All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f1_4185.eps} \end{figure}$ Figure 1: Observed light-curves points of the SN Ia SNLS-04D3fk in $g_{\rm M}$ , $r_{\rm M}$ , $i_{\rm M}$ and $z_{\rm M}$ bands, along with the multi-color light-curve model (described in Sect. 5.1). Note the regular sampling of the observations both before and after maximum light. With a SN redshift of 0.358, the four measured pass-bands lie in the wavelength range of the light-curve model, defined by rest-frame U to R bands, and all light-curves points are therefore fitted simultaneously with only four free parameters (photometric normalization, date of maximum, a stretch and a color parameter).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f2_4185.eps} \end{figure}$ Figure 2: Observed light-curves points of the SN Ia SNLS-04D3gx at z=0.91. With a SN redshift of 0.91, only two of the measured pass-bands lie in the wavelength range of the light-curve model, defined by rest-frame U to R bands, and are therefore used in the fit (shown as solid lines). Note the excellent quality of the photometry at this high redshift value. Note also the clear signal observed in $r_{\rm M}$ and even in $g_{\rm M}$ , which correspond to central wavelength of respectively $\lambda\sim3200~\AA$ and $\lambda\sim2500~\AA$ in the SN rest-frame.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f3_4185.eps} \end{figure}$ Figure 3: The calibration residuals - i.e. the residuals around the mean magnitude of each Deep field tertiary standard - in the bands $g_{\rm M}$ , $r_{\rm M}$ , $i_{\rm M}$ and $z_{\rm M}$ , for all CCDs and fields, with one entry per star and epoch. The dispersion is below 1% in $g_{\rm M}$ , $r_{\rm M}$ and $i_{\rm M}$ , and about 1.5% in $z_{\rm M}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f4_4185.eps} \end{figure}$ Figure 4: Hubble diagram of SNLS and nearby SNe Ia, with various cosmologies superimposed. The bottom plot shows the residuals for the best fit to a flat $\Lambda$ cosmology.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{f5_4185.eps} \end{figure}$ Figure 5: Contours at 68.3%, 95.5% and 99.7% confidence levels for the fit to an $(\Omega _{\rm M},\Omega _\Lambda )$ cosmology from the SNLS Hubble diagram (solid contours), the SDSS baryon acoustic oscillations (Eisenstein et al. 2005, dotted lines), and the joint confidence contours (dashed lines).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{f6_4185.eps} \end{figure}$ Figure 6: Contours at 68.3%, 95.5% and 99.7% confidence levels for the fit to a flat $(\Omega _{\rm M},w)$ cosmology, from the SNLS Hubble diagram alone, from the SDSS baryon acoustic oscillations alone (Eisenstein et al. 2005), and the joint confidence contours.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f7_4185.eps}\end{figure}$ Figure 7: The stretch (s parameter) distributions of nearby (hashed blue) and distant (thick black with filled symbols) SNLS SNe with z<0.8. These distributions are very similar with averages of $0.920~\pm~0.018$ and $0.945\pm 0.013$ , respectively (1 $\sigma$ apart).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f8_4185.eps} \end{figure}$ Figure 8: The color (c parameter) distributions for nearby (hashed blue) and distant (thick black with filled symbols) SNe with z<0.8. These distributions are very similar, with averages of $0.059\pm 0.014$ and $0.029\pm 0.015$ , respectively (1.5 $\sigma$ apart).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f9_4185.eps} \end{figure}$ Figure 9: Residuals in the Hubble diagram as a function of stretch (s parameter), for nearby (blue open symbols) and distant (z<0.8, black filled symbols). This diagram computes distance modulus $\mu _B$ without the stretch term $\alpha (s-1)$ , and returns the well-known brighter-slower relationship with a consistent behavior for nearby and distant SNe Ia.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f10_4185.eps} \end{figure}$ Figure 10: Residuals in the Hubble diagram as a function of color (c parameter), for nearby (blue open symbols) and distant (z<0.8, black filled symbols). This diagram computes distance modulus $\mu _B$ without the color term $\beta c$ , and returns the brighter-bluer relationship with a consistent behavior for nearby and distant SNe Ia. Notice that the bluest SNLS objects are compatible with the bulk behavior.