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[Abridged] We searched for diffuse stellar emission around BCGs in three ofthe most X-ray luminous clusters found at z~0.3 in the REFLEX cluster surveyand observed with XMM-Newton. These systems (RXCJ0014.3-3022, RXCJ0232.2-4420,and RXCJ2308.3-0211) are in different dynamical states, as witnessed by theirX-ray morphology and optical appearence (e.g. multiplicity of BCGs). [Abridged]Diffuse stellar emission is robustly detected down to a surface brightness of26 R-mag/arcsec^2 (observed frame) around a total of seven BCGs, extending upto galactocentric distances of ~100 kpc. In particular, it surrounds a pair ofBCGs in RXCJ0232.2-4420, while it bridges two BCGs associated with the minorsubcomponent of the merging cluster RXCJ0014.3-3022. The diffuse light detectedat the greatest distances from the BCGs of the rather regular clustersRXCJ0232.2-4420 and RXCJ2308.3-0211 follows the ICM distribution. Its B-Rcolour is consistent with the colours measured within the BCG effective radii.The diffuse light around the two pairs of BCGs in RXCJ0014.3-3022 exhibitsbluer colours than the BCG central regions by up to 0.5 mag. If thecontribution of the intracluster light (ICL) to the detected diffuse lightaround BCGs is not negligible, ICL and BCGs have similar stellar populations inrelatively relaxed clusters. Merging on a cluster scale eventually addsgravitational stresses to BCGs and other galaxies in subcluster cores. Thisevent may affect the properties of the diffuse stellar emission around BCGs.Shredding of star-forming, low-metallicity dwarf galaxies is favoured as thecause of the bluer B-R colours of the diffuse stellar component around the twopairs of BCGs in the merging cluster RXCJ0014.3-3022.

Diffuse stellar emission in X-ray luminous galaxy clusters at z~0.3 I. Is the diffuse optical light boosted and rejuvenated in merging clusters?