All Figures

$\begin{figure} \par\includegraphics[width=14.6cm,clip]{fig2.eps} \end{figure}$ Figure 2: AB_0.2 - AB_0.44 vs. AB_0.44 - AB_0.65 diagram for the UV sources (points). Asterisks are the starbursts galaxies from Gordon et al. (1997). Triangles are galaxies from the Coma cluster from Donas et al. (1995). Crosses are the FAUST galaxies from Deharveng et al. (1994). Solid and dashed lines represent synthetic models of galaxies following the Hubble sequence from PEGASE (Fioc & Rocca-Volmerange 1997) and Boselli et al. (2003) respectively. The bold square represents the position of an instantaneous burst of star formation 3 Myr old, as determined from Starburst99. The shaded region corresponds to the approximate loci occupied by the real galaxies. The data are not corrected for Galactic extinction. The arrow at the bottom left corner shows the extinction vector corresponding to the maximum Galactic extinction for our UV sources.
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In the text

$\begin{figure} \par\includegraphics[width=2cm,clip]{m010_445.ps}\includegraphics... ...1.ps}\includegraphics[width=2cm,clip]{m067_105.ps}\hspace*{3.2cm}}\end{figure}$ Figure 3: $2 \times 2$ arcmin² extracts of the DSS plates of the optical counterparts of the UV sources for which the AB_0.2 - AB_0.44 and AB_0.44 - AB_0.65 colors are consistent with those of galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{fig4.eps} \end{figure}$ Figure 4: Distance distribution of the galaxies in the UVsel sample. The shaded bins correspond to the distribution of the galaxies non associated with clusters.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{fig5.eps} \end{figure}$ Figure 5: Bright UV galaxy counts from several sources of the literature: pluses are from Milliard et al. (1992), asterisks from Deharveng et al. (1994). Open triangles correspond to our total UVsel sample and open squares correspond to the UVsel galaxies not associated to clusters. The symbols corresponding to both sets of data were slightly shifted along the X-axis in order to avoid superposition. The dashed straight line corresponds to the extrapolation to the FOCA counts of Milliard et al. with slope 0.6.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{fig6.eps} \end{figure}$ Figure 6: UV luminosity function of the total UVsel sample (open triangles) and excluding the cluster galaxies (asterisks). The symbols corresponding to both sets of data were slightly shifted along the X-axis in order to avoid superposition. The dashed line corresponds to the best fit to a Schechter function of the luminosity function of Sullivan et al. using the $1/V_{\rm max}$ method. UV magnitudes are not corrected for internal extinction. The histograms show the magnitude distributions of the total sample (solid line) and the subsample without cluster galaxies (dashed line). The number of galaxies in each bin are indicated at the top of the bins.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{fig7.eps} \end{figure}$ Figure 7: Distance distribution of the galaxies in the FIRsel sample. The shaded bins correspond to the distribution of the galaxies not associated with clusters.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{fig8.eps} \end{figure}$ Figure 8: Galaxy counts as a function of f₆₀ for the FIRsel sample. Asterisks correspond to the total FIRsel sample whereas open diamonds correspond to the galaxies of the FIRsel sample not associated with clusters. The symbols corresponding to both sets of data were slightly shifted along the X-axis to avoid superposition. The dashed line corresponds to average counts presented by Saunders et al. (2000) for three different subsamples of the PSCz.