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\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces {\relax \fontsize  {8}{9.5}\normalfont  {\bf  (a) Left Panel:} The SCP SNe Ia Hubble diagram broken into host galaxy types from Sullivan et al.\ (2003). The SNe in elliptical hosts (filled red circles) show significantly less dispersion, $\sigma = 0.16$ mag, including measurement error. (This ground-based measurement error for this $z \sim 0.5$ sample is quite close to the HST measurement error at $z>1$ in this proposal.) {\bf  (b) Right Panel:} The comparison of the Hubble diagram, before and after extinction correction, for a mixture of SNe Ia in all host types shows the dramatic increase in error bars due to the uncertainty in $B - V$ color being multiplied by $R_B \approx 4$ and by the uncertainty in $R_B$. The data shown is from the SCP (Knop et al.\ 2003) and the Riess et al.\ 2004 GOODS search samples. For the SNe at redshifts $z > 1$ this yields an uncertainty of $\sim $0.5 mag, which is consistent with the measured dispersion of 0.5 mag. The ratio of this dispersion to the elliptical-hosted dispersion of panel (a) makes the elliptical-hosted SNe each worth 6 to 9 of the extinction-corrected others.}}}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces {\relax \fontsize  {8}{9.5}\normalfont  {\bf  (a) Left Panel:} Simulated 68\% confidence region on $w^\prime $ vs $w_0$ for the current literature SN sample but with underlying cosmology ($w_0 = -1$; $w^\prime =0$). The parameters are poorly constrained because color errors are magnified by $R_B \approx 4$. {\bf  (b) Middle Panel:} The solid red contour shows reduced uncertainties (excluding systematic bias) using a Baysian prior on the extinction distribution prior to suppress color errors. The short-dashed contour shows that this approach is sensitive to precise knowledge of $R_B$ and its variation with redshift; the example shifts from 4.1 to 2.6. Similarly, asymmetric priors can also introduce systematic biases (arrows). The filled gray contour is from Riess {\it  et al.}\ 2004 using such a prior. {\bf  (c) Right Panel:} Simulated 68\% region for the proposed new set of $\sim 20$ $z \mathrel {\raise 0.27ex\hbox {$>$}\kern -0.70em \lower 0.71ex\hbox {{$\scriptstyle \sim $}}}1$ SNe Ia found in cluster ellipticals (from Cycle 14 \& 15) if combined with 120 SNe Ia in ellipticals at the lower redshifts now being produced by the ground-based CFHT SNe Legacy Survey, the CTIO Essence survey, and (at $z< 0.1$) the Nearby SNe Factory. This approach addresses the large statistical error problem of panel (a) and the systematics problem of panel (b). The projected constraints from the ground-based surveys alone are given by the the outer contour, and the constraints from adding the 3 cluster-elliptical SNe found so far in the first third of Cycle 14 are the dashed contours. The almost-imperceptably-smaller innermost (dotted) contour shows the effect of adding $\sim 10$ SNe in {\em  field} ellipticals (if one is willing to risk using them at $z>1$ along with the {\em  cluster} ellipticals), also expected from Cycle 14 and 15 as well as from previous GOODS surveys. }}}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces {\relax \fontsize  {8}{9.5}\normalfont  {\bf  (a) Left Panel:} The dust-free nature of cluster ellipticals (circles) and S0 galaxies (squares) in RDCS 1252-2927 at $z=1.24$ is supported by the small scatter of the color-magnitude relation (CMR) when ACS quality photometry is used (from Blakeslee {\it  et al.}\ 2003). The CMR in this same cluster using data from the VLT FORS and ISAAC (transformed to the ACS i,z passbands) exhibits nearly 8 times the scatter demonstrating the need for HST imaging. With this large ground-based scatter, the outliers from the space-based CMR (indicated by open symbols) cannot be distinguished. {\bf  (b) Right Panel:} The scatter about the early-type red sequence in clusters from $0.02 < z < 1.3.$ The three clusters at $z > 1$ are RDCS0910+5422, RDCS1252-2927, and RDCS0848+4452 -- in both the GTO cluster survey and this SNe survey. }}}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces {\relax \fontsize  {8}{9.5}\normalfont  {\bf  (a) Left Panel:} The overdensity of $z > 1$ ellipticals achieved by centering on $z > 1$ clusters is typically in the range 6 - 20. The histograms show the color distribution of field ellipticals (nearly all at $z < 1$) and red sequence cluster ellipticals relative to the mean color of the red sequence galaxies. Also shown are the best fit Gaussians to the field and red sequence elliptical galaxy color distributions, where the gaussian fit to the field is based on additional ACS fields with no clusters. Galaxies with colors indicating $z >1$ are shown by the filled regions under the gaussian fits. The top panel is a composite from 3 clusters from the GTO at redshifts of $z = 1.10,\ 1.24$ and $1.27$. The bottom panel shows the same for two RCS clusters at $z = 0.95$ and $1.03$. {\bf  (b): Right Side:} The upper panel shows the redshift distribution of the expected number of SNe per year in the clusters (left axis) and the number of clusters being searched (right axis). The actual cluster SNe that have been found so far in our Cycle 14 data are indicated by filled boxes (E indicates an elliptical host.) The lower panel shows the redshift distribution of the expected number of SNe per year in the field, with the actual field SNe discovered so far indicated by filled boxes. }}}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces {\relax \fontsize  {8}{9.5}\normalfont  {\bf  (a) Left Panel:} The unshaded region to the left displays the preliminary lightcurves of the 8 SNe discovered in the first third of Cycle 14, while the shaded region shows simulated data for the remaining two-thirds. With our chosen cadence, which is also proposed for cycle 15, we obtain typical fit peak magnitude total uncertainties of 0.07 to 0.15 mag, including the lightcurve time stretch correction uncertainty. {\bf  (b): Right Panel:} Ground-based spectra (VLT, Keck, Subaru) in the redshift range 0.9 -- 1.4 (solid curves) de-redshifted to the SN restframe. Host galaxy light has been removed and a low-pass filter applied to remove any unrelated features, i.e. with widths narrower than that of a SN. The spectrum second from the top is that of the first cluster SN discovered in our cycle 14 program. The other spectra were obtained in previous SCP SN campaigns and are shown to demonstrate ground-based spectroscopy out to z=1.4. For each spectrum, a matching template spectrum from a well-studied nearby SN is shown (dashed curves). }}}{9}}