Kavli Affiliate: Mark Vogelsberger
| First 5 Authors: Alvaro Pozo, Alvaro Pozo, , ,
| Summary:
The initial gravitational collapse of Dark Matter and gas forms a universal
filamentary network where the first galaxies form, with shapes and sizes that
depend on the choice of Dark Matter. Claims from deep space imaging surveys
that elongated galaxies predominate at $z > 3$ are examined here by comparison
with detailed hydrodynamical simulations of Cold Dark Matter (CDM), Warm Dark
Matter (WDM), and Wave/Fuzzy Dark Matter, $psi$DM. For CDM and WDM we have
sufficient volume, $10^3,mathrmMpc/h^3$, to generate galaxies with
stellar masses $> 10^9,M_odot$ at $z > 2$, allowing comparison with the
CEERS and CANDELS surveys. We find the observed tendency towards elongated,
prolate-shaped young galaxies is well matched by WDM, from material accreted
along smooth filaments during the first $simeq 500,mathrmMyr$, with little
dependence on stellar mass. This contrasts with CDM, where the stellar
morphology is mainly spheroidal, formed from merging of fragmented filaments.
For CDM, several subhalos are predicted to be visible, whereas for WDM and
$psi$DM, early merging is rare. Our findings show how the shapes and sizes of
early galaxies are sensitive to the smoothness of the underlying filament
network, providing a new constraint on the nature of dark matter.
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