  We have observed the eclipsing, post-common envelope white dwarf-brown dwarf
binary, SDSS141126.20+200911.1, in the near-IR with the HAWK-I imager, and
present here the first direct detection of the dark side of an irradiated brown
dwarf in the $H$ band, and a tentative detection in the $K_s$ band. Our
analysis of the lightcurves and indicates that the brown dwarf is likely to
have an effective temperature of 1300 K, which is not consistent with the
effective temperature of 800 K suggested by its mass and radius. As the brown
dwarf is already absorbing almost all the white dwarf emission in the $K_s$
band we suggest that this inconsistency may be due to the UV-irradiation from
the white dwarf inducing an artificial brightening in the $K_s$ band, similar
to that seen for the similar system WD0137-349B, suggesting this brightening
may be characteristic of these UV-irradiated binaries.
