All Figures

$\begin{figure} \par\includegraphics[width=15cm,clip]{5468fig1.eps} \end{figure}$ Figure 1: The relation between the flux from the CO(1-0) line and at 100 $\mu$ m, plotted as a full line, with the representative points of the single galaxies plotted with different symbols. The crosses at the upper left of the figures represent the mean errors for the fluxes in the whole sample. For comparison, the relation found by Bregman et al. (1992) for a sample of early-type galaxies is shown as a dotted line. The early-type galaxies and early spirals from E to Sb are plotted in the left panel, while the late spirals are plotted in the right panel.
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In the text

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{5468fig2.eps} \end{figure}$ Figure 2: Left: the X-ray luminosity plotted vs. blue luminosity, in solar units, for late-type, non-active galaxies. The relation corresponding to emission caused by discrete sources, indicated in Eq. (4) is plotted as a dotted line. Right: X-ray luminosity vs. FIR luminosity, in solar units for the late-type, non-active galaxies. The linear relation indicated in Eq. (7) is plotted as a dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{5468fig3.eps} \end{figure}$ Figure 3: Left: the X-ray luminosity plotted vs. blue luminosity, for early-type, non-active galaxies. The relation corresponding to emission caused by diffuse gas, valid for early-type galaxies and indicated in Eq. (10) is plotted as a full line. Right: X-ray luminosity vs. FIR luminosity for the early-type galaxies. The linear relation for late-type, non-active galaxies indicated in Eq. (7) is plotted as a dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{5468fig4.eps} \end{figure}$ Figure 4: Left: the X-ray luminosity plotted vs. blue luminosity for active galaxies, separated according to the type of activity. The relation corresponding to emission caused by diffuse gas, valid for early-type galaxies and indicated in Eq. (10) is plotted as a full line. Right: X-ray luminosity vs. FIR luminosity for the active galaxies. The linear relation for late-type galaxies indicated in Eq. (7) is plotted as a dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{5468fig5.eps} \end{figure}$ Figure 5: Top panel: the masses of stars (continuous line) and gas (dashed line) for the dynamical model of $1.6 \times 10^{11}~ M_{\odot}$ baryonic mass as a function of the number of virial radii. The virial radius for this model is about 300 kpc. Bottom panel: the same as the upper panel, but for the dynamical model of baryonic mass $3.5 \times 10^{9} ~M_{\odot}$ . For this model the virial radius is about 42 kpc.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5468fig6.eps} \end{figure}$ Figure 6: The averaged density profiles of gas and stars for the model of $1.6 \times 10^{11}~ M_{\odot}$ baryonic mass at the age of 13 Gyr. The continuous lines are the best fit obtained.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{5468fig7.eps} \end{figure}$ Figure 7: Basic quantities of the chemical models for a prototype early-type galaxy of $1.6 \times 10^{11} M_{\odot }$ baryonic mass as a function of the age. Top-left panel: the star formation rate obtained from the chemo-dynamical model of $1.6 \times 10^{11}~ M_{\odot}$ baryonic mass (SFR). Top-right panel: the evolution of the metallicity Z. Bottom-left panel: the masses for both the classical and the chemo-dynamical model of baryonic matter (thick and thin dashed lines), stars (thick and thin continuous lines), and gas (thick and thin dotted lines) are shown. The mass of gas and stars inside 25 kpc are also shown (open circles) for the age of 13 Gyr. Bottom-right panel: the fractional masses for both the models of stars (thick and thin continuous lines) and gas (thick and thin dotted lines) are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5468fig8.eps} \end{figure}$ Figure 8: The same as in Fig. 7, but for the model with total baryonic mass of $3.5 \times 10^{9} ~M_{\odot}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5468fig9.eps} \end{figure}$ Figure 9: $L_{\rm FIR}$ vs. $L{_{\rm X}}$ diagram as in Fig. 3, right panel, but with the values deduced for the two template models of the early-type galaxy (filled circles). The diamonds represent the E-S0 galaxies, the triangles the S0a-Sb galaxies. The masses of the two theoretical models are also indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5468fg10.eps} \end{figure}$ Figure 10: Models of the $1.6 \times 10^{11}~ M_{\odot}$ baryonic mass galaxy in the $L_{\rm FIR}$ vs. $L{_{\rm X}}$ diagram with the variation of the galactic radius (filled circles), the mass of stars (filled diamonds), and finally, the mass of gas (empty circles). We represented: E galaxies (empty diamonds), E/S0 galaxies (pluses), S0 galaxies (crosses), S0sgalaxies (empty squares), Sa-Sb (empty triangles).