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GPI Spectra of HR 8799 c, d, and e from 1.5 to 2.4 μm with KLIP Forward Modeling

  • Author(s): Greenbaum, AZ
  • Pueyo, L
  • Ruffio, JB
  • Wang, JJ
  • Rosa, RJD
  • Aguilar, J
  • Rameau, J
  • Barman, T
  • Marois, C
  • Marley, MS
  • Konopacky, Q
  • Rajan, A
  • Macintosh, B
  • Ansdell, M
  • Arriaga, P
  • Bailey, VP
  • Bulger, J
  • Burrows, AS
  • Chilcote, J
  • Cotten, T
  • Doyon, R
  • Duchêne, G
  • Fitzgerald, MP
  • Follette, KB
  • Gerard, B
  • Goodsell, SJ
  • Graham, JR
  • Hibon, P
  • Hung, LW
  • Ingraham, P
  • Kalas, P
  • Larkin, JE
  • Maire, J
  • Marchis, F
  • Metchev, S
  • Millar-Blanchaer, MA
  • Nielsen, EL
  • Norton, A
  • Oppenheimer, R
  • Palmer, D
  • Patience, J
  • Perrin, MD
  • Poyneer, L
  • Rantakyrö, FT
  • Savransky, D
  • Schneider, AC
  • Sivaramakrishnan, A
  • Song, I
  • Soummer, R
  • Thomas, S
  • Wallace, JK
  • Ward-Duong, K
  • Wiktorowicz, S
  • Wolff, S
  • et al.

We explore KLIP forward modeling spectral extraction on Gemini Planet Imager coronagraphic data of HR 8799, using PyKLIP, and show algorithm stability with varying KLIP parameters. We report new and re-reduced spectrophotometry of HR 8799 c, d, and e in the H and K bands. We discuss a strategy for choosing optimal KLIP PSF subtraction parameters by injecting simulated sources and recovering them over a range of parameters. The K1/K2 spectra for HR 8799 c and d are similar to previously published results from the same data set. We also present a K-band spectrum of HR 8799 e for the first time and show that our H-band spectra agree well with previously published spectra from the VLT/SPHERE instrument. We show that HR 8799 c and d show significant differences in their H and K spectra, but do not find any conclusive differences between d and e, nor between c and e, likely due to large error bars in the recovered spectrum of e. Compared to M-, L-, and T-type field brown dwarfs, all three planets are most consistent with mid- and late-L spectral types. All objects are consistent with low gravity, but a lack of standard spectra for low gravity limit the ability to fit the best spectral type. We discuss how dedicated modeling efforts can better fit HR 8799 planets' near-IR flux, as well as how differences between the properties of these planets can be further explored.

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