Astronomy & Astrophysics

Table 1: Summary of the observations. For each observation, the epoch and observing wavelength is shown, together with the recovered binary separation (in both mas and AU for the assumed distance), position angle (measured anticlockwise from north), and flux ratio (typical uncertainty 10-20%). Where photometric calibration was performed, the individual magnitudes of the components are also given.
Table 2: Parameters of the various fitted orbits shown in Fig. 3. The parameters shown are the mass of the primary, mass of the secondary, major axis length, eccentricity, period, position angle of the ascending node (measured anticlockwise from north in the plane of the sky), inclination between the orbital plane and the plane of the sky, and the longitude of periastron, defined as the angle between the ascending node and the periastron measured in the plane of the true orbit and taken in the direction of the secondary's motion. All the orbits appear prograde on the sky. The last line, labelled "Straight Line'', shows the $\chi ^{2}$ for the best straight-line fit.
Table 3: Fitted parameters for HK Ori. A disk mass of $0.06~\ensuremath{M_\odot}$ is derived from these parameters. The parameters obtained by Hillenbrand et al. (1992) are given in italic when available.