0 Assigned ID: 1115 ----- Attempting Submission 1 (Wed Feb 27 09:03:38 GMT 2013) ----- HST Phase I Proposal 1115 (1558_hstcycle21.apt) successfully submitted. ----- Attempting Submission 2 (Wed Feb 27 23:56:54 GMT 2013) ----- HST Phase I Proposal 1115 (1558_hstcycle21.apt) successfully submitted. ----- Attempting Submission 3 (Fri Mar 01 11:58:33 GMT 2013) ----- I resubmited the phase II proposal after revising it. The points we have revised are as follow. (1) We reduced the number of orbits per one visit. Thus, our observation consists of 5 visits with 2 orbits each. (2) We changed the parameters for WFC3 exposure. We use SPARS50 exposures with NSAMP of 14. (3) In connection with the revision (2), we chaged the dithering pattern of WFC3 observation which is eight points dithering defined by "WFC3-IR-DITHER-BLOB". Finally, I also update the "Observing Description". 1329138029 ----- Attempting Submission 1 (Fri Jun 21 02:41:32 GMT 2013) ----- HST Phase II Proposal 13291 (hayashi_phase2_cycle21.apt) successfully submitted. ----- Attempting Submission 2 (Mon Jul 22 01:02:50 GMT 2013) ----- Resolving internal structures of the progenitors of early-type galaxies in a vigorously forming cluster at z=2.5 In our recent near-infrared narrow-band imaging surveys, we have identified the densest complex of Halpha emitters associated to a radio galaxy at z=2.5. Together with a large statistical excess of massive red galaxies (Distant Red Galaxies: DRGs), this region is probably the best candidate of a proto-cluster which is destined to evolve to a rich galaxy cluster today dominated by early-type galaxies. Therefore we are surely witnessing the clustered vigorous formation of the progenitors of present-day early-type galaxies. As such, this proto-cluster serves us the unique opportunity to investigate the physical processes in their formation and early evolution, and its environmental dependence for the first time. Note that because our targets are strongly clustered, we can efficiently make a statistical sample with a small number of pointings hence a relatively short investment of time. By spatially resolving the morphologies and internal structures of these galaxies by the proposed high-resolution HST imaging with ACS/F814W and WFC3/F160W, we will focus on the following critical issues; (1) first appearance of the morphology-density relation, (2) identification of the progenitors of massive, quiescent, compact galaxies, (3) environmental dependence of the mass-size relation, and (4) frequency of clumps/mergers and the mode of star formation (compactness/dustiness). The proposed observations will shed light on the physical processes "in action" on the progenitors of massive early-type galaxies in clusters for the first time. We will conduct the primary observation in the proto-cluster USS 1558-003 at z=2.53 in 3 pointings with WFC3/IR and F160W filter and in 2 pointings with ACS/WFC and F814W filter. To fully cover the three groups where Halpha emitters (HAEs) and DRGs are clustered without any space, we request the observation conducting all the exposures with the specific values of ORIENT. We request 5 visits with 2 orbits each. Our priority of the visits is as follows; (1st) POS3 with WFC3, (2nd) POS5 with ACS, (3rd) POS2 with WFC3, (4th) POS4 with ACS, and (5th) POS1 with WFCS3. As described in scientific justification of phase-I proposal, one of our main objectives is to measure the profile of stellar component and then derive the morphology and size of HAEs in the proto-cluster environment at z=2.53. We require the depth of at least ~27.5 (27.0) ABmag in ACS/F814W (WFC3/F160W) for point source, respectively, which are comparable to the wide survey data of CANDELS. The required depth is justified by the paper of van der Wel et al. (2012). They measured the structural parameters of H(F160W)-selected galaxies by fitting Sersic profile to CANDELS data, and investigated systematic and random uncertainties in structural parameters as a function of