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

Author

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, Cotton, TH, Hung, LW, 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, JB, Ruiz, MT, Sadakuni, N, Saddlemyer, L, Salama, M, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, and Vasisht, G

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
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 × 10-6and 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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2. The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au

Author

Nielsen, EL, De Rosa, RJ, Macintosh, B, Wang, JJ, Ruffio, JB, Chiang, E, Marley, MS, Saumon, D, Savransky, D, Mark Ammons, S, Bailey, VP, Barman, T, Blain, C, Bulger, J, Burrows, A, Chilcote, J, Cotten, T, Czekala, I, Doyon, R, Duchene, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, BL, Goodsell, SJ, Graham, Greenbaum, AZ, Hibon, P, Hinkley, S, Hirsch, LA, Hom, J, Hung, LW, Ilene Dawson, R, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Lee, EJ, Lin, JW, Maire, J, Marchis, F, Marois, C, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Pueyo, L, Rafikov, RR, Rajan, A, Rameau, J, Rantakyrö, FT, Ren, B, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Tallis, M, Thomas, S, Ward-Duong, K, and Wolff, S

Subjects
planets and satellites: detection, 13. Climate action, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, instrumentation: adaptive optics, planetary systems, Astrophysics::Galaxy Astrophysics
Abstract

We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey (GPIES). This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semi-major axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M $>$ 1.5 $M_\odot$ more likely to host planets with masses between 2-13 M$_{\rm Jup}$ and semi-major axes of 3-100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semi-major axis (a) for planet populations around high-mass stars (M $>$ 1.5M$_\odot$) of the form $\frac{d^2 N}{dm da} \propto m^\alpha a^\beta$, finding $\alpha$ = -2.4 $\pm$ 0.8 and $\beta$ = -2.0 $\pm$ 0.5, and an integrated occurrence rate of $9^{+5}_{-4}$% between 5-13 M$_{\rm Jup}$ and 10-100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with 0.8$^{+0.8}_{-0.5}$% of stars hosting a brown dwarf companion between 13-80 M$_{\rm Jup}$ and 10-100 au. Brown dwarfs also appear to be distributed differently in mass and semi-major axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semi-major axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the RV method, our results are consistent with a peak in occurrence of giant planets between ~1-10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability.

3. The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics From 10-100 AU

Author

Eric L. Nielsen, Robert J. De Rosa, Bruce Macintosh, Jason J. Wang, Jean-Baptiste Ruffio, Eugene Chiang, Mark S. Marley, Didier Saumon, Dmitry Savransky, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Célia Blain, Joanna Bulger, Adam Burrows, Jeffrey Chilcote, Tara Cotten, Ian Czekala, Rene Doyon, Gaspard Duchêne, Thomas M. Esposito, Daniel Fabrycky, Michael P. Fitzgerald, Katherine B. Follette, Jonathan J. Fortney, Benjamin L. Gerard, Stephen J. Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Sasha Hinkley, Lea A. Hirsch, Justin Hom, Li-Wei Hung, Rebekah Ilene Dawson, Patrick Ingraham, Paul Kalas, Quinn Konopacky, James E. Larkin, Eve J. Lee, Jonathan W. Lin, Jérôme Maire, Franck Marchis, Christian Marois, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Katie M. Morzinski, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Laurent Pueyo, Roman R. Rafikov, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Melisa Tallis, Sandrine Thomas, Kimberly Ward-Duong, Schuyler Wolff, Nielsen, EL [0000-0001-6975-9056], De Rosa, RJ [0000-0002-4918-0247], Macintosh, B [0000-0003-1212-7538], Wang, JJ [0000-0003-0774-6502], Ruffio, JB [0000-0003-2233-4821], Chiang, E [0000-0002-6246-2310], Marley, MS [0000-0002-5251-2943], Saumon, D [0000-0001-6800-3505], Savransky, D [0000-0002-8711-7206], Mark Ammons, S [0000-0001-5172-7902], Bailey, VP [0000-0002-5407-2806], Barman, T [0000-0002-7129-3002], Bulger, J [0000-0003-4641-2003], Burrows, A [0000-0002-3099-5024], Chilcote, J [0000-0001-6305-7272], Cotten, T [0000-0003-0156-3019], Czekala, I [0000-0002-1483-8811], Esposito, TM [0000-0002-0792-3719], Fabrycky, D [0000-0003-3750-0183], Fitzgerald, MP [0000-0002-0176-8973], Follette, KB [0000-0002-7821-0695], Fortney, JJ [0000-0002-9843-4354], Gerard, BL [0000-0003-3978-9195], Goodsell, SJ [0000-0002-4144-5116], Greenbaum, AZ [0000-0002-7162-8036], Hibon, P [0000-0003-3726-5494], Hinkley, S [0000-0001-8074-2562], Hung, LW [0000-0003-1498-6088], Ilene Dawson, R [0000-0001-9677-1296], Ingraham, P [0000-0003-3715-8138], Konopacky, Q [0000-0002-9936-6285], Larkin, JE [0000-0001-7687-3965], Lee, EJ [0000-0002-1228-9820], Marchis, F [0000-0001-7016-7277], Marois, C [0000-0002-4164-4182], Metchev, S [0000-0003-3050-8203], Millar-Blanchaer, MA [0000-0001-6205-9233], Morzinski, KM [0000-0002-1384-0063], Oppenheimer, R [0000-0001-7130-7681], Perrin, M [0000-0002-3191-8151], Rafikov, RR [0000-0002-0012-1609], Rajan, A [0000-0002-9246-5467], Rameau, J [0000-0003-0029-0258], Rantakyrö, FT [0000-0002-9667-2244], Ren, B [0000-0003-1698-9696], Schneider, AC [0000-0002-6294-5937], Sivaramakrishnan, A [0000-0003-1251-4124], Song, I [0000-0002-5815-7372], Soummer, R [0000-0003-2753-2819], Tallis, M [0000-0002-5917-6524], Thomas, S [0000-0002-9121-3436], Ward-Duong, K [0000-0002-4479-8291], Wolff, S [0000-0002-9977-8255], and Apollo - University of Cambridge Repository

