J/A+AS/126/297 J/A+AS/126/297 PN abundances M A Ratag S R Pottach M Dennefeld J Menzies Astron. Astrophys. Suppl. Ser. 126 297 1997 1997A&AS..126..297R V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) Abundances Planetary nebulae Galaxy: center ISM: abundances planetary nebulae: general Abundance determinations of about 110 planetary nebulae, which are likely to be in the Galactic Bulge are presented. Plasma diagnostics have been performed by making use of the available forbidden line ratios combined with radio continuum measurements. Chemical abundances of He, O, N, Ne, S, Ar, and Cl are then derived by employing theoretical nebular models as interpolation devices in establishing the ionization correction factors (ICFs) used to estimate the distribution of atoms among unobserved ionization stages. The overall agreement between the results derived by using the model-ICFs and those obtained from the theoretical models is reasonably good. The uncertainties related to the total abundances show a clear dependence on the level of excitation. In most cases, the abundances of chlorine can be derived only in objects with a relatively high Cl-abundance. Contrary to the conclusion previously drawn by Webster (1988MNRAS.230..377W), we found the excitation classes are not uniformly distributed. A clear peak at about classes 5 and 6 is noticed. The distribution is shifted toward a lower excitation range with respect to that of the nearby nebulae, reflecting the difference in the central star temperature distribution between the two samples.

PK PK name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Name PK name in Simbad --- PN Planetary nebula name --- Lambda Wavelength --- Ident Wavelength identification --- l_Int Limit lfag on Int --- Int Line intensity number=2 Additional and adopted line intensities: Line intensities of the wavelengths marked with "w" are adopted from Webster (1988MNRAS.230..377W), while those with "a" from Aller and Keyes (1987ApJS...65..405A). 0-2.3 5007w, 5755w 0+3.1 4712w, 4740w 1-3.1 5007w, 6300w, 5698=1.04 2-6.1 6300a 2-4.2 4648=3.8, 5150=0.53, 5412=1.68, 5665+5680=2.6, 7236=1.36 ([ArIV], CII) 2-4.1 9069=18.0, 9532=48.0 2-3.5 3868a, 4471a 2-3.3 4415=1.1; 4553=1.52; 4570=1.62; 4681=3.9, 5698=2.8; Central star is probably a Wolf-Rayet. 2-2.4 5517a, 5537a 3-4.9 5412=2.2, 7236=1.1 ([ArIV],CII) 3-4.4 4648=3.8, 5412=4.2 4-22.1 Sum 4640-4648=7.4 6+4.2 5810=28.6 (broad) 6+8.1 4570=0.74; 7236=0.26 ([ArIV],CII) 7-4.1 3727a, 3968a, 5698=1.65 12-2.1 5698=1.37 349+4.1 4415=5.6 351+5.1 7236=0.77: ([ArIVl,CII) 353+6.2 6300a 355-6.1 5412=0.52 355-4.2 5517w, 5537w, 7236=0.7: ([ArIV],CII) 355-2.3 3425=87.1. Peculiar, if this is originated from [NeV], since no HeII line is detected. 357-7.1 4640w, 4686w 358+1.1 4686w, 4712w, 5755w 359-4.2 3425=251 (see remarks for PK 355-2.3) 359-2.3 5412=1.37 359-1.2 5876w 359-1.1 5412=3.1, 7012=1.70, sum (5517+5537)w 3-4.3 3727a, 4471a, 5876a, 6678a, 6717a, 6731a 3+3.1 5696=1.86: 4+6.2 7080=1.02 357+4.1 Sum (6717 +6731)w 359-2.4 4712w, 5200w, 6312w, 7325w 359+3.4 5412=7.8, 7005=6.0 --- u_Int Note number=1 ':' Uncertainty flag '?' Line not observed '*' Saturated line 'b' Blended with the preceding or next line --- PK PK number --- Name Planetary nebula name --- Class Exc. class --- l_S6cm Limit flag on S6cm --- S6cm Flux density at 6cm mJy u_S6cm Uncertainty flag on S6cm --- logF(Hbeta) H{beta} flux [mW/m2] u_logF(Hbeta) Uncertainty flag on logF(Hbeta) --- l_Diam Limit flag on Diam --- Diam Diameter arcsec E(B-V)B Extinction E(B-V) from Balmer line mag E(B-V)r Extinction E(B-V) from radio/H{beta} mag u_E(B-V)r Uncertainty flag on E(B-V)r --- Te[OIII] Electron temperature from [OIII] 10+4K Te[NII] Electron temperature from [NII] 10+4K u_Te[NII] Uncertainty flag on Te[NII] --- Te Average electron temperature 10+4K u_Te Uncertainty flag on Te --- Ne Electron density 10+3cm-3 Vlsr LSR velocity km/s Fl/F(Hbeta) F_lambda_(5325A)/F(H{beta}) ratio 10+7m-1 FIR Total IR flux 10-13W/m2 IRE IR excess --- Ref References number=1 A: Acker et al. (1989A&AS...80..201A) A2: Acker et al. (1989A&AS...77..487A) AK: Aaquist and Kwok (1990A&AS...84..229A) AK1: Aller and Keyes (1987ApJS...65..405A) AL: Allen (1979Obs....99...83A) G: Gathier et al. (1983A&A...128..325G) KFL: Kinman et al. (1988AJ.....95..804K) MA: Milne and Aller (1975A&A....38..183M, 1982A&AS...50..209M) P: Pottasch et al. (1988A&A...205..248P) PK: Perek and Kohoutek (1967PKCat.C......1P) R: Ratag et al. (1990A&A...233..181R) S: Schneider et al. (1983ApJS...52..399S) SK: Shaw and Kaler (1989ApJS...69..495S) W: Webster (1988MNRAS.230..377W) W83: Webster (1983PASP...95..610W) Z: Zilstra et al. (1989IAUS..131..210Z) --- PK PK name --- Name Other name --- [He] Adopted He abundance [Sun] n_[He] Note on [He] --- [O] Adopted O abundance [Sun] n_[O] Note on [O] --- [N] Adopted N abundance [Sun] n_[N] Note on [N] --- [Ne] Adopted Ne abundance [Sun] n_[Ne] Note on [Ne] --- [S] Adopted S abundance [Sun] n_[S] Note on [S] --- [Ar] Adopted Ar abundance [Sun] n_[Ar] Note on [Ar] --- u_[Ar] Uncertainty flag on [Ar] --- [Cl] Adopted Cl abundance [Sun] n_[Cl] Note on [Cl] --- Teff Effective temperature 10+3K logg Surface gravity [cm/s2] Notes Notes number=1 (1) Kurucz (1979ApJS...40....1K) (2) Clegg and Middlemass (1987MNRAS.228..759C) (3) Husfeld et al. (1984A&A...134..139H) (4) Planckian distribution. (5) The derived electron temperature, Te, is uncertain. (6) The electron density, Ne is derived from [ArIV] doublet. (7) The adopted electron density is uncertain. (8) The faintness, due to the very large interstellar extinction and/or due to the intrinsically low surface brightness of the nebula, causes the line intensities blueward of H{beta} to be poorly determined. (9) The observed line intensity ratio of [OII]{lambda}3727/{lambda}3725 cannot be reproduced by the model. The line intensity at {lambda}7325 predicted by the model is much lower than the observed one. Dielectronic recombination may play an important role (Rubin, 1986ApJ...309..334R). --- Patricia Bauer CDS 1997Oct14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_126_297.xml