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We present mock observations of forming planets with ALMA. The possibledetections of circumplanetary disks (CPDs) were investigated around planets ofSaturn, 1, 3, 5, and 10 Jupiter-masses that are placed at 5.2 AU from theirstar. The radiative, three dimensional hydrodynamic simulations were thenpost-processed with RADMC3D and the ALMA Observation Simulator. We found thateven though the CPDs are too small to be resolved, they are hot due to theaccreting planet in the optically thick limit, therefore the best chance todetect them with continuum observations in this case is at the shortest ALMAwavelengths, such as Band 9 (440 microns). Similar fluxes were found in thecase of Saturn and Jupiter-mass planets, as for the 10 $\mathrm{M_{Jup}}$gas-giant, due to temperature weighted optical depth effects: when no deep gapis carved, the planet region is blanketed by the optically thick circumstellardisk leading to a less efficient cooling there. A test was made for a 52 AUorbital separation, showed that optically thin CPDs are also detectable in band7 but they need longer integration times ($>$5hrs). Comparing the gap profilesof the same simulation at various ALMA bands and the hydro simulation confirmedthat they change significantly, first because the gap is wider at longerwavelengths due to decreasing optical depth; second, the beam convolution makesthe gap shallower and at least 25% narrower. Therefore, caution has to be madewhen estimating planet masses based on ALMA continuum observations of gaps.

Observability of Forming Planets and their Circumplanetary Disks I. -- Parameter Study for ALMA