Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[height=5.5cm]{1068f1.ps}\end{figure}$ Figure 1: Evolution with redshift of the ultraviolet background radiation intensity.
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In the text

$\begin{figure} \par\includegraphics[height=6.cm]{1068f2a.ps} \includegraphics[height=6.cm]{1068f2b.ps} \includegraphics[height=6.cm]{1068f2c.ps}\end{figure}$ Figure 2: Isocontours of the baryonic mass fraction per interval of the baryonic density contrast and per interval of temperature computed for the G1 and GP simulations at z=0 and for GNE at z=5 ( top, middle and bottom panels, respectively). The increase in the mass fraction scales from dark to light. Note that G1 and GNE are, for these plots, computed without galaxy formation. Solid curves on the top panel show the ratios $t_{\rm cool}/t_{\rm ff}=0.1$ , 1, 10.
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In the text

$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f3.ps}\end{figure}$ Figure 3: Evolution with redshift of the cosmic "stellar'' mass formation rate density for the G1 (dashed line), G0 (dot-dashed line) and GP (dotted line) simulations. The observational data of the star formation rate density are overplotted for our cosmology: H $\alpha$ data: Gallego et al. (1995) (filled circle), Tresse & Maddox (1998) (filled triangle), Yan et al. (1999) (filled star), Hopkins et al. (2000) (hollow diamond); UV data: Connolly et al. (1997) (open square), Treyer et al. (1998) (open triangle), Steidel et al. (1999) (open circle), Sullivan et al. (2000) (diamond); FIR data: Rowan-Robinson et al. (1997) (heavy cross), Flores et al. (1999) (cross); 1.4 GHz data: Condon (1989) (filled square), Haarsma et al. (2000) (six-pointed star), Serjeant et al. (2002) (open star). UV data and data by Gallego et al. (1995) are corrected forextinction.
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In the text

$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f4.ps}\end{figure}$ Figure 4: Same as Fig. 3 but for a SCDM scenario, for the G1 (dashed line) and G0 (dot-dashed line) simulations. The observation points are the same as described in Fig. 3 but overplotted for a SCDM cosmology.
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f15.ps}\end{figure}$ Figure 5: Evolution with redshift of the baryonic mass fractions computed in different temperature ranges, for the G0 simulation but without galaxy formation: $T<9\times 10^3$ K ("diffuse'', dot-dot-dashed line), $9\times 10^3 \leq T< 2\times 10^4$ K ("cold'', dashed line), $2\times 10^4 \leq T< 5\times 10^5$ K ("warm'', dot-dashed line), $T \geq 5\times 10^5$ K ("hot'', dotted line).
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f16.ps}\end{figure}$ Figure 6: Same as Fig. 5, but for the G1 simulation without galaxyformation.
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In the text

$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f5a.ps}\par\includegraphics[height=8cm, angle=-90]{1068f5b.ps}\end{figure}$ Figure 7: Galaxy-like object mass function at different redshifts for the G0 simulation.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=7.5cm, angle=-90]{1068f6a.ps}\h... ...space{.5cm} \includegraphics[height=7.5cm, angle=-90]{1068f6d.ps} } \end{figure}$ Figure 8: Analytical fits (solid curve) of the galaxy-like object mass function (cross) for the G0 and G1 simulations at z=0 and z=1. Fits are computed using Eq. (11).
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f7a.ps}\par\includegraphics[height=7.5cm, angle=-90]{1068f7b.ps}\end{figure}$ Figure 9: Dark matter halo mass function at different redshifts for the G0 simulation.
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f8a.ps}\hspace{.5cm} \includegraphics[height=7.5cm, angle=-90]{1068f8b.ps}\end{figure}$ Figure 10: Analytical fits (solid curve) of the dark matter halo mass function (cross) for the G0 simulation at z=0 and z=1, computed using Eq. (12). Dashed curve (identical to the solid curve at M>10¹⁰ $M_{\odot }$ ) is a three power-law analytical fit.
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In the text

$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f9.ps}\end{figure}$ Figure 11: Conditional mean of the galaxy-like object epoch of formation given a mass M, $\langle t\vert M \rangle$ , for the G0 simulation catalog at z=0 (today is at the upper end of the ordinate axis). The dispersion $\pm \sigma$ around the conditional mean is shown by the error bars.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm, angle=-90]{1068f10.ps}\end{figure}$ Figure 12: Top panel: projected distribution of the galaxy-like objects inside a radius $<R=400 \ h^{-1}\ {\rm kpc}$ around the mass center of three dark matter halos with a mass higher than $10^{13} ~ M_{\odot}$ , for the G0 simulation. The halo mass centers are at the origin of each plots, scaled in $h^{-1}\ {\rm Mpc}$ . Each symbol represents the mass range of galaxies: $10^8<M<10^9 ~ M_{\odot}$ (cross), $10^9<M<10^{11}~ M_{\odot}$ (triangle), $M>10^{11} ~ M_{\odot}$ (circle). Lower panel: same as the top panel, but for $R=600 \ h^{-1}\ {\rm kpc}$ .
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In the text

$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f11.ps}\end{figure}$ Figure 13: Galaxy-like object mass function for the GP (cross) and G1 (square) simulations at z=0.
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In the text

$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f12.ps}\end{figure}$ Figure 14: Same as Fig. 11 but for the GP simulation.
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f17.ps}\end{figure}$ Figure 15: Same as Fig. 5, but for the GNE simulation without galaxy formation.
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In the text

