  The primary X-ray emission from AGN, described by a power law, irradiates the
accretion disc producing reflection features in the spectrum. The reflection
features arising from the inner regions of the disc can be significantly
modified by the relativistic effects near the black hole. We investigate the
relationship between the relativistic reflection fraction $R_f$, defined as the
ratio of the coronal intensity that illuminates the accretion disc to the
coronal intensity observed directly, and the hard X-ray photon index $\Gamma$
of a NuSTAR sample of Seyfert 1 galaxies. The X-ray spectra are modelled using
relxill code which helps to directly obtain the reflection fraction of a
relativistically smeared reflection component. The parameter $R_f$ depends on
the amount of Comptonised X-ray emission intercepted by the inner accretion
disc. We found a positive correlation between $\Gamma$ and $R_f$ in our sample.
Seed photons from a larger area of an accretion disc entering the corona will
result in increased cooling of the coronal plasma, giving rise to steeper X-ray
spectrum. The corona irradiating the larger area of the disc will result in
higher reflection fraction. Thus, the observed $R_f-\Gamma$ relation is most
likely related to the variations in the disc-corona geometry of AGN.
