J/A+A/336/667 PN abundances in five galaxies (Stasinska+ 1998)
The planetary nebulae populations in five galaxies:
abundance patterns and evolution
Stasinska G., Richer M.G., Mc Call M.L.
<Astron. Astrophys. 336, 667 (1998)>
=1998A&A...336..667S 1998A&A...336..667S (SIMBAD/NED BibCode)
ADC_Keywords: Planetary nebulae ; Abundances ; Opacities
Keywords: planetary nebulae: general - stars: AGB and post-AGB -
galaxies: abundances
Abstract:
We 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☉, 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 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.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 122 329 Reddening corrected line intensities on the
scale I(Hβ)=100 and logarithms of
[OIII] luminosities in solar units
table2.dat 134 329 Electron temperatures and densities, elemental
and ionic abundances
models.dat 32 94 Summary of photoionization models
npgrid/* . 94 A grid of photoionization models for evolving
planetary nebulae
--------------------------------------------------------------------------------
Byte-by-byte Description of file: models.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- FileName Model filename (in subdirectory "npgrid")
15- 16 I2 km/s Vexp Expansion velocity
19- 22 F4.2 solMass Mneb Nebular mass
25- 28 F4.2 solMass Mstar Mass of the central star
30- 32 F3.1 [Sun] Z Abundance relative to the Sun
--------------------------------------------------------------------------------
Description of files: npgrid/*
The models are computed using the photoionization code PHOTO in the
same conditions as Stasinska (1990A&AS...83..501S 1990A&AS...83..501S) but with atomic
data updated as reported in Stasinska & Leitherer
(1996ApJS..107..661S 1996ApJS..107..661S).
The planetary nebulae are modeled as uniformly expanding spherical
shells of constant total mass and constant relative thickness
δR/R, in which the density, assumed uniform, is varying with
time appropriately.
The evolution of the central stars is interpolated from the hydrogen
burning post-AGB evolutionary tracks of Blocker (1995,
Cat. J/A+A/299/755). The stars are assumed to radiate like
blackbodies.
The files containing the models are named mMvVsSSZ.res, where
M defines the total nebular mass MNEB:
m=1 stands for Mneb= 0.1 solar mass
m=2 stands for Mneb= 0.2 solar mass
m=4 stands for Mneb= 0.4 solar mass
V defines the expansion velocity VEXP of the outer edge
v=1 stands for Vexp=10 km/sec
v=2 stands for Vexp=20 km/sec
v=4 stands for Vexp=40 km/sec
SS defines the central star mass Mstar (in units of hundredths of a
solar mass)
ex: ss=58 stands for Mstar=0.58 solar mass
Z is a character defining the abundance set with respect to the
solar value Zsol
In the present grid, the values of z are defined as follows:
h for Z=0.5Zsol
e for Z=0.1Zsol
k for Z=2.0Zsol
the abundance ratios are defined as in
Stasinska & Leitherer, 1996ApJS..107..661S 1996ApJS..107..661S.
The grid is composed of the following 94 ascii files of record length 132:
m1v1s56h.res m1v4s62h.res m2v2s62k.res m4v1s61h.res
m1v1s57h.res m1v4s63h.res m2v2s63h.res m4v1s62h.res
m1v1s58h.res m1v4s64h.res m2v2s64e.res m4v1s63h.res
m1v1s59h.res m2v1s56h.res m2v2s64h.res m4v1s64h.res
m1v1s60h.res m2v1s57h.res m2v2s64k.res m4v2s56h.res
m1v1s61h.res m2v1s58h.res m2v2s65h.res m4v2s57h.res
m1v1s62h.res m2v1s59h.res m2v2s66h.res m4v2s58h.res
m1v1s63h.res m2v1s60h.res m2v2s70h.res m4v2s59h.res
m1v1s64h.res m2v1s61h.res m2v2s80h.res m4v2s60h.res
m1v2s56h.res m2v1s62h.res m2v2s90h.res m4v2s61h.res
m1v2s57h.res m2v1s63h.res m2v4s56h.res m4v2s62h.res
m1v2s58h.res m2v1s64h.res m2v4s57h.res m4v2s63h.res
m1v2s59h.res m2v2s56h.res m2v4s58h.res m4v2s64h.res
m1v2s60h.res m2v2s57h.res m2v4s59h.res m4v4s56h.res
m1v2s61h.res m2v2s58e.res m2v4s60h.res m4v4s57h.res
m1v2s62h.res m2v2s58h.res m2v4s61h.res m4v4s58h.res
m1v2s63h.res m2v2s58k.res m2v4s62h.res m4v4s59h.res
m1v2s64h.res m2v2s59h.res m2v4s63h.res m4v4s60h.res
m1v4s56h.res m2v2s60e.res m2v4s64h.res m4v4s61h.res
m1v4s57h.res m2v2s60h.res m4v1s56h.res m4v4s62h.res
m1v4s58h.res m2v2s60k.res m4v1s57h.res m4v4s63h.res
m1v4s59h.res m2v2s61h.res m4v1s58h.res m4v4s64h.res
m1v4s60h.res m2v2s62e.res m4v1s59h.res
m1v4s61h.res m2v2s62h.res m4v1s60h.res
A file is composed of a series of models computed at time intervals
of 500 years.
