The orbital period and inclination of the neutron star X-ray transient MAXI J1807+132
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| Autores principales: | , , , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| author | Saavedra, E. A. Muñoz-Darias, T. Torres, M. A. P. Yanes-Rizo, I. V. Padilla, M. Armas Álvarez-Hernández, A. Casares, J. Sánchez, D. Mata Rout, S. K. Navarro, S. |
| author_facet | Saavedra, E. A. Muñoz-Darias, T. Torres, M. A. P. Yanes-Rizo, I. V. Padilla, M. Armas Álvarez-Hernández, A. Casares, J. Sánchez, D. Mata Rout, S. K. Navarro, S. |
| contents | The neutron star X-ray transient MAXI J1807+132 has undergone outbursts in 2017, 2019, and 2023. We conducted an $R$-band time series photometry campaign using the Isaac Newton Telescope during the 2022 quiescent state. We detected a periodic variation in the light curve, consistent with ellipsoidal modulation, which allowed us to determine an orbital period of $P_{\rm orb} = 4.258 \pm 0.008$ hr. By modelling the light curve, we obtained a binary inclination of $ i = 72\pm5 \, °$ and a mass ratio $q = 0.24^{+0.19}_{-0.14}$ ($68$ per cent confidence level). Furthermore, our analysis supports an early M-dwarf companion that contributes between 30 and 50 per cent to the total flux in the $R$-band. We extend the previously established absolute magnitude versus orbital period correlation for black hole X-ray transients to neutron star systems. We applied the correlation to MAXI J1807+132, estimating its distance as $6.3 \pm 0.7$ kpc and its height above the Galactic plane to be $1.6 \pm 0.2$ kpc. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_20178 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The orbital period and inclination of the neutron star X-ray transient MAXI J1807+132 Saavedra, E. A. Muñoz-Darias, T. Torres, M. A. P. Yanes-Rizo, I. V. Padilla, M. Armas Álvarez-Hernández, A. Casares, J. Sánchez, D. Mata Rout, S. K. Navarro, S. High Energy Astrophysical Phenomena The neutron star X-ray transient MAXI J1807+132 has undergone outbursts in 2017, 2019, and 2023. We conducted an $R$-band time series photometry campaign using the Isaac Newton Telescope during the 2022 quiescent state. We detected a periodic variation in the light curve, consistent with ellipsoidal modulation, which allowed us to determine an orbital period of $P_{\rm orb} = 4.258 \pm 0.008$ hr. By modelling the light curve, we obtained a binary inclination of $ i = 72\pm5 \, °$ and a mass ratio $q = 0.24^{+0.19}_{-0.14}$ ($68$ per cent confidence level). Furthermore, our analysis supports an early M-dwarf companion that contributes between 30 and 50 per cent to the total flux in the $R$-band. We extend the previously established absolute magnitude versus orbital period correlation for black hole X-ray transients to neutron star systems. We applied the correlation to MAXI J1807+132, estimating its distance as $6.3 \pm 0.7$ kpc and its height above the Galactic plane to be $1.6 \pm 0.2$ kpc. |
| title | The orbital period and inclination of the neutron star X-ray transient MAXI J1807+132 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2508.20178 |