ORIENT constraints improved (relaxed) for ACS visits 01 and 02 to facilitate scheduling in summer 2018.1852342689----- Attempting Submission 2 (Wed May 30 21:45:30 GMT 2018) -----A precise measurement of the mass distribution of the massive cluster lens eMACSJ1341.9-2442We propose multi-band imaging with ACS and WFC3 for a gravitation-lensing measurement of the mass distribution in the core of the massive galaxy cluster eMACSJ1341.9-2442 (z=0.835), responsible for the 30-fold magnification of eMACSJ1341-QG-1 (z=1.59), a recently discovered quiescent galaxy that is representative of ultra-compact early-type galaxies at z~1.5.
The goal of the requested observations is to reveal additional strong-lensing features that will allow us to create a robust lens model, thus permitting us to reconstruct the lensed galaxy's intrinsic properties in the source plane as a critical prerequisite for an in-depth, spatially resolved study of the properties and quenching mechanisms governing the evolution of this still poorly understood population of galaxies.
As a bonus, the proposed observations will reveal cluster substructure on scales of tens of kpc and hence clues to the merger geometry and formation history of one of the most massive clusters known at z>0.8.Building on the existing WFC3 F110W/F140W SNAPshot images of the core of eMACSJ1341.9-2442, this program will add substantially deeper observations at higher resolution in F606W and F814W (both ACS), as well as additional imaging in F105W and F140W (both WFC3). All observations will use dithering to ensure coverage of chip gaps, as well as efficient removal of artifacts and cosmic rays.
To maximize our ability to detect and identify multiple-image families from the matching colors and morphologies of all family members, we devote two orbits each to observations in ACS/F606W and F814W and (acknowledging the higher throughput of WFC3) a single orbit to imaging with WFC3, split 2:1 between F105W and F140W. The chosen uneven split between the two NIR passbands will result in even 2/3-orbit coverage across both filters, once the existing 1/3 orbit in F140W is added.
We minimize time losses incurred by buffer dumps by chosing sufficiently long integration times. For ACS, this means two sets of exposures in a box pattern, resulting in eight integrations for each filter (average exposure time per integration: 560s); for the WFC3 observations we use three sets of exposures along a 2-position line dither for our F105W observation and a single set of exposures in a 3-position line pattern for the F140W observation, each exposure being 278s long.CosmologyGalaxies and the IGM3falsefalsefalsefalsefalsefalsefalseSUPPORTEDCLUSTER OF GALAXIESGRAVITATIONAL LENSJ2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF140WPOS-TARGDITHERDITHER43.034ACS-WFC-DITHER-BOXfalse68.14true0.1920.262285.29POS-TARGACS-WFC-DITHER-LINE18.391truePOS-TARGDITHER0.605LINEfalsefalse341.788WFC3-IR-DITHER-LINE-3PT2falsePOS-TARGDITHER0.636LINEfalsefalse241.788WFC3-IR-DITHER-LINE3falseThe scheduling data was generated by CASM 26.0.CASM was run in Phase II mode./private/var/folders/bf/0pxwhb748xlfn8001s6vx6y00000gp/T/OPVisit146146834082250785.xml(Tic-Visit
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