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 \micron ) , we detect the highly inclined ( i = 85 \degr ) ring of debris down to a projected separation of { \sim } 12 au ( { \sim } 0 \farcs 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 \arcsec ) .
We measure the ring ’ s scattering phase function and polarization fraction over scattering angles of 22 \degr – 125 \degr , showing a preference for forward scattering and a polarization fraction that peaks at { \sim } 30 % near the ansae .
Modeling of the scattered-light disk indicates that the ring spans radii of { \sim } 60 –220 au , has a vertical thickness similar to that of other resolved dust rings , and contains grains as small as 1.5 \micron 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 .