![\begin{figure}
\par {\includegraphics[width=8.2cm,clip]{2068f1a.eps} }
\par\vspace*{4mm}
\par {\includegraphics[width=8.2cm,clip]{2068f1b.eps} }
\end{figure}](/articles/aa/full/2005/47/aa2068-04/img49.gif) |
Figure 1: Differential number counts in the I-band for all of our fields and separately for the mid-z and hi-z samples. Counts are given as the number per square degree per 0.5 mag bin. For comparison we also show deeper counts for the two Hubble Deep Fields (Metcalfe et al. 2001) and for the FORS Deep Field (Heidt et al. 2003) as well as shallower counts over a wider area from the COMBO-17 survey (private communication, see Wolf et al. 2003). The thin solid line connects median count values for the ten EDisCS fields in each plot. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par {\includegraphics[width=8.2cm,clip]{2068f2a.eps} }
{\includegraphics[width=8.2cm,clip]{2068f2b.eps} }
\end{figure}](/articles/aa/full/2005/47/aa2068-04/img50.gif) |
Figure 2: Errors in our "total'' I-band magnitudes and in our V-I colours are shown as a function of "total'' I-band magnitude for typical fields from our mid-z and hi-z samples. These values were derived from Monte Carlo evaluation of the background count variance in apertures of the size used to measure the actual galaxy magnitudes (see text for details). |
| Open with DEXTER | |
In the text
 |
Figure 4: "Total'' I-band apparent magnitudes and V-I colours of our BCG candidates are plotted against redshift. The lines in each plot are taken from a Bruzual & Charlot (2003) model which assumes passive evolution after a single, solar metallicity burst of star formation at z=3. The luminosity of the model is normalized so that at z=0 it reproduces the V-band absolute magnitude of NGC 4889, the brightest galaxy in the Coma cluster. In both plots, open symbols correspond to the clusters cl1059.2-1253 and cl1037.9-1243, for which we do not have a spectroscopic redshift for the object identified as BCG. In these cases, we use the cluster redshift. The filled squares correspond to the BCG candidates in the two additional structures away from the LCDCS detection in field 1103.7-1245. |
| Open with DEXTER | |
In the text
 |
Figure 3:
False colour images of the central regions of each of
our EDisCS fields. Each image is
and is centred
on our BCG candidate (except for cl1227.9-1138, see text). The images
are made by combining the seeing matched images in our three optical
bands with a colour stretch which maximizes the variation of image colour
with galaxy spectral energy distribution. These colour scales are the
same within the mid-z and within the hi-z sample but differ between
the two. In each image north is at the top and east is to the left.
Images of our mid-z sample in RA order are followed by images of our
hi-z sample also in RA order. |
| Open with DEXTER | |
In the text
 |
Figure 3: continued. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par {\includegraphics[width=15cm]{2068f5a.ps} }
\end{figure}](/articles/aa/full/2005/47/aa2068-04/img92.gif) |
Figure 5:
V-I versus I colour-magnitude diagrams
for galaxies projected within 1.0 Mpc of the BCG candidate (except for
cl1227.9-1138, see text) in each of our 20 EDisCS fields. Galaxies
for which our photometric redshift routines give a low probability of
being near the cluster redshift have been eliminated. The BCG candidate
itself is shown with a large cross. (Note that for cl1227.9-1138 the
BCG candidate is outside our 1 Mpc circle.) The expected position of the
red sequence is shown by a solid line, while a band within 
mag of this sequence is delineated by dashed lines. We use the
count of galaxies within this band and brighter than the vertical solid
line to estimate the richness of each cluster. Steeply slanting dashed
lines show 1, 3 and 
detection limits for our V-band
photometry. The final panel shows a colour-magnitude plot for the two
additional structures away from the LCDCS detection in the field
cl1103.7-1245. Filled circles represent here all the galaxies within
the largest square field for which we have both IR and optical data. |
| Open with DEXTER | |
In the text
 |
Figure 5: continued. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par {\includegraphics[width=15cm]{2068f6a.eps} }
\end{figure}](/articles/aa/full/2005/47/aa2068-04/img94.gif) |
Figure 6:
Adaptively smoothed isopleths for the surface
density of galaxies brighter than I =25 for a
EDisCS region centred on the BCG candidate (except for cl1227.9-1138,
see text) in each of our fields. Stars and galaxies with photometric
redshifts inconsistent with being close to the cluster redshift are
eliminated before contouring. The lowest contour level plotted
corresponds to 7.2 galaxies per square arcminute. Subsequent contours
correspond to further steps of 7.2 galaxies per square arcminute for
clusters cl1232.5-1250, cl1037.9-1243, cl1054.4-1146,
cl1054.7-1245 and cl1216.8-1201. In all other cases subsequent
contours correspond to steps of half this size. The position of our BCG
candidate is noted in each plot by a cross. As in Fig. 1,
north is at the top and east at the left of each map. The final panel
shows isopleths for the two additional structures away from the LCDCS
detection in the field cl1103.7-1245. |
| Open with DEXTER | |
In the text
 |
Figure 6: continued. |
| Open with DEXTER | |
In the text