Notes. The presented sets of parameters correspond to the best-fit solutions from two approaches to shape modelling; in the “Light curve” column for the output of convex-light-curve inversion, and in the “Radar and light curve” column for a result of a global shape modelling that included both the radar and light-curve data. The table lists: the ecliptic coordinates of the rotation pole, longitude (λ) and latitude (β), the “Pole error” radius, the model epoch (T₀), the sidereal rotation period (P) with uncertainty (Δ_P), and the YORP spin-up factor (ν), which is an upper limit for the convex light-curve inversion and a quadratic fit to the phase offset measurements for the radar-derived constant-period solution. Due to the rotational pole location at low ecliptic latitude, the uncertainty in pole determination is given as a radius of a circle on the celestial sphere. The uncertainties in pole and period are given as standard deviation of the model within 10% increase of the minimum χ² value. The obliquity, the angle between the rotational pole of the asteroid and its orbital momentum, listed in the last row is calculated assuming an orbital inclination 5.3° and longitude of the ascending node 124.5° (JPL solution number 245 from the Horizons ephemeris system, https://ssd.jpl.nasa.gov/).