Assigned ID: 546
----- Attempting Submission 1 (Fri Feb 24 18:22:10 GMT 2012) -----Error in Row Overlap of ACS cross-gap mosaic corrected, changed from 15% (default) to 98%.----- Attempting Submission 1 (Thu Jun 28 11:19:42 GMT 2012) -----
HST Phase II Proposal 13039 (qsophase2.apt) successfully submitted.
----- Attempting Submission 2 (Fri Jul 13 17:14:08 GMT 2012) -----
HST Phase II Proposal 13039 (qsophase2.apt) successfully submitted.
----- Attempting Submission 3 (Thu Sep 06 10:05:52 GMT 2012) -----The proposal has warnings about mising POS TARG and Center_Pattern=Yes.
These observations are of an area of sky, rather than a single object, and therefore the fact that the target is not at the centre of the pattern is unimportant (the offsets are small).The environment of the z=7.085 QSO ULAS J1120+0641We propose to take ACS and WFC3/IR observations of a 1-Mpc region around the recently-discovered redshift z=7.085 quasar ULAS J1120+0641 to test the hypothesis that, while distant active galaxies represent the densest regions in the early Universe, their radiation fields can hinder galaxy formation in the immediate vicinity. Observations of quasars and radio galaxies at z~5 have shown that they are the sites of galaxy overdensities, and revealed a segregration between companion galaxies selected by the Lyman break technique compared to those found via their Lyman-alpha emission. This has been interpreted as due to suppression of star formation in low-mass haloes by ionizing radiation from the central source. Since our target lies within the Epoch of Reionization, the scale over which this process acts is much smaller and more readily accessible to HST. Our observations will detect z~7 Lyman break galaxies as faint as the characteristic galaxy luminosity L* and their surface density can be directly compared to that derived from observations made in deep blank-field surveys, allowing us to quantify the environment around the quasar. Approved deep narrow-band imaging from the ground will measure the number of Lyman-alpha emitters and thus uniquely allow us to test the hypothesis that the ionizing radiation field results in spatial segregation between galaxies in different mass haloes.We propose to make observations of the field of the z=7.085 quasar ULAS J1120+0641 with ACS/WFC in F814W, and with WFC3/IR in F105W and F125W. These filters are identical to those used in the CANDELS survey, and the deep program covers 120 sq.arcmin, providing excellent statistics for a measurement of the z~7 field galaxy density. We will take a single ACS pointing, but make a 2x2 mosaic of WFC3/IR images to cover a similar-sized field and ensure that we probe a transverse physical scale exceeding 1 Mpc.
From a combination of ultra-deep (in the HUDF) and deep (WFC3 Early Release Science) HST imaging data, the rest-frame UV luminosity function has been well-determined at z~7. Bouwens et al. (2011) and McLure et al. (2010) both measure M*_UV=-20.11+/-0.28 for their sample of z~6.8 z-band dropouts, corresponding to m*_Y=26.9 at z=7.085. We model our galaxies as 100-Myr-old simple stellar populations (from Bruzual & Charlot 2003), normalized to Y=26.9, and attenuated by the IGM according to the prescription of Fan et al. (2006). A galaxy at z=7.085 is expected to have F105W-F125W=0.4 and F814W-F105W=5.2.
Galaxies at z~7 detected in WFC3/IR observations have a median half-light radius of 0.16$" (800 pc), and we assume that 60% of the flux is enclosed in our WFC3/IR images (70% for ACS) in a 0.5-arcsec diameter photometric aperture (as used by Oesch et al. 2010 and others). Our minimum requirement is to obtain S/N=5 in both the Y and J filters for an L* galaxy, and this requires 4700 and 2500 seconds, respectively. Since our target has a visibility of 50 minutes (reduced from 54 to allow increased scheduling flexibility), we can fit each WFC3 Y and J band observation into 2 and 1 orbits, respectively, requiring a total of 12 orbits to produce the four-image mosaic in both filters.
In order to select z~7 galaxies, we require a deep image in F814W, since they will have essentially zero flux shortward of the Lyman break. Statistically, we will be 90% complete for LBGs by selecting objects with S/N<1.3, but the more important requirement is to avoid contamination from other sources if our image is not deep enough. Despite their red colours, stars are not a contaminant because z~7 galaxies will appear extended, even at low signal-to-noise ratios (Bouwens et al. 2011). Furthermore, our target is at high Galactic latitude and a low-mass star would have to be far out of the plane of the Galaxy (>1kpc) to be as faint as a z=7 L* galaxy; we estimate fewer than one such object in our field (N. Deacon, priv. comm.).
The reddest contaminating galaxies will be ellipticals at z>1.5, which have F814W-F105W~1.8 and we must reach a depth such that the F814W photometric error is small enough to not scatter these into our selection box. These factors combine to require a S/N=3 limit of F814W=28.6, needing 32,000 seconds of exposure. We can obtain this with 13 orbits. Our total request for the WFC3 and ACS observations is therefore 25 orbits.The WFC3 and ACS mosaics both cover approximately square regions on the sky, and should be performed in such a way that the sides of these squares are aligned (a tolerance of 5 degrees has been allowed), although the orientation on the sky is not constrained.
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:pcs-time 333
:si-vis-utilization 2436
:al-overhead-at-end 0
:internal-dur-at-end 347
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "Y"
:pcs-visibility 2769
:pcs-gap 175
)true10