  We present the results of a wide-field spectroscopic analysis of the galaxy
population of the massive cluster MACSJ0717.5+3745 and the surrounding
filamentary structure (z=0.55), as part of our systematic study of the 12 most
distant clusters in the MACS sample. Of 1368 galaxies spectroscopically
observed in this field, 563 are identified as cluster members; of those, 203
are classified as emission-line galaxies, 260 as absorption-line galaxies, and
17 as E+A galaxies (defined by $\frac{H_{\delta}+H_{\gamma}}{2}>6$\AA and no
detection of [OII] and $H_{\beta}$ in emission). The variation of the fraction
of emission- and absorption-line galaxies as a function of local projected
galaxy density confirms the well-known morphology-density relation, and becomes
flat at projected galaxy densities less than $\sim 20Mpc^{-2}. Interestingly,
16 out of 17 E+A galaxies lie (in projection) within the ram-pressure stripping
radius around the cluster core, which we take to be direct evidence of
ram-pressure stripping being the primary mechanism that terminates
star-formation in the E+A population of galaxy clusters. This conclusion is
supported by the rarity of E+A galaxies in the filament which rules out galaxy
mergers as the dominant driver of evolution for E+A galaxies in clusters. In
addition, we find the 42 e(a) and 27 e(b) member galaxies, i.e., the
dusty-starburst and starburst galaxies respectively, to be spread out across
almost the entire study area. Their spatial distribution, which shows a strong
preference for the filament region, suggests that starbursts are triggered in
relatively low-density environments as galaxies are accreted from the field
population.
