 | Photometric vs. spectroscopic redshifts for galaxies in the cluster field and in the magnitude range $\mathrm{18\, \leq \, R_C\, \leq \, 24}$. Black dots represent spectroscopically confirmed members. The two horizontal lines indicate the $\mathrm{z_{phot}}$ range chosen for membership selection of the galaxies without z. Within this range only galaxies with chosen colors are selected as members. In this diagram these galaxies are indicated as red dots. Blue crosses are galaxies outside the spectroscopical and photometrical membership selections. |
 | Galaxy stellar mass as function of $\mathrm{R_C}$ magnitude for cluster members. The points are color coded according to their $\mathrm{B\,-\,R_C}$ color. The vertical dashed line represents the completeness magnitude of our sample, and the horizontal dashed line represents the corresponding completeness mass. |
 | Distribution of the sSFR for the total sample of cluster galaxies. The red curve represents the best-fit to this distribution with two Gaussians. |
 | Completeness of the $\mathrm{z_{phot}}$ sample as a function of the $\mathrm{R_C}$ magnitude, separately for red ($\mathrm{B\, -\, R_C} \geq 1.5$, red dots) and blue ($\mathrm{B\, -\, R_C} < 1.5$, blue diamonds) galaxies. The dashed line represents the adopted completeness as a function of $\mathrm{R_C}$ for the sample of passive members, and, down to $\mathrm{R_C}=23$, for the sample of SF members also. For $\mathrm{R_C}>23$, we adopt the same completeness used for brighter SF members. |
 | The membership correction factor $\mathrm{f_{M}}$ (see text) as a function of $\mste$ (left panel) and clustercentric radius R (right panel). We adopt a correction factor independent of $\mste$ and dependent on R, the same for the samples of passive (red dots) and SF (blue diamonds) members. |
 | SMF for passive and SF cluster members (red triangles and blue demi-circles, respectively) and their best-fit Schechter functions (red triple-dot-dashed and blue dashed lines). The sum of the two SMFs is shown as a solid violet line. Violet diamonds are the counts obtained by considering all cluster members. The points represent counts in bins of 0.2 dex in $\mste$ divided for the bin size, and the counts have been corrected for completeness and membership. The (1~$\sigma$) errors on the counts have been estimated via the bootstrap resampling procedure. |
 | Best-fit Schechter parameters $\mathrm{M^*}$ and $\mathrm{\alpha}$ and 1~$\sigma$ likelihood contours. |
 | SMFs of SF and passive galaxies in different cluster regions and in the field. Upper left (resp. right) panel: SMFs of SF (resp. passive) cluster galaxies beyond and within $\mathrm{r_{200}}$. Bottom left panel: SMFs of passive cluster galaxies in four different regions, defined by their distances from the cluster center (see text). Bottom right panel: SMFs of passive cluster galaxies in four different regions, defined by their local number densities. SMFs are normalized to the total number of galaxies contained in the respective samples. |
 | Best-fit Schechter parameters $\mathrm{M^*}$ and $\mathrm{\alpha}$ and 1~$\sigma$ likelihood contours, after marginalizing over the $\mathrm{\Phi^*}$ parameter for the SMFs of SF and passive galaxies in different cluster regions and in the field. The panels correspond one-to-one to those of Fig.~\ref{f:smfs}. |
 | Spatial distribution of cluster members. The local number density is color coded as indicated by the bar at the right side of the plot. Coordinates are in arcmin with respect to the position of the BCG, see Table~\ref{t:props}. Galaxies belonging to Regions (a), (b), (c), which are defined in Sect.~\ref{sss:dens}, are those inside the red, blue, and purple solid lines, respectively. Galaxies belonging to Region (d) are the outer points. |
 | The number ratio of giant galaxies ($\mathrm{\log \mste/\msun \geq 10.5}$) and subgiant galaxies ($\mathrm{\log \mste/\msun < 10.5}$), GSNR, for different samples of passive galaxies (red dots: Regions 1--4 and $\mathrm{R>r_{200}}$; magenta squares: Regions (a)--(d)) and SF galaxies (blue diamonds: within and outside the virial radius). For Regions (a)--(d) the point abscissae are set at the average clustercentric radii of the galaxies in the subsamples selected on the base of local density. The vertical dashed line indicates the location of $\mathrm{r_{200}}$. |
 | The stellar mass density profile (dots) and the number density profile (squares) and their best-fit projected NFW models (red and blue curves). The 1 $\sigma$ errors are shown, and evaluated using a bootstrap procedure. Both densities are space densities. The vertical dashed green line indicates the location of $\mathrm{r_{200}}$. |
 | Top panel: the ratio of the stellar mass density and number density profiles. Middle panel: the ratio of the total mass density and number density profiles. Bottom panel: the ratio of the stellar mass density and total mass density profiles. Dashed lines indicate 1 $\sigma$ confidence regions. All densities are volume densities. The vertical dash-dotted line indicates the location of $\mathrm{r_{200}}$. The horizontal gray area indicates the cosmic value of the stellar mass fraction at the cluster mean redshift and its 1$\mathrm{\sigma}$ uncertainty. |