  Our discovery of 1SWASP J093010.78+533859.5 as a probable doubly eclipsing
quadruple system containing a contact binary with P~0.23 d and a detached
binary with P~1.31 d was announced in 2013. Subsequently Koo et al. confirmed
the detached binary spectroscopically and identified a fifth set of static
spectral lines at its location, corresponding to a further non-eclipsing
component of the system. Here we present new spectroscopic and photometric
observations, allowing confirmation of the contact binary and improved
modelling of all four eclipsing components. The detached binary is found to
contain components of masses 0.837(8) and 0.674(7) M_sol, with radii of
0.832(18) and 0.669(18) R_sol and effective temperatures of 5185(-20,+25) and
4325(-15,+20) K respectively, the contact system has masses 0.86(2) and
0.341(11) M_sol, radii of 0.79(4) and 0.52(5) R_sol respectively, and a common
T_eff of 4700(50) K. The fifth star is of similar temperature and spectral type
to the primaries in the two binaries. Long-term photometric observations
indicate the presence of a spot on one component of the detached binary, moving
at an apparent rate of approximately one rotation every two years. Both
binaries have consistent system velocities around -11 to -12 km/s, which match
the average radial velocity of the fifth star, consistent distance estimates
for both subsystems of d=78(3) and d=73(4) pc are also found, and (with some
further assumptions) of d=83(9) pc for the fifth star. These findings strongly
support the claim that both binaries (and very probably all five stars) are
gravitationally bound in a single system. The consistent angles of inclination
found for the two binaries (88.2(3) and 86(4) degrees) may also indicate that
they originally formed by fragmentation (~9-10 Gyr ago) from a single
protostellar disk and subsequently remained in the same orbital plane.
