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

Alexandra Z. Greenbaum, Laurent Pueyo, Jean Baptiste Ruffio, Jason J. Wang, Robert J.De Rosa, Jonathan Aguilar, Julien Rameau, Travis Barman, Christian Marois, Mark S. Marley, Quinn Konopacky, Abhijith Rajan, Bruce Macintosh, Megan Ansdell, Pauline Arriaga, Vanessa P. Bailey, Joanna Bulger, Adam S. Burrows, Jeffrey Chilcote, Tara CottenRene Doyon, Gaspard Duchêne, Michael P. Fitzgerald, Katherine B. Follette, Benjamin Gerard, Stephen J. Goodsell, James R. Graham, Pascale Hibon, Li Wei Hung, Patrick Ingraham, Paul Kalas, James E. Larkin, Jérôme Maire, Franck Marchis, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Andrew Norton, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Marshall D. Perrin, Lisa Poyneer, Fredrik T. Rantakyrö, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Rémi Soummer, Sandrine Thomas, J. Kent Wallace, Kimberly Ward-Duong, Sloane Wiktorowicz, Schuyler Wolff

Research output: Contribution to journalArticle

12 Scopus citations

Abstract

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.

Original languageEnglish (US)
Article number226
JournalAstronomical Journal
Volume155
Issue number6
DOIs
StatePublished - Jun 2018

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • planets and satellites: gaseous planets
  • stars: individual (HR 8799)

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    Greenbaum, A. Z., Pueyo, L., Ruffio, J. B., Wang, J. J., Rosa, R. J. D., Aguilar, J., Rameau, J., Barman, T., Marois, C., Marley, M. S., Konopacky, Q., Rajan, A., Macintosh, B., Ansdell, M., Arriaga, P., Bailey, V. P., Bulger, J., Burrows, A. S., Chilcote, J., ... Wolff, S. (2018). GPI Spectra of HR 8799 c, d, and e from 1.5 to 2.4 μm with KLIP Forward Modeling. Astronomical Journal, 155(6), [226]. https://doi.org/10.3847/1538-3881/aabcb8