| DOI | Resolve DOI: https://doi.org/10.1126/science.aac5891 |
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| Author | Search for: Macintosh, B.; Search for: Graham, J. R.; Search for: Barman, T.; Search for: De Rosa, R. J.; Search for: Konopacky, Q.; Search for: Marley, M. S.; Search for: Marois, C.1; Search for: Nielsen, E. L.; Search for: Pueyo, L.; Search for: Rajan, A.; Search for: Rameau, J.; Search for: Saumon, D.; Search for: Wang, J. J.; Search for: Patience, J.; Search for: Ammons, M.; Search for: Arriaga, P.; Search for: Artigau, E.; Search for: Beckwith, S.; Search for: Brewster, J.; Search for: Bruzzone, S.; Search for: Bulger, J.; Search for: Burningham, B.; Search for: Burrows, A. S.; Search for: Chen, C.; Search for: Chiang, E.; Search for: Chilcote, J. K.; Search for: Dawson, R. I.; Search for: Dong, R.; Search for: Doyon, R.; Search for: Draper, Z. H.1; Search for: Duchêne, G.; Search for: Esposito, T. M.; Search for: Fabrycky, D.; Search for: Fitzgerald, M. P.; Search for: Follette, K. B.; Search for: Fortney, J. J.; Search for: Gerard, B.1; Search for: Goodsell, S.; Search for: Greenbaum, A. Z.; Search for: Hibon, P.; Search for: Hinkley, S.; Search for: Cotton, T. H.; Search for: Hung, L.-W.; Search for: Ingraham, P.; Search for: Johnson-Groh, M.1; Search for: Kalas, P.; Search for: Lafreniere, D.; Search for: Larkin, J. E.; Search for: Lee, J.; Search for: Line, M.; Search for: Long, D.; Search for: Maire, J.; Search for: Marchis, F.; Search for: Matthews, B. C.1; Search for: Max, C. E.; Search for: Metchev, S.; Search for: Millar-Blanchaer, M. A.; Search for: Mittal, T.; Search for: Morley, C. V.; Search for: Morzinski, K. M.; Search for: Murray-Clay, R.; Search for: Oppenheimer, R.; Search for: Palmer, D. W.; Search for: Patel, R.; Search for: Perrin, M. D.; Search for: Poyneer, L. A.; Search for: Rafikov, R. R.; Search for: Rantakyrö, F. T.; Search for: Rice, E. L.; Search for: Rojo, P.; Search for: Rudy, A. R.; Search for: Ruffio, J.-B.; Search for: Ruiz, M. T.; Search for: Sadakuni, N.; Search for: Saddlemyer, L.1; Search for: Salama, M.; Search for: Savransky, D.; Search for: Schneider, A. C.; Search for: Sivaramakrishnan, A.; Search for: Song, I.; Search for: Soummer, R.; Search for: Thomas, S.; Search for: Vasisht, G.; Search for: Wallace, J. K.; Search for: Ward-Duong, K.; Search for: Wiktorowicz, S. J.; Search for: Wolff, S. G.; Search for: Zuckerman, B. |
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| Affiliation | - National Research Council of Canada. National Science Infrastructure
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| Format | Text, Article |
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| Subject | methane; absorption; astronomy; imaging method; Jupiter; methane; planet; planetary evolution; spectroscopy; air temperature; contrast; Gemini Planet Imager; luminance; molecular weight; near infrared spectroscopy; photometry; sun; telescope; water vapor |
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| 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. |
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| Publication date | 2015-10-02 |
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| In | |
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| Language | English |
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| Peer reviewed | Yes |
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| NPARC number | 21277402 |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | 5f6d98db-3f3d-4c56-b8d7-f824fdcb790f |
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| Record created | 2016-03-09 |
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| Record modified | 2020-04-22 |
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