HR 7578

HR 7578 is a triple star system in the constellation of Sagittarius. Their combined apparent magnitude is 6.18, making it very faintly visible to the naked eye of an observer under a dark sky, far from any city. Parallax measurements by the Gaia spacecraft put the system at 46 light-years away, making this a nearby system.
The two main stars of HR 7578 are fairly old, older than the Pleiades but possibly younger than the Hyades. The stars are between and years old. Both are K-type main-sequence stars. Both stars have a minimum mass of, and are unusually metal-rich, showing high amounts of cyanide and sodium in their spectra.
In 1982, Francis C. Fekel and Willet I. Beavers suggested that HR 7578 might be a variable star, based on their spectroscopic observations. James T. Hooten and Douglas S. Hall confirmed that the star's brightness varies, in 1990. It was given its variable star designation, V4200 Sagittarii, in 1993. HR 7578 is a BY Draconis variable. This is a class of variable star whose variability comes from starspots on the stars' surfaces. HR 7578 also has a common proper motion companion, 2MASS J19542064−2356398. It is a red dwarf that is at least 580 astronomical units from the central star system. There is another star that is separated about 40 away and is 4.4 magnitudes fainter, but is not physically associated with HR 7578.