We analyze archival data from Bailey and co-workers from the Magellan adaptive optics system and present the first 0.9 ~ { } \mu m detection ( z ^ { \prime } = 20.3 \pm 0.4 mag ; \Delta z ^ { \prime } = 13.0 \pm 0.4 mag ) of the 11 M _ { \mathrm { Jup } } circumbinary planet HD 106906AB b , as well as the 1 and 3.8 ~ { } \mu m detections of the debris disk around the binary .
The disk has an east–west asymmetry in length and surface brightness , especially at 3.8 ~ { } \mu m where the disk appears to be one-sided .
The spectral energy distribution of b , when scaled to the K _ { S } -band photometry , is consistent with 1800 K atmospheric models without significant dust reddening , unlike some young , very red , low-mass companions such as CT Cha B and 1RXS 1609 B .
Therefore , the suggested circumplanetary disk of Kalas and co-workers might not contain much material , or might be closer to face-on .
Finally , we suggest that the widest ( a \gtrsim 100 AU ) low mass ratio ( M _ { \mathrm { p } } / M _ { \mathrm { \star } } \equiv q \lesssim 0.01 ) companions may have formed inside protoplanetary disks , but were later scattered by binary/planet interactions .
Such a scattering event may have occurred for HD 106906AB b with its central binary star , but definitive proof at this time is elusive .