All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f1.ps}\end{figure}$ Figure 1: a). Quantitative change in log of the comoving luminosity density, ${\cal L}$ , as a function of the faint-end slope, $\alpha$ , of the LF for fixed L^* and $\phi ^*$ values, compared to Log ${\cal L}$ for $\alpha =-1$ . b) Fraction of ${\cal L}$ as a function of $\alpha$ due to sources fainter than L^* (dotted line), 0.4L^* (dashed line), and 0.1L^* (dot-dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f2.ps}\end{figure}$ Figure 2: The estimated non dust-corrected comoving luminosity densities in the rest-frame B-4400 passband as a function of $\log(1+z)$ and represented with filled circles. The crosses are the minimal comoving densities, derived from the observed luminosities without extrapolation neither at the bright nor at the faint part of the LF. Data are displayed at the mean redshift of the galaxies within each redshift bin. Error bars are derived from the 2.3 $\sigma$ error contours of the Schechter parameters, except at z<0.2 where M^* is fixed and at z>1.2 where $\alpha$ is fixed. The dot at z=0.1 is the SDSS local point. The VVDS B-band luminosity densities increase as (1+z)^1.14 up to z=1.1. Data are listed in Table 1. The open triangles and open circles are the DEEP2 and COMBO-17 data displayed for clarity at -0.05 and +0.05 in redshift respectively and taken from Table 2 in Faber et al. (2005), the open squares are the HDF data from Poli et al. (2003), and the open stars are the FDF data from Gabasch et al. (2004).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f3.ps}\end{figure}$ Figure 3: Comoving non dust-corrected luminosity densities in the rest-frame V-5500, R-6500, and I-7900 passbands. The filled circles, crosses, and the dot are the same as in Fig. 2. The VVDS V-, R-, and I-band densities increase as (1+z)^0.73, (1+z)^0.42, and (1+z)^0.30 up to z=1.1 respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f4.ps}\end{figure}$ Figure 4: Comoving non dust-corrected luminosity densities in the rest-frame U-3600, NUV-2800, and FUV-1500 passbands. The filled circles, crosses, open stars, and the dot come from the same data as in Fig. 2. The VVDS U-, NUV-, and FUV-band densities increase as (1+z)^1.92, (1+z)^1.94, and (1+z)^2.05 up to z=1.1 respectively. The asterisk is the FUV-band local point from the GALEX-2dFGRS survey ( $\langle z \rangle =0.055$ Wyder et al. 2005). The plain squares are the FUV-band data, displayed for clarity at +0.02 in redshift, and taken from the GALEX-VVDS survey (Schiminovich et al. 2005). The small open circles are the NUV-band points from the SDSS (Baldry et al. 2005).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f5.ps}\end{figure}$ Figure 5: Comoving non dust-corrected VVDS luminosity densities in the rest-frame FUV-1500, NUV-2800, U-3600, B-4400, V-5500, R-6500, and I-7900 passbands from bottom to top respectively, as displayed in Figs. 2-4. The solid line connects points where the rest-frame band is observed in the optical.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{6330f6.ps}\end{figure}$ Figure 6: Rest-frame B-band comoving non dust-corrected luminosity densities with the ( $\Omega _{\rm M}$ , $\Omega _{\Lambda }$ , h)=(1, 0, 0.5) cosmology at 0<z<1 of the I-selected CFRS and VVDS surveys. Values are listed in Table 2. For clarity the z>0.2 data are represented by symbols slightly displaced horizontally from the center of the redshift bins delimited with the vertical dotted lines. The plain square points at z=0.05, 0.07, and 0.1 are local points from the SAPM (Loveday et al. 1992), the 2dFGRS (Norberg et al. 2002), and SDSS (Blanton et al. 2003) respectively. The dashed line shows the best-fit power law and its associated uncertainties for the "LF-estimated'' ${\cal L}_{\rm 4400~\AA}$ of the CFRS 17.5-22.5 data derived in Lilly et al. (1996), $(1+z)^{2.72\pm 0.5}$ , and the solid line is the one for the VVDS 17.5-24.0 data, $(1+z)^{2.05\pm 0.06}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f7.ps}\end{figure}$ Figure 7: Comoving non dust-corrected luminosity densities in the rest-frame B-passband from early to late galaxy types (see details in Sect. 6.1). For clarity, data are represented by symbols slightly displaced horizontally from the center of the redshift bins. Error bars are at 1 $\sigma$ . The irregular-like type emissivity decreases markedly by a factor 4, while the elliptical-like type increases by a factor 1.7 from z=1.1 to z=0.2. We note that at z<0.4 the total emissivity is dominated by the early-type population.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{6330f8.ps} \end{figure}$ Figure 8: Unweighted non dust-corrected luminosity functions in the rest-frame FUV-1500 passband estimated with $\alpha$ fixed to -1.60. The circles and the solid line represent the $V_{\max}$ and the STY estimates for the extended dataset where the number of galaxies is given within parenthesis next to the redshift range. The vertical dot-dashed line corresponds to the faint absolute magnitude limits considered in the STY estimate (see Sect. 3.2). The hashed area is limited by the LFs derived with $\alpha$ fixed to -1.20 and -1.75. The dotted lines represent the STY estimates with $\alpha$ fixed to -1.60 for the standard dataset. The standard dataset LF is below the extended dataset LF since it does not include quality flags 1 (see Sect. 7.1). In the top-left panel, the long-dashed line is the incompleteness-corrected dataset FUV-1500 LF at 3<z<4 derived as in Paltani et al. (2007), with fixed $\alpha =-1.4$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f9.ps}\end{figure}$ Figure 9: Comoving non dust-corrected FUV luminosity densities from z=0 to z=5. The plain circles represent the 1500 Å VVDS data (0.05<z<5) (see values and error bars in Tables 1 & 4), the plain triangle represents the 1500 Å VVDS data at 3<z<4 derived as in Paltani et al. (2007), and the plain squares represent the 1500 Å GALEX-VVDS data at z<1, plotted at +0.02 in redshift for clarity, from Schiminovich et al. (2005). Other data are the 1500 Å GALEX-2dFGRS from Wyder et al. (2005) (asterisk), the 1500 Å HDF data from Arnouts et al. (2005) (crossed circles), the 1700 Å KDF data from Sawicki & Thompson (2006b) (open rhombus), the 1500 Å FDF data from Gabasch et al. (2004) (open stars), and the 1700 Å data from Iwata et al. (2007) (crossed square).
