Proof of principle X-ray reflection mass measurement of the black hole in H1743−322.

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 |$12\pm 2~\text{M}_\odot {}$| (⁠|$1\sigma$| 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 |$a_*=0.47\pm 0.10$|⁠. 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. [ABSTRACT FROM AUTHOR]