Table 2: Average number of images and nights per band for each SNLS light-curve. Note that there is less data in $g_{\rm M}$ and $z_{\rm M}$ . The $\chi ^2_n$ column refers to the last fit that imposes equal fluxes on a given night. The expected value is 1.25 (due to pixel correlations), so we face a moderate scatter excess of about 12% over photon statistics. The larger values in $i_{\rm M}$ and $z_{\rm M}$ indicate that fringes play a role in this excess. The last column displays the average wavelength of the effective filters in Å.
Band Average nb. Average nb. $\chi ^2_n$ Central

of images of epochs per d.o.f. wavelength

$g_{\rm M}$ 40 9.8 1.50 4860

$r_{\rm M}$ 75 14.4 1.40 6227

$i_{\rm M}$ 100 14.8 1.63 7618

$z_{\rm M}$ 60 7.9 1.70 8823

**Table 2:** Average number of images and nights per band for each SNLS light-curve. Note that there is less data in $g_{\rm M}$ and $z_{\rm M}$ . The $\chi ^2_n$ column refers to the last fit that imposes equal fluxes on a given night. The expected value is 1.25 (due to pixel correlations), so we face a moderate scatter excess of about 12% over photon statistics. The larger values in $i_{\rm M}$ and $z_{\rm M}$ indicate that fringes play a role in this excess. The last column displays the average wavelength of the effective filters in Å.
Band	Average nb.	Average nb.	$\chi ^2_n$	Central
	of images	of epochs	per d.o.f.	wavelength
$g_{\rm M}$	40	9.8	1.50	4860
$r_{\rm M}$	75	14.4	1.40	6227
$i_{\rm M}$	100	14.8	1.63	7618
$z_{\rm M}$	60	7.9	1.70	8823

Source LaTeX | All tables | In the text