Rediscussion of eclipsing binaries. Paper XX. HO Tel checkout

TL;DR

This paper provides a detailed analysis of the HO Tel eclipsing binary system using TESS light curves and radial velocity data, deriving stellar parameters and comparing them with theoretical models, highlighting minor discrepancies and future prospects.

Contribution

It offers the first comprehensive set of stellar parameters for HO Tel using combined photometric and spectroscopic data, and discusses the system's distance and model discrepancies.

Findings

Derived stellar masses and radii with high precision.

Distance measurement consistent with Gaia parallax.

Identified small discrepancies between observations and models.

Abstract

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: M_A = 1.906 +/- 0.031 Msun, M_B = 1.751 +/- 0.034 Msun, R_A = 2.296 +/- 0.027 Rsun and R_B = 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.