|The LIGO-Virgo-KAGRA collaboration has reported over 90 compact binary coalescence events until the second half of the third observing run. The majority of the events are binary black hole (BBH) mergers. The evolution of these merger events can be suitably divided into three distinct phases: inspiral, merger, and ringdown. The low-frequency perturbative inspiral part is accurately described by the post-Newtonian (PN) theory, while to describe the high-frequency non-perturbative merger-ringdown part, one uses Numerical Relativity (NR). Spins of individual black holes in a binary system are one of the most important physical effects that potentially modify the gravitational waveforms and may lead to significant biases in the analysis of the observed GW data if ignored. These effects can be computed from the source multipole moments describing the system using the inputs from PN theory. Here, we present the spin effects in the spherical harmonic mode amplitudes of the gravitational waveform for spinning eccentric BBH systems within the PN framework. Further, the results are explicitly expressed in terms of parameters describing a spinning compact binary in an elliptical orbit.