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Assigned ID: 395
----- Attempting Submission 1 (Fri Apr 10 07:20:24 GMT 2015) -----
HST Phase I Proposal 395 (uv_frontier2.apt) successfully submitted.
Receipt: # 395-1
----- Attempting Submission 2 (Fri Apr 10 19:27:52 GMT 2015) -----
HST Phase I Proposal 395 (uv_frontier2.apt) successfully submitted.
Receipt: # 395-2
----- Attempting Submission 3 (Fri Apr 10 23:36:51 GMT 2015) -----
HST Phase I Proposal 395 (uv_frontier2.apt) successfully submitted.
Receipt: # 395-3
----- Attempting Submission 4 (Fri Apr 10 23:45:26 GMT 2015) -----
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
I have increased the post-flash levels in F336W exposures from 3 to 4 e-/pixel.
-162413669
----- Attempting Submission 1 (Tue Jul 07 20:52:26 GMT 2015) -----
----- Attempting Submission 2 (Tue Jul 21 18:57:52 GMT 2015) -----
In the Observing Description, I have justified the post-flash levels. I do not believe they're too high.
The Final UV Frontier: Legacy Near-UV Imaging of the Frontier Fields
The Hubble Frontier Fields (HFFs) are proving to be as scientifically interesting at z < 3.5, as at z>7, the epoch for which it was designed. In Cycle 21, we observed three HFFs with WFC3/UVIS near-UV (NUV) imaging (8 orbits each of F275W, F336W). Here we propose to image the remaining three fields (which offer higher magnification at z<1.5) to enable the following:
The high magnification provided by gravitational lensing enables study of star formation (SF) in dwarf galaxies at 0.75<z<1.5. With typical sensitivities of >0.03 M_sun/yr, we can study the burstiness of SF (by comparing to grism Halpha), the UV spectral slopes and extinction curves, and the sizes and luminosities of SF clumps on scales <100 pc.
The NUV identifies the Lyman break of dwarf galaxies at 1.5<z<3.5 that often have featureless continua, enabling measure of the global SF rate density at its peak epoch. This is the redshift range of 80% of multiply-imaged systems, the primary constraints on the cluster mass models. The NUV will help identify multiply-imaged systems, ensuring that the HFF program attains its stated goals.
At z~2.4, F275W can detect escaping Lyman continuum behind clusters much more efficiently than in the field.
Within cluster galaxies, the NUV provides a high-resolution probe of SF (>0.02 M_sun/yr) not available with existing data sets. We will characterize galaxies transitioning between the blue cloud and red sequence, including "jellyfish" galaxies with SF tails of stripped gas, and ellipticals and S0s with residual SF only apparent in the UV. Completing the sample will provide insight into how cluster mass and dynamical state affect quenching of cluster galaxies.
We are targeting the remaining three Frontier Field clusters (MACSJ0416, Abell S1063, Abell 370) with the WFC3/UVIS camera.
Filters and Depths:
We will observe each cluster for 8 orbits in both F275W and F336W. Because we are required to add post-flash to have a background of 12 e- in each exposure, our depth goes as the sqrt(number of exposures), regardless of exposure time. Thus, we are doing full-orbit exposures (as with our previous program, 13389) to minimize the number of exposures and maximize depth. We will be doing 4 orbit visits, with a standard four point dither pattern (WFC3-UVIS-DITHER-BOX) performed during each visit. Each visit will be offset in both x and y to cover the chip gap and to smooth out the "blotchy" dark structure that isn't fully removed (see Rafelski et al. 2015). Specifically, one dither pattern will be centered at (x=-0.42",y=-2.02") from the center coordinates and the other dither pattern will be centered at (x=0.42", y=2.02"). These offsets (POSTARGs) are 4.13" away from each other, ensuring that we can remove (or smooth out) artifacts smaller than this (like the blotchy dark pattern).
Pointing:
We will center the UVIS field (UVIS-CENTER aperture) at the same position as the Hubble Frontier Field WFC3/IR pointings. We will also use the exact same orientation to ensure that the coordinated parallels with ACS/WFC lie on the HFF parallel fields as well.
Post-flash:
The current recommendation to migigate charge transfer inefficiency (CTI) is to have a background of at least 12 e-/pix per exposure. This recommended level has apparently not increased as CTI increases. We want to ensure that all regions of the detector achieve this average level of flux. We have used our other UVIS observations to determine conservative (low) estimates for the expected background per orbit of 0 e-/pix in F275W and 6 e-/pix in F336W. However, both the WFC3 ETC and some of the exposures from program 13872 show that the expected background can be a bit lower in F336W (3-4 e-/pix). We also expect a dark current of nearly 5 electrons/pixel/0.75 hours (where 0.75 hours is the approximate exposure time). Thus, without post-flash, we expect a (conservatively low) background of >5 e- and >9 e- in F275W and F336W, respectively. Keeping in mind that some parts of the detector will have 20% less post-flash than the requested average, we then determine that we need 9 e- and 4e- in F275W and F336W, respectively. We believe this will result in > 12 e-, on average, in all regions of the detector.
Coordinated Parallels:
For coordinated parallels, we will allocate 10 orbits to F435W and 6 orbits in F606W, to approximately increase the exposure in these filters by ~55%. We use these filters because observations at these wavelengths will not be possible with JWST, but will nonetheless be very important for studying the rest-frame UV at 2<z<4.
COSMOLOGY
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