0Assigned ID: 758
----- Attempting Submission 1 (Fri Apr 08 20:03:24 GMT 2016) -----
HST Phase I Proposal 758 (HST_Phase1_APT.apt) successfully submitted.
Receipt: # 758-1
----- Attempting Submission 2 (Fri Apr 08 20:37:24 GMT 2016) -----SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATEResubmitted with shorter single-orbit visits that fit within SCHED100 timing constraints to enable scheduling in Cycle 24.
These visits have 3-week windows in Jan/Feb 2017 as opposed to just 3 days for the longer two-orbit visits. Please see further
discussion in Change Request #85569. We acknowledge the warning for Same-Pos-As, which is required to ensure that all exposures in
the visit are taken at the same POS TARG position.1980247192----- Attempting Submission 1 (Tue Jul 12 22:45:07 GMT 2016) -----
----- Attempting Submission 2 (Sat Sep 03 15:56:34 GMT 2016) -----There was a warning about "same POS may not be appropriate", but we think this
observational setup is correct. Co-I Brammer checked this phase II in detail,
and we believe that we should not need to worry about this warning.A Chance Alignment: Resolving a Massive Compact Galaxy Actively Quenching at z=1.8Using HST imaging from the Sloan Giant Arcs Survey, we have identified a strongly-lensed massive (log M/Msun = 10.4) red galaxy at z=1.8 that is remarkably compact (r~0.7 kpc). This galaxy, 0851-E, is already structurally similar to quiescent, massive galaxies and appears to be in the process of quenching, with a gas fraction <10%. Using WFC3/G141 grism spectroscopy, we propose to measure age gradients and emission line diagnostics ([OIII]/Hbeta) in the inner 1 kpc and in the outskirts. This spatially resolved study will enable us to distinguish between physical mechanisms that are hypothesized to form and quench star-formation in massive galaxies, leading to the eventual buildup of the red sequence. Resolved spectroscopic studies of compact galaxies are only possible due to the lensing magnification and distortion, which boosts HST's already excellent spatial resolution; these observations will develop necessary analysis tools for the JWST era. This novel HST program will be the first study to spatially resolve the stellar populations and emission line diagnostics of a compact star-forming galaxy that is "running on empty". We will provide strong constraints on the physical mechanisms driving a short-lived but key phase of massive galaxy formation.The goal of this program is to obtain a deep WFC3/IR grism spectrum of a bright (H=20.7 mag) quadruply lensed compact star-forming galaxy in the Sloan Giant Arcs Survey (08:51:40.03, +33:30:49.86). We will observe this source for a total of 12 orbits at two different orientations, which were selected to minimize contamination of the resulting grism spectrum from neighboring sources. The central coordinates for the observations will be matched to the original HST/GO program 13003 (PI: Gladders; 08:51:38.9810, +33:31:10.83) in which this target was discovered, facilitating ancillary science.
Our observation strategy is to obtain 6 visits of one orbit at two different orientations. Each visit contains one short pre-image of either F160W or F105W each followed by two long G141 grism exposures to fill the orbit. The six separate visits are dithered following our successful 4-point dithering strategy used for the 3D-HST survey (e.g., Brammer et al. 2012). I.e. we set POS-TARG: (0,0) (1.355,0.424) (0.881,1.212) (-0.474,0.788). The F160W direct image filter is chosen as it both overlaps with the G141 grism to allow calibrations, but will also increase the depth of the existing 1200s F160W image. The F105W direct image filter similarly overlaps the G141 grism at the bluest wavelengths to allow calibrations, and will be adding vital photometric coverage of the 4000 Angstrom break of our target galaxy. The existing HST images in this field include F390W, F814W, F125W and F160W. Adding F105W will cover a key wavelength range for the pixel-by-pixel analysis of the main target, while also satisfying the requirements for a direct image.
We estimate that the spacecraft will leave the earth shadow at the *end* of the orbit in Jan/Feb 2017, so we put the direct imaging exposures at the end of the orbit as these are less sensitive to the helium airglow backgrounds observed out of the shadow. This will minimize the impact of background variations on our G141 science exposures. The requirement for the non-interruptible sequence is done to avoid these highest backgrounds at the end of the physical spacecraft orbit.
The aperture is set to GRISM1024, which uses the same reference pixel and definition for both the direct image and the G141 grism. G141 exposures use SPARS100 sampling with NSAMP=13, and F160W/F105W exposures are taken with SPARS50 with NSAMP=6.
Through simulating the grism observations with the existing F160W imaging, we have identified the best roll angles to be ORIENT = 165 and 171, optimally reducing the contamination from nearby objects. We submit 6 visits of 1 orbit duration. Visit 1A has a constraint between ORIENT=165, with Visits 1B-1F adopting the same ORIENT as Visit 1A. Visits 2A-2F will need to be offset by 6 degrees to control systematics and contamination. We request that Vists 2A-2F are taken at the same orient, offset by 6 degrees from Visits 1A-1F, and we have set the "Same Orient as" special requirement accordingly. We note that allowing the ORIENTs to range between 165 and 171 does not improve the scheduling window, but does reduce the potential data quality. These ORIENT constraints and visit lengths allow a three-week window from 1/25/17-2/16/17 for the observations.Galaxies0falsefalsefalsetruefalsefalseSUPPORTEDCLUSTER OF GALAXIESGRAVITATIONAL LENSJ2000J2000H(F160W) = 20.7 ABmagWFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141Hst Same orient constraint links visits (1A 1B 1C 1D 1E 1F)The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode./private/var/folders/0b/8fmqw_g129b_bntxwg1093xw00038r/T/OPVisit1865029195949716415.xml(Tic-Visit
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