MAGELLAN AO SYSTEM z ′, Y S , AND L ′ OBSERVATIONS OF THE VERY WIDE 650 AU HD 106906 PLANETARY SYSTEM
Close, Laird M.
Bailey, Vanessa P.
Rodigas, Timothy J.
Males, Jared R.
Morzinski, Katie M.
Follette, Katherine B.
Hinz, Philip M.
AffiliationUniv Arizona, Steward Observ
instrumentation: adaptive optics
planets and satellites: individual (HD 106906AB b)
stars: individual (HD 106906AB)
techniques: high angular resolution
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PublisherIOP PUBLISHING LTD
CitationMAGELLAN AO SYSTEM z ′, Y S , AND L ′ OBSERVATIONS OF THE VERY WIDE 650 AU HD 106906 PLANETARY SYSTEM 2016, 823 (1):24 The Astrophysical Journal
JournalThe Astrophysical Journal
Rights© 2016. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractWe 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 +/- 0.4 mag; Delta z' = 13.0 +/- 0.4 mag) of the 11 M-Jup circumbinary planet HD 106906AB b, as well as 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 greater than or similar to 100 AU) low mass ratio (M-p/M-star = q less than or similar to 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.
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