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 Cotten; Rene 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

doi:10.3847/1538-3881/aabcb8

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

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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 language	English (US)
Article number	226
Journal	Astronomical Journal
Volume	155
Issue number	6
DOIs	https://doi.org/10.3847/1538-3881/aabcb8
State	Published - 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)

Access to Document

10.3847/1538-3881/aabcb8

Cite this

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

@article{54fc930db1e8467b9db7cf29395d93eb,

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

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.",

keywords = "planets and satellites: gaseous planets, stars: individual (HR 8799)",

author = "Greenbaum, {Alexandra Z.} and Laurent Pueyo and Ruffio, {Jean Baptiste} and Wang, {Jason J.} and Rosa, {Robert J.De} and Jonathan Aguilar and Julien Rameau and Travis Barman and Christian Marois and Marley, {Mark S.} and Quinn Konopacky and Abhijith Rajan and Bruce Macintosh and Megan Ansdell and Pauline Arriaga and Bailey, {Vanessa P.} and Joanna Bulger and Burrows, {Adam S.} and Jeffrey Chilcote and Tara Cotten and Rene Doyon and Gaspard Duch{\^e}ne and Fitzgerald, {Michael P.} and Follette, {Katherine B.} and Benjamin Gerard and Goodsell, {Stephen J.} and Graham, {James R.} and Pascale Hibon and Hung, {Li Wei} and Patrick Ingraham and Paul Kalas and Larkin, {James E.} and J{\'e}r{\^o}me Maire and Franck Marchis and Stanimir Metchev and Millar-Blanchaer, {Maxwell A.} and Nielsen, {Eric L.} and Andrew Norton and Rebecca Oppenheimer and David Palmer and Jennifer Patience and Perrin, {Marshall D.} and Lisa Poyneer and Rantakyr{\"o}, {Fredrik T.} and Dmitry Savransky and Schneider, {Adam C.} and Anand Sivaramakrishnan and Inseok Song and R{\'e}mi Soummer and Sandrine Thomas and Wallace, {J. Kent} and Kimberly Ward-Duong and Sloane Wiktorowicz and Schuyler Wolff",

note = "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, Tecnolog{\'i}a e Innovaci{\'o}n Productiva (Argentina), and Minist{\'e}rio da Ci{\^e}ncia, Tecnologia e Inova{\c c}{\~a}o (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 athttp://www.browndwarfs.org/ spexprism. This research has made use of NASA{\textquoteright}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{\textquoteright}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: {\textcopyright} 2018. The American Astronomical Society. All rights reserved..",

year = "2018",

month = jun,

doi = "10.3847/1538-3881/aabcb8",

language = "English (US)",

volume = "155",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

number = "6",

}

Greenbaum, AZ, Pueyo, L, Ruffio, JB, Wang, JJ, Rosa, RJD, Aguilar, J, Rameau, J, Barman, T, Marois, C, Marley, MS, Konopacky, Q, Rajan, A, Macintosh, B, Ansdell, M, Arriaga, P, Bailey, VP, Bulger, J, Burrows, AS, Chilcote, J, Cotten, T, Doyon, R, Duchêne, G, Fitzgerald, MP, Follette, KB, Gerard, B, Goodsell, SJ, Graham, JR, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Larkin, JE, Maire, J, Marchis, F, Metchev, S, Millar-Blanchaer, MA, Nielsen, EL, Norton, A, Oppenheimer, R, Palmer, D, Patience, J, Perrin, MD, Poyneer, L, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S & 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, vol. 155, no. 6, 226. https://doi.org/10.3847/1538-3881/aabcb8

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 athttp://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)

UR - http://www.scopus.com/inward/record.url?scp=85048144212&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85048144212&partnerID=8YFLogxK

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 -

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

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