J/MNRAS/543/3035 CSPNe extinctions (Csukai+, 2025)
Central-star extinctions towards planetary nebulae.
Csukai A., Zijlstra A.A., Mcdonald I., De Marco O.
<Mon. Not. R. Astron. Soc. 543, 3035 (2025)>
=2025MNRAS.543.3035C 2025MNRAS.543.3035C (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Extinction ; Planetary nebulae
Keywords: (stars:) binaries - (ISM:) dust, extinction -
planetary nebulae: general
Abstract:
Planetary nebulae (PNe) trace the hottest and most luminous phase of
evolution of solar-type stars. We use these hot, bright stars to
investigate extinctions towards a complete sample of 262 confirmed PNe
with large angular diameters, which have the most reliable photometry
and hottest central stars. For 162 of these PNe, we identify central
stars, produce spectral energy distributions from survey data using
pyssed, then fit reddened model spectra to the observed photometry to
obtain extinctions accurate down to E(B-V) of ±0.02mag. The
fitting is performed by Nelder-Mead χ2 minimization, with
uncertainties evaluated through MCMC. The catalogue of stellar
temperatures is updated for our sample for the calculation of
luminosities. The extinctions agree well with interstellar extinction.
We find evidence of circumnebular extinction for one PN, and evaluate
its effect on the PNe luminosity function. Four binaries are
identified from the spectral energy distributions. The binary fraction
in the full sample is between 23 per cent and 36 per cent. We use our
compiled data to evaluate the quality of the central star
identifications in the literature. Three objects in our sample have
previously been classified as post-RGB systems but we find that their
parameters may also be consistent with post-AGB evolution.
Description:
Extended tables of result tables contained within the paper. The CSPN
candidates identfied for each source within the sample are given along
with their reliability grades. The results of the extinction fitting
are given as both E(B-V) and Cbeta, alongside comparison values. A
compilation of literature CSPN temperatures is included.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 140 262 CSPN candidate IDs and reliability assessment
table3.dat 161 255 Extinction fit parameters to CSPN SEDs
table5.dat 113 56 Literature CSPN temperature compilation
refs.dat 64 35 References
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See also:
J/A+A/656/A51 : Planetary nebulae in Gaia EDR3 (Gonzalez-Santamaria+, 2021)
J/A+A/656/A110 : Gaia EDR3 planetary nebula central star distances
(Chornay+ 2021)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- PNG PN G identifier (from HASH)
13- 35 A23 --- Name PN name (from HASH)
37- 55 I19 --- CSPNID ? Gaia DR3 source ID for adopted CSPN
identification
57 I1 --- srcCSPN [0/3]? Source of adopted CSPN identification (1)
59- 62 A4 --- q_CSPNID ? Reliability grade for CSPN identification (G1)
64- 82 I19 --- CWID ? Gaia DR3 source ID for Chornay & Walton
(2021A&A...656A.110C 2021A&A...656A.110C, Cat. J/A+A/656/A110)
CSPN identification
84- 88 F5.3 --- q_CWID ? Reliability score from Chornay & Walton
(2021A&A...656A.110C 2021A&A...656A.110C, Cat. J/A+A/656/A110)
90-108 I19 --- GSID ? Gaia DR3 source ID for Gonzalez-Santamaria et
al. (2021A&A...656A..51G 2021A&A...656A..51G, Cat. J/A+A/656/A51)
CSPN identification
110 A1 --- q_GSID ? Reliability grade from Gonzalez-Santamaria et
al. (2021A&A...656A..51G 2021A&A...656A..51G, Cat. J/A+A/656/A51)
113-121 F9.3 pc Dist ? Distance computed by PySSED
123-130 F8.3 pc e_Dist ? Uncertainty in PySSED distance
132-135 I4 pc SBDist ? Surface brightness distance of Frew et al.
