Abstract
Author(s): Kalas, PG; Rajan, A; Wang, JJ; Millar-Blanchaer, MA; Duchene, G; Chen, C; Fitzgerald, MP; Dong, R; Graham, JR; Patience, J; Macintosh, B; Murray-Clay, R; Matthews, B; Rameau, J; Marois, C; Chilcote, J; Rosa, RJD; Doyon, R; Draper, ZH; Lawler, S; Ammons, SM; Arriaga, P; Bulger, J; Cotten, T; Follette, KB; Goodsell, S; Greenbaum, A; Hibon, P; Hinkley, S; Hung, LW; Ingraham, P; Konapacky, Q; Lafreniere, D; Larkin, JE; Long, D; Maire, J; Marchis, F; Metchev, S; Morzinski, KM; Nielsen, EL; Oppenheimer, R; Perrin, MD; Pueyo, L; Rantakyro, FT; Ruffio, JB; Saddlemyer, L; Savransky, D; Schneider, AC; Sivaramakrishnan, A; Soummer, R; Song, I; Thomas, S; Vasisht, G; Ward-Duong, K; Wiktorowicz, SJ; Wolff, SG | Abstract: We present the first scattered light detections of the HD 106906 debris disk using the Gemini/Gemini Planet Imager in the infrared and Hubble Space Telescope (HST)/Advanced Camera for Surveys in the optical. HD 106906 is a 13 Myr old F5V star in the Sco-Cen association, with a previously detected planet-mass candidate HD 106906b projected 650 AU from the host star. Our observations reveal a near edge-on debris disk that has a central cleared region with radius ∼50 AU, and an outer extent g500 AU. The HST data show that the outer regions are highly asymmetric, resembling the needle morphology seen for the HD 15115 debris disk. The planet candidate is oriented ∼21° away from the position angle of the primary's debris disk, strongly suggesting non-coplanarity with the system. We hypothesize that HD 106906b could be dynamically involved in the perturbation of the primary's disk, and investigate whether or not there is evidence for a circumplanetary dust disk or cloud that is either primordial or captured from the primary. We show that both the existing optical properties and near-infrared colors of HD 106906b are weakly consistent with this possibility, motivating future work to test for the observational signatures of dust surrounding the planet.
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