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We analyze archival data from Bailey and co-workers from the $Magellan$adaptive optics system and present the first 0.9 $\mu$m detection ($z' =20.3\pm0.4$ mag; $\Delta z'=13.0\pm0.4$ mag) of the 11 $M_\mathrm{Jup}$circumbinary planet HD 106906AB b, as well as the 1 and 3.8 $\mu$m detectionsof the debris disk around the binary. The disk has an east-west asymmetry inlength and surface brightness, especially at 3.8 $\mu$m where the disk appearsto be one-sided. The spectral energy distribution of b, when scaled to the$K_S$-band photometry, is consistent with 1800 K atmospheric models withoutsignificant dust reddening, unlike some young, very red, low-mass companionssuch as CT Cha B and 1RXS 1609 B. Therefore, the suggested circumplanetary diskof Kalas and co-workers might not contain much material, or might be closer toface-on. Finally, we suggest that the widest ($a\gtrsim100$ AU) low mass ratio($M_\mathrm{p}/M_\mathrm{\star} \equiv q\lesssim0.01$) companions may haveformed inside protoplanetary disks, but were later scattered by binary/planetinteractions. Such a scattering event may have occurred for HD 106906AB b withits central binary star, but definitive proof at this time is elusive.

Magellan AO System $z'$, $Y_S$, and $L'$ Observations of the Very Wide 650 AU HD 106906 Planetary System