normal distribution with ($\mu, \sigma$) = (0, 1). The comparison quantified using a Kolmogorov–Smirnov test [@kolmogorov33; @smirnov48] indicates that the likelihood that the normalized residuals come from the normal distribution is less than 20%, implying that the low-$z$ solution is not a preferred model for this galaxy.

To further probe the existence of any low level flux below the detection threshold of individual optical bands, we created a stack of [*V$_{606}$*]{}-, [*i$_{775}$*]{}-, [*I$_{814}$*]{}-, and [*z$_{850}$*]{}-band images. Prior to the stacking, the spatial resolution of the images were matched to that of the [*H$_{160}$*]{} band and the units were converted to a physical unit. Then, the stack and stack rms map were generated by inverse-variance weighting, on which the stack flux and flux error were measured within a 04 diameter aperture using the Source Extractor package [@bertin96] and aperture-corrected using the ratio between the flux within a 04 aperture and total flux measured in the [*H$_{160}$*]{} band. We quantified the background noise as the Gaussian width of the flux distribution measured from 10$^4$ randomly placed apertures of the same size used in our original photometry in source-free regions of the stacked image. We checked that the flux error (3.8 nJy) measured 