Dark matter halos of barred disk galaxies
  We use a large volume-limited sample of disk galaxies drawn from the Sloan
Digital Sky Survey Data Release 7 to study the dependence of the bar fraction
on the stellar-to-halo mass ratio, making use of a group catalog, we identify
central and satellite galaxies in our sample. For the central galaxies in the
sample we estimate the stellar-to-halo mass ratio
(M$_{\mathrm{*}}/$M$_{\mathrm{h}}$) and find that the fraction of barred
galaxies is a strong function of this ratio, especially for the case of strong
bars. Bars are more common in galaxies with high
M$_{\mathrm{*}}/$M$_{\mathrm{h}}$ values, as expected from early theoretical
works that showed that systems with massive dark matter halos are more stable
against bar instabilities. We find that the change of the bar fraction with
M$_{\mathrm{h}}$ and M$_{\mathrm{*}}$ is stronger if we consider a relation
with the form
$f_{\mathrm{bar}}=f_{\mathrm{bar}}$(M$_{\mathrm{*}}^{\alpha}/$M$_{\mathrm{h}}$)
with $\alpha=1.5$, and that the bar fraction is largely independent of other
physical properties such as color and spin parameter when
M$_{\mathrm{*}}^{3/2}/$M$_{\mathrm{h}}$ is fixed. With our sample of galaxies
segregated into centrals and satellites, we also compare the fraction of barred
galaxies in each group, finding a slightly higher bar fraction for satellites
when compared with centrals at fixed stellar mass, but at fixed color this
difference becomes very weak. This result, in agreement with previous studies,
confirms that the bar fraction does not directly depend on the group/cluster
environment, but the dependence exists through its dependence on internal
morphology.
