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1. Automated data processing architecture for the gemini planet imager exoplanet survey

Author

Wang, JJ, Wang, JJ, Perrin, MD, Savransky, D, Arriaga, P, Chilcote, JK, De Rosa, RJ, Millar-Blanchaer, MA, Marois, C, Rameau, J, Wolff, SG, Shapiro, J, Ruffio, JB, Maire, J, Marchis, F, Graham, JR, Macintosh, B, Mark Ammons, S, Bailey, VP, Barman, TS, Bruzzone, S, Bulger, J, Cotton, T, Doyon, R, Duchêne, G, Fitzgerald, MP, Follette, KB, Goodsell, S, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, QM, Larkin, JE, Marley, MS, Metchev, S, Nielsen, EL, Oppenheimer, R, Palmer, DW, Patience, J, Poyneer, LA, Pueyo, L, Rajan, A, Rantakyrö, FT, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Kent Wallace, J, Ward-Duong, K, Wiktorowicz, SJ, Wang, JJ, Wang, JJ, Perrin, MD, Savransky, D, Arriaga, P, Chilcote, JK, De Rosa, RJ, Millar-Blanchaer, MA, Marois, C, Rameau, J, Wolff, SG, Shapiro, J, Ruffio, JB, Maire, J, Marchis, F, Graham, JR, Macintosh, B, Mark Ammons, S, Bailey, VP, Barman, TS, Bruzzone, S, Bulger, J, Cotton, T, Doyon, R, Duchêne, G, Fitzgerald, MP, Follette, KB, Goodsell, S, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, QM, Larkin, JE, Marley, MS, Metchev, S, Nielsen, EL, Oppenheimer, R, Palmer, DW, Patience, J, Poyneer, LA, Pueyo, L, Rajan, A, Rantakyrö, FT, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Kent Wallace, J, Ward-Duong, K, and Wiktorowicz, SJ

Abstract

The Gemini Planet Imager Exoplanet Survey (GPIES) is a multiyear direct imaging survey of 600 stars to discover and characterize young Jovian exoplanets and their environments. We have developed an automated data architecture to process and index all data related to the survey uniformly. An automated and flexible data processing framework, which we term the Data Cruncher, combines multiple data reduction pipelines (DRPs) together to process all spectroscopic, polarimetric, and calibration data taken with GPIES. With no human intervention, fully reduced and calibrated data products are available less than an hour after the data are taken to expedite follow up on potential objects of interest. The Data Cruncher can run on a supercomputer to reprocess all GPIES data in a single day as improvements are made to our DRPs. A backend MySQL database indexes all files, which are synced to the cloud, and a front-end web server allows for easy browsing of all files associated with GPIES. To help observers, quicklook displays show reduced data as they are processed in real time, and chatbots on Slack post observing information as well as reduced data products. Together, the GPIES automated data processing architecture reduces our workload, provides real-Time data reduction, optimizes our observing strategy, and maintains a homogeneously reduced dataset to study planet occurrence and instrument performance.

Published
2018

2. Automated data processing architecture for the gemini planet imager exoplanet survey

Author

Wang, JJ, Wang, JJ, Perrin, MD, Savransky, D, Arriaga, P, Chilcote, JK, De Rosa, RJ, Millar-Blanchaer, MA, Marois, C, Rameau, J, Wolff, SG, Shapiro, J, Ruffio, JB, Maire, J, Marchis, F, Graham, JR, Macintosh, B, Mark Ammons, S, Bailey, VP, Barman, TS, Bruzzone, S, Bulger, J, Cotton, T, Doyon, R, Duchêne, G, Fitzgerald, MP, Follette, KB, Goodsell, S, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, QM, Larkin, JE, Marley, MS, Metchev, S, Nielsen, EL, Oppenheimer, R, Palmer, DW, Patience, J, Poyneer, LA, Pueyo, L, Rajan, A, Rantakyrö, FT, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Kent Wallace, J, Ward-Duong, K, Wiktorowicz, SJ, Wang, JJ, Wang, JJ, Perrin, MD, Savransky, D, Arriaga, P, Chilcote, JK, De Rosa, RJ, Millar-Blanchaer, MA, Marois, C, Rameau, J, Wolff, SG, Shapiro, J, Ruffio, JB, Maire, J, Marchis, F, Graham, JR, Macintosh, B, Mark Ammons, S, Bailey, VP, Barman, TS, Bruzzone, S, Bulger, J, Cotton, T, Doyon, R, Duchêne, G, Fitzgerald, MP, Follette, KB, Goodsell, S, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, QM, Larkin, JE, Marley, MS, Metchev, S, Nielsen, EL, Oppenheimer, R, Palmer, DW, Patience, J, Poyneer, LA, Pueyo, L, Rajan, A, Rantakyrö, FT, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Kent Wallace, J, Ward-Duong, K, and Wiktorowicz, SJ

