J/A+A/700/A223 Discovery of seven extragalactic O-rich SNRs (Kravtsov+, 2025)
Discovery of young, oxygen-rich supernova remnants in PHANGS-MUSE galaxies.
Kravtsov T., Anderson J.P., Kuncarayakti H., Maeda K., Mattila S.
<Astron. Astrophys. 700, A223 (2025)>
=2025A&A...700A.223K 2025A&A...700A.223K (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Supernova remnants ; Spectroscopy
Keywords: supernovae: general - galaxies: ISM
Abstract:
Supernova remnants (SNRs) are the late stages of supernovae before
their merging into the surrounding medium. Oxygen-rich supernova
remnants represent a rare subtype with strong visible light oxygen
emission.
We present a new method to detect SNRs exploiting the capabilities of
modern visible-light integral-field units based on the shapes of the
SNR emission lines.
We search for unresolved shocked regions with broadened emission lines
using the medium-resolution integral-field spectrograph MUSE on the
Very Large Telescope. The spectral resolving power allows shocked
emission sources to be differentiated from photoionised sources based
on the linewidths.
We find 307 supernova remnants, including seven O-rich SNRs. For all
O-rich SNRs, we observe the [OIII]λλ4959,5007 emission
doublet. In addition, we observe emissions from
[OI]λλ6300,6364, [O II]λλ7320,7330,
Hα+[NII]λ6583 and [S II]λλ6717,6731 to
varying degrees. The linewidths for the O-rich SNRs are generally
broader than the rest of the SNRs in the sample of this article. The
oxygen emission complexes are reminiscient of SNR 4449-1 and some
long-lasting SNe. For the O-rich SNRs, we also search for counterparts
in archival data of other telescopes; we detect X-ray and mid-IR
counterparts for a number of remnants.
We have shown efficacy of the method to detect SNRs presented in this
article. In addition, the method is also effective in detecting the
rare O-rich SNRs, doubling the sample size in the literature. The
origin of O-rich SNRs and their link to specific SN types or
environments is still unclear, but further work into this new sample
will unquestionably help us shed light on these rare remnants.
Description:
In this appendix we present all of SNRs discovered in our survey of
PHANGS-MUSE galaxies. The selected lines are used in Fig. 3 as a
diagnostic tool to identify them as SNRs.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
appenb.dat 62 306 All of SNRs discovered in our survey of
PHANGS-MUSE galaxies
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Byte-by-byte Description of file: appenb.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Galaxy Galaxy name
9- 10 I2 --- SNRNo Supernova remnant number within the galaxy
12- 13 I2 h RAh Right Ascension (J2000)
15- 16 I2 min RAm Right Ascension (J2000)
18- 22 F5.2 s RAs Right Ascension (J2000)
24 A1 --- DE- Declination sign (J2000)
25- 26 I2 deg DEd Declination (J2000)
28- 29 I2 arcmin DEm Declination (J2000)
31- 35 F5.2 arcsec DEs Declination (J2000)
37- 44 E8.2 mW/m2 F([SII]) Flux of 6717,6731 doublet (erg/cm2/s)
46- 53 E8.2 mW/m2 F([NII]) Flux of [NII]6583 line (erg/cm2/s)
55- 62 E8.2 mW/m2 F(Ha) Flux of Ha6563 line (erg/cm2/s)
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Acknowledgements:
Timo Kravtsov, timokrav(at)gmail.com
(End) Patricia Vannier [CDS] 16-Apr-2025