It has an apparent magnitude of 6.27,[2] placing it near the limit for naked eye visibility, even under ideal conditions.
Gaia DR3 parallax measurements imply a distance of 373 light-years and it is currently receding with a heliocentric radial velocity of 15.5 km/s.
[5] The binarity of the system was first noticed in a 1996 United States Naval Observatory survey.
[14] A Hipparcos proper motion survey published in 2006 catalogued the primary as a probable astrometric binary with an 89.6% chance.
[14] The visible component has a stellar classification of B9 V,[3] indicating that it is an ordinary B-type main-sequence star that is generating energy via hydrogen fusion.