  We report spectroscopic and differential photometric observations of the
A-type system V482 Per that reveal it to be a rare hierarchical quadruple
system containing two eclipsing binaries. One has the previously known orbital
period of 2.4 days and a circular orbit, and the other a period of 6 days, a
slightly eccentric orbit (e = 0.11), and shallow eclipses only 2.3% deep. The
two binaries revolve around their common center of mass in a highly elongated
orbit (e = 0.85) with a period of 16.67 yr. Radial velocities are measured for
all components from our quadruple-lined spectra, and are combined with the
light curves and with measurements of times of minimum light for the 2.4 day
binary to solve for the elements of the inner and outer orbits simultaneously.
The line-of-sight inclination angles of the three orbits are similar,
suggesting they may be close to coplanar. The available observations appear to
indicate that the 6 day binary experiences significant retrograde apsidal
motion in the amount of about 60 degrees per century. We derive absolute masses
for the four stars good to better than 1.5%, along with radii with formal
errors of 1.1% and 3.5% for the 2.4 day binary and about 9% for the 6 day
binary. A comparison of these and other physical properties with current
stellar evolution models gives excellent agreement for a metallicity of [Fe/H]
= -0.15 and an age of 360 Myr.
