Positions of pointings realigned using the orients assigned by Tony. Thank you very much for being so accommodating. -1642785759 ----- Attempting Submission 4 (Fri Jun 21 12:32:19 GMT 2013) ----- Longevity of dark matter substructure in Abell 3827 We will investigate the interaction properties of dark matter, through the infall of substructure into a galaxy cluster with a rare dynamical history. Abell 3827 appears to have grown rapidly through several simultaneous mergers, and currently hosts the stellar remnants of five massive elliptical galaxies within 15 kpc of the core. Only one other well-studied cluster (Abell 2261) contains a distribution of baryonic matter that is even comparably corrugated - and a strong lens threaded through the core of Abell 3827 provides a unique gravitational handle on its distribution of dark matter. We will measure the late-stage dissipation of the dark matter halos that would have initially accompanied the infalling galaxies. The timescale for this dissipation is a key ingredient in models of structure formation. Most interestingly, our analysis of extant ground-based data also found dark matter offset from its stellar counterpart. This is predicted by numerical simulations if dark matter has (even a small) self-interaction cross section. If confirmed by a robust HST analysis, this result would achieve the same level of impact on fundamental physics as did HST confirmation of the Bullet Cluster offset between dark matter and gas. Constraints on both the tidal gravitational stripping and electroweak interactions of dark matter will be especially aided by the simultaneous measurement of multiple substructures within this single extended halo. This project will require UV, optical and NIR imaging, plus a combined strong-lensing, weak-lensing and flexion analysis. We request six orbits with WFC3/UVIS, ACS/WFC and WFC3/IR, and will also exploit new Chandra data already in the archive. Multiband imaging with ACS/WFC, WFC3/UVIS and WFC3/IR of a single galaxy cluster. None. None. There is a brightish (V=12.1) star nearby. The specified orients have been chosen to avoid that star. Different orients would also be acceptable; but if the orient changes, the POS TRAGs must also change. COSMOLOGY 12 false false 0.0 0.0 false false false SUPPORTED CLUSTER OF GALAXIES GRAVITATIONAL LENS MULTIPLE NUCLEI RICH CLUSTER ABELL3827 A3827 J2000 J2000 CLUSTER OF GALAXIES GRAVITATIONAL LENS MULTIPLE NUCLEI RICH CLUSTER ABELL3827 A3827 J2000 J2000 CLUSTER OF GALAXIES GRAVITATIONAL LENS MULTIPLE NUCLEI RICH CLUSTER ABELL3827 A3827 J2000 J2000 CLUSTER OF GALAXIES GRAVITATIONAL LENS MULTIPLE NUCLEI RICH CLUSTER ABELL3827 A3827 J2000 J2000 WFC3/IR Imaging No No F160W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W WFC3/UVIS Imaging No No F336W POS-TARG DITHER DITHER 2 6.10486 Perform subpixel dithering, and ensure that there are at least 3 exposures across the ACS/WFC gap. LINE false false 3.08553 2 91.16385 POS-TARG LINE 85.38987 1 true POS-TARG DITHER DITHER 2 5.183 WFC3-IR-DITHER-LINE false true 0.636 2 41.859 POS-TARG WFC3-IR-DITHER-BLOB 131.788 3 true POS-TARG MOSAIC DITHER 2 2.4 WFC3-UVIS-MOS-DITH-LINE false false 0.119 3 85.754 POS-TARG WFC3-UVIS-MOS-DITH-LINE 33.606 2 true The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. /Users/rjm/Documents/proposals/telescope/2012/HST_Phase_II/OP-cache/A3827_Jun2013_postflash_postargs-v01.xml The F814W imaging should occur immediately after the F606W imaging and with the same orientation, to maximise thermal stability during the F814W exposures. To achieve full depth near the cluster core, one ACS/WFC detector covers it on both orbits; to enlarge the field of view, a different detector is centered for each orbit, with the other one covering an outlying region. 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