0Assigned ID: 193
----- Attempting Submission 1 (Thu Apr 04 14:47:53 GMT 2019) -----
HST Phase I Proposal 193 (z910.apt) successfully submitted.
Receipt: # 193-1
----- Attempting Submission 2 (Fri Apr 05 03:25:10 GMT 2019) -----Be very careful mixing POS TARG and Center_Pattern = Yes
Be very careful mixing POS TARG and Center_Pattern = YesApproved Target update to visit 10 - added POSTARG-979567957----- Attempting Submission 1 (Tue Jul 23 16:51:13 GMT 2019) -----
----- Attempting Submission 2 (Fri May 15 21:53:52 GMT 2020) -----
HST Phase II Proposal 15862 successfully submitted.
Receipt: # 15862-2
----- Attempting Submission 3 (Tue May 19 15:53:02 GMT 2020) -----
----- Attempting Submission 4 (Thu Jun 04 14:54:34 GMT 2020) -----Target not included has been removed.Confirmation of a Large, Robust Sample of z=9-10 Galaxies in the CANDELS FieldsThe galaxy population at z > 8 probes the earliest phases of galaxy evolution, constraining the physical processes regulating gas cooling and star formation. Previous studies using an incomplete filter set found few galaxies at z > 9, implying a sharp drop in the star formation rate (SFR) density. This would be inconsistent with the observed increase in the stellar-mass to halo-mass (SMHM) ratio from z=4 to z=7. Either this SMHM evolutionary trend reverses course just before z=8 (disfavored by the data), or the SFR density at z>9 is larger.
We have built a sample of 11 bright (H<26.5) z=9-10 candidate galaxies in the CANDELS fields, 3X larger than previous samples in these fields, leveraging a HST+Spitzer photometric redshift selection method. This sample favors continued SMHM evolution, but most candidates have significant integrated redshift probability at z < 8 due to incomplete photometric coverage.
We propose followup F105W and F140W imaging that will cover gaps in the wavelength coverage - a robust measurement in F105W will reject lower-redshift solutions, while a detection in F140W will provide a second detection band, ensuring no sources are spurious. This imaging can be accomplished in only 14 orbits, an efficient use leveraging thousands of archival HST orbits and Spitzer/IRAC hours invested in these fields.
Studying these earliest galaxies is one of the main science themes of the James Webb Space Telescope (JWST). Our proposed followup F105W and F140W imaging will yield a reference sample of robust z=9-10 candidate galaxies ready for spectroscopic observations in JWST Cycle 1 (six candidates are in a field due to be observed by a selected ERS program).In this program, we are observing candidate z > 7 galaxies in F105W (1 orbit), to confirm the Lyman break, and in F140W (1 orbit), to better constrain the UV spectral slope. We construct one visit for each source, of either 1 or 2 orbits, depending on whether it needs one or both filters. We set up our exposure to obtain 8 independant dither positions in one orbit, doing a 4-exposure dither blob sequence, then doing a small offset, and repeating. We initially center each pointing on our object of interest, and then explore whether they need to be shifted, either due to proximity to a very bright star, or the edge of existing data. We only shift one pointing, EGS44164 (visit 2), by 20" to the SW, to keep the full F105W frame on top of the existing CANDELS F160W imaging. However, our source of interest is still near the center. We do not require any ORIENT constraints.Our team has a strong track-record for the timely reduction and publication of results based on HST data products. PI Finkelstein is an expert in galaxy evolution at high redshifts, and has played key roles in the planning, execution, and reduction of data from several previous HST WFC3 and ACS programs, including the CANDELS multi-cycle treasury program, the Frontier Fields DDT program, the FIGS and CLEAR large WFC3 grism programs, and the upcoming CEERS JWST ERS program. His analysis of these HST data has led to ~10 first author papers, and ~5 from his students and postdocs. Relevant expertise on the team includes: efficient observation planning (Co-I's Grogin and Lotz), HST data reduction (Co-I's Koekemoer and Bagley), detailed knowledge of noise and persistence properties of WFC3 (Co-I's Pirzkal and Ryan), and years of experience selecting and analyzing extremely distant galaxies (Co-I's Dickinson, Ferguson, Giavalisco, Lotz, Papovich, Song) and accompanying theory work (Co-I's Somerville and Snyder). Co-I's Larson, Jung and Rojas are students working with team leaders, who will perform facets of the analysis.Galaxies and the IGM6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYOffset a few arcsec from the source to put more of the image on the CANDELS fieldJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000WFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF140WPOS-TARGDITHERDITHER45.183WFC3-IR-DITHER-BOX-MINfalse74.653true0.3650.572241.859POS-TARGWFC3-IR-DITHER-BLOB18.5281trueThe scheduling data was generated by CASM 28.0.CASM was run in Phase II mode.1577471381000306.5790015378072(Tic-Visit
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