The High Fraction of Thin Disk Galaxies Continues to Challenge
  {\Lambda}CDM Cosmology
  Any viable cosmological framework has to match the observed proportion of
early- and late-type galaxies. In this contribution, we focus on the
distribution of galaxy morphological types in the standard model of cosmology
(Lambda cold dark matter, $\Lambda$CDM). Using the latest state-of-the-art
cosmological $\Lambda$CDM simulations known as Illustris, IllustrisTNG, and
EAGLE, we calculate the intrinsic and sky-projected aspect ratio distribution
of the stars in subhalos with stellar mass $M_* > 10^{10}\,M_\odot$ at redshift
$z=0$. There is a significant deficit of intrinsically thin disk galaxies,
which however comprise most of the locally observed galaxy population.
Consequently, the sky-projected aspect ratio distribution produced by these
$\Lambda$CDM simulations disagrees with the Galaxy And Mass Assembly (GAMA)
survey and Sloan Digital Sky Survey at $\geq 12.52\sigma$ (TNG50-1) and $\geq
14.82\sigma$ (EAGLE50) confidence. The deficit of intrinsically thin galaxies
could be due to a much less hierarchical merger-driven build-up of observed
galaxies than is given by the $\Lambda$CDM framework. It might also arise from
the implemented sub-grid models, or from the limited resolution of the
above-mentioned hydrodynamical simulations. We estimate that an $8^5$ times
better mass resolution realization than TNG50-1 would reduce the tension with
GAMA to the $5.58\sigma$ level. Finally, we show that galaxies with fewer major
mergers have a somewhat thinner aspect ratio distribution. Given also the high
expected frequency of minor mergers in $\Lambda$CDM, the problem may be due to
minor mergers. In this case, the angular momentum problem could be alleviated
in Milgromian dynamics (MOND) because of a reduced merger frequency arising
from the absence of dynamical friction between extended dark matter halos.
