  Detection of forming planets means detection of the circumplanetary disk
(CPD) in reality, since the planet is still surrounded by a disk at this
evolutionary stage. Yet, no comprehensive CPD modeling was done in
near-infrared wavelengths, where high contrast imaging is a powerful tool to
detect these objects. We combined 3D radiative hydrodynamic simulations of
various embedded planets with RADMC-3D radiative transfer post-processing that
includes scattering of photons on dust particles. We made synthetic images for
VLT NaCo/ERIS in the Ks, L', M' bands as well as examined the spectral energy
distributions (SEDs) of disks between 1 $\mu m$ and 10 cm. We found that the
observed magnitudes from the planet's vicinity will mostly depend on the CPD
parameters, not on the planet's. The CPD is 20-100x brighter than the embedded
planet in near-IR. We also show how the CPD parameters, e.g. the dust-to-gas
ratio will affect the resulting CPD magnitudes. According to the SEDs, the best
contrast ratio between the CPD and circumstellar disks is in sub-mm/radio
wavelengths and between 8-33 microns in case if the planet opened a resolvable,
deep gap ($\ge 5 \rm{M_{Jup}}$), while the contrast is particularly poor in the
near-IR. Hence, to detect the forming planet and its CPD, the best chance today
is targeting the sub-mm/radio wavelengths and the 10-micron silicate feature
vicinity. In order to estimate the forming planet's mass from the observed
brightness, it is necessary to run system specific disk modeling.