Abstract

The Gemini Planet Imager Exoplanet Survey (GPIES) is a multiyear direct imaging survey of 600 stars to discover and characterize young Jovian exoplanets and their environments. We have developed an automated data architecture to process and index all data related to the survey uniformly. An automated and flexible data processing framework, which we term the Data Cruncher, combines multiple data reduction pipelines (DRPs) together to process all spectroscopic, polarimetric, and calibration data taken with GPIES. With no human intervention, fully reduced and calibrated data products are available less than an hour after the data are taken to expedite follow up on potential objects of interest. The Data Cruncher can run on a supercomputer to reprocess all GPIES data in a single day as improvements are made to our DRPs. A backend MySQL database indexes all files, which are synced to the cloud, and a front-end web server allows for easy browsing of all files associated with GPIES. To help observers, quicklook displays show reduced data as they are processed in real time, and chatbots on Slack post observing information as well as reduced data products. Together, the GPIES automated data processing architecture reduces our workload, provides real-Time data reduction, optimizes our observing strategy, and maintains a homogeneously reduced dataset to study planet occurrence and instrument performance.

Published
2018

3. DISCOVERY of A SUBSTELLAR COMPANION to the NEARBY DEBRIS DISK HOST HR 2562

Author

Konopacky, QM, Konopacky, QM, Rameau, J, Duchêne, G, Filippazzo, JC, Godfrey, PAG, Marois, C, Nielsen, EL, Pueyo, L, Rafikov, RR, Rice, EL, Wang, JJ, Ammons, SM, Bailey, VP, Barman, TS, Bulger, J, Bruzzone, S, Chilcote, JK, Cotten, T, Dawson, RI, Rosa, RJD, Doyon, R, Esposito, TM, Fitzgerald, MP, Follette, KB, Goodsell, S, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Lafrenière, D, Larkin, JE, Macintosh, BA, Maire, J, Marchis, F, Marley, MS, Matthews, BC, Metchev, S, Millar-Blanchaer, MA, Oppenheimer, R, Palmer, DW, Patience, J, Perrin, MD, Poyneer, LA, Rajan, A, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, Wolff, SG, Konopacky, QM, Konopacky, QM, Rameau, J, Duchêne, G, Filippazzo, JC, Godfrey, PAG, Marois, C, Nielsen, EL, Pueyo, L, Rafikov, RR, Rice, EL, Wang, JJ, Ammons, SM, Bailey, VP, Barman, TS, Bulger, J, Bruzzone, S, Chilcote, JK, Cotten, T, Dawson, RI, Rosa, RJD, Doyon, R, Esposito, TM, Fitzgerald, MP, Follette, KB, Goodsell, S, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Lafrenière, D, Larkin, JE, Macintosh, BA, Maire, J, Marchis, F, Marley, MS, Matthews, BC, Metchev, S, Millar-Blanchaer, MA, Oppenheimer, R, Palmer, DW, Patience, J, Perrin, MD, Poyneer, LA, Rajan, A, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, and Wolff, SG

Abstract

We present the discovery of a brown dwarf companion to the debris disk host star HR 2562. This object, discovered with the Gemini Planet Imager (GPI), has a projected separation of 20.3 ± 0.3 au (0.″618 ± 0. ″004) from the star. With the high astrometric precision afforded by GPI, we have confirmed, to more than 5?, the common proper motion of HR 2562B with the star, with only a month-long time baseline between observations. Spectral data in the J-, H-, and K-bands show a morphological similarity to L/T transition objects. We assign a spectral type of L7 ± 3 to HR 2562Band derive a luminosity of log(Lbol/L⊙) = -4.62 ± 0.12, corresponding to a mass of 30 ± 15 MJup from evolutionary models at an estimated age of the system of 300-900 Myr. Although the uncertainty in the age of the host star is significant, the spectra and photometry exhibit several indications of youth for HR 2562B. The source has a position angle that is consistent with an orbit in the same plane as the debris disk recently resolved with Herschel. Additionally, it appears to be interior to the debris disk. Though the extent of the inner hole is currently too uncertain to place limits on the mass of HR 2562B, future observations of the disk with higher spatial resolution may be able to provide mass constraints. This is the first brown-dwarf-mass object found to reside in the inner hole of a debris disk, offering the opportunity to search for evidence of formation above the deuterium burning limit in a circumstellar disk.

