  We consider Kerr black holes (BHs) surrounded by perfect dark fluid matter
(PFDM), with an additional parameter ($k$) because of PFDM, apart from mass
($M$) and rotation parameter ($a$) -- the rotating PFDM BHs. We analyze the
photon orbits around PFDM BHs and naked singularities (NSs) and emphasise the
effect of PFDM on photon \emph{boomerangs}. Interestingly, the azimuthal
oscillations first increase and then decrease for retrograde orbits, whereas
they first decrease and then increase for prograde orbits, with increasing $k$.
Unlike in the Kerr NSs, photon \emph{boomerangs} can form around rotating PFDM
NSs. We use the Event Horizon Telescope (EHT) observational results for
Schwarzschild shadow deviations of M87* and Sgr A*,
$\delta_{M87^*}=-0.01\pm0.17$ and $\delta_{Sgr A^*} =
-0.08^{+0.09}_{-0.09}~\text{(VLTI)},-0.04^{+0.09}_{-0.10}~\text{(Keck)}$, to
report the upper bounds on the PFDM parameter: $0\leq k\leq 0.0792M$ and
$k^{max}\in[0.0507M, 0.0611M]$ respectively. Together with the EHT bounds on
the shadows of Sgr A$^*$ and M87$^*$, our analysis concludes that a substantial
part of the rotating PFDM BH parameter space agrees with the EHT observations.
Thus, one must consider the possibility of the rotating PFDM BHs being strong
candidates for the astrophysical BHs.
