The authors numerically showed that angular momentum of isolated galactic halos with mass less than 10^11 solar mass is systematically larger in the f(R) gravity model since they are less affected by shielding via chameleon mechanism.

Using N-body simulation, the authors showed that velocity-dependent self-interacting dark matter gives the inner circular velocity profiles of the most massive subhalos that are compatible with the data of the brightest Milky Way dSphs.

The authors claim a detection of a missing dark satellite in a galaxy-galaxy strong lens system B1938+666. The claimed perturber is located at the brightest region in the lensed image.

Our peculiar velocity with respect to the CMB rest frame can be measured through off-diagonal correlations in harmonic expansion coefficients due to aberration. The author shows that a new technique called "pre-deboosting" will work for detecting such correlations up to l~10000. If the measured residual peculiar velocity is different from the expected value, it would be a hint of some anomalies on superhorizon scales.

From N-body simulation, the authors find that concentration-mass relation displays a turnover for group scale dark matter haloes, for the case of WDM particles with masses of the order ~0.25 keV. This may be interpreted as a hint for top-down structure formation on small scales. Is there any reionization mechanism in this scenario?

1)Because the size of the simulated boxes were ten times smaller in previous studies. 2)Weak lensing at scale below ~1arcsec could work. Their results might be helpful for estimating non-linear power spectrum based on a certain halo model.