Published
2016

4. DISCOVERY of A SUBSTELLAR COMPANION to the NEARBY DEBRIS DISK HOST HR 2562

Author

Konopacky, QM, Konopacky, QM, Rameau, J, Duchêne, G, Filippazzo, JC, Godfrey, PAG, Marois, C, Nielsen, EL, Pueyo, L, Rafikov, RR, Rice, EL, Wang, JJ, Ammons, SM, Bailey, VP, Barman, TS, Bulger, J, Bruzzone, S, Chilcote, JK, Cotten, T, Dawson, RI, Rosa, RJD, Doyon, R, Esposito, TM, Fitzgerald, MP, Follette, KB, Goodsell, S, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Lafrenière, D, Larkin, JE, Macintosh, BA, Maire, J, Marchis, F, Marley, MS, Matthews, BC, Metchev, S, Millar-Blanchaer, MA, Oppenheimer, R, Palmer, DW, Patience, J, Perrin, MD, Poyneer, LA, Rajan, A, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, Wolff, SG, Konopacky, QM, Konopacky, QM, Rameau, J, Duchêne, G, Filippazzo, JC, Godfrey, PAG, Marois, C, Nielsen, EL, Pueyo, L, Rafikov, RR, Rice, EL, Wang, JJ, Ammons, SM, Bailey, VP, Barman, TS, Bulger, J, Bruzzone, S, Chilcote, JK, Cotten, T, Dawson, RI, Rosa, RJD, Doyon, R, Esposito, TM, Fitzgerald, MP, Follette, KB, Goodsell, S, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Lafrenière, D, Larkin, JE, Macintosh, BA, Maire, J, Marchis, F, Marley, MS, Matthews, BC, Metchev, S, Millar-Blanchaer, MA, Oppenheimer, R, Palmer, DW, Patience, J, Perrin, MD, Poyneer, LA, Rajan, A, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, and Wolff, SG

Abstract

We present the discovery of a brown dwarf companion to the debris disk host star HR 2562. This object, discovered with the Gemini Planet Imager (GPI), has a projected separation of 20.3 ± 0.3 au (0.″618 ± 0. ″004) from the star. With the high astrometric precision afforded by GPI, we have confirmed, to more than 5?, the common proper motion of HR 2562B with the star, with only a month-long time baseline between observations. Spectral data in the J-, H-, and K-bands show a morphological similarity to L/T transition objects. We assign a spectral type of L7 ± 3 to HR 2562Band derive a luminosity of log(Lbol/L⊙) = -4.62 ± 0.12, corresponding to a mass of 30 ± 15 MJup from evolutionary models at an estimated age of the system of 300-900 Myr. Although the uncertainty in the age of the host star is significant, the spectra and photometry exhibit several indications of youth for HR 2562B. The source has a position angle that is consistent with an orbit in the same plane as the debris disk recently resolved with Herschel. Additionally, it appears to be interior to the debris disk. Though the extent of the inner hole is currently too uncertain to place limits on the mass of HR 2562B, future observations of the disk with higher spatial resolution may be able to provide mass constraints. This is the first brown-dwarf-mass object found to reside in the inner hole of a debris disk, offering the opportunity to search for evidence of formation above the deuterium burning limit in a circumstellar disk.

Published
2016

5. Polarimetry with the gemini planet imager: Methods, performance at first light, and the circumstellar ring around HR 4796A

