A refined dynamical mass for the black hole in the X-ray transient XTE J1859+226. Issue 1 (4th October 2022)

• Record Type: Journal Article
• Authors: Yanes-Rizo, I V; Torres, M A P; Casares, J; Motta, S E; Muñoz-Darias, T; Rodríguez-Gil, P; Armas Padilla, M; Jiménez-Ibarra, F; Jonker, P G; Corral-Santana, J M; Fender, R
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 517:Issue 1(2022)
• Page Start: 1476
• Page End: 1482
• Publication Date: 2022-10-04
• Subjects: accretion, accretion discs -- binaries: close -- stars: individual: XTE J1859+226 -- X-rays: binaries; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac2719
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We present two contiguous nights of simultaneous time-resolved Gran Telescopio Canarias spectroscopy and William Herschel Telescope photometry of the black hole X-ray transient XTE J1859+226, obtained in 2017 July during quiescence. Cross-correlation of the individual spectra against a late K-type spectral template enabled us to constrain the orbital period to 0.276 ± 0.003 d and the radial velocity semi-amplitude of the donor star to K 2 = 550 ± 59 km s −1 . An ellipsoidal modulation is detected in the photometric r - and i -band light curves, although it is strongly contaminated by flickering activity. By exploiting correlations between the properties of the double-peaked H α emission-line profile and the binary parameters, we derived an orbital inclination of 66.6 ± 4.3 deg, a refined K 2 = 562 ± 40 km s −1 and mass ratio q = M 2 / M 1 = 0.07 ± 0.01. From these values, we obtained an updated black hole mass of M 1 = 7.8 ± 1.9 M⊙ . An independent mass estimate based on X-ray timing agrees well with our value, which gives further support for the outburst quasi-periodic oscillation triplet being explained by the relativistic precession model. We also obtained a companion star mass M 2 = 0.55 ± 0.16 M⊙, which is consistent with its K5-K7 V spectral type.