\relax 
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces (Left): Our major new result based on several cycles of HST data showing the averaged Hubble diagram (SNe within $z < 0.01$ of each other have been combined) for all supernovae from our low-extinction subsample. The solid curve overlaid on the data represents our best-fit flat-universe model, $(\Omega _M,\Omega _\Lambda = (0.25, 0.75)$. Two other cosmological models are shown for compariso. (Center): Our latest joint measurements of $\Omega _M$ and $w$ assuming $\Omega _M + \Omega _\Lambda = 1$ and that $w$ is not time-varying. Confidence regions (95\% and 99\%) are shown for the SCP SN Ia data overlaid with LSS measurements and combined CMB measurements. (Right): 68\% statistical confidence intervals on the dark energy equation of state possible from {\it  SNLS} when it is completed 5 years from now, assuming a flat universe (from CMB measurements), and with (black-solid) and without (blue-dot) a prior on $\Omega _M$ from Large-Scale Structure. If a small systematic error is introduced, the statistical confidence interval will miss the correct simulated $\Lambda $ ($w=-1$) solution by $2\sigma $ (red-dash). }}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces  Illustrations of the CMAGIC method. Left panel, from top to bottom, the I-Band and B-band light curves, and the B-I color curve for a normal supernova are shown. The solid line on the left panel shows the regions where $B$ vs $B$-$I$ can be described by a linear relation. The $B$ vs $B$-$I$ Color-Magnitude Diagram for several example SNe\nobreakspace  {}Ia are shown on the right panel, ordered by host-galaxy extinction going from top to bottom. Only data taken between 0 to 35 days after $B_{max}$ are shown here. The data shown as solid dots correspond to epochs during which the relation between magnitude and color is linear for all SNe (this is 14--29 days after $B_{max}$ for $B$-$I$ for a typical supernova, and scales inversely with $\delta m_{15}$). The linear region shows that the $B$ and $I$ band magnitudes are highly correlated. Observations of a single point in $I$ band within the window where the linear relation holds true would be sufficient to describe accurately the $I$-band light curves in the linear region. Using this linear relation we define fiducial magnitudes, which are found to be better distance indicators than maximum-light magnitudes (Wan03). It was shown that that the slopes of the linear relation are identical for all well-observed nearby SNe, thus a single slope can be used for all SNeIa.}}{12}}