Omega Andromedae (ω And, ω Andromedae) is the Bayer designation for a slowly co-rotating binary star system in the northern constellation of Andromeda. Parallax measurements made during the Gaia mission make this system to be approximately 93.9abbr=offNaNabbr=off from Earth. Its apparent visual magnitude is +4.83, which makes it bright enough to be seen with the naked eye.
The primary component has a stellar classification of F5 IVe. The IV luminosity class indicates that it is probably a subgiant star that is in the process of evolving away from the main sequence as the supply of hydrogen at its core depletes. However, Abt (1985) gives a classification of F3 V, suggesting it is an F-type main-sequence star. The measured angular diameter of the primary star is . At the system's estimated distance this yields a size of about 2.2 times that of the Sun. It is emitting about seven times solar luminosity from its outer atmosphere at an effective temperature of . This heat gives it the yellow-white-hued glow of an F-type star.
In 2008, the companion star was resolved using adaptive optics at the Lick Observatory. Later observations showed the magnitude difference between the two stars is 3.65 ± 0.03 and they are separated by 0.669 arcsecond. Abt (1985) lists the class as F5 V.