The Cosmic Web and galaxy evolution around the most luminous X-ray   cluster: RXJ1347.5-1145
  In this paper we study the large scale structures and their galaxy content around the most X-ray luminous cluster known, RX J1347.5-1145 at z=0.45. We make use of ugriz CFHT MEGACAM photometry and VIMOS VLT spectroscopy to identify structures around the RXJ1347 on a scale of 20x20 Mpc2. We construct maps of the galaxy distribution and the fraction of blue galaxies. We study the photometric galaxy properties as a function of environment, traced by the galaxy density. We identify group candidates based on galaxy overdensities and study their galaxy content. We also use available GALEX NUV imaging to identify strong unobscured star forming galaxies. We find that the large scale structure around RXJ1347 extends in the NE-SW direction for at least 20 Mpc, in which most of the group candidates are located. As other studies, we find that the fraction of blue galaxies (Fblue) is a function of galaxy number density, but the bulk of the trend is due to galaxies belonging to massive systems. The fraction of the UV-bright galaxies is also function of environment, but their relative numbers compared to the blue population seems to be constant regardless of the environment. These UV emitters also have similar properties at all galaxy densities, indicating that the transition between galaxy types occurs in short time-scales. Candidate galaxy groups show a large variation in their galaxy content and Fblue in those groups display little dependence with galaxy density. This may indicate possible differences in their evolutionary status or the processes that are acting in groups are different than in clusters. The large scale structure around rich clusters are dynamic places for galaxy evolution. In the case of RXJ1347 the transformation may start within infalling groups to finish with the removal of the cold gas once galaxies are accreted in massive systems. (ABRIDGED) 
M. Verdugo, M. Lerchster, H. Boehringer, H. Hildebrandt, B. L.   Ziegler, T. Erben, A. Finoguenov, and G. Chon
astro-ph.CO