Fig. C.1
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Top: Radial profile of the cooling timescale β for the disk. The regions of the disk where we find starlight-driven shadows lie in the intermediate cooling timescale regime (1–30 au). Bottom: Vertical profile of the cooling timescale β at R = 1 au. We see that for most of the disk (except for the atmosphere, and outermost regions), optically thick cooling is more dominant.
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