H(F160W) magnitude of galaxy for CANDELS wide survey data. According to Table 3 of van der Wel et al. (2012), structural parameters can be measured accurately for star-forming galaxies with Sersic index n<3 down to 25 ABmag in H(F160W). Therefore, the depth comparable to the CANDELS data is crucial to accomplish our objectives. According to Exposure Time Calculators, 5000 sec on-source exposure with ACS/F814W reaches 27.4 ABmag in 5-sigma for point source in the case measured within a 0.25''-radius aperture, while 4520 sec on-source exposure with WFC3/F160W reaches 27.0 ABmag in 5-sigma. The estimation is conducted under the assumption of the background levels that standard zodical (earth shine) light normalizations is average. Since our target is located at declination of -00:28:48.0, it can be observed for 54 minutes per one orbit. Thus, taking account of the orbit visibility, the required exposure time per one pointing in ACS/F814W (WFC3/F160W) is 5000 (5208) seconds in total with 4 exposures in 4 dithered points, respectively, which requires the 2 orbits per one pointing in both ACS/F814W and WFC3/F160W. Note that obtaining as deep near-infrared data as possible is desirable for us to measure the structural parameters of stellar component for less massive HAEs at z=2.53. We also make sure that almost all of HAEs we have found in the proto-cluster have magnitudes ranging between 21.7-25.0 ABmag in z'-band (Subaru/Suprime-Cam) and 20.0-24.5 ABmag in H-band (Subaru/MOIRCS). Regarding the Charge Transfer Efficiency (CTE) effect, we make sure that the estimated background of ACS images is greater than 20 electrons for the exposure time we plan. We will conduct a standard calibration, so no data is required for special calibration. UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE Default false false false false false SUPPORTED CLUSTER OF GALAXIES HIGH REDSHIFT CLUSTER J2000 J2000 Magnitudes for our main targets, Halpha emitters at z=2.53, range between 21.7-25.0 ABmag in z'-band and 20.0-24.5 ABmag in H-band. CLUSTER OF GALAXIES HIGH REDSHIFT CLUSTER J2000 J2000 Magnitudes for our main targets, Halpha emitters at z=2.53, range between 21.7-25.0 ABmag in z'-band and 20.0-24.5 ABmag in H-band. CLUSTER OF GALAXIES HIGH REDSHIFT CLUSTER J2000 J2000 Magnitudes for our main targets, Halpha emitters at z=2.53, range between 21.7-25.0 ABmag in z'-band and 20.0-24.5 ABmag in H-band. CLUSTER OF GALAXIES HIGH REDSHIFT CLUSTER J2000 J2000 Magnitudes for our main targets, Halpha emitters at z=2.53, range between 21.7-25.0 ABmag in z'-band and 20.0-24.5 ABmag in H-band. CLUSTER OF GALAXIES HIGH REDSHIFT CLUSTER J2000 J2000 Magnitudes for our main targets, Halpha emitters at z=2.53, range between 21.7-25.0 ABmag in z'-band and 20.0-24.5 ABmag in H-band. WFC3/IR Imaging No No F160W ACS/WFC Imaging No No F814W POS-TARG DITHER 0.265 LINE 0.187 false true 69.05 4 20.67 ACS-WFC-DITHER-BOX 2 false POS-TARG DITHER DITHER 4 5.183 WFC3-IR-DITHER-BOX-MIN false 74.653 true 0.365 0.572 2 41.859 POS-TARG WFC3-IR-DITHER-BLOB 18.528 3 true /Users/hayashi/Desktop/OP-cache/hayashi_phase2_cycle21_revised-v01.xml Hst Same orient constraint links visits (01 03 05) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. In this visit, the WFC3 observations with F160W are carried out at three pointings. 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CASM was run in Phase II mode. In this visit, the ACS observations with F814W are carried out at two pointings. 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CASM was run in Phase II mode. /Users/hayashi/Desktop/OP-cache/hayashi_phase2_cycle21_revised-v03.xml In this visit, the WFC3 observations with F160W are carried out at three pointings. 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CASM was run in Phase II mode. /Users/hayashi/Desktop/OP-cache/hayashi_phase2_cycle21_revised-v05.xml In this visit, the WFC3 observations with F160W are carried out at three pointings. 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