  The Kepler mission has discovered thousands of exoplanets around various
stars with different spectral types (M, K, G, and F) and thus different masses
and effective temperatures. Previous studies have shown that the planet
occurrence rate, in terms of average number of planets per star, drops with
increasing stellar effective temperature (Teff). In this paper, with the final
Kepler Data Release (DR25) catalog, we revisit the relation between stellar
effective temperature (as well as mass) and planet occurrence, but in terms of
the fraction of stars with planets and the number of planets per planetary
system (i.e. planet multiplicity). We find that both the fraction of stars with
planets and planet multiplicity decrease with increasing stellar temperature
and mass. Specifically, about 75% late-type stars (Teff<5000 K) have
Kepler-like planets with an average planet multiplicity of ~2.8; while for
early-type stars (Teff>6500 K), this fraction and the average multiplicity fall
down to ~35% and ~1.8, respectively. The decreasing trend in the fraction of
stars with planets is very significant with ${\Delta}$AIC> 30, though the trend
in planet multiplicity is somewhat tentative with ${\Delta}$AIC~5. Our results
also allow us to derive the dispersion of planetary orbital inclinations in
relationship with stellar effective temperature. Interestingly, it is found to
be similar to the well-known trend between obliquity and stellar temperature,
indicating that the two trends might have a common origin.
