J/MNRAS/493/730 Infrared properties of planetary nebulae (Muthumariappan+, 2020)
Infrared properties of planetary nebulae with [WR] and wels central stars.
Muthumariappan C., Parthasarathy M.
<Mon. Not. R. Astron. Soc., 493, 730-746 (2020)>
=2020MNRAS.493..730M 2020MNRAS.493..730M (SIMBAD/NED BibCode)
ADC_Keywords: Planetary nebulae ; Stars, Wolf-Rayet ; Photometry, infrared
Keywords: stars: AGB and post-AGB - stars: evolution -
planetary nebulae: general
Abstract:
We report the infrared (IR) properties of planetary nebulae (PNe) with
Wolf-Rayet (WR) type and wels central stars known to date and compare
them with the IR properties of a sample of PNe with H-rich central
stars. We use near-, mid-, and far-IR photometric data from archives
to derive the IR properties of PNe. We have constructed IR
colour-colour diagrams of PNe using measurements from 2MASS, IRAS,
WISE, and Akari bands. [WR] PNe have a larger near-IR emission from
the hot dust component and also show a tendency for stronger 12µm
emission as compared to the other two groups. Cool asymptotic giant
branch dust properties of all PNe are found to be similar. We derived
the dust colour temperatures, dust masses, dust-to-gas mass ratios, IR
luminosities, and IR excess (IRE) of PNe for these three groups. [WR]
PNe and wels-PNe tend to have larger mean values for dust mass when
compared to the third group. The average dust-to-gas mass ratio is
found to be similar for the three groups of PNe. While there is a
strong correlation of dust temperature and IR luminosity with the age
for the three groups of PNe, the dust mass, dust-to-gas mass ratios,
and IRE are found to be non-varying as the PNe evolve. [WR] PNe and
wels-PNe show very similar distribution of excitation classes and also
show similar distribution with Galactic latitude.
Description:
All the data required for this study were taken from the literature.
The near-IR fluxes were calculated from the magnitudes at respective
wavelengths which were obtained from the 2MASS archive (Cutri et al.
2003tmc..book.....C 2003tmc..book.....C, Cat. II/246) archive. IRAS (Neugebauer et al.
1984ApJ...278L...1N 1984ApJ...278L...1N) fluxes at 12, 25, 60, and 100µm, and WISE
(Wright et al. 2010AJ....140.1868W 2010AJ....140.1868W) fluxes at 3.4, 4.6, 12, and
22µm were used to span the mid- and far-IR emission. In addition,
we have used archived fluxes from Akari (Ishihara et al.
2010A&A...514A...1I 2010A&A...514A...1I, Cat. II/297) at its 65-, 90-, 140-, and 160-µm
bands to trace the emission from cold dust down to ∼30K. The 2MASS and
Akari data used for this study are available at the NASA/IPAC Infrared
Science Archive.
Our sample of [WR] PNe and wels-PNe are from the catalogue of spectral
classification of CSPNe given by Weidmann & Gamen
(2011A&A...526A...6W 2011A&A...526A...6W, Cat. J/A+A/526/A6). We have taken the nebular
Hβ fluxes and electron densities from Stasinska & Szczerba
(1999A&A...352..297S 1999A&A...352..297S, Cat. J/A+A/352/297). Emission-line fluxes of
[OIII] and HeII are obtained from Strasbourg-ESO Catalogue of Galactic
PNe (Acker et al. 1992ESOPN...1....1A 1992ESOPN...1....1A, Cat. V/84). Distances to PNe in
our sample are from Frew, Parker & Bojicic (2016MNRAS.455.1459F 2016MNRAS.455.1459F).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 87 99 Nebular parameters derived for [WR] PNe
table3.dat 65 67 Nebular parameters derived for wels-PNe
table4.dat 67 100 Nebular parameters derived for normal PNe
--------------------------------------------------------------------------------
See also:
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
II/297 : AKARI/IRC mid-IR all-sky Survey (ISAS/JAXA, 2010)
J/A+A/526/A6 : Central stars of galactic planetary nebulae (Weidmann+, 2011)
J/A+A/352/297 : The dust content of planetary nebulae (Stasinska+, 1999)
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae
(Acker+, 1992)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Object name (LLL.l+BB.b)
12 I1 --- Ref ? Reference (G1)
14- 24 A11 --- Class Planetary nebula classification
26- 28 I3 K Td ? Dust colour temperature (G2)
30- 34 F5.2 10-4Msun Md ? Dust mass (G3)
