14 Ewald Puchwein, Volker Springel, Debora Sijacki, & Klaus Dolag GLYPH<BC> GLYPH<B9>GLYPH<BD> GLYPH<B7>GLYPH<BD> GLYPH<BC> GLYPH<B9>GLYPH<BD> GLYPH<B7>GLYPH<BD> GLYPH<BC> GLYPH<B9>GLYPH<BD> GLYPH<B7>GLYPH<BD> GLYPH<BC> GLYPH<B9>GLYPH<BD> GLYPH<B7>GLYPH<BD> GLYPH<BC> GLYPH<B7>GLYPH<BD> GLYPH<B9>GLYPH<BD> GLYPH<BC> GLYPH<B7>GLYPH<BD> GLYPH<B9>GLYPH<BD> GLYPH<BC> GLYPH<B7>GLYPH<BD> GLYPH<B9>GLYPH<BD> GLYPH<BC> GLYPH<B7>GLYPH<BD> GLYPH<B9>GLYPH<BD>  GLYPH<D3>GLYPH<D1>GLYPH<D3> GLYPH<DA>GLYPH<CX>GLYPH<D2>GLYPH<CV>$^{GLYPH<C5>GLYPH<D4>}$$^{ GLYPH<BB>GLYPH<CW>}$  GLYPH<D3>GLYPH<D1>GLYPH<D3> GLYPH<DA>GLYPH<CX>GLYPH<D2>GLYPH<CV> GLYPH<C5>GLYPH<D4>  GLYPH<BB>GLYPH<CW> GLYPH<DE>GLYPH<BP>GLYPH<BC> GLYPH<DE>GLYPH<BP>GLYPH<BD> GLYPH<BT> GLYPH<BU> GLYPH<D7>GLYPH<D8>GLYPH<CP>GLYPH<D6>GLYPH<D7> GLYPH<CU>GLYPH<D6>GLYPH<D3>GLYPH<D1> GLYPH<BT> GLYPH<DE>GLYPH<BP>GLYPH<BC> GLYPH<D7>GLYPH<D8>GLYPH<CP>GLYPH<D6>GLYPH<D7> GLYPH<CU>GLYPH<D6>GLYPH<D3>GLYPH<D1> GLYPH<BU> GLYPH<DE>GLYPH<BP>GLYPH<BC> Figure 14. Distribution of stars in a 10 14 h − 1 M$_{⊙}$ cluster simulated with AGN feedback. The upper left panel shows the stars residing in the cluster’s satellite galaxies ( blue ), BCG ( green ), and ICL ( red ) at redshift z = 0. Grey dots indicate stars that are not part of the clusters FoF group at z = 0. Method 4 was used for making a distinction between BCG and ICL. The upper right panel shows the cluster’s progenitors at z = 1. All star particles are coloured as before, i.e. according to the component in which they end up at z = 0. The circles mark two infalling objects A and B. In the lower panels the positions of the stars that are part of A ( lower left ) and B ( lower right ) at z = 1 are shown at z = 0. Again they are coloured according to the component to which they are assigned at z = 0. All stars that are not part of A or B are show in grey in the lower panels . galaxy. This is illustrated in Fig. 16, which shows the frac- tion of stars that at z = 0 are still bound to a satellite galaxy as a function of the minimum distance of the galaxy’s or- bit from the cluster centre. The fractions are shown for all galaxies that fell into the progenitor of a 3 × 10 $^{14}$h − $^{1}$M ⊙ cluster between redshifts z = 1 . 5 and z = 1. In order to de- termine the minimum distance, the orbit of the galaxy and bound together in a satellite galaxy. Overall, about half of the stars in A end up in the BCG, while the other half be- comes part of the ICL. For object B, only about ∼ 10% of the stars are stripped and become intracluster stars. We have shown in Fig. 13 that the fraction of stars that gets stripped from an infalling galaxy depends on the galaxy’s mass. However, it also depends on the orbit of the c ○ 0000 RAS, MNRAS 000 , 000–000