All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2106fig1.ps}\end{figure}$ Figure 1: The distribution of radio (squares) and field (diamonds, crosses) galaxies in the K-band Hubble diagram, compared to the predicted sequence of elliptical galaxies of masses 10 $^{12}~M_{\odot}$ ; the adopted redshift of formation is $z_{{\rm for}}$ = 30. Sequences with other masses and redshifts of formation were already tested in Rocca-Volmerange et al. (2004). The main emission lines from AGN appearing in the K band for 0 < z < 30 (H $_{\alpha }$ , [OIII]5007 Å + H $_{\beta }$ , [OII]3727 Å and Ly $_{\alpha }$ 1215 Å) are also plotted with a width of 10 Å at z = 0. Previous conclusions are unchanged: 10 $^{12}~M_{\odot}$ is the upper mass limit of galaxies and also the fragmentation limit predicted by the models.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2106fig2.ps}\end{figure}$ Figure 2: The observed energy distribution of 3CR galaxies by Andréani et al. (2002) (full blue line) in a large wavelength range ( $\lambda$ = 10³ to 10¹⁰ Å) is plotted with the stellar SED of the 10 $^{12}~M_{\odot}$ elliptical template (dotted green line) from PÉGASE and the synchrotron power law (full red line). The synchrotron radiation might contribute to the X-ray emission (see discussions on the so-called EXO (Extreme X-ray Objects) below).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2106fig3.ps}\end{figure}$ Figure 3: The three main fluxes contributing to the radiative energy of the 3CR radio galaxy sample are the elliptical SED (green line), the synchrotron power law (red line) and the two blackbody laws (pink lines) of respectively 340 K $\pm$ 50 K and 40 K $\pm$ 16 K. The dust emission (blue lines) is derived from the observations after subtraction of stellar + synchrotron emissions. For $\lambda >$ 3 $\times$ 10⁴ Å, the fit with the sum of two blackbody laws is robust (full line), while for $\lambda <$ 3 $\times$ 10⁴ Å, the peak at the temperature $\simeq$ 900 K (dashed line) is less accurate.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2106fig4.ps}\end{figure}$ Figure 4: Various stellar (blue color) dissipative rates ${\rm d}E/{\rm d}t$ in erg s^-1 as a function of time: stellar continuum (dashed light blue line), ionized gas from massive stars (dash-doubled dot violet line), cold dust depending on metals processed by stars (dashed blue line). Dissipative rates due to the AGN formed at 1 Gyr (pink/red color): ionized gas from AGN (dotted clear pink line), synchrotron (dashed-double dot pink line), hot dust (dashed-dot red line). The total dust emission is the pink full line and the sum of all rates is the full green line. The radiative energy from supernova explosions is too faint and has therefore not been plotted; the energy in neutrinos has not been taken into account.
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In the text