  Large-scale propagating fronts are frequently observed during solar
eruptions, yet it is open whether they are waves or not, partly because the
propagation is modulated by coronal structures, whose magnetic field we still
cannot measure. However, when a front impacts coronal structures, an
opportunity arises for us to look into the magnetic properties of both
interacting parties in the low-$\beta$ corona. Here we studied large-scale EUV
fronts accompanying three coronal mass ejections (CMEs), each originating from
a kinking rope-like structure in the NOAA active region (AR) 12371. These
eruptions were homologous and the surrounding coronal structures remained
stationary. Hence we treated the events as one observed from three different
viewing angles, and found that the primary front directly associated with the
CME consistently transmits through 1) a polar coronal hole, 2) the ends of a
crescent-shaped equatorial coronal hole, leaving a stationary front outlining
its AR-facing boundary, and 3) two quiescent filaments, producing slow and
diffuse secondary fronts. The primary front also propagates along an arcade of
coronal loops and slows down due to foreshortening at the far side, where local
plasma heating is indicated by an enhancement in 211 {\AA} (Fe XIV) but a
dimming in 193 {\AA} (Fe XII) and 171 {\AA} (Fe IX). The strength of coronal
magnetic field is therefore estimated to be $\sim\,$2 G in the polar coronal
hole and $\sim\,$4 G in the coronal arcade neighboring the active region. These
observations substantiate the wave nature of the primary front and shed new
light on slow fronts.
