Gamma Piscis Austrini
Gamma Piscis Austrini, Latinized from γ Piscis Austrini, is three-star system in the southern constellation of Piscis Austrinus. It is visible to the naked eye with a combined apparent visual magnitude of +4.448. Based upon an annual parallax shift of as seen from the Earth, the system is located about 216 light years from the Sun.
The A and B components, as of 2010, are separated by 4 arc seconds in the sky along a position angle of 255°. The "A" component is itself a binary, made up of two stars orbiting each other with an estimated orbital period of 15 years and a separation of nine astronomical units, with a combined apparent magnitude of 4.59. The component Aa has 2.65 times more mass than the Sun and 2.9 times its radius, being a chemically peculiar star with a spectral type. The Ab component is smaller, at 0.94 times the Sun's mass and 0.84 times its radius. The fainter magnitude 8.20 companion, component B, is an F-type main sequence star with a class of F5 V. It has 20% more mass than the Sun and a radius 15% larger.
Gamma Piscis Austrini is moving through the Galaxy at a speed of 24.1 km/s relative to the Sun. Its projected Galactic orbit carries it between and from the center of the Galaxy. It came closest to the Sun 1.8 million years ago at a distance of.
The current age of the system is 350 million years. It will become a triple white dwarf system within 14 billion years.