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We present evidence for a 0.278(8) d (=6.7 h) orbital period in the X-raytransient GRS 1716-249 (=N Oph 93), based on a superhump modulation detectedduring the 1995 mini-outburst plus ellipsoidal variability in quiescence. Witha quiescent magnitude of r=23.19+-0.15 N Oph 93 is too faint to warrant a fulldynamical study through dedicated time-resolved spectroscopy. Instead, we applythe FWHM-K2 correlation to the disc Halpha emission line detected in GranTelescopio Canarias spectra and obtain K2=521+-52 km/s. This leads to a massfunction f(M)=4.1+-1.2 Msun, thus indicating the presence of a black hole inthis historic X-ray transient. Furthermore, from the depth of the Halpha troughand the quiescent light curve we constrain the binary inclination to i=61+-15deg, while the detection of superhumps sets an upper limit to the donor tocompact star mass ratio q=M2/M1<=0.25. Our de-reddened (r-i) colour isconsistent with a ~K6 main sequence star that fills its Roche lobe in a 0.278 dorbit. Using all this information we derive a compact object massM1=6.4+3.2-2.0 Msun at 68 per cent confidence. We also constrain the distanceto GRS 1716-249 to 6.9+-1.1 kpc, placing the binary ~0.8 kpc above the GalacticPlane, in support of a large natal kick.

The orbital period, black hole mass and distance to the X-ray transient GRS 1716-249 (=N Oph 93)