Author

Perrin, MD, Perrin, MD, Duchene, G, Millar-Blanchaer, M, Fitzgerald, MP, Graham, JR, Wiktorowicz, SJ, Kalas, PG, Macintosh, B, Bauman, B, Cardwell, A, Chilcote, J, De Rosa, RJ, Dillon, D, Doyon, R, Dunn, J, Erikson, D, Gavel, D, Goodsell, S, Hartung, M, Hibon, P, Ingraham, P, Kerley, D, Konapacky, Q, Larkin, JE, Maire, J, Marchis, F, Marois, C, Mittal, T, Morzinski, KM, Oppenheimer, BR, Palmer, DW, Patience, J, Poyneer, L, Pueyo, L, Rantakyrö, FT, Sadakuni, N, Saddlemyer, L, Savransky, D, Soummer, R, Sivaramakrishnan, A, Song, I, Thomas, S, Wallace, JK, Wang, JJ, Wolff, SG, Perrin, MD, Perrin, MD, Duchene, G, Millar-Blanchaer, M, Fitzgerald, MP, Graham, JR, Wiktorowicz, SJ, Kalas, PG, Macintosh, B, Bauman, B, Cardwell, A, Chilcote, J, De Rosa, RJ, Dillon, D, Doyon, R, Dunn, J, Erikson, D, Gavel, D, Goodsell, S, Hartung, M, Hibon, P, Ingraham, P, Kerley, D, Konapacky, Q, Larkin, JE, Maire, J, Marchis, F, Marois, C, Mittal, T, Morzinski, KM, Oppenheimer, BR, Palmer, DW, Patience, J, Poyneer, L, Pueyo, L, Rantakyrö, FT, Sadakuni, N, Saddlemyer, L, Savransky, D, Soummer, R, Sivaramakrishnan, A, Song, I, Thomas, S, Wallace, JK, Wang, JJ, and Wolff, SG

Abstract

We present the first results from the polarimetry mode of the Gemini Planet Imager (GPI), which uses anew integral field polarimetry architecture to provide high contrast linear polarimetry with minimal systematic biases between the orthogonal polarizations. We describe the design, data reduction methods, and performance of polarimetry with GPI. Point-spread function (PSF) subtraction via differential polarimetry suppresses unpolarized starlight by a factor of over 100, and provides sensitivity to circumstellar dust reaching the photon noise limit for these observations. in the case of the circumstellar disk around HR 4796A,GPI's advanced adaptive optics system reveals the disk clearly even prior to PSF subtraction. In polarized light, the disk is seen all the way in to its semi-minor axis for the first time. The disk exhibits surprisingly strong asymmetry in polarized intensity, with the west side ≳9 times brighter than the east side despite the fact that the east side is slightly brighter in total intensity. Based on a synthesis of the total and polarized intensities, we now believe that the west side is closer to us, contrary to most prior interpretations. Forward scattering by relatively large silicate dust particles leads to the strong polarized intensity on thewest side, and the ring must be slightly optically thick in order to explain the lower brightness in total intensity there. These findings suggest that the ring is geometrically narrow and dynamically cold, perhaps shepherded by larger bodies in the same manner as Saturn's Fring.

Published
2015

6. Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager.

Author

Macintosh, B, Macintosh, B, Graham, JR, Barman, T, De Rosa, RJ, Konopacky, Q, Marley, MS, Marois, C, Nielsen, EL, Pueyo, L, Rajan, A, Rameau, J, Saumon, D, Wang, JJ, Patience, J, Ammons, M, Arriaga, P, Artigau, E, Beckwith, S, Brewster, J, Bruzzone, S, Bulger, J, Burningham, B, Burrows, AS, Chen, C, Chiang, E, Chilcote, JK, Dawson, RI, Dong, R, Doyon, R, Draper, ZH, Duchêne, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, B, Goodsell, S, Greenbaum, AZ, Hibon, P, Hinkley, S, Cotten, TH, Hung, L-W, Ingraham, P, Johnson-Groh, M, Kalas, P, Lafreniere, D, Larkin, JE, Lee, J, Line, M, Long, D, Maire, J, Marchis, F, Matthews, BC, Max, CE, Metchev, S, Millar-Blanchaer, MA, Mittal, T, Morley, CV, Morzinski, KM, Murray-Clay, R, Oppenheimer, R, Palmer, DW, Patel, R, Perrin, MD, Poyneer, LA, Rafikov, RR, Rantakyrö, FT, Rice, EL, Rojo, P, Rudy, AR, Ruffio, J-B, Ruiz, MT, Sadakuni, N, Saddlemyer, L, Salama, M, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vasisht, G, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, Wolff, SG, Zuckerman, B, Macintosh, B, Macintosh, B, Graham, JR, Barman, T, De Rosa, RJ, Konopacky, Q, Marley, MS, Marois, C, Nielsen, EL, Pueyo, L, Rajan, A, Rameau, J, Saumon, D, Wang, JJ, Patience, J, Ammons, M, Arriaga, P, Artigau, E, Beckwith, S, Brewster, J, Bruzzone, S, Bulger, J, Burningham, B, Burrows, AS, Chen, C, Chiang, E, Chilcote, JK, Dawson, RI, Dong, R, Doyon, R, Draper, ZH, Duchêne, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, B, Goodsell, S, Greenbaum, AZ, Hibon, P, Hinkley, S, Cotten, TH, Hung, L-W, Ingraham, P, Johnson-Groh, M, Kalas, P, Lafreniere, D, Larkin, JE, Lee, J, Line, M, Long, D, Maire, J, Marchis, F, Matthews, BC, Max, CE, Metchev, S, Millar-Blanchaer, MA, Mittal, T, Morley, CV, Morzinski, KM, Murray-Clay, R, Oppenheimer, R, Palmer, DW, Patel, R, Perrin, MD, Poyneer, LA, Rafikov, RR, Rantakyrö, FT, Rice, EL, Rojo, P, Rudy, AR, Ruffio, J-B, Ruiz, MT, Sadakuni, N, Saddlemyer, L, Salama, M, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vasisht, G, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, Wolff, SG, and Zuckerman, B

