0
Assigned ID: 1592
----- Attempting Submission 1 (Thu Apr 08 03:01:44 GMT 2021) -----
HST Phase I Proposal 1592 successfully submitted.
Receipt: # 1592-1
----- Attempting Submission 2 (Fri Apr 09 00:01:24 GMT 2021) -----
HST Phase I Proposal 1592 successfully submitted.
Receipt: # 1592-2
----- Attempting Submission 3 (Fri Apr 09 13:39:12 GMT 2021) -----
HST Phase I Proposal 1592 successfully submitted.
Receipt: # 1592-3
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
0
----- Attempting Submission 1 (Thu Jul 29 02:22:55 GMT 2021) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 2 (Tue May 03 19:51:29 GMT 2022) -----
The recommendation for minimum WFC3/UVIS total image background (dark + sky +
postflash if needed) is now 20e-/pix in order to mitigate the current CTE losses.
The APT warnings can be disregarded.
Calibrating local estimators for the escape fraction of ionizing radiation 2.7Gyrs after the Big Bang
The escape fraction of ionizing radiation (f_esc), a fundamental parameter in modeling of reionization, is impossible to measure at z>6. Therefore, a number of HST studies are calibrating indirect indicators of f_esc, using large samples of local galaxies (z~0.3). What is missing is a comparable sample of galaxies at the highest redshifts where all the necessary observables (covering the full spectrum from 950AA to the rest frame optical) can be measured.
We propose a coordinated HST-NOIRLab program to observe a unique sample of 8 strongly lensed Lyman alpha (Lya) emitters at 2.1<z<2.6. THese observations will enable the measurement of their escape fraction of ionizing radiation and test for evolution in its indirect estimators. WFC3 UVIS imaging will directly measure the emission at ionizing wavelengths (LyC, lambda<912AA). Longer wavelength imaging will constrain the properties of the young stars, including the dust content and the sizes of the star-forming regions. The coordinated NOIRLab Gemini observations, consisting of rest-frame UV+optical IFU spectroscopy, will provide the diagnostics required to quantify the intrinsic ionizing radiation field, nebular dust content, and kinematics of the ISM. Only the combination of the strong magnification and redshifts of these galaxies allow us to perform these measurements, probing a completely unexplored regime of physical sizes (~100s~pc) and intrinsic luminosities (~1/1000 L*UV) at z>0.5. Our sample complement planned JWST programs that are targeting the rest-frame optical for known z~3 bright emitters.
This program images 8 lensed Lyman-alpha emitters in Lyman continuum (either with the F225W or F275W depending on redshift). Additionally, we obtain images in F438W and F814W. For the long UV integration times we utilize half-orbit exposures, with a large dither pattern, in order to minimize post-flash and read-noise, optimize PSF sampling, and enable cleaning of the cosmic rays. For each optical band we obtain at least 3 dithered exposure to ensure cosmic ray rejection. The dither pattern per visit is set 5 times larger than the default box pattern to help minimize the blotchy pattern observed in UV imaging (similar to that seen in Rafelski et al. 2015, AJ, 150 31, Figure 15).
The targets are placed on chip 2 using the UVIS2-C1K1C-CTE aperture, as this places the target centered in the bottom half of chip 2 in quadrant C, which has a lower geometrical distortion and improved focus.
The proposing team includes investigators with expertise in all necessary components of the program, both technical and scientific.
Scientific expertise
Our team includes experts on the problem of the measurement of the escape of ionizing radiation, its evolution with redshift, its link with the escape of Lya radiation, and the study and characterization of indirect indicators from low redshift galaxies to be used at z>4. Additionally, our group includes experts on modeling of gravitational lensing. We have consistently published on these and related issues, with more than 50 papers over the past decade.
Drs. Rutkowski, Scarlata, Teplitz, have lead a number of works on constraining the escape fraction from different types of galaxies, using both HST UV imaging (WFC3, ACS+SBC) and spectroscopy (ACS+SBC), Galex imaging, as well as ground based imaging and spectroscopy. Our work focus on galaxies spanning the full redshift, from galaxies in the nearby universe to objects at z~3.
Drs. Hayes, Henry, Scarlata are expert on the properties of Lyman alpha from galaxies, its resonant nature and how it can be used to trace the distribution of neutral hydrogen gas within and the outskirt of galaxies.
Drs. Hayes, Henry, Scarlata have substantial experience with observations and interpretation of rest frame UV spectra, both of local analogs of high redshift galaxies (e.g., the Green Pea extreme emission line galaxies, the Lyman alpha Reference Sample, etc) and high redshift Lyman Break Galaxies. Additionally, we have substantial experience in rest-frame optical diagnostics.
Technical Expertise
Dr. Rafelski lead the reduction effort for the UV-UDF project (PI-Teplitz) and is a collaborator on CANDELS, and the UV-Frontier Fields (CoPI Scarlata). He is an expert in the reduction and analysis of WFC3 UV imaging data, including the characterization and correction for the charge transfer inefficiency and proper super-darks.
Many of the team members are part of the large UV-UDF (PI: Teplitz) as well as UV-CANDELS (PI: Teplitz). This ensures that we have extensive experience required to design and run UV programs with the WFC3.
Our team also has substantial experience in ground based optical spectroscopy from large ground-based telescopes.
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