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| Main Authors: | , , , , , , |
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| Format: | Preprint |
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2024
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| Online Access: | https://arxiv.org/abs/2410.22073 |
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| _version_ | 1866909370585972736 |
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| author | Venkattu, Deepika Lundqvist, Peter Torres, Miguel Pérez Bonnassieux, Etienne Tasse, Cyril Melchior, Anne-Laure Combes, Francoise |
| author_facet | Venkattu, Deepika Lundqvist, Peter Torres, Miguel Pérez Bonnassieux, Etienne Tasse, Cyril Melchior, Anne-Laure Combes, Francoise |
| contents | We present the first LOFAR image of the centre of M31 at a frequency of 150 MHz. We clearly detect three supernova remnants, which, along with archival VLA data at 3 GHz and other published radio and X-ray data allows us to characterize them in detail. Our observations also allow us to obtain upper limits the historical SN 1885A which is undetected even at a low frequency of 150 MHz. From analytical modelling we find that SN 1885A will stay in its free-expansion phase for at least another couple of centuries. We find an upper limit of $n_{\rm H}~\lesssim 0.04$ cm$^{-3}$ for the interstellar medium of SN 1885A, and that the SN ejecta density is not shallower than $\propto r^{-9}$ (on average). From the $2.6σ$ tentative detection in X-ray, our analysis shows that non-thermal emission is expected to dominate the SN 1885A emission. Comparing our results with those on G1.9+0.3, we find that it is likely that the asymmetries in G1.9+0.3 make it a more efficient radio and X-ray emitter than SN 1885A. For Braun 80, 95 and 101, the other remnants in this region, we estimate ages of 5200, 8100, and 13,100 years, and shock speeds of 1150, 880, and 660 km s$^{-1}$}, respectively. Based on this, the supernova rate in the central 0.5 kpc $\times$ 0.6 kpc of M31 is at least one per $\sim 3000~{\rm yr}$. We estimate radio spectral indices of $-0.66\pm0.05$, $-0.37\pm0.03$ and $-0.50\pm0.03$ for the remnants, respectively, which match fairly well with previous studies. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_22073 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | SN 1885A and supernova remnants in the centre of M31 with LOFAR Venkattu, Deepika Lundqvist, Peter Torres, Miguel Pérez Bonnassieux, Etienne Tasse, Cyril Melchior, Anne-Laure Combes, Francoise High Energy Astrophysical Phenomena We present the first LOFAR image of the centre of M31 at a frequency of 150 MHz. We clearly detect three supernova remnants, which, along with archival VLA data at 3 GHz and other published radio and X-ray data allows us to characterize them in detail. Our observations also allow us to obtain upper limits the historical SN 1885A which is undetected even at a low frequency of 150 MHz. From analytical modelling we find that SN 1885A will stay in its free-expansion phase for at least another couple of centuries. We find an upper limit of $n_{\rm H}~\lesssim 0.04$ cm$^{-3}$ for the interstellar medium of SN 1885A, and that the SN ejecta density is not shallower than $\propto r^{-9}$ (on average). From the $2.6σ$ tentative detection in X-ray, our analysis shows that non-thermal emission is expected to dominate the SN 1885A emission. Comparing our results with those on G1.9+0.3, we find that it is likely that the asymmetries in G1.9+0.3 make it a more efficient radio and X-ray emitter than SN 1885A. For Braun 80, 95 and 101, the other remnants in this region, we estimate ages of 5200, 8100, and 13,100 years, and shock speeds of 1150, 880, and 660 km s$^{-1}$}, respectively. Based on this, the supernova rate in the central 0.5 kpc $\times$ 0.6 kpc of M31 is at least one per $\sim 3000~{\rm yr}$. We estimate radio spectral indices of $-0.66\pm0.05$, $-0.37\pm0.03$ and $-0.50\pm0.03$ for the remnants, respectively, which match fairly well with previous studies. |
| title | SN 1885A and supernova remnants in the centre of M31 with LOFAR |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2410.22073 |