Iota Apodis
Iota Apodis is a binary star system in the southern circumpolar constellation of Apus. Its identifier is a Bayer designation that is Latinized from ι Apodis, and abbreviated Iot Aps or ι Aps, respectively. This system is a faint target at an apparent visual magnitude of 5.41, but still visible to the naked eye from suitably dark skies. The distance to this star can be gauged from parallax measurements, yielding an estimate of with a 6% margin of error. The system is drifting closer with a heliocentric radial velocity of −4.3 km/s.
The dual nature of this system was announced by W. S. Finsen in 1960, who reported an angular separation of. Their orbit has an angular separation of 0.091 arcseconds with an estimated orbital period of 59.32 years and an eccentricity of 0.17. Both stars are B-type [main sequence star]s, which indicates they shine with a blue-white hue. The brighter component has a stellar classification of B9 V and an apparent magnitude 5.90, while the second member is a B9.5 V star with a magnitude of 6.46. They are about 3.89 and 3.45 times as massive as the Sun, respectively.