Abstract

Directly detecting thermal emission from young extrasolar planets allows measurement of their atmospheric compositions and luminosities, which are influenced by their formation mechanisms. Using the Gemini Planet Imager, we discovered a planet orbiting the ~20-million-year-old star 51 Eridani at a projected separation of 13 astronomical units. Near-infrared observations show a spectrum with strong methane and water-vapor absorption. Modeling of the spectra and photometry yields a luminosity (normalized by the luminosity of the Sun) of 1.6 to 4.0 × 10(-6) and an effective temperature of 600 to 750 kelvin. For this age and luminosity, "hot-start" formation models indicate a mass twice that of Jupiter. This planet also has a sufficiently low luminosity to be consistent with the "cold-start" core-accretion process that may have formed Jupiter.

Published
2015

7. Polarimetry with the gemini planet imager: Methods, performance at first light, and the circumstellar ring around HR 4796A

Author

Perrin, MD, Perrin, MD, Duchene, G, Millar-Blanchaer, M, Fitzgerald, MP, Graham, JR, Wiktorowicz, SJ, Kalas, PG, Macintosh, B, Bauman, B, Cardwell, A, Chilcote, J, De Rosa, RJ, Dillon, D, Doyon, R, Dunn, J, Erikson, D, Gavel, D, Goodsell, S, Hartung, M, Hibon, P, Ingraham, P, Kerley, D, Konapacky, Q, Larkin, JE, Maire, J, Marchis, F, Marois, C, Mittal, T, Morzinski, KM, Oppenheimer, BR, Palmer, DW, Patience, J, Poyneer, L, Pueyo, L, Rantakyrö, FT, Sadakuni, N, Saddlemyer, L, Savransky, D, Soummer, R, Sivaramakrishnan, A, Song, I, Thomas, S, Wallace, JK, Wang, JJ, Wolff, SG, Perrin, MD, Perrin, MD, Duchene, G, Millar-Blanchaer, M, Fitzgerald, MP, Graham, JR, Wiktorowicz, SJ, Kalas, PG, Macintosh, B, Bauman, B, Cardwell, A, Chilcote, J, De Rosa, RJ, Dillon, D, Doyon, R, Dunn, J, Erikson, D, Gavel, D, Goodsell, S, Hartung, M, Hibon, P, Ingraham, P, Kerley, D, Konapacky, Q, Larkin, JE, Maire, J, Marchis, F, Marois, C, Mittal, T, Morzinski, KM, Oppenheimer, BR, Palmer, DW, Patience, J, Poyneer, L, Pueyo, L, Rantakyrö, FT, Sadakuni, N, Saddlemyer, L, Savransky, D, Soummer, R, Sivaramakrishnan, A, Song, I, Thomas, S, Wallace, JK, Wang, JJ, and Wolff, SG

Abstract

We present the first results from the polarimetry mode of the Gemini Planet Imager (GPI), which uses anew integral field polarimetry architecture to provide high contrast linear polarimetry with minimal systematic biases between the orthogonal polarizations. We describe the design, data reduction methods, and performance of polarimetry with GPI. Point-spread function (PSF) subtraction via differential polarimetry suppresses unpolarized starlight by a factor of over 100, and provides sensitivity to circumstellar dust reaching the photon noise limit for these observations. in the case of the circumstellar disk around HR 4796A,GPI's advanced adaptive optics system reveals the disk clearly even prior to PSF subtraction. In polarized light, the disk is seen all the way in to its semi-minor axis for the first time. The disk exhibits surprisingly strong asymmetry in polarized intensity, with the west side ≳9 times brighter than the east side despite the fact that the east side is slightly brighter in total intensity. Based on a synthesis of the total and polarized intensities, we now believe that the west side is closer to us, contrary to most prior interpretations. Forward scattering by relatively large silicate dust particles leads to the strong polarized intensity on thewest side, and the ring must be slightly optically thick in order to explain the lower brightness in total intensity there. These findings suggest that the ring is geometrically narrow and dynamically cold, perhaps shepherded by larger bodies in the same manner as Saturn's Fring.

