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arXiv · 2004.06027

The Gemini Planet Imager view of the HD 32297 debris disk

Gaspard Duchene·Malena Rice·Justin Hom·Joseph Zalesky·Thomas M. Esposito·Maxwell A. Millar-Blanchaer·Bin Ren·Paul Kalas·Michael Fitzgerald·Pauline Arriaga·Sebastian Bruzzone·Joanna Bulger·Christine H. Chen·Eugene Chiang·Tara Cotten·Ian Czekala·Robert J. De Rosa·Ruobing Dong·Zachary H. Draper·Katherine B. Follette·James R. Graham·Li-Wei Hung·Ronald Lopez·Bruce Macintosh·Brenda C. Matthews·Johan Mazoyer·Stan Metchev·Jennifer Patience·Marshall D. Perrin·Julien Rameau·Inseok Song·Kevin Stahl·Jason Wang·Schuyler Wolff·Ben Zuckerman·S. Mark Ammons·Vanessa P. Bailey·Travis Barman·Jeffrey Chilcote·Rene Doyon·Benjamin L. Gerard·Stephen J. Goodsell·Alexandra Z. Greenbaum·Pascale Hibon·Patrick Ingraham·Quinn Konopacky·Jerome Maire·Franck Marchis·Mark S. Marley·Christian Marois·Eric L. Nielsen·Rebecca Oppenheimer·David Palmer·Lisa Poyneer·Laurent Pueyo·Abhijith Rajan·Fredrik T. Rantrakiro·Jean-Baptiste Ruffio·Dmitry Savransky·Adam C. Schneider·Anand Sivaramakrishnan·Remi Soummer·Sandrine Thomas
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Abstract

We present new $H$-band scattered light images of the HD 32297 edge-on debris disk obtained with the Gemini Planet Imager (GPI). The disk is detected in total and polarized intensity down to a projected angular separation of 0.15", or 20au. On the other hand, the large scale swept-back halo remains undetected, likely a consequence of its markedly blue color relative to the parent body belt. We analyze the curvature of the disk spine and estimate a radius of $\approx$100au for the parent body belt, smaller than past scattered light studies but consistent with thermal emission maps of the system. We employ three different flux-preserving post-processing methods to suppress the residual starlight and evaluate the surface brightness and polarization profile along the disk spine. Unlike past studies of the system, our high fidelity images reveal the disk to be highly symmetric and devoid of morphological and surface brightness perturbations. We find the dust scattering properties of the system to be consistent with those observed in other debris disks, with the exception of HR 4796. Finally, we find no direct evidence for the presence of a planetary-mass object in the system.

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Gaspard Duchene, Malena Rice, Justin Hom, Joseph Zalesky, Thomas M. Esposito, Maxwell A. Millar-Blanchaer, Bin Ren, Paul Kalas, Michael Fitzgerald, Pauline Arriaga, Sebastian Bruzzone, Joanna Bulger, Christine H. Chen, Eugene Chiang, Tara Cotten, Ian Czekala, Robert J. De Rosa, Ruobing Dong, Zachary H. Draper, Katherine B. Follette, James R. Graham, Li-Wei Hung, Ronald Lopez, Bruce Macintosh, Brenda C. Matthews, Johan Mazoyer, Stan Metchev, Jennifer Patience, Marshall D. Perrin, Julien Rameau, Inseok Song, Kevin Stahl, Jason Wang, Schuyler Wolff, Ben Zuckerman, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Jeffrey Chilcote, Rene Doyon, Benjamin L. Gerard, Stephen J. Goodsell, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Quinn Konopacky, Jerome Maire, Franck Marchis, Mark S. Marley, Christian Marois, Eric L. Nielsen, Rebecca Oppenheimer, David Palmer, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantrakiro, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Remi Soummer, Sandrine Thomas. 2020-04-13. The Gemini Planet Imager view of the HD 32297 debris disk. https://doi.org/10.3847/1538-3881/ab8881

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