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Clusters of galaxies are at the intersection of cosmic filaments and arestill accreting galaxies and groups along these preferential directions, but,because of their relatively low contrast on the sky, they are difficult todetect (unless a large amount of spectroscopic data are available), andunambiguous detections have been limited until now to relatively low redshifts(z<0.3). We searched for extensions and filaments around the thirty clusters ofthe DAFT/FADA survey (redshift range 0.4<z<0.9) with deep wide fieldphotometric data. For each cluster, based on a colour-magnitude diagram, weselected galaxies that were likely to belong to the red sequence, and hence tobe at the cluster redshift, and built density maps. By computing the backgroundfor each map and drawing 3sigma contours, we estimated the elongations of thestructures detected in this way. Whenever possible, we identified the otherstructures detected on the density maps with clusters listed in NED. We foundclear elongations in twelve clusters, with sizes reaching up to 7.6 Mpc. Elevenother clusters have neighbouring structures, but the zones linking them are notdetected in the density maps at a 3sigma level. Three clusters show no extendedstructure and no neighbours, and four clusters are of too low contrast to beclearly visible on our density maps. The simple method we have applied appearsto work well to show the existence of filaments and/or extensions around anumber of clusters in the redshift range 0.4<z<0.9. We plan to apply it toother large cluster samples such as the clusters detected in the CFHTLS andSDSS-Stripe 82 surveys in the near future.

Searching for filaments and large-scale structure around DAFT/FADA clusters