
discovery of CDG-2 strengthens the broader phenomenological case that the dark sector lacks a
rst-order dissipation channel.
Scope of this comparison.
We do not claim that CDG-2 uniquely conrms the SSM. Any
dark-matter model with a non-dissipative dark sector including the standard collisionless
cold-dark-matter paradigm and many wave-like or fuzzy-dark-matter alternatives is consistent
with the existence of almost-dark galaxies. Furthermore, the
99.94
99.99%
halo-mass fraction is
inferred from GC-count scaling relations rather than direct kinematic measurement; the authors
of [20] note that high-precision kinematic and spectroscopic follow-up is needed to conrm the
dark-matter content directly. CDG-2 is therefore one observational data point consistent with
the SSM phenomenology, not a discriminating test against alternative dark-matter models. The
discovery of further almost-dark galaxies, particularly with direct kinematic conrmation of
their halo masses, would extend this class of observation and tighten the constraint on the
morphological predictions of any non-dissipative dark-matter framework.
5.5 Comparison with existing dark matter models
The octahedral-void defect predicted here shares qualitative features with several composite-
dark-matter scenarios in the literature. GeV-scale strongly-coupled hidden-sector models [13, 14]
produce dark baryons whose mass arises from connement dynamics and whose direct-detection
signatures are suppressed relative to weakly-interacting massive particles. Strongly-interacting
massive particle (SIMP) models [15] predict sub-GeV to GeV-scale dark particles with non-trivial
self-interaction. The SSM prediction lies in a similar parameter region (1.7 GeV mass, suppressed
electromagnetic coupling) but diers in origin: the existence and structural properties of the
dark matter candidate are derived from FCC vacuum geometry rather than from cosmological
freeze-out, asymmetric mechanisms, or hidden-sector gauge dynamics.
The closest phenomenological analog in the existing literature is the
sexaquark
[24, 25]: a
hypothesized neutral, avor-singlet, scalar bound state of
uuddss
quarks with baryon number
B = 2
and strangeness
S = −2
, proposed by Farrar as a dark matter candidate. The sexaquark
and the SSM K=6 octahedral defect agree on several non-trivial phenomenological features. Both
are GeV-scale particles with mass
∼ 2m
p
(sexaquark stability requires
m
S
≲ 2054
MeV, with cos-
mological relic-abundance ts favoring 1.51.8 GeV [25]; the SSM prediction
m
DM
= 1.719
GeV
lies inside this preferred range). Both involve a six-fold structure (sexaquark: six quarks; SSM
defect: six bounding vertices). Both are electromagnetically neutral with suppressed hadronic
couplings (sexaquark: avor-singlet decoupling from pions; SSM: absence of square plaquettes
in the bonded subgraph
K
2,2,2
). Both are consistent with the diuse, non-collisional halo phe-
nomenology required by direct-detection nulls and self-interaction constraints.
Three theoretical features distinguish the two models. First, the sexaquark carries
B = 2
and
S = −2
and is therefore strictly distinct from its antiparticle (
¯
S
, with
B = −2
,
S = +2
);
the SSM defect, by contrast, is its own antiparticle by the inversion symmetry of the regular
octahedron (Section 3.5). The Majorana-vs-Dirac character is empirically distinguishable in
indirect-detection signatures (annihilation
χχ
vs.
χ¯χ
) and in cosmological asymmetry channels.
Second, the sexaquark mass is a free phenomenological parameter that lattice QCD cannot yet
predict to the precision required for stability; the SSM mass follows from a closed combinatorial
expansion on
K
2,2,2
with no tted parameters. Third, the sexaquark is a strongly-interacting
QCD bound state (a avor-singlet hadron), whereas the SSM defect carries no SU(3) color charge
(Section 3.4) and does not participate in strong interactions. The two frameworks are therefore
not in direct competition: a denitive sexaquark detection would not falsify the SSM defect, and
vice versa, though discriminating direct-detection, indirect-detection, and accelerator signatures
can be designed.
13