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Lookup NU author(s): Dr Adam IngramORCiD
This work is licensed under a Creative Commons Attribution 4.0 International License (CC BY 4.0).
© 2024 The Author(s). The black hole X-ray binary H1743-322 lies in a region of the Galaxy with high extinction, and therefore it has not been possible to make a dynamical mass measurement. In this paper, we make use of a recent model which uses the X-ray reflection spectrum to constrain the ratio of the black hole mass to the source distance. By folding in a reported distance measurement, we are able to estimate the mass of the black hole to be 12 ± 2 M☉ (1σ credible interval). We are then able to revise a previous disc continuum fitting estimate of black hole spin a∗ (previously relying on a population mass distribution) using our new mass constraint, finding a∗ = 0.47 ± 0.10. This work is a proof of principle demonstration of the method, showing it can be used to find the mass of black holes in X-ray binaries.
Author(s): Nathan E, Ingram A, Steiner JF, Konig O, Dauser T, Lucchini M, Mastroserio G, van der Klis M, Garcia JA, Connors R, Kara E, Wang J
Publication type: Article
Publication status: Published
Journal: Monthly Notices of the Royal Astronomical Society
Year: 2024
Volume: 533
Issue: 2
Pages: 2441-2453
Print publication date: 01/09/2024
Online publication date: 08/08/2024
Acceptance date: 26/07/2024
Date deposited: 10/09/2024
ISSN (print): 0035-8711
ISSN (electronic): 1365-2966
Publisher: Oxford University Press
URL: https://doi.org/10.1093/mnras/stae1896
DOI: 10.1093/mnras/stae1896
Data Access Statement: The observational data used in this research are public and available for download from the HEASARC. The RELTRANS model package is publicly available, and the public version will soon be updated to include the RTDIST model used in this paper.
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