HD 134060

During the NStars project, Grey et al. (2006) found a stellar classification of G0 V Fe+0.4 for this star, matching a Sun-like G-type main-sequence star with an overabundance of iron in its outer atmosphere. However, an older classification of G3 IV is still used, which would suggest it is instead a more evolved subgiant star. HD 134060 has an estimated 1.07 times the mass of the Sun and 1.15 times the Sun's radius. It is radiating 1.63 times the Sun's luminosity from its photosphere at an effective temperature of about 5,965 K.

The survey in 2015 have ruled out the existence of any additional stellar companions at projected distances from 22 to 163 astronomical units.

Planetary system

Based upon an 8-year survey using the HARPS spectrograph at La Silla Observatory, in 2011 the detection of a pair of planets orbiting this star were announced. The inner planet, HD 134060 b, is in a tight, eccentric orbit around the star with a period of just over three days. The second object, HD 134060 c, has a more leisurely period of around 3.2 years and a high orbital eccentricity.

The star was observed for a few hours by the Spitzer Space Telescope in the hopes of observing a transit by the inner planet, but none was detected. HD 134060 displays an infrared excess at a wavelength of 18μm, making it a warm debris disk candidate.