Wu, Ya-LinYa-LinWuClose, Laird M.Laird M.CloseBailey, Vanessa P.Vanessa P.BaileyRodigas, Timothy J.Timothy J.RodigasMales, Jared R.Jared R.MalesMorzinski, Katie M.Katie M.MorzinskiFollette, Katherine B.Katherine B.FolletteHinz, Philip M.Philip M.HinzPUGLISI, Alfio TimothyAlfio TimothyPUGLISIBRIGUGLIO PELLEGRINO, RUNA ANTONIORUNA ANTONIOBRIGUGLIO PELLEGRINOXOMPERO, MARCOMARCOXOMPERO2020-05-122020-05-1220160004-637Xhttp://hdl.handle.net/20.500.12386/24746We analyze archival data from Bailey and co-workers from the Magellan adaptive optics system and present the first 0.9 μm detection (z′ = 20.3 ± 0.4 mag; ∆z′ = 13.0 ± 0.4 mag) of the 11 M <SUB>Jup</SUB> circumbinary planet HD 106906AB b, as well as 1 and 3.8 μm detections of the debris disk around the binary. The disk has an east-west asymmetry in length and surface brightness, especially at 3.8 μm where the disk appears to be one-sided. The spectral energy distribution of b, when scaled to the K <SUB> S </SUB>-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 ≳ 100 AU) low mass ratio (M <SUB>p</SUB>/M <SUB>⋆</SUB> ≡ q ≲ 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. This paper includes data gathered with the 6.5 m Magellan Clay Telescope at Las Campanas Observatory, Chile.STAMPAenArticle10.3847/0004-637X/823/1/242-s2.0-84971659538000377216300024https://iopscience.iop.org/article/10.3847/0004-637X/823/1/24https://arxiv.org/abs/1604.068472016ApJ...823...24WFIS/05 - ASTRONOMIA E ASTROFISICA