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##  Appendix A IRAC catalog

We constructed the IRAC catalog using the deepest IRAC 3.6 and 4.5 $\mu$m
images from the GREATS program (Stefanon et al., 2021). Source detection was
performed using Source Extractor (SE version 2.25.0; Bertin & Arnouts, 1996)
on the background-subtracted 3.6 and 4.5 $\mu$m images, respectively. This is
to help us exclude as many false detections as possible and get pure sources
after cross-matching two catalogs from 3.6 and 4.5 $\mu$m images. Each
detected source was required to have a minimum area of 4 pixels, with each
pixel achieving the threshold of 0.25$\sigma$. The deblending parameters were
optimized by setting DEBLEND_THRESH $=64$ and DEBLEND_MINCONT $=0.0001$, which
were a compromise between de-blending neighboring sources and minimizing a
potential division of a larger object into multiple components. The sky
subtraction was performed with SE, using a bicubic interpolation of the
background with an adopted mesh size of 512 pixels and a median filter size of
5 pixels. A Mexhat filter was used to smooth the images before detection, to
help detect faint and extended objects. The Mexhat filter can very well de-
blend faint sources around the bright source, but it also extracts artifacts
around the bright source caused by diffraction, which needs to be cleaned. We
set CLEAN_PARAM $=$ 1 to clean spurious detections with SE. Then, we visually
inspected images to further remove artifacts around the bight sources. For the
3.6 and 4.5 $\mu$m images, we obtained their source catalogs respectively. The
total sources in the catalogs are 125,338 for 3.6 $\mu$m and 154,234 for 4.5
$\mu$m in the entire GOODS-S field.

To ensure the purity of detections, we then cross-matched two catalogs from
3.6 and 4.5 $\mu$m images with a radius of 1.0′′ ($\sim$0.5$\times$FWHM). For
sources that are simultaneously in the GOODS-ALMA 2.0 catalog (Gómez-Guijarro
et al., 2022a) and detected in at least one IRAC band, we considered them as
real sources and kept them in the final catalog. Finally, we have 5,127 pure
sources detected by both 3.6 and 4.5 $\mu$m bands and/or ALMA 1.13 mm in the
GOODS-ALMA field.

To estimate the completeness of our detection strategy, we employed a Monte
Carlo approach where we simulated 10,000 artificial model sources with random
magnitudes between 14.5 mag and 29 mag. They are point sources with the same
PSF profiles as 3.6 and 4.5 $\mu$m images, respectively. The simulated sources
were allowed to fall at random positions on the real image, including on top
of other sources, to account for the impact of source blending in the real
image. We injected ten sources each time on the IRAC 3.6um and 4.5um images to
avoid excessively artificial source confusion caused by bright fake sources.
After each injection, we performed the same blind source detection procedure
using SE.

In Fig. 12-$left$, we show the completeness as a function of the input flux
density ($S_{\rm in}$) for the simulated sources in 3.6 and 4.5 $\mu$m images.
The survey reaches a 100% completeness for all simulated sources for flux
densities $S_{\rm in}\gtrsim$ 20 $\mu$Jy at both 3.6 and 4.5 $\mu$m
wavelength. To understand the incompleteness of our OFG sample, we need to
know the behavior of completeness as a function of output flux density
($S_{\rm out}$) shown in Fig. 12-$right$, since $S_{\rm out}$ is the parameter
being measured directly.

Figure 12: The completeness as a function of the input flux density ($S_{\rm
in}$; left) and the output flux density ($S_{\rm out}$; right).

##  Appendix B Multiwavelength Postage-stamp

Figure 13: Postage-stamps (4′′ $\times$ 4′′) of our OFGs. From left to right:
HST/WFC3 (F160W), ZFOURGE ($K_{\rm s}$), Spitzer/IRAC (3.6 $\mu$m and 4.5
$\mu$m), and ALMA band 6 (1.13 mm). The white circles mark our target galaxies
with 0.6′′ in radius. The black circles indicate the positions of the ALMA
detections. North is up and East is to the left.

##  Appendix C SEDs for the individual OFGs

Figure 14: UV to millimeter SEDs for 27 OFGs. The symbol convention and lines
are the same as those in Figs. 7. The data from the UV to MIR (16 $\mu$m)
bands are fitted with the FAST++ code (see $\S$4.1). From 24 $\mu$m up to
millimeter wavelengths, we fitted galaxies with a Herschel counterpart using
the CIGALE code (orange solid line) and galaxies without a Herschel
counterpart but with the ALMA 1.13 mm detection using the dust template
libraries (green line; Schreiber et al., 2018c, see $\S$4.2).  Figure 15:
(continued).