The Gemini Planet Imager view of the HD 32297 debris disk

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

Abstract

We present new H-band scattered light images of the HD 32297 edge-on debris disk obtained with the Gemini Planet Imager. The disk is detected in total and polarized intensity down to a projected angular separation of 0."15, or 20 au. 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 ≈100 au 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.

Additional Information

© 2020 The American Astronomical Society. Received 2020 February 11; revised 2020 March 25; accepted 2020 April 3; published 2020 May 7. We are grateful to Glenn Schneider for making his STIS image available for analysis. This work is based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under a cooperative agreement with the National Science Foundation (NSF) on behalf of the Gemini partnership: the NSF (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). This work made use of data from the European Space Agency mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement. This research made use of the SIMBAD and VizieR databases, operated at CDS, Strasbourg, France. This work was supported by NSF grants AST-1411868 (E.L.N., K.B.F., B.M., and J.P.), AST-141378 (G.D.), and AST-1518332 (T.M.E., R.J.D.R., J.R.G., P.K., and G.D.). This work was also supported by NASA grants NNX14AJ80G (E.L.N., B.M., F.M., and M.P.), NNX15AC89G and NNX15AD95G/NExSS (T.M.E., B.M., R.J.D.R., G.D., J.J.W., J.R.G., and P.K.), NN15AB52l (D.S.). M.R. is supported by the NSF Graduate Research Fellowship Program under grant No. DGE-1752134. J.R. and R.D. acknowledge support from the Fonds de Recherche du Quèbec. J.M.'s work was performed in part under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. M.M.B. and J.M. were supported by NASA through Hubble Fellowship grants #51378.01-A and HST-HF2-51414.001, respectively, and I.C. through Hubble Fellowship grant HST-HF2-51405.001-A, awarded by the Space Telescope Science Institute, which is operated by AURA, for NASA, under contract NAS5-26555. J.J.W. is supported by the Heising-Simons Foundation 51 Pegasi b postdoctoral fellowship. This work benefited from NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. Portions of this work were also performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. Facility: Gemini:South. - Software: MCFOST (Pinte et al. 2006), Gemini Planet Imager Data Reduction Pipeline (Perrin et al. 2014, 2016, http://ascl.net/1411.018), pyKLIP (Wang et al. 2015, http://ascl.net/1506.001), NumPy (Oliphant 2006, https://numpy.org), SciPy (Jones et al. 2001, http://www.scipy.org/), Astropy (The Astropy Collaboration et al. 2018), matplotlib (Hunter 2007; Droettboom et al. 2017), iPython (Pérez & Granger 2007), emcee (Foreman-Mackey et al. 2013, http://ascl.net/1303.002), corner (Foreman-Mackey 2016, http://ascl.net/1702.002).

Attached Files

Published - Duchêne_2020_AJ_159_251.pdf

Accepted Version - 2004.06027.pdf

Files

Duchêne_2020_AJ_159_251.pdf

Files (6.3 MB)

Name	Size	Download all
Duchêne_2020_AJ_159_251.pdf md5:2c51645fbf5d49019da5eb2f67b6c725	2.7 MB	Preview Download
2004.06027.pdf md5:f0b6919e1872550f6148474335ef4c05	3.6 MB	Preview Download

Additional details

	All versions	This version
Views	0	0
Downloads	0	0
Data volume	0 Bytes	0 Bytes