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{fig9.eps} \end{figure}$ Figure 9: Luminosity functions of the total FIRsel sample (open triangles) and of the subsample without cluster galaxies (asterisks) as a function of the L₆₀ luminosity. The symbols corresponding to both sets of data were slightly shifted along the X-axis in order to avoid superposition. The dashed and dotted line correspond to the LF of Takeuchi et al. (2003) computed using an analytic method and the $1/V_{\rm max}$ method respectively. The histograms show the luminosity distributions of the total sample (solid line) and the subsample without cluster galaxies (dashed line). The number of galaxies in each bin are indicated at the top of the bins.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{fig10.eps} \end{figure}$ Figure 10: Histograms of $\log~(F_{60}/F_{0.2})$ for the UVsel sample (dashed line) and the FIRsel sample (solid line). The galaxy of the UVsel galaxy with no FIR counterpart is indicated by a star as an upper limit. The four galaxies from the FIRsel sample with no UV counterpart are indicated with filled dots as lower limits.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{fig11.eps} \end{figure}$ Figure 11: $\log F_{60}$ vs. $\log F_{0.2}$ for the FIRsel sample (open diamonds) and the UVsel sample (pluses). The galaxy from the UVsel sample without a FIR counterpart as well as the four galaxies from the FIRsel sample without a detection in UV are represented as upper limits with arrows. Dashed horizontal lines indicate the limiting fluxes of the FOCA experiment, and of the UVsel sample. Dashed vertical lines indicate the limiting fluxes of the FSC and PSCz catalogs. Lines indicating different values of the extinction at 0.2 $\mu$ m are also represented by dotted lines.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{fig12.eps} \end{figure}$ Figure 12: Comparison of different extinction corrections as a function of the $F_{\mbox{\scriptsize FIR}}/F_{\mbox{\scriptsize UV}}$ ratio. The solid line corresponds to the one used throughout this work.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{fig13a.eps}\hspace*{2mm} \... ...cm,clip]{fig13c.eps}\includegraphics[width=8.5cm,clip]{fig13d.eps} \end{figure}$ Figure 13: Comparison of the different estimations of the SFR for the galaxies of the UVsel sample: a) $\log {\it SFR}_{\mbox{\scriptsize UV}}(A_{0.2}=1.07)/{\it SFR}_{\mbox{\scriptsize UV}}$ vs. $\log {\it SFR}_{\mbox{\scriptsize UV}}$ , b) $\log {\it SFR}_{\mbox{\scriptsize dust$+$ UV}}$ vs. $\log {\it SFR}_{\mbox{\scriptsize UV}}$ , c) $\log {\it SFR}(\eta)$ vs. $\log {\it SFR}_{\mbox{\scriptsize UV}}$ , d) $\log {\it SFR}_{\mbox{\scriptsize dust}}$ vs. $\log {\it SFR}_{\mbox{\scriptsize UV}}$ . SFRs are always expressed in $M_{\odot }$ yr^-1. Dashed lines represent the best fits to straight lines. The galaxy without a FIR counterpart is excluded.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{fig14a.eps}\hspace*{2mm} \... ...m,clip]{fig14c.eps}\includegraphics[width=8.5cm,clip]{fig14d.eps} \end{figure}$ Figure 14: Comparison of the different estimations of the SFR for the galaxies of the FIRsel sample: a) $\log \mbox{\it SFR}_{\mbox{\scriptsize dust$+$ UV}}$ vs. $\log \mbox{\it SFR}_{\mbox{\scriptsize dust}}$ , b) $\log \mbox{\it SFR}(\eta)$ vs. $\log \mbox{\it SFR}_{\mbox{\scriptsize dust}}$ , c) $\log \mbox{\it SFR}_{\mbox{\scriptsize UV}}$ vs. $\log \mbox{\it SFR}_{\mbox{\scriptsize dust}}$ , d) $\log \mbox{\it SFR}(\eta)$ vs. $\log \mbox{\it SFR}_{\mbox{\scriptsize UV}}$ . SFRs are always expressed in $M_{\odot }$ yr^-1. Dashed lines represent the best fits to straight lines. The four galaxies without an UV counterpart are excluded.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{fig15.eps} \end{figure}$ Figure 15: $\log {\it SFR}(\eta)$ vs. $A_{\mbox{\scriptsize UV}}$ for the UVsel (asterisks) and FIRsel (pluses) samples. SFRs are expressed in $M_{\odot }$ yr^-1. The UVsel galaxy without a FIR counterpart as well as the four FIRsel galaxies without an UV counterpart are excluded.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{fig16.eps} \end{figure}$ Figure 16: Same as Fig. 15 with the ${\it SFR}(\eta )$ normalized to the optical area of the galaxies in kpc². Symbols are also as in Fig. 15.
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In the text