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{6330f10.ps}\end{figure}$ Figure 10: Comoving rest-frame FUV non dust-corrected luminosity densities from z=0 to z=5 for three bright populations defined as $M_{AB}(1500~\AA)<-19, -20$ , and -21 mag. Symbols are the same as in Fig. 9. Error bars correspond to the fixed slopes, $\alpha =-1.2$ and -1.75 at 0.2<z<5, at 0.05<z<0.2 to the fixed $M^{*}\pm 0.1$ ; those which are not visible are smaller than the size of the data point, i.e. <0.1 dex. We do not plot the local values for M<-21 which have low values, at z=0.14 and 0.055 Log ${\cal L}=12.45\pm 0.55$ and 12.10 Watt Hz^-1 Mpc^-3, respectively. In each panel, the solid line connects the VVDS points of the global FUV luminosity density as displayed in Fig. 9, and the vertical lines delimit the approximative redshift range in which the bright population is more luminous than the characteristic FUV luminosity of the whole population.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f11.ps}\end{figure}$ Figure 11: Comoving rest-frame FUV non dust-corrected VVDS luminosity densities from z=0 to z=5 for three luminosity-class populations defined as $M_{AB}(1500~\AA)>-19$ (dwarf and intermediate-luminosity galaxies, ${<}0.1\ {L}^*_{\rm LBG}$ ), - $21 < M_{AB}(1500~\AA)< -19$ (luminous galaxies), and $M_{AB}(1500~\AA)<-21$ (very luminous galaxies, ${>} {L}^*_{\rm LBG}$ ). We used and connected the same VVDS dataset as displayed in Fig. 10.
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In the text

$\begin{figure*} \par\includegraphics[width=13cm,clip]{6330f12.ps}\end{figure*}$ Figure 12: Star formation rate densities as a function of redshift. Symbols ( plain large circles, plain large squares, asterisk, crossed circles, open rhombus, open stars, crossed square) and error bars are the same as in Fig. 9, and they represent the SFR densities with no reddening correction. The dotted, long-dashed line connects the reddening corrected H $\alpha$ data (small plain circles) from the CFRS (Tresse & Maddox 1998; Tresse et al. 2002). The dotted, short-dashed line connects the 12 $\mu$ m data (small plain squares) from Pérez-Gonzàlez et al. (2005). Models from Somerville et al. (2001), Croton et al. (2006) and Nagamine et al. (2006) are represented with the dashed, the dotted, and the short-long dashed lines respectively. Everything is for a Salpeter (1955) IMF. The derived $A_{\rm FUV}$ dust obscuration between the VVDS data not dust corrected and the 12 $\mu$ m data at z<2 is represented in the inset.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f1.ps}\end{figure}$	Figure 1: a). Quantitative change in log of the comoving luminosity density, ${\cal L}$ , as a function of the faint-end slope, $\alpha$ , of the LF for fixed L^* and $\phi ^$ values, compared to Log ${\cal L}$ for $\alpha =-1$ . b) Fraction of ${\cal L}$ as a function of $\alpha$ due to sources fainter than L^ (dotted line), 0.4L^* (dashed line), and 0.1L^* (dot-dashed line).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f3.ps}\end{figure}$	Figure 3: Comoving non dust-corrected luminosity densities in the rest-frame V-5500, R-6500, and I-7900 passbands. The filled circles, crosses, and the dot are the same as in Fig. 2. The VVDS V-, R-, and I-band densities increase as (1+z)^0.73, (1+z)^0.42, and (1+z)^0.30 up to z=1.1 respectively.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6330f5.ps}\end{figure}$	Figure 5: Comoving non dust-corrected VVDS luminosity densities in the rest-frame FUV-1500, NUV-2800, U-3600, B-4400, V-5500, R-6500, and I-7900 passbands from bottom to top respectively, as displayed in Figs. 2-4. The solid line connects points where the rest-frame band is observed in the optical.
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