Wolff, Schuyler G. and Perrin, Marshall and Millar-Blanchaer, Maxwell A. and Nielsen, Eric L. and Wang, Jason and Cardwell, Andrew and Chilcote, Jeffrey and Dong, Ruobing and Draper, Zachary H. and Duchêne, Gaspard and Fitzgerald, Michael P. and Goodsell, Stephen J. and Grady, Carol A. and Graham, James R. and Greenbaum, Alexandra Z. and Hartung, Markus and Hibon, Pascale and Hines, Dean C. and Hung, Li-Wei and Kalas, Paul and Macintosh, Bruce and Marchis, Franck and Marois, Christian and Pueyo, Laurent and Rantakyrö, Fredrik T. and Schneider, Glenn and Sivaramakrishnan, Anand and Wiktorowicz, Sloane J. (2016) 'The PDS 66 circumstellar disk as seen in polarized light with the Gemini Planet Imager.', Astrophysical journal letters., 818 (1). L15.
We present H- and K-band imaging polarimetry for the PDS 66 circumstellar disk obtained during the commissioning of the Gemini Planet Imager (GPI). Polarization images reveal a clear detection of the disk in to the 0farcs12 inner working angle (IWA) in the H band, almost three times closer to the star than the previous Hubble Space Telescope (HST) observations with NICMOS and STIS (0farcs35 effective IWA). The centro-symmetric polarization vectors confirm that the bright inner disk detection is due to circumstellar scattered light. A more diffuse disk extends to a bright outer ring centered at 80 AU. We discuss several physical mechanisms capable of producing the observed ring + gap structure. GPI data confirm enhanced scattering on the east side of the disk that is inferred to be nearer to us. We also detect a lateral asymmetry in the south possibly due to shadowing from material within the IWA. This likely corresponds to a temporally variable azimuthal asymmetry observed in HST/STIS coronagraphic imaging.
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|Publisher Web site:||https://doi.org/10.3847/2041-8205/818/1/L15|
|Publisher statement:||© 2016. The American Astronomical Society. All rights reserved.|
|Date accepted:||19 January 2016|
|Date deposited:||26 January 2017|
|Date of first online publication:||08 February 2016|
|Date first made open access:||26 January 2017|
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