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5468fg11.eps} \end{figure}$ Figure 11: Models of the more massive galaxy of $1.6 \times 10^{11}~ M_{\odot}$ baryonic mass in the $L_{\rm FIR}$ vs. $L{_{\rm X}}$ diagram for various core radii $r_{\rm c}^{\rm stars}$ and $r_{\rm c}^{\rm gas}$ , plotted as filled circles. The thin arrows indicate the original model, while the thick arrows indicate the shift of the model for various core radii. We represented: E galaxies (empty diamonds), E/S0 galaxies (pluses), S0 galaxies (crosses), S0s galaxies (empty squares), Sa-Sb (empty triangles).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5468fg12.eps} \end{figure}$ Figure 12: $L_{\rm FIR}$ vs. $L{_{\rm X}}$ for galaxy models of spirals and starbursters. Five theoretical models, taken from Piovan et al. (2006b), are represented: three spirals (M 100, M 51 and NGC 6946) and two starbursters (Arp 220 and M 82). Different morphological types are plotted as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5468fg13.eps} \end{figure}$ Figure 13: Different adopted star formation histories for the model of $1.6 \times 10^{11}~ M_{\odot}$ baryonic mass. The SFHs of Piovan et al. (2006b) have been re-calculated for the same mass of the dynamical model. The upper panels represent two spiral-like SFHs, while lower panels show two starburst-like SFHs that peaked in the last million years.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5468fg14.eps} \end{figure}$ Figure 14: $L_{\rm FIR}$ vs. $L{_{\rm X}}$ for galaxy models of fixed $1.6 \times 10^{11}~ M_{\odot}$ baryonic mass for various SFHs (large circles and squares) or at fixed SFH for various masses from $1.6 \times 10^{8}~ M_{\odot}$ to $1.6 \times 10^{11}~ M_{\odot}$ (large filled diamonds). Large circles and squares represent, respectively, models with spiral-like SFH and starburst-like SFH. Large filled circles and squares are obtained using Eq. (4), while large open circles and squares depend on Eq. (10). Different morphological types are plotted as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5468fig6.eps} \end{figure}$	Figure 6: The averaged density profiles of gas and stars for the model of $1.6 \times 10^{11}~ M_{\odot}$ baryonic mass at the age of 13 Gyr. The continuous lines are the best fit obtained.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5468fig8.eps} \end{figure}$	Figure 8: The same as in Fig. 7, but for the model with total baryonic mass of $3.5 \times 10^{9} ~M_{\odot}$ .
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5468fig9.eps} \end{figure}$	Figure 9: $L_{\rm FIR}$ vs. $L{_{\rm X}}$ diagram as in Fig. 3, right panel, but with the values deduced for the two template models of the early-type galaxy (filled circles). The diamonds represent the E-S0 galaxies, the triangles the S0a-Sb galaxies. The masses of the two theoretical models are also indicated.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5468fg12.eps} \end{figure}$	Figure 12: $L_{\rm FIR}$ vs. $L{_{\rm X}}$ for galaxy models of spirals and starbursters. Five theoretical models, taken from Piovan et al. (2006b), are represented: three spirals (M 100, M 51 and NGC 6946) and two starbursters (Arp 220 and M 82). Different morphological types are plotted as in Fig. 11.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5468fg13.eps} \end{figure}$	Figure 13: Different adopted star formation histories for the model of $1.6 \times 10^{11}~ M_{\odot}$ baryonic mass. The SFHs of Piovan et al. (2006b) have been re-calculated for the same mass of the dynamical model. The upper panels represent two spiral-like SFHs, while lower panels show two starburst-like SFHs that peaked in the last million years.
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