J/A+A/680/A104 Galactic metallicity gradients with PNe (Bucciarelli+ 2023)
Tracing the Galactic disk with planetary nebulae using Gaia DR3.
Distance catalog, velocities, populations, and radial metallicity gradients of
Galactic planetary nebulae.
Bucciarelli B., Stanghellini L.
<Astron. Astrophys. 680, A104 (2023)>
=2023A&A...680A.104B 2023A&A...680A.104B (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Planetary nebulae ; Abundances ; Stars, distances ;
Parallaxes, trigonometric
Keywords: planetary nebulae: general - Galaxy: abundances - Galaxy: disk -
stars: distances - methods: statistical -
stars: kinematics and dynamics
Abstract:
We study the population of Galactic planetary nebulae (PNe) and their
central stars (CSs) through the analysis of their distances and
Galactic distribution. The PN distances are obtained by means of a
revised statistical distance scale, based on an
astrometrically-defined sample of CSs from Gaia DR3 as calibrators.
The new statistical distances, together with the proper motion of the
CSs - also from DR3, and with published PN abundances as well as
radial velocities, are used to characterize the PN populations in the
Galaxy, and to derive the radial metallicity gradient.
The statistical scale is applied to infer distances of a significant
number (∼850) of Galactic PNe, for which we deliver a new catalog of
PN distances. By adopting a circular velocity curve of the Galaxy, we
also obtain peculiar 3D velocities for a large sample of PNe (∼300).
Elemental abundances of the PNe are culled from the literature for an
updated catalog, to be used in our analysis and other external
applications.
The radial chemical gradient of the Galactic Disk is traced by PNe
with available chemical abundances and distances, and kinematic data
of the CSs are employed to identify the Halo PN population.We date PN
progenitors based both on abundances and on kinematic properties,
finding a confirmation of the first method with the second. For all
PNe with at least one oxygen determination in the literature, we find
a slope of the radial oxygen gradient equal to
{DELTA}log(O/H)/{DELTA}RG=-0.0144±0.00385 [dex/kpc]. Furthermore, we
estimate radial oxygen gradients for the PNe with old (>7.5Gyr) and
young (<1Gyr) progenitors to be respectively
{DELTA}log(O/H)/{DELTA}RG=-0.0121±0.00465 and -0.022±0.00758
[dex/kpc], thus disclosing a mild steepening of the gradient since
Galaxy formation, with a slope change of 0.01dex. The time evolution
is slightly higher (∼0.015dex) if we select the best available
abundances in the literature. This result is in broad agreement with
previous PN results, but now based on DR3 Gaia analysis, and also in
agreement with what traced by most other Galactic probes. We also find
a moderate oxygen enrichment when comparing the PNe with young and old
progenitors.
Description:
We give Gaia DR3 parallaxes for a set of PN central stars matched with
the HASH database (Parker Q.A. 2016, Journal of Physics Conf. Series,
728, 032008), which we used to recalibrate the PN statistical distance
scale. We present statistical distances, peculiar velocities (obtained
by combining DR3 proper motions and radial velocities from the
literature), and physical parameters (angular radius, Hbeta flux) for
true PN from HASH, along with a kinematical classification of PN
population. Moreover, we list PN chemical abundances culled from
published data plus age classification inferred from such abundances
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 109 401 The PNe identified as potential calibrators
of the distance scale
table3.dat 114 843 Catalog of PNe with estimated statistical
distances and peculiar velocities
table4.dat 69 320 C, N, O average abundances and PN ages
table5.dat 68 320 C, N, O selected abundances and PN ages
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
V/127 : MASH Catalogues of Planetary Nebulae (Parker+ 2006-2008)
http://planetarynebulae.net/EN/hash.php : HASH database Home Page
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 PN name in the usual format: LLL.l+BB.b
12- 30 I19 --- GaiaDR3 Gaia DR3 source ID
32- 42 A11 --- AName Alternate name of the PN
44- 51 F8.6 mas omegac Gaia DR3 parallax of PN central star
corrected for zero-point and biases
(see paper)
53- 60 F8.6 mas e_omegac Parallax uncertainty from Gaia DR3
corrected for known bias (see paper)
62- 69 F8.4 arcsec theta Angular radius of the PN
71- 76 F6.2 [mW/m2] logF(Hb) logarithm of Hβ flux (in erg/cm^2/s)
80- 83 F4.2 [mW/m2] e_logF(Hb) Uncertainty on F(Hb) (in erg/cm^2/s)
85- 93 F9.6 --- c Extinction constant
96- 99 F4.2 --- e_c Uncertainty on c
101-109 F9.6 [Msun] logMi logarithm of PN ionized mass
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- PNG PN name in the usual format: LLL.BB.b
12- 19 F8.4 arcsec theta Angular radius of the PN
21- 26 F6.2 [mW/m2] logF(Hb) logarithm of Hβ flux (in erg/cm^2/s)
30- 33 F4.2 [mW/m2] e_logF(Hb) Uncertainty on F(Hb) (in erg/cm^2/s)
35- 43 F9.6 --- c Extinction constant
46- 49 F4.2 --- e_c Uncertainty on c
51- 62 F12.6 pc Dist PN distance from our distance scale (parsecs)
64- 74 F11.6 pc E_Dist Upper uncertainty of Dist
76- 86 F11.6 pc e_Dist Lower uncertainty of Dist
88- 97 F10.6 km/s Vpec ?=- Peculiar velocity of the PN central star
99-107 F9.6 km/s e_Vpec ?=- Uncertainty on Vpec
110-114 A5 --- PNPop Disk, Bulge, or Halo PN population (1)
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Note (1): See paper for details on PN population classification.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- PNG PN name in the usual format: LLL.l+BB.b
12- 19 F8.6 [-] C/H ?=- Average C/H abundance (G1)
23- 30 F8.6 [-] e_C/H ?=- Uncertainty on C/H
32- 39 F8.6 [-] N/H ?=- Average N/H abundance (G1)
43- 50 F8.6 [-] e_N/H ?=- Uncertainty on N/H
52- 59 F8.6 [-] O/H ?=- Average O/H abundance (G1)
61- 63 F3.1 [-] e_O/H ?=- Uncertainty on O/H
65- 69 A5 --- PNPop [YOUNG OLD -] Assigned age group based on
the abundances (G2)
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- PNG PN name in the usual format: LLL.l+BB.b
14- 21 F8.6 [-] C/H ?=- Selected C/H abundance (G1)
32- 34 F3.1 [-] e_C/H ?=- Uncertainty on C/H
38- 45 F8.6 [-] N/H ?=- Average N/H abundance (G1)
47- 49 F3.1 [-] e_N/H ?=- Uncertainty on N/H
51- 58 F8.6 [-] O/H ?=- Average O/H abundance (G1)
60- 62 F3.1 [-] e_O/H ?=- Uncertainty on O/H
64- 68 A5 --- PNPop [YOUNG OLD -] Assigned age group based on
selected abundances (G2)
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Global notes:
Note (G1): Averages have been calculated on linear X/H, then reported in the
usual format log(X/H)+12. See paper for details on abundance selection.
Note (G2): See paper for details on PN age group criteria.
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Acknowledgements:
Beatrice Buccirelli, beatrice.bucciarelli(at)inaf.it
(End) Patricia Vannier [CDS] 25-Oct-2023