All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4502F1.ps} \end{figure}$ Figure 1: Plotted above are the values of $\Sigma _{{\rm crit}}^{-1}$ as a function of background galaxy redshift for four lens redshifts. The redshifts of the lenses (0.1, 0.25, 0.5, and 0.8) can be determined from where $\Sigma _{{\rm crit}}^{-1}$ becomes 0. While the lower redshift lenses have $\Sigma _{{\rm crit}}^{-1}$ only slowing varying over the expected faint galaxy redshift distribution ( $\sim$ 0.8-2), the higher redshift lenses still have $\Sigma _{{\rm crit}}^{-1}$ being a strong function of background galaxy redshift.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4502F2.ps} \end{figure}$ Figure 2: Shown above are the best fit values for the mean lensing redshift of the background galaxy population as a function of $\bar{\Sigma}_{{\rm ann}}$ , which is the mean surface mass density in the negative annular region for $\zeta _{\rm c}$ (Eq. (7)), for the five clusters with complete X-ray data. The solid lines are the best fit, and the dashed, dot-dashed, and dotted lines are the 1, 2, and 3- $\sigma$ deviations from the best fit respectively. The vertical lines, with associated error bars, are the surface density for the annular region calculated from the best-fit X-ray $\beta$ -model. The horizontal lines, with associated error bars, are the mean lensing redshift calculated from the HDF-S photometric redshift catalog of Fontana et al. (1999) using the same magnitude and color cuts as in the observed data.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4502F3.ps} \end{figure}$ Figure 3: Shown above are the best fit values for $\Sigma _{{\rm crit}}^{-1}$ from comparing the X-ray $\beta$ -models with the weak lensing shear profiles as a function of cluster redshift. The horizontal bars intersecting the error bars indicate how much of the error bar is due to the errors in the weak lensing mass measurement, with the remainder due to the uncertainties in the X-ray mass measurement. The four solid curves are the values of $\Sigma _{{\rm crit}}^{-1}$ for background galaxies at redshifts of 1, 1.5, 2, and 3. The dashed curve, with error bars, shows the value of $\Sigma _{{\rm crit}}^{-1}$ from the HDF-S photo-z galaxy catalog.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4502F4.ps} \end{figure}$ Figure 4: Shown above are values for the mean shear for the background galaxies, divided into four magnitude bins (23-24, 24-25, 25-25.7, and 25.7-26.3), relative to the mean shear of the brightest magnitude bin. Only galaxies located further than 350 h^-1 kpc from the cluster centers were used to compute the mean shear. The mean shear of the three $z\sim 0.55{-}0.6$ clusters are given by the open circles and the mean shear of the three $z\sim 0.8$ clusters are given by the open squares. The filled circles and squares are the expected shear levels based on the photometric redshifts of the HDF-S galaxies in the same magnitude bins for clusters at z=0.55 and z=0.8 respectively.
Open with DEXTER

In the text