36- 40 F5.2 10-4Msun e_Md ? Error on Md
42- 46 F5.2 10-3 md/mg ? Dust-to-gas mass ratio (G4)
48- 51 F4.2 10-3 e_md/mg ? Error on md/mg
53- 59 F7.2 Lsun LIR ? Infrared luminosity (G5)
61- 66 F6.1 Lsun e_LIR ? Error on LIR
68 A1 --- l_IRE Limit flag on IRE
70- 76 F7.2 --- IRE ? Infrared excess (G6)
78- 83 F6.2 --- e_IRE ? Error on IRE
85- 87 A3 --- Excclass ? Excitation class (G7)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Object name (LLL.l+BB.b)
12 I1 --- Ref ? Reference (G1)
14- 16 I3 K Td ? Dust colour temperature (G2)
18- 21 F4.2 10-4Msun Md ? Dust mass (G3)
23- 27 F5.3 10-4Msun e_Md ? Error on Md
29- 30 A2 --- l_md/mg [≥] Limit flag on md/mg
32- 36 F5.2 10-3 md/mg ? Dust-to-gas mass ratio (G4)
38- 42 F5.2 10-3 e_md/mg ? Error on md/mg
44- 47 I4 Lsun LIR ? Infrared luminosity (G5)
49- 52 I4 Lsun e_LIR ? Error on LIR
54- 57 F4.2 --- IRE ? Infrared excess (G6)
59- 62 F4.2 --- e_IRE ? Error on IRE
64- 65 I2 --- Excclass ? Excitation class (G7)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Object name (LLL.l+BB.b)
12 I1 --- Ref ? Reference (G1)
14- 16 I3 K Td ? Dust colour temperature (G2)
18- 21 F4.2 10-4Msun Md ? Dust mass (G3)
23- 26 F4.2 10-4Msun e_Md ? Error on Md6
28- 32 F5.2 10-3 md/mg ? Dust-to-gas mass ratio (G4)
34- 37 F4.2 10-3 e_md/mg ? Error on md/mg
39- 45 F7.2 Lsun LIR ? Infrared luminosity (G5)
47- 52 F6.1 Lsun e_LIR ? Error on LIR
54- 58 F5.2 --- IRE ? Infrared excess (G6)
60- 63 F4.2 --- e_IRE ? Error on IRE
65- 67 A3 --- Excclass ? Excitation class (G7)
--------------------------------------------------------------------------------
Global Notes:
Note (G1): Though, the ionic emission-line fluxes for most PNe were from
Acker et al. (1992ESOPN...1....1A 1992ESOPN...1....1A, Cat. V/84), for some PNe they are
taken from other published results. References as follows:
1 = Escudero & Costa (2001A&A...380..300E 2001A&A...380..300E, Cat. J/A+A/380/300)
2 = Garcia-Rojas et al. (2012A&A...538A..54G 2012A&A...538A..54G, Cat. J/A+A/538/A54)
3 = Phillips (2005MNRAS.361..283P 2005MNRAS.361..283P)
4 = Escudero, Costa & Macial (2004A&A...414..211E 2004A&A...414..211E)
5 = Balick et al. (1994ApJ...424..800B 1994ApJ...424..800B)
6 = Bohigas (2003RMxAA..39..149B 2003RMxAA..39..149B)
7 = Kwitter & Henry (2001ApJ...562..804K 2001ApJ...562..804K)
8 = Madsen et al. (2006IAUS..234..455M 2006IAUS..234..455M)
9 = Perinotto & Corradi (1998A&A...332..721P 1998A&A...332..721P, Cat. J/A+A/332/721)
Note (G2): We derived the characteristic dust colour temperatures Td of PNe
using their IRAS 25- and 60-µm fluxes
Note (G3): The total dust mass of a PN is calculated from the dust temperature
and flux at an IR band in the optically thin limit using the
following relation (Stasinska & Szczerba 1999A&A...352..297S 1999A&A...352..297S,
Cat. J/A+A/352/297):
Md=Fν(λ)D2/Qabs,νBν(Td)
See section 4.3 of the article for details.
Note (G4): The dust-to-gas mass ratios (md/mg) of PNe were calculated using
their IRAS fluxes at 25- and 60-µm bands. Reddening-corrected
nebular Hβ fluxes and the nebular electron temperatures and
densities which are required for estimating md/mg were taken from
the literature.
Note (G5): LIR of a PN is calculated using its IRAS fluxes at 25- and 60-µm
bands. We fitted a modified blackbody flux distribution function with
an emissivity index α=1, and integrated the whole curve to get
LIR.
Note (G6): The IR excess (IRE) represents the excess amount of LIR in terms of
what can be accounted by absorption of Lyα radiation produced
in the nebula. The IRE of a PN was calculated from its LIR and its
reddening corrected nebular Hβ flux using the relation given in
Stasinska & Szczerba (1999A&A...352..297S 1999A&A...352..297S, Cat. J/A+A/352/297;
equation 6)
Note (G7): The excitation class of a PN is an important parameter which
represents the nebular spectral class. It is related to several
parameters of the PN like the nebular structure, mass, chemical
compositions, and the temperature and luminosity of its central star
as discussed by Gurzadyan & Egikyan (1991Ap&SS.175...15G 1991Ap&SS.175...15G)
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 30-Mar-2023