All Figures

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f01.eps} \end{figure}$ Figure 1: Time evolution of the different contributions to the gas binding energy in the bulge of a Milky Way like galaxy: dark matter halo (dashed line), bulge (dotted line), and exponential disk (solid line). In particular, $M_{\rm b} = 2\times 10^{10}~M_{\odot}$ , $R_{\rm e}=2$ kpc, $v_{\rm c}=200$ km s^-1, $M_{\rm d}=10^{11}~M_{\odot}$ , and $R_{\rm d}=4.3$ kpc.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f02A.eps}\par\includegraphics[width=8.8cm, clip, trim=0 275 0 30]{8663f02B.eps} \end{figure}$ Figure 2: Time evolution of the Eddington (dashed line) and Bondi (dot-dashed line) accretion rates for bulges with various masses. The thicker lines indicate the resulting accretion rate, which is assumed to be the minimum between the two.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f03A.eps}\par\includegraphics[width=8.8cm, clip, trim=0 275 0 30]{8663f03B.eps} \end{figure}$ Figure 3: Energy balance as a function of time for bulges with various masses. The figure shows the gas binding energy (solid line) compared to the thermal energy released by supernovae (dashed line) and the accreting black hole (dot-dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f04.eps} \end{figure}$ Figure 4: Star formation rate as a function of time and redshift for bulges with various masses. The peak value of the $M_{\rm b} =2 \times 10^9~M_{\odot}$ case is $\sim$ $40~ M_{\odot}$ /yr.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f05.eps} \end{figure}$ Figure 5: Final black-hole masses as a function of the bulge mass predicted by our models (triangles). The short dashed-long dashed line represents the measured relation of McLure & Dunlop (2002), the dotted line the one of Marconi & Hunt (2003), and the dashed line the one of Häring & Rix (2004).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f06.eps} \end{figure}$ Figure 6: Evolution with time and redshift of the bolometric luminosity emitted by the accreting BH for bulges of various masses. The dotted lines represent the range spanned by observations (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f07.eps} \end{figure}$ Figure 7: Evolution with time (bottom axis) and redshift (top axis) of the metallicity in solar units $Z/Z_{\odot }$ . The different curves denote different bulge masses as indicated in the upper left corner.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f08.eps} \end{figure}$ Figure 8: Evolution with time (bottom axis) and redshift (top axis) of the [Fe/H] abundance ratio in bulges of various masses, as indicated in the lower right corner.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=7.5cm]{8663f09A.eps}\includegrap... ...=7.5cm]{8663f09E.eps}\includegraphics[width=7.5cm]{8663f09F.eps} }\end{figure}$ Figure 9: Evolution with time and redshift of the [X/H] abundance ratios for $\alpha$ -elements (O, Mg, Si, and Ca), C and N in bulges of various masses. The discontinuity at $\sim$ $2\times 10^{8}$ yr in the [Si/H] and [Ca/H] and is due to the occurrence of the galactic wind, which shortly precedes the maximum in the type Ia SN rate. The thin lines in the [N/H] vs. time plot represent the results obtained by adopting primary nitrogen in massive stars, as in Matteucci (1986).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8663f10.eps} \end{figure}$ Figure 10: Correlation with bulge mass of the [X/Fe] abundance ratios for $z \protect\la 6$ for the $\alpha$ -elements O, Mg, Si, Ca.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8663f11.eps} \end{figure}$ Figure 11: Correlation with bulge mass of the [N/C] abundance ratio for $z \protect\la 6$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{8663f12A.eps}\vspace*{1mm} \par\i... ...12B.eps}\vspace*{1mm} \par\includegraphics[width=7cm]{8663f12C.eps} \end{figure}$ Figure 12: Evolution with time and redshift of the [X/H] abundance ratios for Fe, Mg, and N in bulges of various masses and the adoption of a Salpeter (1955) IMF above $1~M_{\odot}$ . The discontinuity at $\sim$ $3\times 10^{8}$ yr in the [Fe/H] and [Si/H] is due to the occurrence of the galactic wind, which shortly precedes the maximum in the type Ia SN rate.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f13.eps} \end{figure}$ Figure 13: Evolution of the predicted (U-B) ( upper panel) and (B-K) ( lower panel) colours for bulge models of three different masses (dotted line: $M_{\rm b} =2 \times 10^9~M_{\odot}$ ; solid line: $M_{\rm b} = 2\times 10^{10}~M_{\odot}$ ; dashed line: $M_{\rm b}=10^{11} ~M_{\odot}$ ), assuming an IMF with x₂ = 0.95.
