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In the context of large scale structure formation, clusters of galaxies arelocated at the nodes of the cosmic web, and continue to accrete galaxies andgroups along filaments. They show sometimes a very large extension and apreferential direction. Brightest cluster galaxies (BCGs) are believed to growthrough the accretion of many small galaxies, and their structural propertiesare expected to vary with redshift. In some cases BCGs show an orientationcomparable to that of the cluster to which they belong. We analyse themorphological properties of 38 BCGs from the DAFT/FADA and CLASH surveys andcompare the position angles of their major axes to the direction of the clusterelongation at Mpc scale. The morphological properties of the BCGs were studiedby applying the GALFIT software to HST images and fitting the lightdistribution with one or two Sersic laws, or with a Nuker plus a Sersic law.The cluster elongations were estimated by computing density maps of redsequence galaxies. The analysis of the 38 BCGs shows that in 11 cases a singleSersic law is sufficient to account for the surface brightness, while for allthe other clusters two laws are necessary. For the outer Sersic component, theeffective radius increases with decreasing redshift, and the effective surfacebrightness decreases with effective radius, following the Kormendy law. Anagreement between the major axis of the BCG and the cluster elongation at largescale within +-30 deg is found for 12 clusters out of the 21 for which both PAscan be defined. The variation with redshift of the effective radius of theouter Sersic component agrees with the growing of BCGs by accretion of smallergalaxies from z=0.9 to 0.2. The directions of the elongations of BCGs and oftheir host clusters and large scale structures agree for 12 objects out of 21,implying that a larger sample is necessary to reach more definite conclusions.

The link between brightest cluster galaxy properties and large scale extensions of 38 DAFT/FADA and CLASH clusters in the redshift range 0.2