A Deep Polarimetric Study of the Asymmetrical Debris Disk HD 106906
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Author
Crotts, K.A.Matthews, B.C.
Esposito, T.M.
Duch ne, G.
Kalas, P.
Chen, C.H.
Arriaga, P.
Millar-Blanchaer, M.A.
Debes, J.H.
Draper, Z.H.
Fitzgerald, M.P.
Hom, J.
Macgregor, M.A.
Mazoyer, J.
Patience, J.
Rice, M.
Weinberger, A.J.
Wilner, D.J.
Wolff, S.
Affiliation
Department of Astronomy, University of ArizonaIssue Date
2021
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IOP Publishing LtdCitation
Crotts, K. A., Matthews, B. C., Esposito, T. M., Duch ne, G., Kalas, P., Chen, C. H., Arriaga, P., Millar-Blanchaer, M. A., Debes, J. H., Draper, Z. H., Fitzgerald, M. P., Hom, J., Macgregor, M. A., Mazoyer, J., Patience, J., Rice, M., Weinberger, A. J., Wilner, D. J., & Wolff, S. (2021). A Deep Polarimetric Study of the Asymmetrical Debris Disk HD 106906. Astrophysical Journal, 915(1).Journal
Astrophysical JournalRights
Copyright © 2021 The American Astronomical Society. All rights reserved.Collection Information
This 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 repository@u.library.arizona.edu.Abstract
Located in the Lower Centaurus Crux group, HD 106906 is a young, binary stellar system. This system is unique among discovered systems in that it contains an asymmetrical debris disk, as well as an 11 M Jup planet companion, at a separation of ∼735 au. Only a handful of other systems are known to contain both a disk and a directly imaged planet, where HD 106906 is the only one in which the planet has apparently been scattered. The debris disk is nearly edge-on and extends to roughly >500 au, where previous studies with the Hubble Space Telescope have shown the outer regions to have high asymmetry. To better understand the structure and composition of the disk, we have performed a deep polarimetric study of HD 106906's asymmetrical debris disk using newly obtained H-, J-, and K1-band polarimetric data from the Gemini Planet Imager. An empirical analysis of our data supports a disk that is asymmetrical in surface brightness and structure, where fitting an inclined ring model to the disk spine suggests that the disk may be highly eccentric (e ⪆ 0.16). A comparison of the disk flux with the stellar flux in each band suggests a blue color that also does not significantly vary across the disk. We discuss these results in terms of possible sources of asymmetry, where we find that dynamical interaction with the planet companion, HD 106906b, is a likely candidate. © 2021. The American Astronomical Society. All rights reserved.Note
Immediate accessISSN
0004-637XVersion
Final published versionae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/abff5c