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f11_4185.eps} \end{figure}$ Figure 11: $\Delta U_3$ , difference between rest-frame U peak magnitude "predicted'' from B and V, and the measured value, as a function of redshift. The error bars reflect photometric uncertainties. The redshift regions have been chosen so that the measured bands roughly sample the UBV rest-frame region. The differences between average values for the three samples agree within statistical uncertainties, indicating that the relation between U, B and V brightnesses does not change with redshift. Although the nearby and intermediate samples have comparable photometric resolution, the intermediate sample exhibits a far smaller scatter. We attribute this difference to the practical difficulties in calibrating U band observations.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[width=4.3cm,clip]{f12_4185.eps}\hspace... ...s}\hspace*{2mm} \includegraphics[width=4.3cm,clip]{f15_4185.eps} }\end{figure}$ Figure 12: Distributions of redshifts, peak $i_{\rm M}$ magnitudes (AB), stretch factors and colors of SNLS supernovae (black dots) together with the distributions obtained with simulated SNe (red histograms).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f16_4185.eps}\par\vspace*{... ...}\par\vspace*{2mm} \includegraphics[width=8.5cm,clip]{f18_4185.eps} \end{figure}$ Figure 13: Stretch, color and Hubble diagram residuals as a function of redshift for SNLS supernovae (gray dots). The black points correspond to average values in redshift bins. The red solid (dashed) lines represent the average (one standard deviation) values obtained with SNe simulations as described in Sect. 7.4. At large redshifts, since only bright SNe are identified, the average stretch factor is larger and the average color bluer. The average distance modulus is less affected by the selection (see text for details).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f3_4185.eps} \end{figure}$	Figure 3: The calibration residuals - i.e. the residuals around the mean magnitude of each Deep field tertiary standard - in the bands $g_{\rm M}$ , $r_{\rm M}$ , $i_{\rm M}$ and $z_{\rm M}$ , for all CCDs and fields, with one entry per star and epoch. The dispersion is below 1% in $g_{\rm M}$ , $r_{\rm M}$ and $i_{\rm M}$ , and about 1.5% in $z_{\rm M}$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f4_4185.eps} \end{figure}$	Figure 4: Hubble diagram of SNLS and nearby SNe Ia, with various cosmologies superimposed. The bottom plot shows the residuals for the best fit to a flat $\Lambda$ cosmology.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{f5_4185.eps} \end{figure}$	Figure 5: Contours at 68.3%, 95.5% and 99.7% confidence levels for the fit to an $(\Omega _{\rm M},\Omega _\Lambda )$ cosmology from the SNLS Hubble diagram (solid contours), the SDSS baryon acoustic oscillations (Eisenstein et al. 2005, dotted lines), and the joint confidence contours (dashed lines).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{f6_4185.eps} \end{figure}$	Figure 6: Contours at 68.3%, 95.5% and 99.7% confidence levels for the fit to a flat $(\Omega _{\rm M},w)$ cosmology, from the SNLS Hubble diagram alone, from the SDSS baryon acoustic oscillations alone (Eisenstein et al. 2005), and the joint confidence contours.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f7_4185.eps}\end{figure}$	Figure 7: The stretch (s parameter) distributions of nearby (hashed blue) and distant (thick black with filled symbols) SNLS SNe with z<0.8. These distributions are very similar with averages of $0.920~\pm~0.018$ and $0.945\pm 0.013$ , respectively (1 $\sigma$ apart).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f8_4185.eps} \end{figure}$	Figure 8: The color (c parameter) distributions for nearby (hashed blue) and distant (thick black with filled symbols) SNe with z<0.8. These distributions are very similar, with averages of $0.059\pm 0.014$ and $0.029\pm 0.015$ , respectively (1.5 $\sigma$ apart).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f9_4185.eps} \end{figure}$	Figure 9: Residuals in the Hubble diagram as a function of stretch (s parameter), for nearby (blue open symbols) and distant (z<0.8, black filled symbols). This diagram computes distance modulus $\mu _B$ without the stretch term $\alpha (s-1)$ , and returns the well-known brighter-slower relationship with a consistent behavior for nearby and distant SNe Ia.
Open with DEXTER

$\begin{figure} \par\mbox{\includegraphics[width=4.3cm,clip]{f12_4185.eps}\hspace... ...s}\hspace*{2mm} \includegraphics[width=4.3cm,clip]{f15_4185.eps} }\end{figure}$	Figure 12: Distributions of redshifts, peak $i_{\rm M}$ magnitudes (AB), stretch factors and colors of SNLS supernovae (black dots) together with the distributions obtained with simulated SNe (red histograms).
Open with DEXTER