  In this paper, we extend the source detection in the GOODS-ALMA field (69
arcmin$^2$, rms sensitivity $\sigma$ $\simeq$ 0.18 mJy.beam$^{-1}$), to deeper
levels than presented in Franco et al. (2018). Using positional information at
3.6 and 4.5 $\mu$m (from Spitzer-IRAC), we explore the presence of galaxies
detected at 1.1 mm with ALMA below our original blind detection limit of
4.8-$\sigma$ at which the number of spurious sources starts to dominate over
that of real sources. In this Supplementary Catalog, we find a total of 16
galaxies, including 2 galaxies with no counterpart in HST images (also known as
optically-dark galaxies) down to a 5$\sigma$ limiting depth of H = 28.2 AB
(HST/WFC3 F160W). This brings the total sample of GOODS-ALMA 1.1 mm sources to
35 galaxies. Galaxies in the new sample cover a wider dynamic range in redshift
($z$ = 0.65 - 4.73), are on average twice as large (1.3 vs 0.65 kpc) and and
have lower stellar mass (M$_{\star}^{\rm SC}$ = 7.6$\times$10$^{10}$M$_\odot$
vs M$_{\star}^{\rm MC}$ = 1.2$\times$10$^{11}$M$_\odot$). Although exhibiting
larger physical sizes, these galaxies have still far-infrared sizes
significantly more compact than inferred from their optical emission. We show
that the astrometry of the HST image does not only suffer from a global
astrometric shift, as already discussed in previous papers, but also from local
shifts. These distortions were artificially introduced in the process of
building the mosaic of the GOODS-South HST image. By comparing the positions of
almost 400 galaxies detected by HST, Pan-STARRS and ALMA, we create a
distortion map which can be used to correct for these astrometric issues.

Astrophysics of Galaxies