(2016MNRAS.455.1459F 2016MNRAS.455.1459F)
137-140 I4 pc e_SBDist ? Uncertainty of Frew et al.
(2016MNRAS.455.1459F 2016MNRAS.455.1459F) distance
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Note (1): Some sources lack any identification.
0 = Identified by this work
1 = Identified by Chornay & Walton (2021A&A...656A.110C 2021A&A...656A.110C)
2 = Identified by Gonzalez-Santamaria et al. (2021A&A...656A..51G 2021A&A...656A..51G)
3 = Identified in HASH
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- PNG PN G identifier (from HASH)
13- 35 A23 --- Name PN name (from HASH)
37- 55 I19 --- CSPNID Gaia DR3 source ID for adopted CSPN
identification
57- 60 A4 --- q_CSPNID Reliability grade for CSPN identification (G1)
62- 67 F6.3 mag E(B-V) ? E(B-V) fit by PySSED
69- 74 F6.3 mag b_E(B-V) ? Lower uncertainty bound on E(B-V) fit
76- 81 F6.3 mag B_E(B-V) ? Upper uncertainty bound on E(B-V) fit
83- 88 F6.3 --- Cbeta ? Extinction fit by PySSED expressed as Cbeta
90- 95 F6.3 --- b_Cbeta ? Lower uncertainty bound on C_beta
97-102 F6.3 --- B_Cbeta ? Upper uncertainty bound on C_beta
104-110 F7.3 --- chi2N ? Naive chi squared of best fit E(B-V)
assuming 5% errors on photometry
112-116 F5.3 --- errB ? Bootstrapped fractional errors by MCMC
118-122 F5.3 --- chi2B ? Chi squared calculated using bootstrapped
errors on photometry
124-125 I2 --- lenSED ? Number of SED points found by PySSED
127-135 F9.3 pc Dist ? Distance computed by PySSED
137-144 F8.3 pc e_Dist ? Uncertainty in PySSED distance
146-155 F10.3 [Lsun] lum100kK ? Luminosity calculated assuming a CSPN
temperature of 100kK
157-161 F5.3 mag GTE(B-V) ? E(B-V) from G-Tomo dust maps
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- PNG PN G identifier (from HASH)
12- 25 A14 --- Name PN name (from HASH)
27- 35 F9.3 [Lsun] lum100kK Luminosity calculated assuming a CSPN
temperature of 100 kK
37- 42 I6 [K] LTeff Literature temperature
44- 49 I6 [K] b_LTeff ? Lower uncertainty bound on literature
temperature
51- 56 I6 [K] B_LTeff ? Upper uncertainty bound on literature
temperature
58- 64 A7 --- r_LTeff Reference for literature temperature, in
refs.dat file
66- 73 F8.3 pc Dist Distance adopted for luminosity determination
75- 82 F8.3 pc e_Dist Uncertainty in adopted distance
84 I1 --- f_Dist [0/1] Source of the adopted distance (1)
86- 94 F9.3 [Lsun] lumTC Temperature corrected luminosity determination
96-103 F8.3 [Lsun] b_lumTC Lower uncertainty bound on temperature
corrected luminosity determination
105-113 F9.3 [Lsun] B_lumTC Upper uncertainty bound on temperature
corrected luminosity determination
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Note (1): Frew distance used when PySSED distance insufficiently accurate.
Code as follows:
0 = PySSED distances
1 = Surface brightness distance of Frewet al. (2016MNRAS.455.1459F 2016MNRAS.455.1459F)
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Ref Reference code
9- 27 A19 --- BibCode BibCode
35- 64 A30 --- Aut Author names
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Global notes:
Note (G1): Grading criteria discussed in the paper. 'A*OB' refers to candidates
dominated by a binary companion in the optical; the extinction fits are
unreliable for these sources.
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Acknowledgements:
Alexander Csukai, alexander.csukai(at)manchester.ac.uk
(End) Patricia Vannier [CDS] 10-Dec-2025