  We present the photometric and spectroscopic studies of a Type Ib SN 2015ap
and a Type Ic SN 2016P. SN 2015ap is one of the bright (M$_{V}$ = $-$18.04 mag)
Type Ib while SN 2016P lies at an average value among the Type Ic SNe (M$_{V}$
= $-$17.53 mag). Bolometric light curve modelling of SNe 2015ap and 2016P
indicates that both the SNe are powered by $^{56}$Ni + magnetar model with
$^{56}$Ni masses of 0.01 M$_{\odot}$ and 0.002 M$_{\odot}$, ejecta masses of
3.75 M$_{\odot}$ and 4.66 M$_{\odot}$, spin period P$_{0}$ of 25.8 ms and 36.5
ms and magnetic field B$_{p}$ of 28.39 $\times$ 10$^{14}$ Gauss and 35.3
$\times$ 10$^{14}$ Gauss respectively. The early spectra of SN 2015ap shows
prominent lines of He with a "W" feature due to Fe complexes while other lines
of Mg II, Na I and Si II are present in both SNe 2015ap and 2016P. Nebular
phase [O I] profile indicates an asymmetric profile in SN 2015ap. The [O I]/[Ca
II] ratio and nebular spectral modelling of SN 2015ap hints towards a
progenitor mass between 12 $-$ 20 M$_{\odot}$.
