The NewHorizon Simulation -- To Bar Or Not To Bar
  We use the NewHorizon simulation to study the redshift evolution of bar
properties and fractions within galaxies in the stellar masses range $M_{\star}
= 10^{7.25} - 10^{11.4} \ \rm{M}_{\odot}$ over the redshift range $z = 0.25 -
1.3$. We select disc galaxies using stellar kinematics as a proxy for galaxy
morphology. We employ two different automated bar detection methods, coupled
with visual inspection, resulting in observable bar fractions of $f_{\rm bar} =
0.070_{{-0.012}}^{{+0.018}}$ at $z\sim$ 1.3, decreasing to $f_{\rm bar} =
0.011_{{-0.003}}^{{+0.014}}$ at $z\sim$ 0.25. Only one galaxy is visually
confirmed as strongly barred in our sample. This bar is hosted by the most
massive disk and only survives from $z=1.3$ down to $z=0.7$. Such a low bar
fraction, in particular amongst Milky Way-like progenitors, highlights a
missing bars problem, shared by literally all cosmological simulations with
spatial resolution $<$100 pc to date. The analysis of linear growth rates,
rotation curves and derived summary statistics of the stellar, gas and dark
matter components suggest that galaxies with stellar masses below
$10^{9.5}-10^{10} \ \rm{M}_{\odot}$ in NewHorizon appear to be too dominated by
dark matter to form a bar, while more massive galaxies typically have formed
large bulges that prevent bar persistence at low redshift. This investigation
confirms that the evolution of the bar fraction puts stringent constraints on
the assembly history of baryons and dark matter onto galaxies.
