Dynamical confirmation of a black hole in the X-ray transient Swift J1727.8-1613
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| Main Authors: | , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866917903877537792 |
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| author | Sanchez, D. Mata Torres, M. A. P. Casares, J. Munoz-Darias, T. Padilla, M. Armas Yanes-Rizo, I. V. |
| author_facet | Sanchez, D. Mata Torres, M. A. P. Casares, J. Munoz-Darias, T. Padilla, M. Armas Yanes-Rizo, I. V. |
| contents | The X-ray transient Swift J1727.8-1613 ended its 10-month discovery outburst on June of 2024, when it reached an optical brightness comparable to pre-discovery magnitudes. With the aim of performing a dynamical study, we launched an optical spectroscopy campaign with the GTC telescope. We detect the companion star and construct its radial velocity curve, yielding a binary orbital period of Porb = 10.8038 +- 0.0010 h and a radial velocity semi-amplitude of K2 = 390 +- 4 km/s. This results in a mass function of f(M1)=2.77 +- 0.09 Msun. Combined with constraints on the binary inclination, it sets a lower limit to the compact object mass of M1 > 3.12 +- 0.10 Msun, dynamically confirming the black hole nature of the accretor. Comparison of the average spectrum in the rest frame of the companion with synthetic stellar templates supports a K4V donor partially veiled (74%) by the accretion disc. A refined distance measurement of 3.7+- 0.3 kpc, together with the astrometric proper motion and the systemic velocity derived from the radial velocity curve (-181 +-4 km/s), supports a natal kick velocity of 220 +40 -50 km/s, at the upper end of the observed distribution. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2408_13310 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Dynamical confirmation of a black hole in the X-ray transient Swift J1727.8-1613 Sanchez, D. Mata Torres, M. A. P. Casares, J. Munoz-Darias, T. Padilla, M. Armas Yanes-Rizo, I. V. High Energy Astrophysical Phenomena The X-ray transient Swift J1727.8-1613 ended its 10-month discovery outburst on June of 2024, when it reached an optical brightness comparable to pre-discovery magnitudes. With the aim of performing a dynamical study, we launched an optical spectroscopy campaign with the GTC telescope. We detect the companion star and construct its radial velocity curve, yielding a binary orbital period of Porb = 10.8038 +- 0.0010 h and a radial velocity semi-amplitude of K2 = 390 +- 4 km/s. This results in a mass function of f(M1)=2.77 +- 0.09 Msun. Combined with constraints on the binary inclination, it sets a lower limit to the compact object mass of M1 > 3.12 +- 0.10 Msun, dynamically confirming the black hole nature of the accretor. Comparison of the average spectrum in the rest frame of the companion with synthetic stellar templates supports a K4V donor partially veiled (74%) by the accretion disc. A refined distance measurement of 3.7+- 0.3 kpc, together with the astrometric proper motion and the systemic velocity derived from the radial velocity curve (-181 +-4 km/s), supports a natal kick velocity of 220 +40 -50 km/s, at the upper end of the observed distribution. |
| title | Dynamical confirmation of a black hole in the X-ray transient Swift J1727.8-1613 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2408.13310 |