Each model is described by a group of 51 rows.
The structure of a file is the following:
-------------------------------------------------------------------------------
row Explanation
-------------------------------------------------------------------------------
1: name, time and date of creation
2: format (5(1x,a6,1p,e10.3): defining parameters
PNVEXP: expansion velocity in km/sec
PNDRSR: delta R/R=0.3 for all the models in this grid
PNMDH: total nebular mass in units of solar masses
PNNMASS: mass of the central star in units of solar masses
3-53: 1st model of the series
54-104: 2nd model of the series
105-155: 3rd model of the series
etc...
-------------------------------------------------------------------------------
Each model is listed as a series of figures corresponding to input or output
values. Some of them are of no utility to the user and will be named x in the
present description.
-------------------------------------------------------------------------------
r 3: separator (--------------)
r 4: format (a6,2x,a8,2x,3(1x,a6,i10),3(1x,a6,1p,e10.3))
1-model name (NAME),
2-serial number (ISERI), the value of ISER is defined by IAGE=ISERI*500
where IAGE is the age in years. Models have only been calculated when
the estimated total Hβ luminosity was greater than a certain
value. Therefore, there may be no outputs for certain values of ISERI.
3- x, 4- x, 5- x, 6- x, 7-x
r 5-13: format (7(1x,a6,1p,e10.3) : defining parameters and global results
listed as follows:
r 5: elemental abundances relative to H of H, He, C, N, O, Ne
r 6: elemental abundances relative to H of Mg, Si, S, Cl, Ar, Fe, Ca
r 7: 1- x, 2- hydrogen density in cm-3 (NH), 3- x, 4- x,
5- inner radius in cm (R_IN), 6- x, 7- x
r 8: 1- x, 2- x, 3- x
r 9: 1- effective temperature of the star (TSTAR), 2- stellar radius
in cm (GSTAR), 3- age in yrs (AGE), AGE is equal to ISERI*500,
4- x, 5- x, 6- x, 7- x.
r 10: 1- total luminosity of the ionizing star in solar units (LUM*),
2- number of stellar photons above the ionization threshold of H0
in units of 1.e44 photons/sec (Q44H0),
3- number of stellar photons above the ionization threshold of HE0
in units of 1.e44 photons/sec (Q44HE0),
4- number of stellar photons above the ionization
threshold of HE+ in units of 1.e44 photons/sec (Q44HE+),
5- U4IN=Q44H*1.e44/(4*3.1416*RIN**2*NH*3.e+10),
ionization parameter at the inner edge
6- x, 7- x
r 11: 1- x, 2- x, 3- x, 4- x, 5- x, 6- x
r 12: 1- outer radius of the ionized region in cm (R_OUT),
2- outer electron temperature (TE_OUT),
3- outer H+/H fraction (FH_OUT),
4- outer He+/H fraction (FHE_OUT), 5- optical thickness of the nebula
at 13.6eV from center to outer radius (TO13.6),
6- optical thickness at 24.6eV (TO24.6),
7- optical thickness at 54.4eV (TO54.4).