$\begin{figure} \par\includegraphics[height=6.5cm]{1068f13.ps}\end{figure}$ Figure 16: Evolution with redshift of the stellar particle mean mass (solid lines) with the dispersion $\pm \sigma$ around the mean (dashed and dotted lines) for the GNE (thick lines) and G1 simulations (thin lines).
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f14a.ps}\par\includegraphics[height=7.5cm, angle=-90]{1068f14b.ps}\end{figure}$ Figure 17: Galaxy-like object mass function for the GNE (square) and G1 (open square) simulations at z=8 and z=6.
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In the text

$\begin{figure} \par\includegraphics[height=7cm, angle=-90]{1068fA1a.ps}\vspace{3... ...ps}\vspace{3mm} \includegraphics[height=7cm, angle=-90]{1068fA1c.ps}\end{figure}$ Figure A.1: Evolution with redshift of the stellar particle mass function for the G1, GP and GNE simulations (from top to bottom panels, respectively). The mass function is shown at z=9, 8, 7, 6, 4, 2, 0 for the G1 and GNE simulations and at z=8, 7, 5, 4, 2, 0 for the GP simulation (alternatively filled and open circles, from bottom to top).

In the text

$\begin{figure} \par\includegraphics[height=7cm, angle=-90]{1068fB1a.ps}\vspace{3... ...ps}\vspace{3mm} \includegraphics[height=7cm, angle=-90]{1068fB1c.ps}\end{figure}$ Figure A.2: Galaxy-like object mass function for the G0 ( $L_{\rm box}=32$ ) and G1 ( $L_{\rm box}=16$ ) simulations at z=0 computing by considering different values of $\eta$ (top panel) and $M_{\rm min}$ (middle panel). The bottom panel compares both resolutions.

In the text

$\begin{figure} \par\includegraphics[height=5.5cm]{1068f1.ps}\end{figure}$	Figure 1: Evolution with redshift of the ultraviolet background radiation intensity.
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$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f4.ps}\end{figure}$	Figure 4: Same as Fig. 3 but for a SCDM scenario, for the G1 (dashed line) and G0 (dot-dashed line) simulations. The observation points are the same as described in Fig. 3 but overplotted for a SCDM cosmology.
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$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f15.ps}\end{figure}$	Figure 5: Evolution with redshift of the baryonic mass fractions computed in different temperature ranges, for the G0 simulation but without galaxy formation: $T<9\times 10^3$ K ("diffuse'', dot-dot-dashed line), $9\times 10^3 \leq T< 2\times 10^4$ K ("cold'', dashed line), $2\times 10^4 \leq T< 5\times 10^5$ K ("warm'', dot-dashed line), $T \geq 5\times 10^5$ K ("hot'', dotted line).
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$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f16.ps}\end{figure}$	Figure 6: Same as Fig. 5, but for the G1 simulation without galaxyformation.
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$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f5a.ps}\par\includegraphics[height=8cm, angle=-90]{1068f5b.ps}\end{figure}$	Figure 7: Galaxy-like object mass function at different redshifts for the G0 simulation.
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$\begin{figure} \par\mbox{\includegraphics[height=7.5cm, angle=-90]{1068f6a.ps}\h... ...space{.5cm} \includegraphics[height=7.5cm, angle=-90]{1068f6d.ps} } \end{figure}$	Figure 8: Analytical fits (solid curve) of the galaxy-like object mass function (cross) for the G0 and G1 simulations at z=0 and z=1. Fits are computed using Eq. (11).
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$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f7a.ps}\par\includegraphics[height=7.5cm, angle=-90]{1068f7b.ps}\end{figure}$	Figure 9: Dark matter halo mass function at different redshifts for the G0 simulation.
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$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f8a.ps}\hspace{.5cm} \includegraphics[height=7.5cm, angle=-90]{1068f8b.ps}\end{figure}$	Figure 10: Analytical fits (solid curve) of the dark matter halo mass function (cross) for the G0 simulation at z=0 and z=1, computed using Eq. (12). Dashed curve (identical to the solid curve at M>10¹⁰ $M_{\odot }$ ) is a three power-law analytical fit.
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$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f9.ps}\end{figure}$	Figure 11: Conditional mean of the galaxy-like object epoch of formation given a mass M, $\langle t\vert M \rangle$ , for the G0 simulation catalog at z=0 (today is at the upper end of the ordinate axis). The dispersion $\pm \sigma$ around the conditional mean is shown by the error bars.
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$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f11.ps}\end{figure}$	Figure 13: Galaxy-like object mass function for the GP (cross) and G1 (square) simulations at z=0.
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$\begin{figure} \par\includegraphics[height=8cm, angle=-90]{1068f12.ps}\end{figure}$	Figure 14: Same as Fig. 11 but for the GP simulation.
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$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f17.ps}\end{figure}$	Figure 15: Same as Fig. 5, but for the GNE simulation without galaxy formation.
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$\begin{figure} \par\includegraphics[height=6.5cm]{1068f13.ps}\end{figure}$	Figure 16: Evolution with redshift of the stellar particle mean mass (solid lines) with the dispersion $\pm \sigma$ around the mean (dashed and dotted lines) for the GNE (thick lines) and G1 simulations (thin lines).
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$\begin{figure} \par\includegraphics[height=7.5cm, angle=-90]{1068f14a.ps}\par\includegraphics[height=7.5cm, angle=-90]{1068f14b.ps}\end{figure}$	Figure 17: Galaxy-like object mass function for the GNE (square) and G1 (open square) simulations at z=8 and z=6.
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