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Direct imaging has paved the way for atmospheric characterization of youngand self-luminous gas giants. Scattering in a horizontally-inhomogeneousatmosphere causes the disk-integrated polarization of the thermal radiation tobe linearly polarized, possibly detectable with the newest generation ofhigh-contrast imaging instruments. We aim to investigate the effect oflatitudinal and longitudinal cloud variations, circumplanetary disks,atmospheric oblateness, and cloud particle properties on the integrated degreeand direction of polarization in the near-infrared. We have developed athree-dimensional Monte Carlo radiative transfer code (ARTES) for scatteredlight simulations in (exo)planetary atmospheres. The code is applicable tocalculations of reflected light and thermal radiation in a spherical grid witha parameterized distribution of gas, clouds, hazes, and circumplanetarymaterial. The disk-integrated degree of polarization of ahorizontally-inhomogeneous atmosphere is maximal when the planet is flattened,the optical thickness of the equatorial clouds is large compared to the polarclouds, and the clouds are located at high altitude. For a flattened planet,the integrated polarization can both increase or decrease with respect to aspherical planet which depends on the horizontal distribution and opticalthickness of the clouds. The direction of polarization can be either parallelor perpendicular to the projected direction of the rotation axis when cloudsare zonally distributed. Rayleigh scattering by submicron-sized cloud particleswill maximize the polarimetric signal whereas the integrated degree ofpolarization is significantly reduced with micron-sized cloud particles as aresult of forward scattering. The presence of a cold or hot circumplanetarydisk may also produce a detectable degree of polarization ($\lesssim$1%) evenwith a uniform cloud layer in the atmosphere.

Polarized scattered light from self-luminous exoplanets. Three-dimensional scattering radiative transfer with ARTES