GPI Spectra of HR 8799 c, d, and e from 1.5 to 2.4 μm with KLIP Forward Modeling
- Department of Astronomy, University of Michigan, Ann Arbor, MI 48109 (United States)
- Space Telescope Science Institute, Baltimore, MD 21218 (United States)
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305 (United States)
- Department of Astronomy, University of California, Berkeley, CA 94720 (United States)
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States)
- Institut de Recherche sur les Exoplanètes, Département de Physique, Université de Montréal, Montréal QC, H3C 3J7 (Canada)
- Lunar and Planetary Laboratory, University of Arizona, Tucson AZ 85721 (United States)
- National Research Council of Canada Herzberg, 5071 West Saanich Rd, Victoria, BC, V9E 2E7 (Canada)
- NASA Ames Research Center, Mountain View, CA 94035 (United States)
- Center for Astrophysics and Space Science, University of California San Diego, La Jolla, CA 92093 (United States)
- School of Earth and Space Exploration, Arizona State University, PO Box 871404, Tempe, AZ 85287 (United States)
- Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States)
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States)
- Subaru Telescope, NAOJ, 650 North A’ohoku Place, Hilo, HI 96720 (United States)
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.
- OSTI ID:
- 22897482
- Journal Information:
- Astronomical Journal (New York, N.Y. Online), Vol. 155, Issue 6; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-3881
- Country of Publication:
- United States
- Language:
- English
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