr abundance relative to Hlog(Sun)phys.abundfloatnullablee_[Kr/H][0.1/0.5]? [Kr/H] uncertaintylog(Sun)stat.error;phys.abundfloatnullablef_[Kr/H][de, ] [Kr/H] may be not reliable (1)meta.codecharl_[Kr/O]Limit flag on [Kr/O]meta.code.errorchar[Kr/O][-0.7/2.1]? Kr abundance relative to O (2)log(Sun)phys.abundfloatnullablee_[Kr/O][0.1/0.8]? [Kr/O] uncertaintylog(Sun)stat.errorfloatnullablef_[Kr/O][cdeo, ] [Kr/O] may be not reliable (1)meta.codechar[Kr/Ar][-0.4/2.1]? Kr abundance relative to Ar (2)log(Sun)phys.abundfloatnullablee_[Kr/Ar][0.1/0.8]? [Kr/Ar] uncertaintylog(Sun)stat.errorfloatnullablef_[Kr/Ar][cde, ] [Kr/Ar] may be not reliable (1)meta.codecharl_[Se/H]Limit flag on [Se/H]meta.code.error;phys.abundchar[Se/H][-1/1.5]? Se abundance relative to Hlog(Sun)phys.abundfloatnullablef_[Se/H][d] Flag on [Se/H] may be not reliable (1)meta.codecharl_[Se/O]Limit flag on [Se/O]meta.code.errorchar[Se/O]Se abundance relative to O (2)log(Sun)phys.abundchare_[Se/O][0.08/1]? [Se/O] uncertaintylog(Sun)stat.errorfloatnullablef_[Se/O][cdeo, ] [Se/O] may be not reliable (1)meta.codecharl_[Se/Ar]Limit flag on [Se/Ar]meta.code.errorchar[Se/Ar][-1.1/1.7]? Se abundance relative to Ar (2)log(Sun)phys.abundfloatnullablee_[Se/Ar][0.1/1]? [Se/Ar] uncertaintylog(Sun)stat.errorfloatnullablef_[Se/Ar][cde, ] [Se/Ar] may be not reliable (1)meta.codecharRefNear-infrared reference starting by "IR" and optical/UV/MIR reference (see refs.dat file)meta.refchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/ApJS/218/25/pneObservational data references, model input parameters and comparison of modeled Se and Kr abundances for the 15 PNe exhibiting emission lines from multiple Kr ionsBib3Other bibcodemeta.bibcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintANumber of abundances (table4)meta.ref.urlintnullableA2Number of Se and Kr abundances derived with the new ICFs (Ionization Correction Factors; table 14)meta.ref.urlintnullableAuthOptical data author's name(s)meta.bib.authorcharBib1Optical data bibcodemeta.bibcharBib2Second optical bibcodemeta.bibcharc(Hb)[0.06/1.93] Extinction coefficient c(H{beta})phys.absorption.coefffloatnullableAuth3Other reference author's name(s)meta.bib.authorcharf_Bib3Flag on Bib (1)meta.bibcharAuth4Other reference author's namemeta.bib.authorcharBib4Second other bibcodemeta.bibcharLDisplay the predicted ion value for this PNmeta.ref.urlcharSimbadSimbad column added by the CDSmeta.ref.urlcharNEDSimbad column added by the CDSmeta.ref.urlcharIDPlanetary nebula identifier (or "Solar")meta.id;meta.maincharf_IDa: From Asplund et al. (2009ARA&A..47..481A)meta.codecharTeff[38/189]? Stellar effective temperaturekKphys.temperature.effectivefloatnullablee_Teff[3/30]? Teff uncertaintykKstat.error;phys.temperature.effectivefloatnullablelogg[3.4/8]? Log of surface gravitylog(cm.s**-2)phys.gravityfloatnullableLum[520/12400]? Luminosity (L/L_{sun}_)solLumphys.luminosityintnullablenH[1.6/59]? Nebular hydrogen density1000cm**-3phys.densityfloatnullablelogRin[-3/-1.6]? Log of nebular inner radiu(R_in_)log(pc)phys.size.radiusfloatnullablelogRout[-1.9/-0.8]? Log of outer radius (R_out_)log(pc)phys.size.radiusfloatnullableHe/H[0.08/0.2] He/H abundance (linear scale)phys.abundfloatC/H[8.2/9.1] 12+log(C/H) abundancephys.abundfloatN/H[7.5/8.7] 12+log(N/H) abundancephys.abundfloatO/H[8.3/9.1] 12+log(O/H) abundancephys.abundfloatNe/H[7.7/8.4] 12+log(Ne/H) abundancephys.abundfloatS/H[6.3/7.3] 12+log(S/H) abundancephys.abundfloatCl/H[4.2/5.5] 12+log(Cl/H) abundancephys.abundfloatAr/H[5.7/6.6] 12+log(Ar/H) abundancephys.abundfloatSe/H[2.9/3.7]? 12+log(Se/H) abundancephys.abundfloatnullablee_Se/H[0.03/0.2]? Se/H uncertaintyphys.abundfloatnullableKr/H[3.1/4.2] 12+log(Kr/H) abundancephys.abundfloate_Kr/H[0.1/0.3]? Kr/H uncertaintyphys.abundfloatnullableSe[2.9/3.7]? This work 12+log(Se/H) abundancephys.abundfloatnullablee_Se[0.03/0.2]? Se uncertaintystat.errorfloatnullableSe1[2.8/3.8]? 12+log(Se/H) abundance from Paper I (Sterling et al. 2007ApJS..169...37S)phys.abundfloatnullablee_Se1[0.05/0.2]? Se1 uncertaintystat.errorfloatnullableKr[3.1/4.2] Adopted 12+log(Kr/H) abundancephys.abundfloatnullablee_Kr[0.1/0.3] Kr uncertaintystat.errorfloatnullableKr0[3.1/4.3] Kr abundance without adjustmentphys.abundfloatnullableKr1[3.2/4.3]? 12+log(Kr/H) abundance from Paper I (Sterling et al. 2007ApJS..169...37S)phys.abundfloatnullablee_Kr1[0.1/0.3]? Kr1 uncertaintystat.errorfloatnullable_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.mainnullable_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainnullable