We propose ACS, NICMOS, and Chandra observations of the central region of the extraordinary and newly discovered galaxy cluster: RCS2-2327.4-0204 at z=0.700. This cluster shows 3 or more arcs in ground-based imaging, with an Einstein radius of 49". Such a large Einstein radius (3-4 times larger than seen in most clusters) has been seen in precisely one other cluster in the universe - namely Abell 1689 at z=0.18. From our proposed data we expect to see ~70 lensed source images, from ~20 image families. We will use both strong and weak lensing constraints from these data to construct the central mass profile of the cluster, which, when combined with ground based data extending to a half degree FOV, will allow us to measure critically important dark matter halo parameters (such as concentration). The target cluster is selected from a large ongoing survey with a well-defined search volume, which allows us to compare our results to expectations from simulations. We will also compare the lensing derived mass profiles to the x-ray equivalent measures; this will illuminate whether the dominant baryonic component is in equilibrium with the potential. The area of high magnification behind this cluster is an order of magnitude larger than typical lensing clusters observed previously by HST; this order of magnitude increase in area directly translates into a 10 times better chance for finding very high redshift galaxies. Many of the highest redshift galaxies found to date have been found behind massive lensing clusters observed by HST, and we expect to add to that sample dramatically.

This program aims to take deep multi-color imaging of a very massive high-redshift galaxy cluster, for the principal purpose of constraining the core mass distribution using strong lensing. The cluster seems comparable to the famous Abell 1689 which was observed by the ACS GTO team, albeit at a much higher redshift, and we expect equally impressive arcs. Ground based imaging already shows a number of bright arcs, and HST is expected to uncover many more. The HST observation consists of 10 orbits with ACS, from which we will identify strong lensing features (center of image) and make measurements of the weak lensing shear at larger cluster-centric distances. 12 orbits with NICMOS provide further information on the cluster core, with coordinated ACS parallels providing additional weak-lensing shear measurements at larger radii from the principal target. The plan proposed and approved in Phase 1 calls for 3 orbits in each NICMOS filter (F110 and F160), repeated at two orientations separated by 45 degrees. This target is acessible from orients of 209.63-273.83 (a range of 64.2 degrees) ; this is hopefully sufficient to to allow for scheduling. A quick check of visit scheduling with and without the specified orientation constraints shows it makes little difference to the overall availability of the visits. The purpose of dividing the data into two orients is twofold: 1) the stacked NICMOS final images more closely sample an ideal circular FOV (lensed arcs are to first order distributed in a circular fashion about the cluster center) and 2) this splits the parallels across two fields which provides 2x better sampling of the shear wrt to azimuth. In scheduling the visits this has been done by allowing the first visit to have free orient, making the second (other filter) match, and then specifying visits 3 and 4 at -45 degrees off of the orient of visit 1. The simplist natural way to divide the 3 orbits in each filter at each orient into four mosaiced pointings is to do 3 dither positions at each mosaic position. Consequently canned dither routines would be broken up across orits (which the APT did not like!) and so we have defined each dither position separately. This seems to have no significant impact on orbit packing. ACS observations in the F814W and F606W filters occupy four orbits each, divided into a total of 4 2-orbit visits. Each orbit contains four exposures in a small box dither, and in aggregate the two visits for each filter sample 4 principal positions, arranged to maximise the radial coverage while providing greater depth in the strong lensing region of the target (i.e. the region covered by the NICMOS observations). The orients have been fixed to be the same as Visit 1, since this gives best azimuthal sampling angle wrt to the parallels. This constraint can be relaxed if it significantly impacts scheduling. The final ACS observation is a 2-orbit visit in F435W to provide bluer sampling of the arcs in the central region; each orbit again is divided into 4 exposures in a small box dither, with each orbit offset slightly to opposites side of the target center to provide sampling across the chip gap. Note NO crsplitting has be used throughout. The ACS parallel observations use only the F606W and F814W filters (we have arbitrarily paired F606W with the NIC-3 F110W observations, and F814W with NIC-3 F160W). The 'four-pointings-per-orbit' strategy adopted for the NICMOS tiling naturally also allows for 4 ACS parallels per orbit. The current Phase 2 configuration generates a significant number of 'POS TARG OUTSIDE OF APERTURE' warnings for visits 1-4 (NICMOS). These are due to the 4-point mosaic - the fiducial target center at the center of the 4 pointings is indeed often outside the aperture, by design. 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