a point kernel [see @Beckwith] which should lead to noise that is uncorrelated between adjacent pixels. We verified that this is the case by measuring the autocorrelation function of the noise after masking galaxies. We measured the noise on various scales, including 50 pixel apertures as used by @Beckwith. Our most conservative (largest) noise measurements are 31 to 37% smaller than those reported by @Beckwith [their Table 5].

@Dunlop report faint detections of positive flux in the ACS $V$, $i$ and $z$-bands, which, taken together, drive their photometric redshift estimate to favor a lower value, $z \approx 2.15$. We do not reproduce these measurements; using a $1\farcs0$ diameter aperture and our noise measurements, and the correction of $\sim$0.1 mag for the energy falling outside the aperture reported in @Sirianni [Table 3], we find the $2\sigma$ photometric limits given in Table 2. These are $\sim$0.8 mag brighter than the limits reported in Mobasher et al. (2005), mainly due to the larger aperture adopted here. It is possible that the positive flux detected in the Dunlop et al. measurements arises in part from the faint neighboring galaxies.

The NICMOS $J_{110}$ photometry and $H_{160}$ photometry in @Mobasher are very similar to those in 