Journal
ASTRONOMICAL JOURNAL
Volume 155, Issue 6, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-3881/aabcb8
Keywords
planets and satellites: gaseous planets; stars: individual (HR 8799)
Categories
Funding
- Spanish MINECO [AyA2014-55216]
- National Science Foundation Graduate Research Fellowship Program [DGE1232825]
- NASA [APRA08-0117, NNX14AJ80G, NNX15AC89G, NNX15AD95G/NEXSS, NNX15AE19G]
- STScI Directors Discretionary Research Fund
- NSF [AST-1411868, AST-1518332]
- NASA's Science Mission Directorate
- NASA WFIRST-SIT award [NNG16PJ24C]
- NASA JPL [1538907, 1529729, 1513640, 1534432-B-4.25]
- Division Of Astronomical Sciences [1518332, 1413744, 1411868] Funding Source: National Science Foundation
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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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