J/ApJ/714/1096 Galactic planetary nebulae (Stanghellini+, 2010)
The Galactic structure and chemical evolution traced by the population of
planetary nebulae.
Stanghellini L., Haywood M.
<Astrophys. J., 714, 1096-1107 (2010)>
=2010ApJ...714.1096S 2010ApJ...714.1096S
ADC_Keywords: Planetary nebulae ; Milky Way ; Abundances ; Stars, distances
Keywords: Galaxy: disk - Galaxy: evolution - Galaxy: structure -
planetary nebulae: general
Abstract:
We use an extended and homogeneous data set of Galactic planetary
nebulae (PNe) to study the metallicity gradients and the Galactic
structure and evolution. The most up-to-date abundances, distances
(calibrated with Magellanic Cloud PNe), and other parameters have been
employed, together with a novel homogeneous morphological
classification, to characterize the different PN populations. We
studied the α-element distribution within the Galactic disk, and
found that the best selected disk population (i.e., excluding bulge
and halo component), together with the most reliable PN distance scale
yields to a radial oxygen gradient of
Δlog(O/H)/ΔRG=-0.023±0.006dex/kpc for the whole disk
sample, and of Δlog(O/H)/ΔRG=-0.035±0.024,
-0.023±0.005, and -0.011±0.013dex/kpc, respectively for Type I,
II, and III PNe, i.e., for high-, intermediate-, and low-mass
progenitors. We also extend the Galactic metallicity gradient
comparison by revisiting the open cluster [Fe/H] data from high
resolution spectroscopy.
Description:
In this paper, we use the Magellanic Cloud-calibrated Galactic PN
distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to
examine the population of PNe in our Galaxy. We extend the Perinotto
et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the
abundances published more recently, and calculate the metallicity
gradients for the different populations, and homogeneously classify
the Galactic PN morphology for further insight on population
selection.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 66 728 Distances, radii, fluxes, and morphology
table2.dat 83 224 Abundances and PN type
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See also:
IV/24 : Catalogue of Galactic Planetary Nebulae (Kohoutek, 2001)
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992)
J/ApJ/711/619 : Alpha element abundances in Galactic PNe (Milingo+, 2010)
J/A+A/494/591 : Abundances in planetary nebulae (Chiappini+, 2009)
J/A+A/500/1089 : Abundances in planetary nebulae (Gorny+, 2009)
J/PAZh/35/574 : He, C, N and O abundances in PNe (Milanova+, 2009)
J/ApJ/689/194 : Distances of galactic planetary nebulae (Stanghellini+, 2008)
J/A+A/479/155 : Proper motions of Galactic Planetary Nebulae (Kerber+, 2008)
J/MNRAS/349/793 : Galactic PNe abundances (Perinotto+, 2004)
J/A+A/423/199 : Chemical abundances of planetary nebulae (Costa+, 2004)
J/A+A/408/1029 : Coordinates of Galactic planetary nebulae (Kerber+, 2003)
J/A+A/345/629 : Abundance gradients in planetary nebulae (Maciel+, 1999)
J/AJ/115/1989 : Distances of galactic planetary nebulae (Tajitsu+, 1998)
J/AZh/74/853 : Distances and physical parameters of PNe (Mal'kov, 1997)
J/ApJS/98/659 : Galactic PNe statistical distance scale (Zhang 1995)
J/ApJS/91/347 : A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)
J/A+A/280/581 : Chemical abundances of PNe (Pasquali+, 1993)
J/A+AS/94/399 : Absolute fluxes and distances of PN (Cahn+, 1992)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- PNG Designation (as in Acker et al. Cat. V/84;
LLL.l+BB.b)
12- 18 F7.4 kpc d Heliocentric distance (1)
20- 27 F8.5 kpc e_d Uncertainty in d
29- 36 F8.5 kpc RG Galactocentric distance (2)
38- 47 F10.7 kpc e_RG Uncertainty in RG
49- 54 F6.2 arcsec theta Angular radius
56- 63 F8.6 Jy F5GHz The 5GHz flux density
65- 66 A2 --- Morph New morphological classification (3)
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Note (1): The heliocentric distance calculated from the Magellanic Cloud
re-calibration of the Cahn et al., 1992 (Cat. J/A+AS/94/399) scale,
except for bipolar PNe where we used the Magellanic Cloud
re-calibration of the SB-RPN relation, and where the uncertainties
are assumed to be 20% for all PNe. See section 2.2.
Note (2): Galactocentric distances, RG, are calculated by de-projecting
heliocentric distances onto the Galactic plane with the usual relation
RG=(R2☉+(dcosb)2-2R☉dcosbcosl)0.5, where d is the
PN heliocentric distance, R☉=8.0kpc is the solar distance to the
Galactic center, and b and l are the Galactic coordinates of the
nebulae. See section 2.2 for further explanations.
Note (3): Classification as follows:
R = Round;
E = Elliptical;
BC = Bipolar Core;
B = Bipolar.
? = Morphology was not defined due to lack of clarity in the images
or to very small nebular size.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- PNG Designation (as in Acker et al. Cat. V/84;
LLL.l+BB.b)
12- 16 F5.2 [---] A(He) ?=99.99 12+log(He/H) number abundance
18- 27 F10.7 [---] e_A(He) ?=99.99 Uncertainty in A(He)
29- 34 F6.3 [---] A(N) ?=99.99 12+log(N/H) number abundance
36- 42 F7.4 [---] e_A(N) ?=99.99 Uncertainty in A(N)
44- 49 F6.3 [---] A(O) ?=99.99 12+log(O/H) number abundance
51- 58 F8.5 [---] e_A(O) ?=99.99 Uncertainty in A(O)
60- 65 F6.3 [---] A(Ne) ?=99.99 12+log(Ne/H) number abundance
67- 74 F8.5 [---] e_A(Ne) ?=99.99 Uncertainty in A(Ne)
76- 83 A8 --- Type PN type (Type I, II, III, bulge or halo)
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 18-Apr-2012