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Author
Millar-Blanchaer, Maxwell A.
Wang, Jason J.

Kalas, Paul
Graham, James R.
Duchêne, Gaspard
Nielsen, Eric L.

Perrin, Marshall

Moon, Dae-Sik

Padgett, Deborah

Metchev, Stanimir A.

Ammons, S. Mark

Bailey, Vanessa P.
Barman, Travis S.

Bruzzone, Sebastian
Bulger, Joanna
Chen, Christine H.

Chilcote, Jeffrey
Cotten, Tara

Rosa, Robert J. De
Doyon, Rene
Draper, Zachary H.

Esposito, Thomas M.

Fitzgerald, Michael P.

Follette, Katherine B.

Gerard, Benjamin L.

Greenbaum, Alexandra Z.

Hibon, Pascale

Hinkley, Sasha

Hung, Li-Wei
Ingraham, Patrick
Johnson-Groh, Mara

Konopacky, Quinn
Larkin, James E.

Macintosh, Bruce

Maire, Jérôme
Marchis, Franck

Marley, Mark S.

Marois, Christian

Matthews, Brenda C.

Oppenheimer, Rebecca

Palmer, David
Patience, Jennifer
Poyneer, Lisa
Pueyo, Laurent
Rajan, Abhijith

Rameau, Julien

Rantakyrö, Fredrik T.

Savransky, Dmitry

Schneider, Adam C.

Sivaramakrishnan, Anand

Song, Inseok

Soummer, Remi

Thomas, Sandrine
Vega, David
Wallace, J. Kent

Ward-Duong, Kimberly
Wiktorowicz, Sloane

Wolff, Schuyler

Affiliation
Univ Arizona, Lunar & Planetary LabIssue Date
2016-10-20
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IOP PUBLISHING LTDCitation
IMAGING AN 80 au RADIUS DUST RING AROUND THE F5V STAR HD 157587 2016, 152 (5):128 The Astronomical JournalJournal
The Astronomical JournalRights
© 2016. 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
We present H-band near-infrared polarimetric imaging observations of the F5V star HD 157587 obtained with the Gemini Planet Imager (GPI) that reveal the debris disk as a bright ring structure at a separation of similar to 80-100 au. The new GPI data complement recent Hubble Space Telescope/STIS observations that show the disk extending out to over 500 au. The GPI image displays a strong asymmetry along the projected minor axis as well as a fainter asymmetry along the projected major axis. We associate the minor and major axis asymmetries with polarized forward scattering and a possible stellocentric offset, respectively. To constrain the disk geometry, we fit two separate disk models to the polarized image, each using a different scattering phase function. Both models favor a disk inclination of similar to 70 degrees and a 1.5 +/- 0.6 au stellar offset in the plane of the sky along the projected major axis of the disk. We find that the stellar offset in the disk plane, perpendicular to the projected major axis is degenerate with the form of the scattering phase function and remains poorly constrained. The disk is not recovered in total intensity due in part to strong adaptive optics residuals, but we recover three point sources. Considering the system's proximity to the galactic plane and the point sources' positions relative to the disk, we consider it likely that they are background objects and unrelated to the disk's offset from the star.ISSN
1538-3881Version
Final published versionSponsors
NASA's NEXSS program [NNX15AD95G]; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; NSF [AST-1413718, AST-1518332]; NASA [NNX15AC89G]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]Additional Links
http://stacks.iop.org/1538-3881/152/i=5/a=128?key=crossref.de019cbc0cb15346f58c754c7c6d227aae974a485f413a2113503eed53cd6c53
10.3847/0004-6256/152/5/128