Subjects
planets and satellites: detection, 010504 meteorology & atmospheric sciences, Stellar mass, detection [planets and satellites], Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, adaptive optics [instrumentation], Astronomy & Astrophysics, instrumentation: adaptive optics, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Mass distribution, Giant planet, Astronomy and Astrophysics, Exoplanet, Stars, 13. Climate action, Space and Planetary Science, astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey (GPIES). This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semi-major axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M $>$ 1.5 $M_\odot$ more likely to host planets with masses between 2-13 M$_{\rm Jup}$ and semi-major axes of 3-100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semi-major axis (a) for planet populations around high-mass stars (M $>$ 1.5M$_\odot$) of the form $\frac{d^2 N}{dm da} \propto m^\alpha a^\beta$, finding $\alpha$ = -2.4 $\pm$ 0.8 and $\beta$ = -2.0 $\pm$ 0.5, and an integrated occurrence rate of $9^{+5}_{-4}$% between 5-13 M$_{\rm Jup}$ and 10-100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with 0.8$^{+0.8}_{-0.5}$% of stars hosting a brown dwarf companion between 13-80 M$_{\rm Jup}$ and 10-100 au. Brown dwarfs also appear to be distributed differently in mass and semi-major axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semi-major axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the RV method, our results are consistent with a peak in occurrence of giant planets between ~1-10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability., Comment: 52 pages, 18 figures. AJ in press

Published
2019

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

Author

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 LW, 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 JB, 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., (Copyright © 2015, American Association for the Advancement of Science.)

Published
2015
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5. First light of the Gemini Planet imager.

Author

Macintosh B, Graham JR, Ingraham P, Konopacky Q, Marois C, Perrin M, Poyneer L, Bauman B, Barman T, Burrows AS, Cardwell A, Chilcote J, De Rosa RJ, Dillon D, Doyon R, Dunn J, Erikson D, Fitzgerald MP, Gavel D, Goodsell S, Hartung M, Hibon P, Kalas P, Larkin J, Maire J, Marchis F, Marley MS, McBride J, Millar-Blanchaer M, Morzinski K, Norton A, Oppenheimer BR, Palmer D, Patience J, Pueyo L, Rantakyro F, Sadakuni N, Saddlemyer L, Savransky D, Serio A, Soummer R, Sivaramakrishnan A, Song I, Thomas S, Wallace JK, Wiktorowicz S, and Wolff S

Abstract

The Gemini Planet Imager is a dedicated facility for directly imaging and spectroscopically characterizing extrasolar planets. It combines a very high-order adaptive optics system, a diffraction-suppressing coronagraph, and an integral field spectrograph with low spectral resolution but high spatial resolution. Every aspect of the Gemini Planet Imager has been tuned for maximum sensitivity to faint planets near bright stars. During first-light observations, we achieved an estimated H band Strehl ratio of 0.89 and a 5-σ contrast of 10(6) at 0.75 arcseconds and 10(5) at 0.35 arcseconds. Observations of Beta Pictoris clearly detect the planet, Beta Pictoris b, in a single 60-s exposure with minimal postprocessing. Beta Pictoris b is observed at a separation of 434 ± 6 milliarcseconds (mas) and position angle 211.8 ± 0.5°. Fitting the Keplerian orbit of Beta Pic b using the new position together with previous astrometry gives a factor of 3 improvement in most parameters over previous solutions. The planet orbits at a semimajor axis of [Formula: see text] near the 3:2 resonance with the previously known 6-AU asteroidal belt and is aligned with the inner warped disk. The observations give a 4% probability of a transit of the planet in late 2017.

Published
2014
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