From: Lifan Wang <lifan@panisse.lbl.gov>
Date: January 22, 2004 9:05:17 PM PST
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To: Lifan Wang <lifan@panisse.lbl.gov>
From: Tony Spadafora <ALSpadafora@lbl.gov>
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\caption{ 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 noraml
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~Ia are shown on the right panel, ordered by 
host-galaxy extinction going from top to bottom.ÊOnly data taken 
between 0 to 35 days after $B_{max}$ are shown here.ÊThe data shown as 
solid dots correspond to epochs during which the relation between magnitude 
and color is linear of 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 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 observe
nearby SNe, thus A single slope can be used for all SNeIa.}

Ê