r 13: 1- nebular mass inside R_OUT in solar units (GASMAS),
2- Hβ luminosity of the nebula in solar units (LHBETA),
3- luminosity of the nebula adding all the lines in solar units (LLTOT),
4- x, 5- x,
6- equivalent width in angstroms of the Hβ emitted by the nebula
taking into account the stellar + nebular continuum (EWHB*N),
7- same as EWHB*N but taking into account only the
stellar continuum (EWHB*)
r 14: blank
r 15-16: format (6(1x,a2,2x,0p,f8.0,1p,e9.2)): luminosity of the stellar
continuum at selected wavelengths in erg/cm3/sec/Angstrom
divided by nebular Hβ luminosity in erg/cm3/sec
r 17: blank
r 18-19: format (6(1x,a2,2x,0p,f8.0,1p,e9.2)): luminosity of the nebular
continuum at selected wavelengths in erg/cm3/sec/Angstrom
divided by nebular Hβ luminosity in erg/cm3/sec
r 20: blank
r 21-39: format (6(1x,a2,i2,0p,f8.0,1p,e9.2)): nebular emission in selected
lines. For each line is given the parent ion (format a2,i2),
the approximate wavelength in Angstroms (format f8.0), and the
intensity with respect to Hβ.
r 40: blank
r 41-51: mean ionic fractions as defined in Stasinska (1990A&AS...83..501S 1990A&AS...83..501S)
r 41: format (a6,10(3x,1p,e9.2) ionic fractions for
H1, H2, He1, He2, He3
r 42: format (6x,10(3x,1p,e9.2) ionic fractions for the 6 ions of C
r 43: format (6x,10(3x,1p,e9.2) ionic fractions for the 7 ions of N
r 44: format (6x,10(3x,1p,e9.2) ionic fractions for the 8 ions of O
r 45: format (6x,10(3x,1p,e9.2) ionic fractions for the 10 first
ions of Ne
r 46: format (6x,10(3x,1p,e9.2) ionic fractions for the 10 first
ions of Mg
r 47: format (6x,10(3x,1p,e9.2) ionic fractions for the 10 first
ions of Si
r 48: format (6x,10(3x,1p,e9.2) ionic fractions for the 10 first
ions of S
r 49: format (6x,10(3x,1p,e9.2) ionic fractions for the 10 first
ions of Cl
r 50: format (6x,10(3x,1p,e9.2) ionic fractions for the 10 first
ions of Ar
r 51: format (6x,10(3x,1p,e9.2) ionic fractions for the 10 first
ions of Fe
r 52: blank
r 53: format (2x,13(a3,F7.0) mean ionic temperatures as defined in Stasinska
(1990A&AS...83..501S 1990A&AS...83..501S) for H II, He II, He III, C II, C III, C IV,
N II, N III, N IV, O II, O III, O IV, O V
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Region [abcde] Region (1)
3- 5 I3 --- Object Object number
7- 14 A8 ---- PN PN name
16- 18 A3 --- Ref Reference (2)
20 A1 --- l_3727 Limit flag on 3727
21- 25 F5.1 --- 3727 Reddening corrected line intensity at 3727AA (3)
26 A1 --- u_3727 Uncertainty flag on 3727
28- 32 F5.1 --- 3869 Reddening corrected line intensity at 3869AA (3)
33 A1 --- u_3869 Uncertainty flag on 3869
35 A1 --- l_4363 Limit flag on 4363
36- 39 F4.1 --- 4363 Reddening corrected line intensity at 4363AA (3)
40 A1 --- u_4363 Uncertainty flag on 4363
42 A1 --- l_4686 Limit flag on 4686
43- 47 F5.1 --- 4686 Reddening corrected line intensity at 4686AA (3)
48 A1 --- u_4686 Uncertainty flag on 4686
50 A1 --- l_5007 Limit flag on 5007
51- 56 F6.1 --- 5007 Reddening corrected line intensity at 5007AA (3)
57 A1 --- u_5007 Uncertainty flag on 5007
59 A1 --- l_5755 Limit flag on 5755
60- 63 F4.1 --- 5755 Reddening corrected line intensity at 5755AA (3)
64 A1 --- u_5755 Uncertainty flag on 5755
66 A1 --- l_5876 Limit flag on 5876
67- 70 F4.1 --- 5876 Reddening corrected line intensity at 5876AA (3)
71 A1 --- u_5876 Uncertainty flag on 5876
73 A1 --- l_6300 Limit flag on 6300
74- 78 F5.1 --- 6300 Reddening corrected line intensity at 6300AA (3)
