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From Gl229B to HR8799bcd: 15 years of direct exoplanet imaging research Christian Marois Herzberg Institute of Astrophysics Kyoto, Japan May 2009 From Gl229B to HR8799bcd: 15 years of direct exoplanet imaging research Christian Marois

  1. From Gl229B to HR8799bcd: 15 years of direct exoplanet imaging research Christian Marois Herzberg Institute of Astrophysics Kyoto, Japan May 2009

  2. From Gl229B to HR8799bcd: 15 years of direct exoplanet imaging research Christian Marois Herzberg Institute of Astrophysics Kyoto, Japan May 2009

  3. Stars vs Brown Dwarfs vs Planets Earth 75 MJup 13.6 MJup

  4. Stars vs Brown Dwarfs vs Planets Earth Burrows 75 MJup 13.6 MJup

  5. The challenge Everest mount (10km) Jupiter: basketball Earth: ant

  6. Gl229B

  7. Gl229B

  8. Star Forming Region 5-15 MJup Free-floating in star forming regions? Zapatero Osorio et al. 2000

  9. Star Forming Region 5-15 MJup Free-floating in star forming regions? Zapatero Osorio et al. 2000 Luhman

  10. 2MASS Free-floating in space?

  11. What is an exoplanet? Less than 13.6 Jupiter mass (13.6-75MJup = brown dwarfs) In orbit around a star Form in a disk (?) Initial formation energy, than cool down with time. “hot start model” “core accretion model”

  12. Designing a Direct Imaging Exoplanet Survey Need to be able to resolve the system Need to be able to see the planets before they cool down Find nearby & young stars

  13. Palomar AO Survey Ben Oppenheimer et al. : < 8pc survey (163 stars) Stan Metchev et al. : 266 stars 3Myr-3Gyr at Palomar & Keck - BD statistics 28-1590AU 3.2% [+3.1-2.7]

  14. Young star HST survey 2M1207b 116 nearby young stars - NICMOS 2 coronagraph Inseok Song et al.

  15. Keck AO survey Kaisler, Macintosh, Zuckerman, Song et al. M. Liu Stan Metchev

  16. VLT/Arizona AO survey Laird Close/R. Lenzen SDI-camera 60 stars survey (B. Billers) Nielson 20-100AU >4MJup <20% Chauvin et al. Phil Henz Clio L-band IR camera Neuhauser et al <6pc survey

  17. Subaru AO survey Nakajima < 20 pc survey Motohide Tamura TTauri star survey

  18. Gemini AO survey Altair commissioning ~2003

  19. Altair@Gemini N David Lafreniere: GDPS (2004-2007) 86 GKM stars <300 Myr Christian Marois: IDPS (2007-now) ~100 AF stars <300 Myr & some dusty AF stars David Lafreniere: Young star associations Markus Janson: ~10 OB stars

  20. Our Gemini Survey History 2002: ADI initial idea 2003: Initial ADI testing at Gemini North (Altair SV). 2004-2007: 86 GKM stars ADI survey at Gemini North - no detection (Lafreniere et al. 2007). 2007-now: 80 AF stars ADI survey (Gemini North, Keck II & VLT). 2007-now: Young star association (Lafreniere)

  21. Angular Differential Imaging Image 1 Image 2 (+ 5 minutes)

  22. Angular Differential Imaging Image 1 Image 2 (+ 5 minutes) Subtraction

  23. Angular differential imaging Camera South East West

  24. Angular differential imaging Camera South East West

  25. Angular differential imaging Camera South East West

  26. Angular differential imaging Camera South East West

  27. Angular differential imaging Camera South East West

  30. +

  31. + =

  34. ADI gain

  35. The GDPS ADI Survey

  36. The GDPS ADI Survey No detection

  37. The IDPS survey Remove the late type bias Focus on young & close AF-type stars + some dusty Combine the Gemini N, Keck and VLT

