HD 111232 is a star in the southern constellation of Musca. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 7.59.^[2] The distance to this star is 94.5 light years based on parallax.^[1] It is drifting away from the Sun with a radial velocity of +104 km/s,^[2] having come to within 14.1 light-years some 264,700 years ago.^[9] The absolute magnitude of this star is 5.25,^[2] indicating it would have been visible to the naked eye at that time.

This is an ancient, thick disk population II^[10][7] star with an estimated age of twelve billion years.^[5] It is a G-type main-sequence star with a stellar classification of G8 V Fe-1.0,^[3] indicating an anomalous underabundance of iron in the stellar atmosphere. The star has 80% of the mass of the Sun and 88% of the Sun's radius. It is spinning slowly with a projected rotational velocity of 0.4 km/s.^[6] X-ray emission has not been detected, suggesting a low level of coronal activity.^[11][12] The star is radiating 70% of the luminosity of the Sun from its photosphere at an effective temperature of 5,648 K.^[5]

A superjovian planetary companion was detected by the CORALIE team, based on observations beginning in 2003.^[7][12] Planets around such metal-poor stars are rare (the only two known similar cases as of 2019 are HD 22781 and HD 181720).^[13] An astrometric measurement of the planet's inclination and true mass was published in 2022 as part of Gaia DR3.^[14] Later in 2022, these parameters were revised along with the detection of a second substellar companion, likely a brown dwarf.^[15]