  The motion of photons around the Kerr-Newman-dS black hole surrounded by
quintessence and a cloud of strings is investigated. The existence of the
Carter constant leads to that of unstable circular photon orbits on a
two-dimensional plane not limited to the equatorial plane and unstable
spherical photon orbits in the three-dimensional space. These circular or
spherical photon orbits can determine two impact parameters, which are used to
calculate black hole shadows. For the case of a spherically symmetric
nonrotating black hole, the black hole shadow is circular and its size is
independent of an observation angle and a plane on which a circular photon
orbit exists. The shadow sizes are significantly influenced by the parameters
involving the cloud of strings, quintessence parameter, magnitude of
quintessential state parameter, and cosmological constant. When the black hole
is spinning and axially symmetric, the black hole shadow is dependent on the
observation angle. The effects of the parameters excluding the spin parameter
on the sizes of black hole shadows in the rotating case are similar to those in
the nonrotating case. Based on the Event Horizon Telescope observations of
M87*, the constraint of the curvature radius is used to constrain these
parameters. For slowly rotating black holes, the allowed regions of the
parameters including the cosmological constant are given.
