Searching for Balmer-dominated Type Ia Supernova Remnants in M33

We searched for Balmer-dominated Type Ia supernova remnants (SNRs) in M33 by selecting thermal X-ray sources with L X ≥ 5 × 10 35 erg s−1, identifying associated H emission features, and checking their [S ii] and [O iii] emission properties. Our search did not find any Balmer-dominated Type Ia SNRs...

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Bibliographic Details
Published in:The Astrophysical journal 2020-09, Vol.900 (2), p.149
Main Authors: Lin, Chris Ding-Jyun, Chu, You-Hua, Ou, Po-Sheng, Li, Chuan-Jui
Format: Article
Language:English
Subjects:
Astrophysics
Crystals
Delay time
Distribution functions
Emission
Galaxies
H alpha line
Interstellar
Interstellar medium
Ionization
Magellanic clouds
Metallicity
Spiral galaxies
Star & galaxy formation
Star formation
Supernova
Supernova remnants
Triangulum Galaxy
Type Ia supernovae
X ray sources
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Summary:We searched for Balmer-dominated Type Ia supernova remnants (SNRs) in M33 by selecting thermal X-ray sources with L X ≥ 5 × 10 35 erg s−1, identifying associated H emission features, and checking their [S ii] and [O iii] emission properties. Our search did not find any Balmer-dominated Type Ia SNRs in M33. This result is puzzling because M33 is 2-3 times more massive than the Large Magellanic Cloud (LMC), yet the LMC hosts five Balmer-dominated Type Ia SNRs and M33 has none. We have considered observational biases; interstellar densities and ionization conditions; the Type Ia SN rate expected from the star formation history and Type Ia SN delay time distribution function; and the metallicity effect. None of these can explain the absence of X-ray-bright Balmer-dominated Type Ia SNRs in M33. It is intriguing that the Galaxy has X-ray-bright and thermal Type Ia SNRs (Kepler and Tycho), as well as X-ray-faint and nonthermal Type Ia SNRs (G1.9+0.3, SN1006, and RCW86), while the LMC does not have the X-ray-faint and nonthermal ones and M33 does not have the X-ray-bright and thermal ones.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/abac68