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Multiband polarimetric imaging of HR 4796A with the Gemini Planet Imager

From National Research Council Canada

DOIResolve DOI: https://doi.org/10.3847/1538-3881/ab91b1
AuthorSearch for: ORCID identifier: https://orcid.org/0000-0001-6364-2834; Search for: ORCID identifier: https://orcid.org/0000-0002-0176-8973; Search for: ORCID identifier: https://orcid.org/0000-0002-5092-6464; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0001-6205-9233; Search for: ORCID identifier: https://orcid.org/0000-0002-3191-8151; Search for: ORCID identifier: https://orcid.org/0000-0002-8382-0447; Search for: ORCID identifier: https://orcid.org/0000-0002-9133-3091; Search for: ORCID identifier: https://orcid.org/0000-0002-4918-0247; Search for: ORCID identifier: https://orcid.org/0000-0002-5407-2806; Search for: ORCID identifier: https://orcid.org/0000-0002-7129-3002; Search for: ORCID identifier: https://orcid.org/0000-0003-4641-2003; Search for: ORCID identifier: https://orcid.org/0000-0001-6305-7272; Search for: ORCID identifier: https://orcid.org/0000-0003-0156-3019; Search for: ; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0002-0792-3719; Search for: ORCID identifier: https://orcid.org/0000-0002-7821-0695; Search for: 1ORCID identifier: https://orcid.org/0000-0003-3978-9195; Search for: ORCID identifier: https://orcid.org/0000-0002-4144-5116; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0002-7162-8036; Search for: ORCID identifier: https://orcid.org/0000-0003-3726-5494; Search for: ORCID identifier: https://orcid.org/0000-0001-9994-2142; Search for: ORCID identifier: https://orcid.org/0000-0003-1498-6088; Search for: ORCID identifier: https://orcid.org/0000-0003-3715-8138; Search for: ORCID identifier: https://orcid.org/0000-0002-9936-6285; Search for: ORCID identifier: https://orcid.org/0000-0003-1212-7538; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0001-7016-7277; Search for: ORCID identifier: https://orcid.org/0000-0002-5251-2943; Search for: 1ORCID identifier: https://orcid.org/0000-0002-4164-4182; Search for: ORCID identifier: https://orcid.org/0000-0003-3050-8203; Search for: ORCID identifier: https://orcid.org/0000-0001-6975-9056; Search for: ORCID identifier: https://orcid.org/0000-0001-7130-7681; Search for: ; Search for: ; Search for: ; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0002-9246-5467; Search for: ORCID identifier: https://orcid.org/0000-0003-0029-0258; Search for: ORCID identifier: https://orcid.org/0000-0002-9667-2244; Search for: ORCID identifier: https://orcid.org/0000-0003-2233-4821; Search for: ORCID identifier: https://orcid.org/0000-0002-8711-7206; Search for: ORCID identifier: https://orcid.org/0000-0002-6294-5937; Search for: ORCID identifier: https://orcid.org/0000-0003-1251-4124; Search for: ORCID identifier: https://orcid.org/0000-0002-5815-7372; Search for: ORCID identifier: https://orcid.org/0000-0003-2753-2819; Search for: ORCID identifier: https://orcid.org/0000-0002-9121-3436; Search for: ORCID identifier: https://orcid.org/0000-0003-0774-6502; Search for: ORCID identifier: https://orcid.org/0000-0002-4479-8291; Search for: ORCID identifier: https://orcid.org/0000-0002-9977-8255
Affiliation
  1. National Research Council of Canada. Herzberg Astronomy and Astrophysics
FunderSearch for: NASA; Search for: Lawrence Livermore National Laboratory
FormatText, Article
Physical description13 p.
Subjectdebris disks (363); circumstellar disks (235); circumstellar dust (236); polarimetry (1278); near infrared astronomy (1093); coronagraphic imaging (313)
Abstract
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 K1-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.
Publication date
PublisherIOP
In
  • The Astronomical Journal 160, no. 2, 79 (23 July 2020).
LanguageEnglish
Peer reviewedYes
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Record identifier7a3e8ae5-78b0-4458-8270-2693eedeb4fa
Record created2022-05-16
Record modified2022-05-16
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