Published
2015

8. Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager.

Author

Macintosh, B, Macintosh, B, Graham, JR, Barman, T, De Rosa, RJ, Konopacky, Q, Marley, MS, Marois, C, Nielsen, EL, Pueyo, L, Rajan, A, Rameau, J, Saumon, D, Wang, JJ, Patience, J, Ammons, M, Arriaga, P, Artigau, E, Beckwith, S, Brewster, J, Bruzzone, S, Bulger, J, Burningham, B, Burrows, AS, Chen, C, Chiang, E, Chilcote, JK, Dawson, RI, Dong, R, Doyon, R, Draper, ZH, Duchêne, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, B, Goodsell, S, Greenbaum, AZ, Hibon, P, Hinkley, S, Cotten, TH, Hung, L-W, Ingraham, P, Johnson-Groh, M, Kalas, P, Lafreniere, D, Larkin, JE, Lee, J, Line, M, Long, D, Maire, J, Marchis, F, Matthews, BC, Max, CE, Metchev, S, Millar-Blanchaer, MA, Mittal, T, Morley, CV, Morzinski, KM, Murray-Clay, R, Oppenheimer, R, Palmer, DW, Patel, R, Perrin, MD, Poyneer, LA, Rafikov, RR, Rantakyrö, FT, Rice, EL, Rojo, P, Rudy, AR, Ruffio, J-B, Ruiz, MT, Sadakuni, N, Saddlemyer, L, Salama, M, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vasisht, G, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, Wolff, SG, Zuckerman, B, Macintosh, B, Macintosh, B, Graham, JR, Barman, T, De Rosa, RJ, Konopacky, Q, Marley, MS, Marois, C, Nielsen, EL, Pueyo, L, Rajan, A, Rameau, J, Saumon, D, Wang, JJ, Patience, J, Ammons, M, Arriaga, P, Artigau, E, Beckwith, S, Brewster, J, Bruzzone, S, Bulger, J, Burningham, B, Burrows, AS, Chen, C, Chiang, E, Chilcote, JK, Dawson, RI, Dong, R, Doyon, R, Draper, ZH, Duchêne, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, B, Goodsell, S, Greenbaum, AZ, Hibon, P, Hinkley, S, Cotten, TH, Hung, L-W, Ingraham, P, Johnson-Groh, M, Kalas, P, Lafreniere, D, Larkin, JE, Lee, J, Line, M, Long, D, Maire, J, Marchis, F, Matthews, BC, Max, CE, Metchev, S, Millar-Blanchaer, MA, Mittal, T, Morley, CV, Morzinski, KM, Murray-Clay, R, Oppenheimer, R, Palmer, DW, Patel, R, Perrin, MD, Poyneer, LA, Rafikov, RR, Rantakyrö, FT, Rice, EL, Rojo, P, Rudy, AR, Ruffio, J-B, Ruiz, MT, Sadakuni, N, Saddlemyer, L, Salama, M, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vasisht, G, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, Wolff, SG, and Zuckerman, B

Abstract

Directly detecting thermal emission from young extrasolar planets allows measurement of their atmospheric compositions and luminosities, which are influenced by their formation mechanisms. Using the Gemini Planet Imager, we discovered a planet orbiting the ~20-million-year-old star 51 Eridani at a projected separation of 13 astronomical units. Near-infrared observations show a spectrum with strong methane and water-vapor absorption. Modeling of the spectra and photometry yields a luminosity (normalized by the luminosity of the Sun) of 1.6 to 4.0 × 10(-6) and an effective temperature of 600 to 750 kelvin. For this age and luminosity, "hot-start" formation models indicate a mass twice that of Jupiter. This planet also has a sufficiently low luminosity to be consistent with the "cold-start" core-accretion process that may have formed Jupiter.

Published
2015

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