Assigned ID: 912 ----- Attempting Submission 1 (Fri Feb 24 23:30:04 GMT 2012) ----- HST Phase I Proposal 912 (FLS.apt) successfully submitted. ----- Attempting Submission 2 (Fri Feb 24 23:47:11 GMT 2012) ----- HST Phase I Proposal 912 (FLS.apt) successfully submitted. ----- Attempting Submission 3 (Sat Feb 25 00:04:31 GMT 2012) ----- resubmission on August 3 to correct for > 10 mins ACS exposures (in response to an email from Ralph on August 3rd). ----- Attempting Submission 1 (Wed Jun 27 21:55:45 GMT 2012) ----- HST Phase II Proposal 13045 (HST_phaseII_13045v2.apt) successfully submitted. ----- Attempting Submission 2 (Wed Aug 01 01:45:33 GMT 2012) ----- HST Phase II Proposal 13045 (HST_phaseII_13045v3.apt) successfully submitted. ----- Attempting Submission 3 (Fri Aug 03 20:14:29 GMT 2012) ----- We propose HST/WFC3 and ACS observations in 5 bands to characterize the nature and the environment of the most distant sub-mm galaxy (SMG) known today, FLS3, at a redshift of 6.337. The galaxy was discovered in Herschel-HerMES with redshift measured from mm-wave spectroscopy. It is IR luminous (3x10^13 L_sun), gas rich (10^11 M_sun), dusty and star-bursting. Deep optical and K-band ground-based imaging showed a near-by galaxy at 0.5 arcsecond from FLS3 with a measured redshift of 2.1. HST resolution imaging are needed to properly separate the two galaxies and constrain a lensing magnification of FLS3, if any. Previously known z < 4 SMGs are in dense proto-cluster environments. The discovery of FLS3 suggests that it may also be in a proto-cluster. The HST imaging is also aimed at identifying Lyman dropout samples at z~6.4 associated with FLS3. With proposed data we will complete the SED and determine the stellar mass of FLS at better than 30%, a key quantity needed to understand the nature of FLS3 when combined with its star-formation rate. We will also measure the UV slope-SFR relation for a galaxy at z > 6 and compare to measurements at z~0 to 3. With dropouts we will establish the presence of a proto-cluster and establish the dark matter halo mass scale of FLS3, a key ingredient needed to connect its evolution with massive elliptical and other galaxies seen today. The program is related to a detection and characterization of a extremely luminous and massive dusty, starburst galaxy (hereafter FLS3) found with Herschel at z=6.34, during the epoch of reionization, and its environment. The galaxy is detected in a deep LGS-AO image with KeckII/NIRC2 in the K-band with a AB magnitude of 23.5. The most basic goals of this program involving deep WFC3 and ACS observations of FLS3 are (i) determine the rest-frame UV SED, (ii) determine the location and size of the foreground galaxy at 0.500 away for a lens model, and (iii) identify other z =6.3 galaxies to determine the FLS3 environment and estimate the proto-cluster, if there is one associated with FLS3. To measure stellar mass and other properties of FLS3 we make use of WFC3/F160W,F125W, and F105W filters. ACS/F814W observations are needed to look for z=6 dropouts and to characterize the foreground lensing galaxy. We have used the on-line calculator to estimate the exposure time necessary to detect the background source with a signal-to-noise ratio (SNR) >10 in the WFC3 bands. The expected depths are obtained after scaling a range of SED templates to the K-band detection. These SEDs are appropriate for dusty starbursts and range from Arp220 to the average sub-mm galaxy SED at z of 2 to 3. We take the lowest flux density expected and require 10 sigma detections. The total of 6 HST orbits are distributed to 3 WFC3 bands and 1 ACS/F814W band. The ACS band in the optical allow a precise detection of the nearby z=2.1 galaxy about 0.5 arcseconds away from FLS3; at the shortest optical band, FLS3 is a dropout and we can measure the size and mass of the foreground galaxy accurately for a precise lensing model. A quantification of the lensing magnification is one of the goals of the approved HST program. The immediate environment of FLS3 will be characterized with a combination of F814W, F105W and F125W images. The extended environment of FLS3, overlapping with two other sources seen within 3 to 6 arcminutes from JCMT/SCUBA2 will be imaged with coordinated-parallel observations using ACS/F814W taken over 4 orbits. To cover the interesting sub-mm/mm SCUBA2 detected targets within 3 to 6 arcminutes of FLS3 we request coordinated-parallel observations that involved WFC3 and ACS over 4 orbits. These observations require the orientation to be 10 and 120 degrees to maximize the ACS coverage of the intersting sources. The two orbits with ACS/F14W imaging that is mosacing the region around FLS3 also require a range of possible orientations. They range from 60 to 160 degrees and 240 to 340 degrees. COSMOLOGY 12 false 0.0 0.0 false false false false SUPPORTED GALAXY HIGH REDSHIFT GALAXY PROTOGALAXY J2000 J2000 K-band (2.146 microns) 1.46 muJy (23.5 AB) WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F098M ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F814W POS-TARG DITHER 0.572 LINE 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 1 false POS-TARG MOSAIC DITHER 2 45.00 ACS-WFC-DITHER-LINE false false 3.011 2 90.0 POS-TARG ACS-WFC-MOSAIC-LINE 85.28 2 true 1344024673372 /private/var/folders/kn/pslb0xt88v55zk006s6hv7mr0000gn/T/OPVisit8429407847308375146.xml The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. 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