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tokens: clarity only scales are shown. Left: total fraction of fake sources recovered as a function of input H 160 -band magnitude. Recovery of faint sources is improved with the wavelet subtraction method. Bright sources are lost as they are subtracted in the wavelet decomposition process; to ensure that we can detect bright as well as faint sources, we therefore use both the original and wavelet-subtracted images for source detection. Middle: recovered−input magnitudes of fake sources as a function of input magnitudes for sources detected in the original and wavelet-subtracted images, but all photometry measured in the original image. The accuracy of photometry is noticeably affected when the objects are detected in images subtracted to scale 3. Right: same as the middle panel, but with photometry measured in the wavelet-subtracted images. Here, we recover systematically fainter magnitudes, as part of the light of some of the galaxies is subtracted during the wavelet subtraction procedure. We also note that detection in the wavelet-subtracted images is hampered for bright galaxies as they get removed when we perform the subtraction to smaller scales. Although we do not expect to find any high-redshift galaxies in this regime, we nonetheless choose to combine catalogs from the wavelet-subtracted and original images in order to ensure that we include potential bright or extended sources. 4. Source Selection We detect galaxies in these fields using SExtractor in dual image mode, where one detection image is used to measure photometry in each of the seven available HST filters. In order to maximize our sensitivity to faint high-redshift galaxies at a range of different colors, we use 11 different detection images: each of the four HST /WFC3 filters , plus seven stacked combinations of these images: , , , , , , and . We carry out this process with detection in both the original PSF-matched images and the wavelet-subtracted ones, for a total of 22 detection images. In all cases, photometry is measured from the original, PSF-matched images in all seven filters, as well as from the wavelet-subtracted images. We use the wavelet-subtracted photometry where it is within 1 σ of the photometry from the original image in every band, because the signal-to-noise ratio is higher, especially in the central regions of the clusters. Where the photometry differs (i.e., where some part of the Galaxy has been subtracted in the wavelet decomposition process), we use the photometry from the original image. We also visually inspect every galaxy to ensure that no part of the Galaxy has been subtracted; we find that all partially subtracted galaxies have photometry that differs by between the original and wavelet-subtracted images, so the original image photometry is used. We then combine our 22 catalogs into a single master catalog, selecting unique sources within a matching radius of 02. We measure photometry in the small Kron aperture flux, with the SExtractor parameter