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Multiband Polarimetric Imaging of HR 4796A with the Gemini Planet Imager

Arriaga, Pauline and Fitzgerald, Michael P. and Duchêne, Gaspard and Kalas, Paul and Millar-Blanchaer, Maxwell A. and Perrin, Marshall D. and Chen, Christine H. and Mazoyer, Johan and Ammons, Mark and Bailey, Vanessa P. and Barman, Trafis S. and Bulger, Joanna and Chilcote, Jeffrey K. and Cotten, Tara and De Rosa, Robert J. and Doyon, Rene and Esposito, Thomas M. and Follette, Katherine B. and Gerard, Benjamin L. and Goodsell, Stephen and Graham, James R. and Greenbaum, Alexandra Z. and Hibon, Pascale and Hom, Justin and Hung, Li-Wei and Ingraham, Patrick and Konopacky, Quinn M. and Macintosh, Bruce A. and Maire, Jérôme and Marchis, Franck and Marley, Mark S. and Marois, Christian and Metchev, Stanimir and Nielsen, Eric L. and Oppenheimer, Rebecca and Palmer, David W. and Patience, Jenny and Poyneer, Lisa A. and Pueyo, Laurent and Rajan, Abhijith and Rameau, Julien and Rantakyrö, Fredrik T. and Ruffio, Jean-Baptiste and Savransky, Dmitry and Schneider, Adam C. and Sivaramakrishnan, Anand and Song, Inseok and Soummer, Remi and Thomas, Sandrine and Wang, Jason J. and Ward-Duong, Kimberly and Wolff, Schuyler G. (2020) Multiband Polarimetric Imaging of HR 4796A with the Gemini Planet Imager. Astronomical Journal, 160 (2). Art. No. 79. ISSN 1538-3881.

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HR4796A hosts a well-studied debris disk with a long history due to its high fractional luminosity and favorable inclination, which facilitate both unresolved and resolved observations. We present new J- and K 1-band images of the resolved debris disk HR4796A taken in the polarimetric mode of the Gemini Planet Imager (GPI). The polarized intensity features a strongly forward-scattered brightness distribution and is undetected at the far side of the disk. The total intensity is detected at all scattering angles and also exhibits a strong forward-scattering peak. We use a forward-modeled geometric disk in order to extract geometric parameters, polarized fraction, and total intensity scattering phase functions for these data as well as H-band data previously taken by GPI. We find the polarized phase function becomes increasingly more forward-scattering as wavelength increases. We fit Mie and distribution of hollow spheres (DHS) grain models to the extracted functions. We find that it is possible to generate a satisfactory model for the total intensity using a DHS model, but not with a Mie model. We find that no single grain population of DHS or Mie grains of arbitrary composition can simultaneously reproduce the polarized fraction and total intensity scattering phase functions, indicating the need for more sophisticated grain models.

Item Type:Article
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URLURL TypeDescription Paper
Arriaga, Pauline0000-0001-6364-2834
Fitzgerald, Michael P.0000-0002-0176-8973
Duchêne, Gaspard0000-0002-5092-6464
Kalas, Paul0000-0002-6221-5360
Millar-Blanchaer, Maxwell A.0000-0001-6205-9233
Perrin, Marshall D.0000-0002-3191-8151
Chen, Christine H.0000-0002-8382-0447
Mazoyer, Johan0000-0002-9133-3091
Ammons, Mark0000-0002-4918-0247
Bailey, Vanessa P.0000-0002-5407-2806
Barman, Trafis S.0000-0002-7129-3002
Bulger, Joanna0000-0003-4641-2003
Chilcote, Jeffrey K.0000-0001-6305-7272
Cotten, Tara0000-0003-0156-3019
De Rosa, Robert J.0000-0002-4918-0247
Esposito, Thomas M.0000-0002-0792-3719
Follette, Katherine B.0000-0002-7821-0695
Gerard, Benjamin L.0000-0003-3978-9195
Goodsell, Stephen0000-0002-4144-5116
Greenbaum, Alexandra Z.0000-0002-7162-8036
Hibon, Pascale0000-0003-3726-5494
Hom, Justin0000-0001-9994-2142
Hung, Li-Wei0000-0003-1498-6088
Ingraham, Patrick0000-0003-3715-8138
Konopacky, Quinn M.0000-0002-9936-6285
Macintosh, Bruce A.0000-0003-1212-7538
Marchis, Franck0000-0001-7016-7277
Marley, Mark S.0000-0002-5251-2943
Marois, Christian0000-0002-4164-4182
Metchev, Stanimir0000-0003-3050-8203
Nielsen, Eric L.0000-0001-6975-9056
Oppenheimer, Rebecca0000-0001-7130-7681
Pueyo, Laurent0000-0003-3818-408X
Rajan, Abhijith0000-0002-9246-5467
Rameau, Julien0000-0003-0029-0258
Rantakyrö, Fredrik T.0000-0002-9667-2244
Ruffio, Jean-Baptiste0000-0003-2233-4821
Savransky, Dmitry0000-0002-8711-7206
Schneider, Adam C.0000-0002-6294-5937
Sivaramakrishnan, Anand0000-0003-1251-4124
Song, Inseok0000-0002-5815-7372
Soummer, Remi0000-0003-2753-2819
Thomas, Sandrine0000-0002-9121-3436
Wang, Jason J.0000-0003-0774-6502
Ward-Duong, Kimberly0000-0002-4479-8291
Wolff, Schuyler G.0000-0002-9977-8255
Additional Information:© 2020. The American Astronomical Society. Received 2020 March 10; revised 2020 April 28; accepted 2020 May 8; published 2020 July 23. This research was supported in part by NSF AST-1413718 and AST-1615272, AST-NNX15AC89G, AST-1413718, AST-1615272. J.M. acknowledges support for this work provided by NASA through the NASA Hubble Fellowship grant #HST-HF2-51414.001, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Portions of this work were performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. 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 was supported by the NSF AST-1518332 (T.M.E., R.J.D.R., J.R.G., P.K., G.D.) and NASA grants NNX15AC89G and NNX15AD95G/NExSS (T.M.E., B.M., R.J.D.R., G.D., J.J.W, J.R.G., P.K.). This work benefited from NASA's Nexus for Exoplanet System Science (NExSS) research coordination network, sponsored by NASA's Science Mission Directorate. G.D. acknowledges support from NSF grants AST-141378 and AST-1518332, as well as NASA grants NNX15AC89G and NNX15AD95G/NExSS. Software: Gemini Planet Imager Data Pipeline (Perrin et al. 2014), PyKLIP (Wang et al. 2014), MCFOST (Pinte et al. 2006a), emcee (Foreman-Mackey et al. 2013).
Funding AgencyGrant Number
NASA Hubble FellowshipHST-HF2-51414.001
Department of Energy (DOE)DE-AC52-07NA27344
Heising-Simons Foundation51 Pegasi b Fellowship
Subject Keywords:Debris disks ; Circumstellar disks ; Circumstellar dust ; Polarimetry ; Near infrared astronomy ; Coronagraphic imaging
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Debris disks (363); Circumstellar disks (235); Circumstellar dust (236); Polarimetry (1278); Near infrared astronomy (1093); Coronagraphic imaging (313)
Record Number:CaltechAUTHORS:20200724-100653276
Persistent URL:
Official Citation:Pauline Arriaga et al 2020 AJ 160 79
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104557
Deposited By: George Porter
Deposited On:24 Jul 2020 21:39
Last Modified:24 Jul 2020 21:39

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