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

Reconciling low multipole anomalies and reheating in single field inflationary models