  The multi-phase circumgalactic medium (CGM) arises within the complex
environment around a galaxy, or collection of galaxies, and possibly originates
from a wide range of physical mechanisms. In this paper, we attempt to
disentangle the origins of these multi-phase structures and present a detailed
analysis of the quasar field Q0122-003 field using Keck/KCWI galaxy
observations and HST/COS spectra probing the CGM. Our re-analysis of this field
shows that there are two galaxies associated with the absorption. We have
discovered a dwarf galaxy, G_27kpc ($M_{\star}=10^{8.7}$ M$_{\odot}$), at
z=0.39863 that is 27 kpc from the quasar sightline. G_27kpc is only +21 km/s
from a more massive ($M_{\star}=10^{10.5}$ M$_{\odot}$) star-forming galaxy,
G_163kpc, at an impact parameter of 163 kpc. While G_163kpc is actively forming
stars (SFR=6.9 M$_{\odot}$ yr$^{-1}$), G_27kpc has a low star-formation rate
(SFR=$0.08\pm0.03$ M$_{\odot}$ yr$^{-1}$) and star formation surface density
($\Sigma_{SFR}=0.006$ M$_{\odot}$ kpc$^{-2}$ yr$^{-1}$), implying no active
outflows. By comparing galaxy SFRs, kinematics, masses and distances from the
quasar sightline to the absorption kinematics, column densities and
metallicities, we have inferred the following: (1) Part of the low-ionization
phase has a metallicity and kinematics consistent with being accreted onto
G_27kpc. (2) The remainder of the low ionization phase has metallicities and
kinematics consistent with being intragroup gas being transferred from G_27kpc
to G_163kpc. (3) The high ionization phase is consistent with being produced
solely by outflows originating from the massive halo of G_163kpc. Our results
demonstrate the complex nature of the multi-phase CGM, especially around galaxy
groups, and that detailed case-by-case studies are critical for disentangling
its origins.
