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Aims: The inner regions of high-mass protostars are often invisible in thenear-infrared. We aim to investigate the inner gaseous disc of IRAS11101-5829through scattered light from the outflow cavity walls.  Methods: We observed the environment of the high-mass young stellar objectIRAS11101-5829 and the closest knots of its jet, HH135-136, with theVLT/SINFONI. We also retrieved archival data from the high-resolution long-slitspectrograph VLT/X-shooter.  Results: We detect the first three bandheads of the $\upsilon=2-0$ COvibrational emission for the first time in this object. It is coincident withcontinuum and Br$\gamma$ emission and extends up to $\sim10000$ au to thenorth-east and $\sim10 000$ au to the south-west. The line profiles have beenmodelled as a Keplerian rotating disc assuming a single ring in LTE. The modeloutput gives a temperature of $\sim3000$ K, a CO column density of$\sim1\times10^{22}\mathrm{ cm^{-2}}$, and a projected Keplerian velocity$v_\mathrm{K}\sin i_\mathrm{disc} \sim 25\mathrm{ km s^{-1}}$, which isconsistent with previous modelling in other high-mass protostars. Inparticular, the low value of $v_\mathrm{K}\sin i_\mathrm{disc}$ suggests thatthe disc is observed almost face-on, whereas the well-constrained geometry ofthe jet imposes that the disc must be close to edge-on. This apparentdiscrepancy is interpreted as the CO seen reflected in the mirror of theoutflow cavity wall.  Conclusions: From both jet geometry and disc modelling, we conclude that allthe CO emission is seen through reflection by the cavity walls and notdirectly. This result implies that in the case of highly embedded objects, asfor many high-mass protostars, line profile modelling alone might be deceptiveand the observed emission could affect the derived physical and geometricalproperties; in particular the inclination of the system can be incorrectlyinterpreted.

Mirror, mirror on the outflow cavity wall. Near-infrared CO overtone disc emission of the high-mass YSO IRAS 11101-5829