Assigned ID: 749
----- Attempting Submission 1 (Fri Feb 26 22:59:25 GMT 2010) -----** Copy of visit 01 (orbit 3) into visit 51 for rescheduling. Last orbit of visit 01 lost due to HST safing 9/9/10 **----- Attempting Submission 1 (Tue Jul 06 02:43:47 GMT 2010) -----
HST Phase II Proposal 12265 (sxds_z7blob_phaseII_v4.apt) successfully submitted.
----- Attempting Submission 2 (Fri Jul 09 07:25:13 GMT 2010) -----
----- Attempting Submission 3 (Mon Sep 13 13:42:03 GMT 2010) -----
----- Attempting Submission 4 (Wed Sep 15 12:27:02 GMT 2010) -----scheduling issues will be solved in-houseDetermining the Physical Nature of a Unique Giant Lya Emitter at z=6.595We propose deep WFC3/IR imaging for a giant Lya emitter (LAE) with a
Keck spectroscopic redshift of z=6.595 discovered by extensive narrow-band
imaging with Subaru in the SXDS-UKIDSS/UDS field. This remarkable object
is unique in many respects including its large stellar mass and luminous
nebula which extends over 17 kpc; no equivalent source has been found in
other surveys. The nature of this rare object is unclear. Fundamental
to progress is determining the origin of star formation in such an early
massive object; if the age of the stellar population is short we are
likely witnessing a special moment in the formation history of a massive
galaxy. The heating source for the nebula is also unclear; options include
intense star formation, the infall of cold gas onto a dark halo or shock
heating from a merger. We will take deep broad-band (F125W and F160W) images
and an intermediate-band (F098M) image which will be analyzed in conjunction
with ultra-deep IRAC 3.6 and 4.5 micron data being taken by
the Spitzer/SEDS project. These data will enable us to constrain the star
formation rate and stellar age. Moreover, the UV continuum morphology and
Lya-line distribution will be investigated for evidence of a major merger,
cold accretion, or hot bubbles associated with outflows. We will address
the physical origin of the remarkable object observed at an epoch where
massive galaxies are thought to begin their assembly.We will carry out WFC3/IR observations for our giant LAE with F125W, F160W, and F098M filters. With our 18 orbits, we will spend observing time equivalent to 5, 7, and 6 orbits for F125W, F160W, and F098M bands, respectively, which has been approved in the phase I. This 18-orbit program is composed of 6 visits that consist of 3 orbits. Because we aim to obtain deep images with a good PSF resampling, we perform 1 band (2 bands at most) observations in one visit with 4-point dither of WFC3-IR-DITHER-BOX. This strategy will accomplish subpixel sampling accurately without large offsets made by pointing repeatability of different visits. If there are 3 (or 2) orbits repeating the 4-point dither in one visit, we give 1/4-pixel offsets of (+2.75,+2.75)pix for the second orbit, and (-2.75,+2.25)pix for the third orbit. Moreover, if there is another set of the 3-orbit visit for the same band, we provide another set of 1/4-pixel offsets of (+2.75,-2.75)pix and (-2.75,-2.25)pix for the second and third orbits, respectively, in the visit. Although any visit orientations can be taken, but all of our visits should have the same visit orientation to realize a good subpixel sampling. We have chosen SPARS25 for F125W and F160W bands and SPARS50 for F098M band, following the WFC3 instrument handbook. To avoid over runs of orbit visibility, NSAMP is not 15, but 13-14. We think that these integration time will provide background limited images. Our field includes a bright star that is located about 48" away from our target. The brightness of the star is 6.8e7, 4.6e7, and 1.5e8 electrons in F125W, F160W, and F098M, respectively. We assume that the bright star gives no serious effects, such as ghost, on our target.COSMOLOGY12false0.00.0falsefalsefalsefalsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYz'=25.5+/-0.3 (including Lya emission and Gunn-Peterson trough)J200002 17 57.5630+05 08 44.45J2000WFC3/IRImagingNoNoF125WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF098MPOS-TARGDITHER0.572LINE0.365falsefalse74.653418.528WFC3-IR-DITHER-BOX-MIN1falseSame orient constraint links visits (01 02 03 04 05 06 52)The scheduling data was generated by CASM 18.3.1.CASM was run in Phase II mode.F125Wx3 orbits1284054462000275.0(Tic-Visit
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