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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2026
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2604.16882 |
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| _version_ | 1866910143305744384 |
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| author | Lazarević, S. Brose, R. Oskinova, L. M. Chernyakova, M. Dai, S. Kargaltsev, O. Freund, S. Maitra, C. Filipović, M. D. Edwards, P. G. Mellah, I. El Guo, Z. Osses, J. van Soelen, B. Potter, S. B. Kothes, R. Rowell, G. P. Velović, V. Ahmad, A. Ball, B. D. Burger-Scheidlin, C. Galvin, T. J. Gordon, Y. A. Hopkins, A. M. Leahy, D. Pritchard, J. West, J. |
| author_facet | Lazarević, S. Brose, R. Oskinova, L. M. Chernyakova, M. Dai, S. Kargaltsev, O. Freund, S. Maitra, C. Filipović, M. D. Edwards, P. G. Mellah, I. El Guo, Z. Osses, J. van Soelen, B. Potter, S. B. Kothes, R. Rowell, G. P. Velović, V. Ahmad, A. Ball, B. D. Burger-Scheidlin, C. Galvin, T. J. Gordon, Y. A. Hopkins, A. M. Leahy, D. Pritchard, J. West, J. |
| contents | In a search for low surface brightness radio nebulae using the ASKAP-EMU survey, we discovered a faint radio shell, G289.6+5.8, and its central point radio source at the position of the soft gamma-ray source IGR J11187-5438. The central radio source is spatially coincident with a previously known low-mass X-ray binary (LMXB) with an M-type donor star. However, the newly determined Gaia DR3 distance of 267 pc and correspondingly low X-ray luminosity (3 x 10e31 erg/s) cast doubt on the LMXB classification. Neither radio nor X-ray pulsations are detected. Chance-alignments between radio shell, central radio source, optical star, gamma-ray, and X-ray sources appear unlikely. By combining all currently available evidence, we conclude that G289.6+5.8 is a remnant of a low-energy core-collapse explosion of an intermediate mass star (~8Msun) in a binary system with an M-type secondary, which remained bound after the explosion. In this scenario, G289.6+5.8 is a supernova remnant, while the central gamma- and X-ray source is associated with a young neutron star driving a pulsar wind interacting with its M-type stellar companion, making IGR J11187-5438 a nascent spider-type X-ray binary. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2604_16882 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | A newly born spider system at the core of a radio shell: Evidence for a low-energy supernova Lazarević, S. Brose, R. Oskinova, L. M. Chernyakova, M. Dai, S. Kargaltsev, O. Freund, S. Maitra, C. Filipović, M. D. Edwards, P. G. Mellah, I. El Guo, Z. Osses, J. van Soelen, B. Potter, S. B. Kothes, R. Rowell, G. P. Velović, V. Ahmad, A. Ball, B. D. Burger-Scheidlin, C. Galvin, T. J. Gordon, Y. A. Hopkins, A. M. Leahy, D. Pritchard, J. West, J. High Energy Astrophysical Phenomena In a search for low surface brightness radio nebulae using the ASKAP-EMU survey, we discovered a faint radio shell, G289.6+5.8, and its central point radio source at the position of the soft gamma-ray source IGR J11187-5438. The central radio source is spatially coincident with a previously known low-mass X-ray binary (LMXB) with an M-type donor star. However, the newly determined Gaia DR3 distance of 267 pc and correspondingly low X-ray luminosity (3 x 10e31 erg/s) cast doubt on the LMXB classification. Neither radio nor X-ray pulsations are detected. Chance-alignments between radio shell, central radio source, optical star, gamma-ray, and X-ray sources appear unlikely. By combining all currently available evidence, we conclude that G289.6+5.8 is a remnant of a low-energy core-collapse explosion of an intermediate mass star (~8Msun) in a binary system with an M-type secondary, which remained bound after the explosion. In this scenario, G289.6+5.8 is a supernova remnant, while the central gamma- and X-ray source is associated with a young neutron star driving a pulsar wind interacting with its M-type stellar companion, making IGR J11187-5438 a nascent spider-type X-ray binary. |
| title | A newly born spider system at the core of a radio shell: Evidence for a low-energy supernova |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2604.16882 |