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We present a detailed analysis of the detached eclipsing binary system HO Telescopii, which contains two A-type stars in a circular orbit of period 1. 613 d. We use light curves from the Transiting Exoplanet Survey Satellite (TESS), which observed HO Tel in three sectors, to determine its photometric properties and a precise orbital ephemeris. We augment these results with radial velocity measurements from Surgit et al. to determine the masses and radii of the component stars: MA = 1. 906 +/- 0. 031 Msun, MB = 1. 751 +/- 0. 034 Msun, RA = 2. 296 +/- 0. 027 Rsun and RB = 2. 074 +/- 0. 028 Rsun. Combined with temperature measurements from Surgit et al. and optical-infrared apparent magnitudes from the literature, we find a distance to the system of 280. 8 +/- 4. 6 pc which agrees well with the distance from the Gaia DR3 parallax measurement. Theoretical predictions do not quite match the properties of the system, and there are small discrepancies in measurements of the spectroscopic orbits of the stars. Future observations from Gaia will allow further investigation of these issues.
J. Southworth (Fri,) studied this question.