The spin measurement of the black hole in 4U 1543-47 constrained with the X-ray reflected emission

Abstract

4U 1543-47 is a low-mass X-ray binary that harbours a stellar-mass black hole located in our Milky Way galaxy. In this paper, we revisit seven data sets that were in the Steep Power Law state of the 2002 outburst. The spectra were observed by the Rossi X-ray Timing Explorer. We have carefully modelled the X-ray reflection spectra and made a joint-fit to these spectra with relxill for the reflected emission. We found a moderate black hole spin, which is 0.67^(+0.15)_(−0.08) at 90 per cent statistical confidence. Negative and low spins (<0.5) at more than 99 per cent statistical confidence are ruled out. In addition, our results indicate that the model requires a supersolar iron abundance: 5.05^(+1.21)_(−0.26), and the inclination angle of the inner disc is 36.3^(+5.3)_(−3.4) deg. This inclination angle is appreciably larger than the binary orbital inclination angle (∼21 deg); this difference is possibly a systematic artefact of the artificially low density employed in the reflection model for this X-ray binary system.

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