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We explore KLIP forward modeling spectral extraction on Gemini Planet Imagercoronagraphic data of HR 8799, using PyKLIP and show algorithm stability withvarying KLIP parameters. We report new and re-reduced spectrophotometry of HR8799 c, d, and e in H & K bands. We discuss a strategy for choosing optimalKLIP PSF subtraction parameters by injecting simulated sources and recoveringthem over a range of parameters. The K1/K2 spectra for HR 8799 c and d aresimilar to previously published results from the same dataset. We also presenta K band spectrum of HR 8799 e for the first time and show that our H-bandspectra agree well with previously published spectra from the VLT/SPHEREinstrument. We show that HR 8799 c and d show significant differences in theirH & K spectra, but do not find any conclusive differences between d and e or cand e, likely due to large error bars in the recovered spectrum of e. Comparedto M, L, and T-type field brown dwarfs, all three planets are most consistentwith mid and late L spectral types. All objects are consistent with low gravitybut a lack of standard spectra for low gravity limit the ability to fit thebest spectral type. We discuss how dedicated modeling efforts can better fit HR8799 planets' near-IR flux and discuss how differences between the propertiesof these planets can be further explored.

GPI spectra of HR 8799 c, d, and e from 1.5 to 2.4$\mu$m with KLIP Forward Modeling