TY - JOUR
T1 - GPI Spectra of HR 8799 c, d, and e from 1.5 to 2.4 μm with KLIP Forward Modeling
AU - Greenbaum, Alexandra Z.
AU - Pueyo, Laurent
AU - Ruffio, Jean Baptiste
AU - Wang, Jason J.
AU - Rosa, Robert J.De
AU - Aguilar, Jonathan
AU - Rameau, Julien
AU - Barman, Travis
AU - Marois, Christian
AU - Marley, Mark S.
AU - Konopacky, Quinn
AU - Rajan, Abhijith
AU - Macintosh, Bruce
AU - Ansdell, Megan
AU - Arriaga, Pauline
AU - Bailey, Vanessa P.
AU - Bulger, Joanna
AU - Burrows, Adam S.
AU - Chilcote, Jeffrey
AU - Cotten, Tara
AU - Doyon, Rene
AU - Duchêne, Gaspard
AU - Fitzgerald, Michael P.
AU - Follette, Katherine B.
AU - Gerard, Benjamin
AU - Goodsell, Stephen J.
AU - Graham, James R.
AU - Hibon, Pascale
AU - Hung, Li Wei
AU - Ingraham, Patrick
AU - Kalas, Paul
AU - Larkin, James E.
AU - Maire, Jérôme
AU - Marchis, Franck
AU - Metchev, Stanimir
AU - Millar-Blanchaer, Maxwell A.
AU - Nielsen, Eric L.
AU - Norton, Andrew
AU - Oppenheimer, Rebecca
AU - Palmer, David
AU - Patience, Jennifer
AU - Perrin, Marshall D.
AU - Poyneer, Lisa
AU - Rantakyrö, Fredrik T.
AU - Savransky, Dmitry
AU - Schneider, Adam C.
AU - Sivaramakrishnan, Anand
AU - Song, Inseok
AU - Soummer, Rémi
AU - Thomas, Sandrine
AU - Wallace, J. Kent
AU - Ward-Duong, Kimberly
AU - Wiktorowicz, Sloane
AU - Wolff, Schuyler
N1 - Funding Information:
A.Z.G. and A.S. acknowledge support from NASA grant APRA08-0117 and the STScI Directors Discretionary Research Fund. The research was supported by NSF grant AST-1411868 and NASA grant NNX14AJ80G (J-BR). P.K., J.R.G., R.J.D., and J.W. thank support from NSF AST-1518332, NASA NNX15AC89G and NNX15AD95G/NEXSS.
Funding Information:
We thank the anonymous referee for helpful comments. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CON-ICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). This research has made use of the SVO Filter Profile Service (http://svo2.cab.inta-csic.es/theory/fps/), supported by the Spanish MINECO through grant AyA2014-55216. This research has benefited from the SpeX Prism Library maintained by Adam Burgasser athttp://www.browndwarfs.org/ spexprism. This research has made use of NASA’s Astrophysics Data System and the AstroBetter blog and wiki. Work from A.Z.G. was supported in part by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE1232825. A.Z.G. and A.S. acknowledge support from NASA grant APRA08-0117 and the STScI Directors Discretionary Research Fund. The research was supported by NSF grant AST-1411868 and NASA grant NNX14AJ80G (J-BR). P.K., J.R.G., R.J.D., and J.W. thank support from NSF AST-1518332, NASA NNX15AC89G and NNX15AD95G/NEXSS. This work benefited from NASAʼs Nexus for Exoplanet System Science (NExSS) research coordination network, sponsored by NASA’s Science Mission Directorate. A.B. would like to acknowledge support for this research under their NASA WFIRST-SIT award #NNG16PJ24C, NASA Grant NNX15AE19G, and NASA JPL subcontracts no. 1538907, 1529729, 1513640, & 1534432–B–4.25. Facility: Gemini-S.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved..
PY - 2018/6
Y1 - 2018/6
N2 - 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.
AB - 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.
KW - planets and satellites: gaseous planets
KW - stars: individual (HR 8799)
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U2 - 10.3847/1538-3881/aabcb8
DO - 10.3847/1538-3881/aabcb8
M3 - Article
AN - SCOPUS:85048144212
SN - 0004-6256
VL - 155
JO - Astronomical Journal
JF - Astronomical Journal
IS - 6
M1 - 226
ER -