Evidence for Type Ib/c origin of the supernova remnant G292.0+1.8
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| Main Authors: | , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866914957750173696 |
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| author | Narita, Takuto Uchida, Hiroyuki Vink, Jacco Katsuda, Satoru Umeda, Hideyuki Yoshida, Takashi Sato, Toshiki Matsunaga, Kai Tsuru, Takeshi Go |
| author_facet | Narita, Takuto Uchida, Hiroyuki Vink, Jacco Katsuda, Satoru Umeda, Hideyuki Yoshida, Takashi Sato, Toshiki Matsunaga, Kai Tsuru, Takeshi Go |
| contents | Circumstellar material (CSM) produced by mass loss from massive stars ($\gtrsim10 M_{\odot}$) through strong stellar winds or binary stripping provides rich information for understanding progenitors of core-collapse supernova remnants. In this paper we present a grating spectroscopy of a Galactic SNR G292.0+1.8, which is claimed to be a Type Ib/c remnant in a binary system according to recent studies. If G292.0+1.8 was experienced a strong mass-loss via binary interactions before its explosion, an oxygen-rich material produced in the He-burning layer is expected to be observed in the central belt-like structure formed by shock-heated CSM. Using the Reflection Grating Spectrometer onboard XMM-Newton, we detect N VII Ly$α$ line (0.50 keV) for the first time in G292.0+1.8 and find that the abundance ratio of nitrogen to oxygen is significantly lower (N/O$=0.5\pm0.1$) than the solar value. This low N/O suggests that the progenitor of experienced strong mass-loss and ended up to a Wolf-Rayet (WR) star exposing the He-burning layer at the pre-supernova. Comparing our result and the evolution models of single stars and binaries, we conclude that the progenitor of G292.0+1.8 experienced strong mass-loss enough to occur a Type Ib/c supernova. Our finding is another crucial piece of evidence for a stripped-envelope supernova such as Type Ib/c as the origin of G292.0+1.8. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2409_17542 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Evidence for Type Ib/c origin of the supernova remnant G292.0+1.8 Narita, Takuto Uchida, Hiroyuki Vink, Jacco Katsuda, Satoru Umeda, Hideyuki Yoshida, Takashi Sato, Toshiki Matsunaga, Kai Tsuru, Takeshi Go High Energy Astrophysical Phenomena Circumstellar material (CSM) produced by mass loss from massive stars ($\gtrsim10 M_{\odot}$) through strong stellar winds or binary stripping provides rich information for understanding progenitors of core-collapse supernova remnants. In this paper we present a grating spectroscopy of a Galactic SNR G292.0+1.8, which is claimed to be a Type Ib/c remnant in a binary system according to recent studies. If G292.0+1.8 was experienced a strong mass-loss via binary interactions before its explosion, an oxygen-rich material produced in the He-burning layer is expected to be observed in the central belt-like structure formed by shock-heated CSM. Using the Reflection Grating Spectrometer onboard XMM-Newton, we detect N VII Ly$α$ line (0.50 keV) for the first time in G292.0+1.8 and find that the abundance ratio of nitrogen to oxygen is significantly lower (N/O$=0.5\pm0.1$) than the solar value. This low N/O suggests that the progenitor of experienced strong mass-loss and ended up to a Wolf-Rayet (WR) star exposing the He-burning layer at the pre-supernova. Comparing our result and the evolution models of single stars and binaries, we conclude that the progenitor of G292.0+1.8 experienced strong mass-loss enough to occur a Type Ib/c supernova. Our finding is another crucial piece of evidence for a stripped-envelope supernova such as Type Ib/c as the origin of G292.0+1.8. |
| title | Evidence for Type Ib/c origin of the supernova remnant G292.0+1.8 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2409.17542 |