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In the text

$\begin{figure}\includegraphics[width=8.8cm,clip,trim=0 0 0 -12]{8663f14.eps} \end{figure}$ Figure 14: Evolution of the predicted (U-B) ( upper panel) and (B-K) ( lower panel) colours for a bulge model of mass $M_{\rm b} = 2\times 10^{10}~M_{\odot}$ assuming two different IMFs. The solid lines represent the colours computed by assuming x₂=0.95, whereas the dotted lines are computed assuming x₂=1.35.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f15.eps} \end{figure}$ Figure 15: Predicted and observed colour-magnitude relation for bulges. The solid line and the dotted lines are the regression and the dispersion of CMR observed by Itoh & Ichikawa (1998), respectively. The solid circles and open squares are our predictions for the three bulge models studied in this paper, computed by assuming for the IMF x₂=0.95 and x₂=1.35, respectively. Panel b) R vs. (U-R) diagram. The open circles are the data by Peletier & Balcells (1996). Solid circles and open squares as in panel a). Panel c) R vs. (R-K) diagram. Open circles, solid circles, and open squares as in panel a).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8663f01.eps} \end{figure}$	Figure 1: Time evolution of the different contributions to the gas binding energy in the bulge of a Milky Way like galaxy: dark matter halo (dashed line), bulge (dotted line), and exponential disk (solid line). In particular, $M_{\rm b} = 2\times 10^{10}~M_{\odot}$ , $R_{\rm e}=2$ kpc, $v_{\rm c}=200$ km s^-1, $M_{\rm d}=10^{11}~M_{\odot}$ , and $R_{\rm d}=4.3$ kpc.
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$\begin{figure} \par\includegraphics[width=8.8cm]{8663f02A.eps}\par\includegraphics[width=8.8cm, clip, trim=0 275 0 30]{8663f02B.eps} \end{figure}$	Figure 2: Time evolution of the Eddington (dashed line) and Bondi (dot-dashed line) accretion rates for bulges with various masses. The thicker lines indicate the resulting accretion rate, which is assumed to be the minimum between the two.
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$\begin{figure} \par\includegraphics[width=8.8cm]{8663f03A.eps}\par\includegraphics[width=8.8cm, clip, trim=0 275 0 30]{8663f03B.eps} \end{figure}$	Figure 3: Energy balance as a function of time for bulges with various masses. The figure shows the gas binding energy (solid line) compared to the thermal energy released by supernovae (dashed line) and the accreting black hole (dot-dashed line).
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$\begin{figure} \par\includegraphics[width=8.8cm]{8663f04.eps} \end{figure}$	Figure 4: Star formation rate as a function of time and redshift for bulges with various masses. The peak value of the $M_{\rm b} =2 \times 10^9~M_{\odot}$ case is $\sim$ $40~ M_{\odot}$ /yr.
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$\begin{figure} \par\includegraphics[width=8.8cm]{8663f05.eps} \end{figure}$	Figure 5: Final black-hole masses as a function of the bulge mass predicted by our models (triangles). The short dashed-long dashed line represents the measured relation of McLure & Dunlop (2002), the dotted line the one of Marconi & Hunt (2003), and the dashed line the one of Häring & Rix (2004).
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$\begin{figure} \par\includegraphics[width=8.8cm]{8663f06.eps} \end{figure}$	Figure 6: Evolution with time and redshift of the bolometric luminosity emitted by the accreting BH for bulges of various masses. The dotted lines represent the range spanned by observations (see text for details).
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$\begin{figure} \par\includegraphics[width=8.8cm]{8663f07.eps} \end{figure}$	Figure 7: Evolution with time (bottom axis) and redshift (top axis) of the metallicity in solar units $Z/Z_{\odot }$ . The different curves denote different bulge masses as indicated in the upper left corner.
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$\begin{figure} \par\includegraphics[width=8.8cm]{8663f08.eps} \end{figure}$	Figure 8: Evolution with time (bottom axis) and redshift (top axis) of the [Fe/H] abundance ratio in bulges of various masses, as indicated in the lower right corner.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8663f10.eps} \end{figure}$	Figure 10: Correlation with bulge mass of the [X/Fe] abundance ratios for $z \protect\la 6$ for the $\alpha$ -elements O, Mg, Si, Ca.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8663f11.eps} \end{figure}$	Figure 11: Correlation with bulge mass of the [N/C] abundance ratio for $z \protect\la 6$ .
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$\begin{figure} \par\includegraphics[width=7cm]{8663f12A.eps}\vspace{1mm} \par\i... ...12B.eps}\vspace{1mm} \par\includegraphics[width=7cm]{8663f12C.eps} \end{figure}$	Figure 12: Evolution with time and redshift of the [X/H] abundance ratios for Fe, Mg, and N in bulges of various masses and the adoption of a Salpeter (1955) IMF above $1~M_{\odot}$ . The discontinuity at $\sim$ $3\times 10^{8}$ yr in the [Fe/H] and [Si/H] is due to the occurrence of the galactic wind, which shortly precedes the maximum in the type Ia SN rate.
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$\begin{figure} \par\includegraphics[width=8.8cm]{8663f13.eps} \end{figure}$	Figure 13: Evolution of the predicted (U-B) ( upper panel) and (B-K) ( lower panel) colours for bulge models of three different masses (dotted line: $M_{\rm b} =2 \times 10^9~M_{\odot}$ ; solid line: $M_{\rm b} = 2\times 10^{10}~M_{\odot}$ ; dashed line: $M_{\rm b}=10^{11} ~M_{\odot}$ ), assuming an IMF with x₂ = 0.95.
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$\begin{figure}\includegraphics[width=8.8cm,clip,trim=0 0 0 -12]{8663f14.eps} \end{figure}$	Figure 14: Evolution of the predicted (U-B) ( upper panel) and (B-K) ( lower panel) colours for a bulge model of mass $M_{\rm b} = 2\times 10^{10}~M_{\odot}$ assuming two different IMFs. The solid lines represent the colours computed by assuming x₂=0.95, whereas the dotted lines are computed assuming x₂=1.35.
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