  A 13x13 degree image of Balmer H-alpha emission at galactic latitude -65
degrees is presented. Sensitivity is limited in part by confusion: the
peak-to-valley anisotropy of the H-alpha surface brightness is 0.2 Rayleighs on
angular scales of 0.1 to 1.0 degrees. The morphology of the H-alpha emission is
similar to that of the 100 um emission previously observed by the Infrared
Astronomical Satellite (IRAS). A point-by-point comparison of the two shows a
marginally detected (3-sigma) positive correlation, rho = +0.14 (+-0.04). The
slope of the correlated components of the 100 um and H-alpha emissions is 1.26
(+0.45) (-0.32) MJy/sr/R. Using parameters from the literature, we predict that
emission from dust and ionized gas at high latitudes produces 3 times more
H-alpha emission per unit 100 um emission than does backscattering of H-alpha
emission from Galactic H II regions by dust at high latitude. Observations of
this type may allow us to distinguish between Galactic foreground and cosmic
background for both the free-free emission and the thermal dust emission
associated with the warm ionized medium of the Milky Way.
