Direct Imaging of the HD 35841 Debris Disk: A Polarized Dust Ring from Gemini Planet Imager and an Outer Halo from /STIS
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Author
Esposito, Thomas M.
Duchêne, Gaspard
Kalas, Paul
Rice, Malena
Choquet, Élodie
Ren, Bin
Perrin, Marshall

Chen, Christine H.
Arriaga, Pauline

Chiang, Eugene

Nielsen, Eric L.

Graham, James R.
Wang, Jason J.

Rosa, Robert J. De
Follette, Katherine B.

Ammons, S. Mark

Ansdell, Megan
Bailey, Vanessa P.
Barman, Travis
Bruzzone, Juan Sebastián
Bulger, Joanna

Chilcote, Jeffrey
Cotten, Tara

Doyon, Rene
Fitzgerald, Michael P.

Goodsell, Stephen J.
Greenbaum, Alexandra Z.

Hibon, Pascale

Hung, Li-Wei

Ingraham, Patrick

Konopacky, Quinn
Larkin, James E.

Macintosh, Bruce

Maire, Jérôme
Marchis, Franck

Marois, Christian

Mazoyer, Johan
Metchev, Stanimir
Millar-Blanchaer, Maxwell A.
Oppenheimer, Rebecca

Palmer, David

Patience, Jennifer
Poyneer, Lisa
Pueyo, Laurent
Rajan, Abhijith
Rameau, Julien

Rantakyrö, Fredrik T.

Ryan, Dominic
Savransky, Dmitry

Schneider, Adam C.

Sivaramakrishnan, Anand

Song, Inseok

Soummer, Rémi
Thomas, Sandrine
Wallace, J. Kent

Ward-Duong, Kimberly

Wiktorowicz, Sloane

Wolff, Schuyler
Affiliation
Univ Arizona, Lunar & Planetary LabIssue Date
2018-08Keywords
circumstellar matterinfrared
planetary systems
stars: individual (HD 35841)
techniques: high angular resolution
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IOP PUBLISHING LTDCitation
Thomas M. Esposito et al 2018 AJ 156 47Journal
ASTRONOMICAL JOURNALRights
© 2018. 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 new high resolution imaging of a light-scattering dust ring and halo around the young star HD 35841. Using spectroscopic and polarimetric data from the Gemini Planet Imager in H-band (1.6 mu m), we detect the highly inclined (i = 85 degrees) ring of debris down to a projected separation of similar to 12 au (similar to 0.'' 12) for the first time. Optical imaging from HST/STIS shows a smooth dust halo extending outward from the ring to >140 au (>1.'' 1 4). We measure the ring's scattering phase function and polarization fraction over scattering angles of 22 degrees-125 degrees, showing a preference for forward scattering and a polarization fraction that peaks at similar to 30% near the ansae. Modeling of the scattered-light disk indicates that the ring spans radii of similar to 60-220 au, has a vertical thickness similar to that of other resolved dust rings, and contains grains as small as 1.5 mu m in diameter. These models also suggest the grains have a low porosity, are more likely to consist of carbon than astrosilicates, and contain significant water ice. The halo has a surface brightness profile consistent with that expected from grains pushed by radiation pressure from the main ring onto highly eccentric but still bound orbits. We also briefly investigate arrangements of a possible inner disk component implied by our spectral energy distribution models, and speculate about the limitations of Mie theory for doing detailed analyses of debris disk dust populations.ISSN
1538-3881Version
Final published versionSponsors
NASA [NAS 5-26555, NNX15AC89G, NNX15AD95G/NEXSS]; NSF [AST-1518332]; NASA's Science Mission Directorate; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; [GO-13381]Additional Links
http://stacks.iop.org/1538-3881/156/i=2/a=47?key=crossref.6c6f62a3ca823c022172c85148808d7bae974a485f413a2113503eed53cd6c53
10.3847/1538-3881/aacbc9