79 A1 --- u_6300 Uncertainty flag on 6300
81- 85 F5.1 --- 6563 Reddening corrected line intensity at 6563AA (3)
87 A1 --- l_6583 Limit flag on 6583
88- 93 F6.1 --- 6583 Reddening corrected line intensity at 6583AA (3)
94 A1 --- u_6583 Uncertainty flag on 6583
96 A1 --- l_6717 Limit flag on 6717
97-101 F5.1 --- 6717 Reddening corrected line intensity at 6717AA (3)
102 A1 --- u_6717 Uncertainty flag on 6717
104 A1 --- l_6731 Limit flag on 6731
105-109 F5.1 --- 6731 Reddening corrected line intensity at 6731AA (3)
110 A1 --- u_6731 Uncertainty flag on 6731
112-115 F4.1 --- 7325 Reddening corrected line intensity at 7325AA (3)
116 A1 --- u_7325 Uncertainty flag on 7325
118-122 F5.2 [Sun] logL5007 ? [OIII] luminosity
--------------------------------------------------------------------------------
Note (1): Region takes the values
a: M 31
b: Milky Way bulge
c: M 32
d: LMC
e: SMC
Note (2):
M31, M32: a Richer, Stasinska, Mc Call, 1998, A&AS, submitted
Milky Way bulge: a Aller & Keyes, 1987ApJS...65..405A 1987ApJS...65..405A
b Webster, 1988MNRAS.230..377W 1988MNRAS.230..377W
c Ratag et al., 1997, Cat. J/A+AS/126/297
LMC: a Meatheringham & Dopita, 1991, Cat. J/ApJS/75/407
b Meatheringham & Dopita, 1991, Cat. J/ApJS/76/1085
c Jacoby & Kaler, 1993ApJ...417..209J 1993ApJ...417..209J
d Boroson & Liebert, 1989ApJ...339..844B 1989ApJ...339..844B
e Leisy & Dennefeld, 1996, Cat. J/A+AS/116/95
f Monk, Barlow & Clegg, 1988, Cat. J/MNRAS/234/583
g Vassiliadis et al., 1992, Cat. J/ApJS/83/87
m Jacoby, Walker & Ciardullo, 1990ApJ...365..471J 1990ApJ...365..471J
o Wood et al., 1987ApJ...320..178W 1987ApJ...320..178W
s Meatheringham, Dopita & Morgan, 1988ApJ...329..166M 1988ApJ...329..166M
SMC: a Aller et al., 1981MNRAS.194..613A 1981MNRAS.194..613A
b Barlow, 1987MNRAS.227..161B 1987MNRAS.227..161B
c Boroson & Liebert, 1989ApJ...339..844B 1989ApJ...339..844B
d Jacoby & Kaler, 1993ApJ...417..209J 1993ApJ...417..209J
e Leisy & Dennefeld, 1996, Cat. J/A+AS/116/95
f Meatheringham & Dopita, 1991, Cat. J/ApJS/75/407
g Meatheringham & Dopita, 1991, Cat. <J/ApJS/76/1085
h Meyssonnier, 1995A&AS..110..545M 1995A&AS..110..545M
i Monk, Barlow & Clegg ,1988, Cat. J/MNRAS/234/583
j Vassiliadis et al., 1992, J/ApJS/83/87
k Meatheringham et al., 1990ApJ...361..101M 1990ApJ...361..101M
Note (3): Hβ=100
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Region [abcde] Region
3- 5 I3 --- Object Object number
7- 14 A8 --- PN NP name
16- 23 E8.2 --- He/H He/H abundance ratio
25- 32 E8.2 --- N/H N/H abundance ratio
34- 41 E8.2 --- O/H O/H abundance ratio
43- 50 E8.2 --- Ne/H Ne/H abundance ratio
52- 59 E8.2 cm-3 ne(SII) Electronic density deduced from [S II]6717/6730
61- 65 I5 K T(O3) Electronic temperature deduced from
[O III]4363/5007
67- 71 I5 K T(N2) Electronic temperature deduced from
[N II]5755/6584
73- 80 E8.2 --- O+3727/H O+/H value deduced from [O II]3727/Hβ
82- 89 E8.2 --- O+7325/H O+/H value deduced from [O II]7325/Hβ
91- 98 E8.2 --- O++/H O^++/H abundance ratio
100-107 E8.2 --- N+/H N^+/H abundance ratio
109-116 E8.2 --- Ne++/H Ne++/H abundance ratio
118-125 E8.2 --- He+/H He+/H abundance ratio
127-134 E8.2 --- He++/H He++/H abundance ratio
--------------------------------------------------------------------------------
Acknowledgements: Grazyna Stasinska
History:
* 28-May-1998: files received from Grazyna Stasinska
* 07-Aug-1999/ added the file "models.dat" with initial parameters of
the models.
(End) Patricia Bauer [CDS] 28-May-1998