  38. HR 8799 Characteristics A5V star V~6 39 pc (130 ly) Pegasus Lambda Boo, Gamma Dor and Vega-like star (disk ~90AU)

  39. HR 8799 Characteristics A5V star V~6 39 pc (130 ly) Pegasus Lambda Boo, Gamma Dor and Vega-like star (disk ~90AU)

  40. HR 8799 Characteristics A5V star V~6 39 pc (130 ly) Pegasus Lambda Boo, Gamma Dor and Vega-like star (disk ~90AU)

  41. The Initial Discovery (March 2008) October 2007 NRC Canada Gemini North

  42. The Initial Discovery (March 2008) October 2007 NRC Canada Gemini North

  43. The Initial Discovery (March 2008) October 2007 NRC Canada Gemini North

  44. A third planet! September 2008 NRC Keck II

  45. A third planet! September 2008 September 2008 NRC Gemini NRC Keck II

  46. A system not that easy to see... Gemini N, Altair/NIRI &10s K-band

  47. A system not that easy to see... Gemini N, Altair/NIRI &10s K-band ADI processing

  48. Voyager 1 (43 AU) 18 cm diameter Keck 2 (130 ly), 10m diameter Neptune 8 200 000 AU

  49. Voyager 1 (43 AU) 18 cm diameter Keck 2 (130 ly), 10m diameter Neptune 8 200 000 AU

  50. Voyager 1 (43 AU) 18 cm diameter Keck 2 (130 ly), 10m diameter Neptune 8 200 000 AU

  51. Keck 2004 old data Add 4 more years of orbital motion!

  52. July 2004 July 2004 PM July 2008

  54. Multi-band photometry @ Keck HR 8799 age?

  55. Multi-band photometry @ Keck HR 8799 age?

  56. HR 8799 Age Estimation Low in the HR diagram, under Pleiades. Galactic Space motion consistent with being young - between TW Hya and Pleiades Lambda Boo & Gamma Dor stars generally considered young. Massive debris disk - lower probability at older ages. Isolated field star. HR 8799 age = 30-160 Myr

  57. HR 8799 Age Estimation Low in the HR diagram, under Pleiades. Galactic Space motion consistent with being young - between TW Hya and Pleiades Lambda Boo & Gamma Dor stars generally considered young. Massive debris disk - lower probability at older ages. Isolated field star. HR 8799 age = 30-160 Myr

  58. HR 8799 Age Estimation Low in the HR diagram, under Pleiades. Galactic Space motion consistent with being young - between TW Hya and Pleiades Lambda Boo & Gamma Dor stars generally considered young. Massive debris disk - lower probability at older ages. Isolated field star. HR 8799 age = 30-160 Myr

  59. Mass, radius & Teff estimations from cooling tracks

  60. The 3 planet’s colors are more consistent Bright with Pleiades low mass ~11MJup objects and 2M1207b than field BDs. Physics untested - No Blue Faint Red corresponding objects in the field.

  61. Planetary System Formation Solar system Niel Brandt

  63. HR 8799 Planetary System Probably formed in a disk September 2008 July 2004 July 2004 PM July 2008 Star slow rotation

  64. HR 8799bcd Characteristics Period Radius Mass Separation Temperature HR 8799 (AU) (years) (K) (RJup) (MJup) b 68 ~460 820 1.30 7 c 38 ~190 1000 1.25 10 d 25 ~100 1000 1.20 10 Circular 60 Myr face-on

  65. E. Becklin 1998 HST data

  66. Lefreniere et al. 2009 ~10x better PSF subtraction!

  67. Lefreniere et al. 2009, submitted New 1998 epoch! F160W point consistent with water bands!

  68. 2nd HST paper in prep. Lefreniere et al. 2009

  69. 2nd HST paper in prep. Lefreniere et al. 2009 Marois et al., in prep.

  70. Finalizing the current AO survey (2010) Nearly 100 massive stars have been observed 79 candidates (3 real!) Increasing the survey to 250 stars (250h for 2009B) Now with NICI, NIRI, Nirc2 & Conica

  71. Finalizing the current AO survey (2010) Nearly 100 massive stars have been observed 79 candidates (3 real!) Increasing the survey to 250 stars (250h for 2009B) Now with NICI, NIRI, Nirc2 & Conica

  72. 1RXS J160929.1-210524 330 AU & 8 MJup Bound? Lafreniere et al. 2008

  73. NICI@Gemini S 50 nights survey in 2-3 years PI: M. Liu & L. Close

  74. GPI@Gemini S/N

  75. 10s 20 minutes (ADI) 10s

  76. 10s 20 minutes (ADI) 10s

  77. Direct exoplanet imaging - active on all 8-10m class telescopes equipped with an AO system (Gemini, Subaru, Keck, MMT & VLT). Gemini played a very important role in this field: Development of a key observing strategy (ADI) Lead one of the most complete imaging survey (GDPS) Ongoing 2nd generation survey aimed at young/close more massive stars (IDPS) Ongoing NICI survey 2nd generation dedicated instrumentations: GPI (2011) Gemini commitment lead to the HR 8799 discovery, the first directly image multi-planet system. First at separations similar to the outer planets of our solar system + detected Keplerian orbital motion. More to come...

  78. Conclusions Direct exoplanet imaging - active on all 8-10m class telescopes equipped with an AO system (Gemini, Subaru, Keck, MMT & VLT). Gemini played a very important role in this field: Development of a key observing strategy (ADI) Lead one of the most complete imaging survey (GDPS) Ongoing 2nd generation survey aimed at young/close more massive stars (IDPS) Ongoing NICI survey 2nd generation dedicated instrumentations: GPI (2011) Gemini commitment lead to the HR 8799 discovery, the first directly image multi-planet system. First at separations similar to the outer planets of our solar system + detected Keplerian orbital motion. More to come...

  81. Dynamic Analysis Fabrycky & Murray-Clay 2009 Not perfectly face-on & not perfectly circular 4:2:1 resonance Non-resonance cases = masses need to be lower (< 2Mjup) 2:1 resonance for c & d: some cases stable for age 4:2:1 resonance: stable up to ~20 MJup. Younger age / model over predict mass / 4:2:1 resonance

  82. Do cooling tracks overestimate the mass? Dupuy et al. 2008

  83. Gozdziewski & Migaszewski 2009 4:2:1 resonance could be unstable in 400Myr Planet d would be ejected from the system

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