Surface density distributions of the gas in our hydrodynamical simulations. In the top row, we show the azimuthally averaged profiles for the planets located at 10AU (first column), 50AU (second column) and 100AU (third column). The color and style of the lines show the different planet masses. The vertical matching lines are located at r_p ± 2r_H in order to estimate the gap width. We clearly see that most massive planets produce deeper and wider gaps. The remaining panels show the 2D density maps for the different planet semi-major axes (columns) and masses (rows). The dashed red lines show again the gap width based on the planet’s Hill sphere. The 5 M_J planet located at 10AU produces an eccentric gap, which produces a less deep gap than in the circular cases.