Figures 10-12

*Figure 10*

CDM evolution in the Compton drag epoch.
If baryons contribute a significant fraction
of the total matter density, CDM growth will be slowed between equality
and the drag epoch. Held by Compton drag, the baryons do not contribute
their self-gravity. For the numerical results, we choose a model that
never recombined so that $a_d \gg a_{eq}$.

*Figure 11*

Velocity overshoot effect. Below the horizon at the drag epoch
$k\eta_d \gg 1$, the acoustic velocity at $z_d$ dominates the growing
mode and hence the final transfer function. Near the horizon, the
acoustic density becomes comparable and shifts the zero points of
the oscillation.

*Figure 12*

Adiabatic CDM transfer function in a high $\Omega_b/\Omega_0=2/3$ case.
The analytic solution is essentially exact
in the small scale limit. Simple fits based on the BBKS form
can cause large errors at the small scale: PD (Peacock \& Dodds 1994)
and S (Sugiyama 1995).
The fitting function developed here [see equation
\Edis\EeqnScaling] works at the $1\%$ level even for this extreme case.