  Reheating phase of inflationary Universe can be modeled by parameters
$T_{\text{reh}}$, $\bar{w}_{\text{reh}}$ and $N_{\text{reh}}$, which can be
constrained by the scalar spectral amplitude $A_{s}$ and the scalar spectral
index $n_{s}$. On the other hand the low multipole anomalies in the CMB can be
modeled by suitable features in the inflaton potential. We show that the
parameters of these features in the inflaton potential provide additional
constraints on the reheating parameters. For several single field models we
find that the reheating parameters are substantially more constrained by the
requirement of compatibility with the proposed explanation for low multipole
anomalies.
