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J/A+AS/126/297 PN abundances (Ratag+ 1997)
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Abundances in planetary nebulae near the galactic centre.
I. Abundance determinations
Ratag M.A., Pottach S.R., Dennefeld M., Menzies J.
<Astron. Astrophys. Suppl. Ser. 126, 297 (1997)>
=1997A&AS..126..297R (SIMBAD/NED BibCode)
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ADC_Keywords: Planetary nebulae ; Abundances
Keywords: planetary nebulae - ISM: abundances - Galaxy: center
Abstract:
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.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
pos2000 46 46 Planetary nebulae J2000 positions
table1 38 1135 Line Intensities corrected for interstellar
extinction
table2a 110 45 Fundamental data of the newly observed objects
table2b 117 52 Fundamental data of the objects with published
spectra
table5 85 95 Adopted abundances for the nebulae
table6 81 8 Abundances from the literature
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See also:
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992)
Byte-by-byte Description of file: pos2000
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [PK]
4- 11 A8 --- PK PK name
13- 14 I2 h RAh Right ascension (J2000)
16- 17 I2 min RAm Right ascension (J2000)
19- 22 F4.1 s RAs Right ascension (J2000)
24 A1 --- DE- Declination sign
25- 26 I2 deg DEd Declination (J2000)
28- 29 I2 arcmin DEm Declination (J2000)
31- 32 I2 arcsec DEs Declination (J2000)
35- 45 A11 --- Name PK name in Simbad
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Byte-by-byte Description of file: table1
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Bytes Format Units Label Explanations
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1- 8 A8 --- PK Planetary nebula name
10- 13 I4 --- Lambda Wavelength
15- 26 A12 --- Ident Wavelength identification
29 A1 --- l_Int Limit lfag on Int
30- 36 F7.2 --- Int ? Line intensity (2)
37- 38 A2 --- u_Int [*:? b] Note (1)
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Note (1): ':' Uncertainty flag
'?' Line not observed
'*' Saturated line
'b' Blended with the preceding or next line
Note (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
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Byte-by-byte Description of file: table2a table2b
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Bytes Format Units Label Explanations
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1- 8 A8 --- PK PK number
10- 17 A8 --- Name Planetary nebula name
19- 22 A4 --- Class Exc. class
24 A1 --- l_S6cm Limit flag on S6cm
25- 28 F4.1 mJy S6cm ? Flux density at 6cm
29 A1 --- u_S6cm Uncertainty flag on S6cm
30- 35 F6.2 [mW/m2] logF(Hbeta) ? H{beta} flux
36 A1 --- u_logF(Hbeta) Uncertainty flag on logF(Hbeta)
37 A1 --- l_Diam Limit flag on Diam
38- 42 F5.2 arcsec Diam ? Diameter
44- 47 F4.2 mag E(B-V)B ? Extinction E(B-V) from Balmer line
49- 52 F4.2 mag E(B-V)r ? Extinction E(B-V) from radio/H{beta}
53 A1 --- u_E(B-V)r Uncertainty flag on E(B-V)r
55- 58 F4.2 10+4K Te[OIII] ? Electron temperature from [OIII]
60- 63 F4.2 10+4K Te[NII] ? Electron temperature from [NII]
64 A1 --- u_Te[NII] Uncertainty flag on Te[NII]
66- 69 F4.2 10+4K Te ? Average electron temperature
70 A1 --- u_Te Uncertainty flag on Te
72- 76 F5.2 10+3cm-3 Ne ? Electron density
78- 83 F6.1 km/s Vlsr ? LSR velocity
85- 89 F5.2 10+7m-1 Fl/F(Hbeta) ? F_lambda_(5325A)/F(H{beta}) ratio
91- 95 F5.2 10-13W/m2 FIR ? Total IR flux
97-101 F5.2 --- IRE ? IR excess
103-117 A15 --- Ref References (1)
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Note (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)
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Byte-by-byte Description of file: table5 table6
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Bytes Format Units Label Explanations
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1- 8 A8 --- PK PK name
10- 16 A7 --- Name Other name
18- 22 F5.2 [Sun] [He] Adopted He abundance
23- 24 A2 --- n_[He] Note on [He]
26- 29 F4.2 [Sun] [O] Adopted O abundance
30- 31 A2 --- n_[O] Note on [O]
33- 36 F4.2 [Sun] [N] ? Adopted N abundance
37- 38 A2 --- n_[N] Note on [N]
40- 43 F4.2 [Sun] [Ne] ? Adopted Ne abundance
44- 45 A2 --- n_[Ne] Note on [Ne]
47- 50 F4.2 [Sun] [S] ? Adopted S abundance
51- 52 A2 --- n_[S] Note on [S]
54- 57 F4.2 [Sun] [Ar] ? Adopted Ar abundance
58- 59 A2 --- n_[Ar] Note on [Ar]
60 A1 --- u_[Ar] Uncertainty flag on [Ar]
61- 64 F4.2 [Sun] [Cl] ? Adopted Cl abundance
65- 66 A2 --- n_[Cl] Note on [Cl]
68- 72 F5.1 10+3K Teff Effective temperature
74- 77 F4.2 [cm/s2] logg ? Surface gravity
79- 85 A7 --- Notes Notes (1)
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Note (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).
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History: Prepared via OCR at CDS.
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(End) Patricia Bauer [CDS] 14-Oct-1997