The double nature of this system was discovered by German astronomer Carl Rümker in 1835. As of 2016, the companion lay at an angular separation of 18.5″ along a position angle of 289° from the primary.[15] They form a co-moving pair with a projected separation of 1,566 AU.[16] The more luminous member is a B-type main-sequence star with a stellar classification of B9V.[13] Its fainter companion is an F-type main-sequence star with a class of F0Vn, where the 'n' suffix indicates that the metal absorption lines in its spectrum are unusual broad ("nebulous") and indicative of rapid rotation.[4][5] Based upon discrepancies in the proper motion measurements, there are hints of a third member of this system.[13]
^ abSkiff, B. A. (2014), "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009- )", VizieR On-line Data Catalog, Bibcode:2014yCat....1.2023S.
^ abGahm, G. F.; Ahlin, P.; Lindroos, K. P. (1983), "A study of visual double stars with early type primaries. I. Spectroscopic results", Astronomy and Astrophysics Supplement Series, 51: 143, Bibcode:1983A&AS...51..143G.
^ abcdDavid, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID33401607.
^Lindroos, K. P. (1985), "A study of visual double stars with early type primaries. IV Astrophysical data", Astronomy and Astrophysics Supplement Series, 60: 183, Bibcode:1985A&AS...60..183L.