J/A+A/693/A247 SMGPS supernova remnant candidates images (Anderson+, 2025)
Supernova remnant candidates discovered by the SARAO MeerKAT
Galactic Plane Survey.
Anderson L.D., Camilo F., Faerber T., Bietenholz M., Bordiu C., Bufano F.,
Chibueze J.O., Cotton W.D., Ingallinera A., Loru S., Rigby A., Riggi S.,
Thompson M.A., Trigilio C., Umana G., Williams G.M.
<Astron. Astrophys. 693, A247 (2025)>
=2025A&A...693A.247A 2025A&A...693A.247A (SIMBAD/NED BibCode)
ADC_Keywords: Supernova remnants ; Radio sources
Keywords: H II regions - ISM: supernova remnants - radio continuum: ISM
Abstract:
Sensitive radio continuum data could bring the number of known
supernova remnants (SNRs) in the Galaxy more in line with what is
expected. Due to confusion in the Galactic plane, however, faint SNRs
can be challenging to distinguish from brighter HII regions and
filamentary radio emission. We exploited new 1.3GHz SARAO MeerKAT
Galactic Plane Survey (SMGPS) radio continuum data, which cover
251°<l<358° and 2°<l<61° at |b|<1.5°, to search
for SNR candidates in the Milky Way disk. We also used mid-infrared
data from the Spitzer GLIMPSE, Spitzer MIPSGAL, and WISE surveys to
help identify SNR candidates. These candidates are sources of extended
radio continuum emission that lack mid-infrared counterparts, are not
known as HII regions in the WISE Catalog of Galactic HII Regions, and
have not been previously identified as SNRs. We locate 237 new
Galactic SNR candidates in the SMGPS data. We also identify and
confirm the expected radio morphology for 201 objects classified in
the literature as SNRs and 130 previously identified SNR candidates.
The known and candidate SNRs have similar spatial distributions and
angular sizes. The SMGPS data allowed us to identify a large
population of SNR candidates that can be confirmed as true SNRs using
radio polarization measurements or by deriving radio spectral indices.
If the 237 candidates are confirmed as true SNRs, it would
approximately double the number of known Galactic SNRs in the survey
area, alleviating much of the discrepancy between the known and
expected populations.
Description:
Tables A.1-A.5 in the paper. Locations and sizes for SNR and SNR
candidates in the SMGPS area. Each source has the coordinates and
radius given. Previously identified sources use the source names in
the original publications, but the source centers and radii were
determined by-eye from SMGPS data assuming circular morphologies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
kgreen.dat 36 184 Known SNRs from the online Green catalog
(table A1)
ksnrcat.dat 36 30 Known SNRs from the online SNRCat
(table A2)
candid.dat 47 130 Previously identified SNR candidates
(table A3)
meerkatc.dat 39 237 SNR candidates identified from the SMGPS
(table A4)
meerkato.dat 36 49 Unusual sources in the SMGPS (table A5)
list.dat 131 693 List of fits images
fits/* . 693 Individual fits images
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Byte-by-byte Description of file: kgreen.dat ksnrcat.dat meerkat?.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Name Name (GLLL.l+B.b or GLLL.lll+BB.bbb)
17- 23 F7.3 deg GLON Galactic Longitude
25- 30 F6.3 deg GLAT Galactic Latitude
32- 35 F4.1 arcmin Rad Radius assuming circular morphology
37- 39 A3 --- Rel From I to III in decreasing reliability
(only for meerkatc.dat) (1)
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Note (1): Sources with I are the most reliable and have clear SMGPS emission
that is not confused with that of other SNRs or HII regions, with a morphology
that is similar to that of known SNRs; II sources are less reliable and are
either in confused regions with other SNRs or HII regions or have a morphology
that is slightly ambiguous; III sources are the least reliable and are badly
confused with other SNRs or HII regions, have spatially coincident radio and
MIR emission that may indicate that at least some of the radio emission is
thermal, or are incomplete shells.
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Byte-by-byte Description of file: candid.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Name as in the original publications
20- 26 F7.3 deg GLON Galactic Longitude
28- 33 F6.3 deg GLAT Galactic Latitude
35- 38 F4.1 arcmin Rad Radius assuming circular morphology
40- 47 A8 --- Ref Reference (1)
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Note (1): References as follows:
1 = Trushkin (2001, in ESA Special Publication, Vol. 459, Exploring the
Gamma-Ray Universe, ed. A. Gimenez, V. Reglero, & C. Winkler, 109-111)
2 = Brogan et al. (2006ApJ...639L..25B 2006ApJ...639L..25B)
3 = Helfand et al. (2006AJ....131.2525H 2006AJ....131.2525H, Cat. J/AJ/131/2525)
4 = Anderson et al. (2017A&A...605A..58A 2017A&A...605A..58A)
5 = Hurley-Walker et al. (2019PASA...36...48H 2019PASA...36...48H, see Cat. VIII/102))
6 = Maxted et al. (2019ApJ...885..129M 2019ApJ...885..129M)
7 = Bamba et al. (2003ApJ...589..253B 2003ApJ...589..253B)
8 = Dokara et al. (2018ApJ...866...61D 2018ApJ...866...61D)
9 = Sidorin et al. (2014A&A...565A...6S 2014A&A...565A...6S)
10 = Driessen et al. (2018ApJ...860..133D 2018ApJ...860..133D)
11 = Supan et al. (2018A&A...616A..98S 2018A&A...616A..98S)
12 = Dokara et al. (2021A&A...651A..86D 2021A&A...651A..86D, Cat. J/A+A/651/A86)
13 = Whiteoak & Green (1996A&AS..118..329W 1996A&AS..118..329W, Cat. J/A+AS/116/329)
14 = Ball et al. (2023MNRAS.524.1396B 2023MNRAS.524.1396B)
15 = Sushch et al. (2017A&A...605A.115S 2017A&A...605A.115S)
16 = Kaplan et al. (2002ApJ...566..378K 2002ApJ...566..378K)
17 = Gaensler et al. (2001ApJ...559..963G 2001ApJ...559..963G)
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Name
20 A1 --- --- [G]
21- 29 F9.5 deg GLON Gagalcitc longitude of center (J2000)
30- 38 F9.5 deg GLAT Galactic latitude of center (J2000)
40- 43 I4 --- Nx Number of pixels along X-axis
45- 48 I4 --- Ny Number of pixels along Y-axis
50- 59 A10 "datime" Obs.date Observation date
61- 66 I6 Kibyte size Size of FITS file
68-106 A39 --- FileName Name of FITS file, in subdirectory fits
108-131 A24 --- Title Title of the FITS file
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Acknowledgements:
Loren Anderson, loren.anderson(at)mail.wvu.edu
(End) Patricia Vannier [CDS] 09-Dec-2024