The Paleoclimatic evidence for Strongly Interacting Dark Matter Present
  in the Galactic Disk
  Using a recent geochemical reconstruction of the Phanerozoic climate which
exhibits a 32 Ma oscillation with a phase and the secondary modulation expected
from the vertical the motion of the solar system perpendicular to the galactic
plane (shaviv et al. 2014), we show that a kinematically cold strongly
interacting disk dark matter (dDM) component is necessarily present in the
disk. It has a local density $\rho_\mathrm{dDM} = 0.11 \pm 0.03$
M$_{\odot}/$pc$^3$. It is also consistent with the observed constraints on the
total gravitating mass and the baryonic components, and it is the natural value
borne from the Toomre stability criterion. It also has surface density
$\Sigma_\mathrm{dDM} = 15 \pm 5$ M$_{\odot}/$pc$^2$ and a vertical velocity
dispersion of $\sigma_{W} = 8.0 \pm 4.5$ km/s. A dense ("dinosaur killing")
thin disk is ruled out. The "normal" halo dark matter (hDM) component should
then have a local density $\rho_\mathrm{hDM} \lesssim 0.01$ M$_{\odot}/$pc$^3$.
If the dDM component follows the baryons, its average density parameter is
$\Omega_\mathrm{dDM} = 1.5 \pm 0.5\%$ and it comprises about 1/8 to 1/4 of
Milky Way (MW) mass within the solar circle.
