J/MNRAS/493/2706 Dusty supernova remnants in the Galactic plane (Chawner+, 2020)
A complete catalogue of dusty supernova remnants in the Galactic plane.
Chawner H., Gomez H.L., Matsuura M., Smith M.W.L., Papageorgiou A., Rho J.,
Noriega-Crespo A., De Looze I., Barlow M.J., Cigan P., Dunne L., Marsh K.
<Mon. Not. R. Astron. Soc., 493, 2706-2744 (2020)>
=2020MNRAS.493.2706C 2020MNRAS.493.2706C (SIMBAD/NED BibCode)
ADC_Keywords: Supernova remnants ; Interstellar medium ; Milky Way ; Infrared ;
Millimetric/submm sources
Keywords: ISM: supernova remnants - infrared: ISM - submillimetre: ISM
Abstract:
We search for far-infrared (FIR) counterparts of known supernova
remnants (SNRs) in the Galactic plane (360° in longitude and
b=±1°) at 70-500µm with Herschel. We detect dust signatures
in 39 SNRs out of 190, made up of 13 core-collapse supernovae (CCSNe),
including 4 Pulsar Wind Nebulae (PWNe), and 2 Type Ia SNe. A further
24 FIR detected SNRs have unknown types. We confirm the FIR detection
of ejecta dust within G350.1-0.3, adding to the known sample of ∼10
SNRs containing ejecta dust. We discover dust features at the location
of a radio core at the centre of G351.2+0.1, indicating FIR emission
coincident with a possible Crab-like compact object, with dust
temperature and mass of Td=45.8K and Md=0.18M☉, similar to
the PWN G54.1+0.3. We show that the detection rate is higher among
young SNRs. We produce dust temperature maps of 11 SNRs and mass maps
of those with distance estimates, finding dust at temperatures
15~<Td~<40K. If the dust is heated by shock interactions the shocked
gas must be relatively cool and/or have a low density to explain the
observed low grain temperatures.
Description:
We searched for FIR counterparts of known supernova remnants (SNRs) in
the entire Galactic Plane, as surveyed by Herschel at 70-500µm, to
supplement the first-look catalogue of 71 SNRs studied by Chawner et
al. (2019MNRAS.483...70C 2019MNRAS.483...70C). Of 119 sources studied here, we find that
10 (8 per cent) have a clear FIR detection of dust associated with the
SNR. When combined with Chawner et al. (2019MNRAS.483...70C 2019MNRAS.483...70C), this
gives a total of 39 FIR detected sources out of 190 known remnants
with |b|=<1° across the entire Galactic Plane (a detection rate of
21 per cent): with dust signatures detected in the remnants of 13
core-collapse supernovae (SNe), including 4 Pulsar Wind Nebulae
(PWNe), and 2 Type Ia SNe. A further 24 are detected in sources with
unknown types.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 141 200 Supernova remnants in the Hi-GAL Survey
refs.dat 74 146 References for Table A1
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Supernova remnant name (GLLL.l+BB.b)
12- 33 A22 --- OName Alternative name
35- 42 A8 arcmin Size Radio size from Green's catalogue
(Green 2004BASI...32..335G 2004BASI...32..335G)
44 A1 --- PWN [?Y ] Indicates if the source contains an
associated PWN
46 A1 --- FIR [?YN ] Indicates if there is a FIR detection
of the PWN
48- 49 A2 --- l_Age [~=<> ] Limit flag on Age
51- 60 A10 kyr Age Age of the SNR
62- 78 A17 --- SNType Supernova type
80- 81 A2 --- Hi-GAL [1234i ] Level of detection for Herschel
Hi-GAL (1)
83 A1 --- C19 [Y ] Indicates if the source was studied in
Chawner et al. (2019MNRAS.483...70C 2019MNRAS.483...70C)
85-126 A42 --- Dust Location of FIR detected dust features
128-129 A2 --- Comp Waveband of previous detection to which FIR
structure is compared (O=optical, R=radio,
X=X-ray)
131-141 A11 --- Ref References for Age and SNType
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Note (1): Level of detection as follows:
1 = detection (FIR emission which is clearly correlated with radio, MIR, or
X-ray structure and can be distinguished from the ISM)
2 = possible detection (FIR emission in the region of the SNR, potentially
related to radio, MIR, or X-ray structure but confused with ISM)
3 = unlikely detection (detection of FIR emission which is probably
unrelated to the SNR)
4 = no detection of FIR emission
i = the only dust signatures associated with the SNR (via radio and/or
X-ray emission) are found in regions where the shell is known to be
interacting with a molecular cloud
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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- 3 I3 --- Ref [1/146] Reference number
5- 23 A19 --- BibCode BibCode
25- 55 A31 --- Aut Author's name
57- 74 A18 --- Com Comments
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 18-Apr-2023