Thomas M. Esposito, University of California, Berkeley
Gaspard Duchne, University of California, Berkeley
Paul Kalas, University of California, Berkeley
Malena Rice, University of California, Berkeley
Ilodie Choquet, California Institute of Technology
Bin Ren, Johns Hopkins University
Marshall D. Perrin, Space Telescope Science Institute
Christine H. Chen, Space Telescope Science Institute
Pauline Arriaga, University of California, Los Angeles
Eugene Chiang, University of California, Berkeley
Eric L. Nielsen, SETI Institute
James R. Graham, University of California, Berkeley
Jason J. Wang, University of California, Berkeley
Robert J.De Rosa, University of California, Berkeley
Katherine B. Follette, Kavli Institute for Particle Astrophysics and Cosmology
S. Mark Ammons, Lawrence Livermore National Laboratory
Megan Ansdell, University of California, Berkeley
Vanessa P. Bailey, Jet Propulsion Laboratory
Travis Barman, The University of Arizona
Juan Sebastián Bruzzone, Western University
Joanna Bulger, National Institutes of Natural Sciences - National Astronomical Observatory of Japan
Jeffrey Chilcote, Kavli Institute for Particle Astrophysics and Cosmology
Tara Cotten, University of Georgia
Rene Doyon, Institut de Recherche sur les Exoplanètes
Michael P. Fitzgerald, University of California, Los Angeles
Stephen J. Goodsell, Gemini Observatory
Alexandra Z. Greenbaum, University of Michigan, Ann Arbor
Pascale Hibon, Gemini ObservatorySouthern Operations Center
Li Wei Hung, University of California, Los Angeles
Patrick Ingraham, Large Synoptic Survey Telescope
Quinn Konopacky, Center for Astrophysics & Space Sciences
James E. Larkin, University of California, Los Angeles
Kimberly Ward-Duong, Amherst CollegeFollow
et al, Various Institutions

Document Type


Publication Date


Publication Title

Astronomical Journal


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 μm), we detect the highly inclined (i = 85°) ring of debris down to a projected separation of ∼12 au (∼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.″4). We measure the ring's scattering phase function and polarization fraction over scattering angles of 22°-125°, showing a preference for forward scattering and a polarization fraction that peaks at ∼30% near the ansae. Modeling of the scattered-light disk indicates that the ring spans radii of ∼60-220 au, has a vertical thickness similar to that of other resolved dust rings, and contains grains as small as 1.5 μm 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.


circumstellar matter, infrared: planetary systems, stars: individual (HD 35841), techniques: high angular resolution










© 2018. The American Astronomical Society.


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