There is a magnitude 10.24 star at an angular separation of 29.7″ from the primary, along a position angle of 2° as of 2015. The Washington Double Star Catalog (2001) notes this is an "optical pair, based on study of relative motion of the components,"[8] whereas Eggleton and Tokovinin (2008) list it as a binary system.[9] However, astrometric measurements by the Gaia spacecraft confirm the companion is not gravitationally bound, with a measured parallax of 1.1416±0.0162 mas implying a distance around 876 pc (2,860 ly), as well as radically different proper motions.[10]
^ abHouk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H
^ abJohnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
^ abOttoni, G.; Udry, S.; Ségransan, D.; Buldgen, G.; Lovis, C.; Eggenberger, P.; Pezzotti, C.; Adibekyan, V.; Marmier, M.; Mayor, M.; Santos, N. C.; Sousa, S. G.; Lagarde, N.; Charbonnel, C. (2022-01-01), "CORALIE radial-velocity search for companions around evolved stars (CASCADES). I. Sample definition and first results: Three new planets orbiting giant stars", Astronomy and Astrophysics, 657: A87, arXiv:2201.01528, Bibcode:2022A&A...657A..87O, doi:10.1051/0004-6361/202040078, ISSN0004-6361.
