The binary mass ratio in the black hole transient MAXI J1820+070

Abstract

We present intermediate resolution spectroscopy of the optical counterpart to the black hole X-ray transient MAXI J1820+070 (=ASASSN-18ey) obtained with the OSIRIS spectrograph on the 10.4-m Gran Telescopio Canarias. The observations were performed with the source close to the quiescent state and before the onset of renewed activity in August 2019. We make use of these data and K-type dwarf templates taken with the same instrumental configuration to measure the projected rotational velocity of the donor star. We find $v_{rot}\sin i=84\pm 5$ km s${}^{-1}$ ($1-\sigma$), which implies a donor to black-hole mass ratio $q=M_2/M_1=0.072\pm 0.012$ for the case of a tidally locked and Roche-lobe filling donor star. The derived dynamical masses for the stellar components are $M_1=(5.95\pm 0.22){\sin }^{-3}i$ $M_{\odot }$ and $M_2=(0.43\pm 0.08){\sin }^{-3}i$ $M_{\odot }$. The use of $q$, combined with estimates of the accretion disk size at the time of the optical spectroscopy, allows us to revise our previous orbital inclination constraints to $66^{\circ }<i<81^{\circ }$. These values lead to 95% confidence level limits on the masses of $5.73<M_1(M_{\odot })<8.34$ and $0.28<M_2(M_{\odot })<0.77$. Adopting instead the $63\pm 3^{\circ }$ orientation angle of the radio jet as the binary inclination leads to $M_1=8.48_{-0.72}^{+0.79}{M}_{\odot }$ and $M_2=0.61_{-0.12}^{+0.13}{M}_{\odot }$ ($1-\sigma$).

arXiv comment8 pages, 2 figures. Accepted for publication in ApJL

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• Discovery of optical and infrared accretion disc wind signatures in the black hole candidate MAXI J1348-630
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• The origin of optical emission lines in the soft state of X-ray binary outbursts: the case of MAXI J1820+070
• A Phase-resolved View of the Low-frequency Quasiperiodic Oscillations from the Black Hole Binary MAXI J1820+070
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