$\begin{figure} \par\includegraphics[width=12.4cm,clip]{figa1a.eps}\par\vspace*{2mm} \includegraphics[width=12.4cm,clip]{figa1b.eps} \end{figure}$ Figure A.1: Comparison between the B photometry of the USNO-B1.0 catalog with other catalogs: Tycho2 a) and ASCC-2.5 b).

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{m010-C119047-r.ps}\include... ...50-N4411b-r.ps}\includegraphics[width=7.5cm,clip]{m050-N4411-r.ps} \end{figure}$ Figure 1: $5 \times 5$ arcmin² extracts of the UV (FOCA) and optical (DSS) blue frames of the UVsel galaxies.
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In the text

$\begin{figure}\par\includegraphics[width=7.5cm,clip]{m050-N4416-r.ps}\includegra... ...{m067-N3883-r.ps}\includegraphics[width=7.5cm,clip]{m067-U6697-r.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=7.5cm,clip]{m067-U6743-r.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=2cm,clip]{m010_445.ps}\includegraphics... ...1.ps}\includegraphics[width=2cm,clip]{m067_105.ps}\hspace*{3.2cm}}\end{figure}$	Figure 3: $2 \times 2$ arcmin² extracts of the DSS plates of the optical counterparts of the UV sources for which the AB_0.2 - AB_0.44 and AB_0.44 - AB_0.65 colors are consistent with those of galaxies.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{fig4.eps} \end{figure}$	Figure 4: Distance distribution of the galaxies in the UVsel sample. The shaded bins correspond to the distribution of the galaxies non associated with clusters.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{fig7.eps} \end{figure}$	Figure 7: Distance distribution of the galaxies in the FIRsel sample. The shaded bins correspond to the distribution of the galaxies not associated with clusters.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{fig10.eps} \end{figure}$	Figure 10: Histograms of $\log~(F_{60}/F_{0.2})$ for the UVsel sample (dashed line) and the FIRsel sample (solid line). The galaxy of the UVsel galaxy with no FIR counterpart is indicated by a star as an upper limit. The four galaxies from the FIRsel sample with no UV counterpart are indicated with filled dots as lower limits.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{fig12.eps} \end{figure}$	Figure 12: Comparison of different extinction corrections as a function of the $F_{\mbox{\scriptsize FIR}}/F_{\mbox{\scriptsize UV}}$ ratio. The solid line corresponds to the one used throughout this work.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{fig15.eps} \end{figure}$	Figure 15: $\log {\it SFR}(\eta)$ vs. $A_{\mbox{\scriptsize UV}}$ for the UVsel (asterisks) and FIRsel (pluses) samples. SFRs are expressed in $M_{\odot }$ yr^-1. The UVsel galaxy without a FIR counterpart as well as the four FIRsel galaxies without an UV counterpart are excluded.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{fig16.eps} \end{figure}$	Figure 16: Same as Fig. 15 with the ${\it SFR}(\eta )$ normalized to the optical area of the galaxies in kpc². Symbols are also as in Fig. 15.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{m010-C119047-r.ps}\include... ...50-N4411b-r.ps}\includegraphics[width=7.5cm,clip]{m050-N4411-r.ps} \end{figure}$	Figure 1: $5 \times 5$ arcmin² extracts of the UV (FOCA) and optical (DSS) blue frames of the UVsel galaxies.
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$\begin{figure}\par\includegraphics[width=7.5cm,clip]{m050-N4416-r.ps}\includegra... ...{m067-N3883-r.ps}\includegraphics[width=7.5cm,clip]{m067-U6697-r.ps}\end{figure}$	Figure 1: continued.
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