0Assigned ID: 653
----- Attempting Submission 1 (Fri Apr 08 18:19:01 GMT 2016) -----
HST Phase I Proposal 653 (morphology_density_z=2.3.apt.2015_04_10_21_38.aptbackup.2016_04_07_08_58.aptbackup) successfully submitted.
Receipt: # 653-1
----- Attempting Submission 2 (Fri Apr 08 18:23:58 GMT 2016) -----8/18/17 - Royle - Opened ORIENT on visit 06 to allow scheduling in 20171180129101----- Attempting Submission 1 (Wed Jul 20 20:51:40 GMT 2016) -----
HST Phase II Proposal 14760 (14760.apt.2016_07_14_19_14.aptbackup) successfully submitted.
Receipt: # 14760-1
----- Attempting Submission 2 (Thu Jul 21 06:12:46 GMT 2016) -----
HST Phase II Proposal 14760 (14760.apt.2016_07_14_19_14.aptbackup) successfully submitted.
Receipt: # 14760-2
----- Attempting Submission 3 (Sun Sep 18 08:10:29 GMT 2016) -----
----- Attempting Submission 4 (Sat Aug 19 01:10:47 GMT 2017) -----in-house processingImaging a Massive Galaxy Overdensity at z=2.3: The Morphology-Density Relation at High RedshiftWe propose deep HST/WFC3 imaging in the density peak area of BOSS1441 protocluster at z = 2.32 traced by an extreme rare group of Ly-alpha absorbers and multiple quasars. This structure is selected from the large survey volume of 1 Gpc^3 covered by SDSS, and is the most overdense and robustly established cluster-sized overdensity at z ~ 2. This massive structure centered on a 7' x7' (12 Mpc x 12 Mpc) sub-region has the highest galaxy overdensity of 10.8+/-1.0, anchored by the largest and most luminous Lyman alpha nebula known at z>2. In this area, our Keck+ LBT observations have obtained the spectra for the unique Ly-alpha nebula, 20 strong Ly-alpha emitting galaxies at z=2.32+/-0.02, and 110 Lyman break galaxies (i < 24.5). This field is also covered in complete wavelength observations from U-band to K-band using ground-based imaging. Here we propose to use nine HST/WFC3 pointings to cover this central region in 9 orbits. We will measure the detailed rest-frame optical morphology of this sample, to determine whether the universal morphology-density relationship observed in the low-redshift universe is already in place in and around most overdense region at z ~ 2. We will also probe the powering mechanism of the largest Ly-alpha nebula, testing if this nebula is powered by merging of separated galaxies. Combining the new HST observations with the existing multi-wavelength imaging ranging from 0.3 - 2.3 microns, optical spectroscopy, and narrow-band imaging, we will provide a complete sample of galaxies in the most massive protocluster at z=2 which could be evolved into the most massive galaxy clusters (10^15 M_sun) in later epoch.Brief Summary of Science:
In our program, we will conduct the deep WFC3 imaging in the most massive protocluster field, BOSS1441, at z=2.32. This field contains a galaxy overdensty compared to the random fields on a large scale of 15 Mpcs. We will use HST WFC3/F160W deep imaging to conduct deep imaging, and study the density-morphology relation in this extremely overdense field in the early Universe.
Description of observations:
Our project contains 9 orbits. In this project, we have 9 targets, with each target representing a different pointings. We will use these 9 different pointings to map the BOSS1441 field. We use 1-orbit for each pointing. Each pointing contains 7 - 15 galaxies that resides at z~ 2.3 and we need to measure the morphology for these galaxies. These galaxies are randomly distributed in the WFC3 field of view.
We have a special setting: we need to set the position angle (PA) for each pointings to specific degree range (typical PA for our fields are ~20 deg). The PA means the angle from the North to the longer axis of the detector, north-east direction. From the current Phase-II, we tentatively set a Orientation Range for each visit, with the minOrient of ~60 and maxOrient of 70 deg. This number is calculated by us and could not be 100% precise. Our purpose is to achieve a PA for each visit. Note we can add 180 deg to any current PA requirements we listed.
For cosmic ray rejection, we use 5 different exposures to populate each orbit. We checked the HST instrumentation handbook and we found it suggests a 5 different exposures to populate a ~3000 sec exposure for a complete rejection of cosmic rays. Specifically, we use a standard 4-point small-scale dither pattern and plus an additional exposure to populate each orbit. We think these arrangements enables us to reject cosmic ray, and provide a half-pixel subsampling of the point-spread function (PSF) for each pointing.
We use a total two visits to populate our 9 orbits. The first visit has 5 orbits. For each orbit in the first visit, we use NSAMP= 12, SPARS=50 for the first four exposures, and NSAMP=10, SPARS=50 for the fifth exposure. The second visit has 4 orbits and we use NSAMP=11 for the first four exposures and NSAMP=13 for the fifth orbits. We use IR-FIX to center each pointing, enabling to perfectly center the pointing in the detector. Our galaxies are randomly distributed in each pointings.GalaxiesfalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYLYMAN ALPHA CLOUDJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000GALAXYHIGH REDSHIFT GALAXYJ2000GALAXYHIGH REDSHIFT GALAXYJ2000GALAXYHIGH REDSHIFT GALAXYJ2000GALAXYHIGH REDSHIFT GALAXYJ2000GALAXYHIGH REDSHIFT GALAXYJ2000GALAXYHIGH REDSHIFT GALAXYJ2000GALAXYHIGH REDSHIFT GALAXYJ2000WFC3/IRImagingNoNoF160WPOS-TARGDITHER0.572LINE0.365falsefalse74.653418.528WFC3-IR-DITHER-BOX-MIN1falseThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.(Tic-Visit
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