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Observations of proto-planetary disks and exo-planets with the JWST

Observations of proto-planetary disks and exo-planets with the JWST. E. Pantin , P.O. Lagage and the MIRI science team. SPITZER (IRAC, 8  m). JWST (MIRI, 7.7  m). Thermal Background. + FGS: Tunable Filter Instrument 1.5-5 um, R= 100, NRM (21 baselines). NIRCAM coronagraphic occulters.

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Observations of proto-planetary disks and exo-planets with the JWST

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  1. Observations of proto-planetary disks and exo-planets with the JWST E. Pantin, P.O. Lagage and the MIRI science team

  2. Disks and exoplanets : sciences cases for interferometry

  3. SPITZER (IRAC, 8 m) JWST (MIRI, 7.7 m) Disks and exoplanets : sciences cases for interferometry

  4. Thermal Background Disks and exoplanets : sciences cases for interferometry

  5. + FGS: Tunable Filter Instrument 1.5-5 um, R= 100, NRM (21 baselines) Disks and exoplanets : sciences cases for interferometry

  6. NIRCAM coronagraphic occulters 2 apodized WEDGES 3 apodized SPOTS Disks and exoplanets : sciences cases for interferometry

  7. MIRI Fields of View, Coronagraphs 4QPM Coronagraphs 15.5µm 11.4µm 10.65µm 24 x 24 arcsec. Imager 75 x 113 arcsec Low Resolution Spectrometer 5 x 0.6 arcsec Medium Resolution Spectrometer > 3.5 x 3.5 arcsec Lyot Mask 23mm 30” x 30” F1550C or (F1550C+ F1140C) => Teff , CO2, clouds F1065C + F1140C => Ammonia, clouds, T° probe F0560W => water F0770W => methane All + modeling => some atmospheric parameters Some degeneracies exist => combination with NIR is crucial Disks and exoplanets : sciences cases for interferometry

  8. Principle of 4QPM (n-1)e =/2 IWA  /D  0.35" Disks and exoplanets : sciences cases for interferometry

  9. Disks and exoplanets : sciences cases for interferometry

  10. Disks and exoplanets : sciences cases for interferometry

  11. Disks and exoplanets : sciences cases for interferometry

  12. Sensitivity Disks and exoplanets : sciences cases for interferometry

  13. Major points: • extreme sensitivity combined fairly good angular resolution ("a VISIR in space") • stability • JWST is not meant to discover new exoplanets but characterize already known ones Disks and exoplanets : sciences cases for interferometry

  14. Exo-planets

  15. Exo-planets imaging science case

  16. Simulated coronagraphic images NIRCAM: M0 star 4 pc 2 Mj 7 AU MIRI: M2V star 10 pc 5, 10, 15 AU 1h integration  = 11.4 m Disks and exoplanets : sciences cases for interferometry

  17. Rejection performance Beichman, 2010 Disks and exoplanets : sciences cases for interferometry

  18. Parameters space NIRCAM/TFI/MIRI M stars GROUND-BASED IMAGING Bright early-type stars Disks and exoplanets : sciences cases for interferometry

  19. Disks and exoplanets : sciences cases for interferometry

  20. JWST exoplanets imaging science case A simulated targets sample for exoplanets detection

  21. Simulated performances Sample program Monte-Carlo ~700 stars) 1000 runs d< ~150 age : 1 Myr- 1 Gyr 25 best (highest detection success rate) 1  dispersion, all stars symbol sizes  fractional detection rate Beichman et al., 2010 Disks and exoplanets : sciences cases for interferometry

  22. Full sample MIRI NIRCAM TFI-NRM Disks and exoplanets : sciences cases for interferometry

  23. M stars only old planets > Mj young planets < Mj NIRCAM MIRI Disks and exoplanets : sciences cases for interferometry

  24. Giant planets formation mechanism around low-mass stars:The M stars niche for MIRI imager

  25. The ("adolescent") M stars opportunity Disks and exoplanets : sciences cases for interferometry

  26. The M stars opportunity • 12 M0-M5 stars • d=10-40 pc • ages < 200 Myr • TW Hya (10 Myr) •  Pic mg (12 Myr) • Tucana-Horologium (30 Myr) • AB doradus (80 Myr) • Castor mg (200 Myr) complementary NIRCAM and TFI observations are compulsory to assess the planetary nature of sources found !! Disks and exoplanets : sciences cases for interferometry

  27. Exoplanets characterization using mid-IR spectroscopy

  28. Exoplanets mid-IR spectra Disks and exoplanets : sciences cases for interferometry

  29. Hot Jupiter primary and secondary transits (NIRCAM, NIRspec) HD209459 b secondary transit primary transit t=6h courtesy of J. Valenti hot neptunes spectra (4 transits) are accessible using NIRCAM-NIRspec instruments Disks and exoplanets : sciences cases for interferometry

  30. Exo-Earths transit spectra (NIRspec, MR) NIRspec simulated spectrum of a (H2 rich) super-Earth exoplanet (GL581-like, M3, 6 pc, 20 transits) Clampin, 2009 Disks and exoplanets : sciences cases for interferometry

  31. MIRI • transit spectroscopy (probably not as performant as NIRCAM/NIRspec, TBC) • imaging (++) • spectral deconvolution using the MRS Disks and exoplanets : sciences cases for interferometry

  32. A couple of (non exhaustive) niches concerning telluric planets !

  33. The molten exo-Earths opportunity • No atmosphere  100 000 yr cooling time • Atmosphere  1-10 Myr cooling time Miller-ricci et al., 2009 Disks and exoplanets : sciences cases for interferometry

  34. Exo-rings SECP rings can survive on Gyr-timescales ! Pantin et al., in prep Disks and exoplanets : sciences cases for interferometry

  35. Exo-rings "Fomalhaut b-like" ring Detection limit Disks and exoplanets : sciences cases for interferometry

  36. Circumstellar disks

  37. Spectroscopy of PP disks

  38. Spectroscopy of PP disks : a key program for MIRI GTO observations • Full inventory of organic (pre-biotic) species : • NH3 • C6H6 • CH4 • HCO+ • HCN Disks and exoplanets : sciences cases for interferometry

  39. Disks and exoplanets : sciences cases for interferometry

  40. THE MIRI GTO imaging proposal on proto-planeteary disks

  41. Goals • study: • large-scale geometry of the disks: • MIRI tremendous sensitivity allows to observe the disks up to very large distances from the star • for the first time, a large sample of T-Tauri disks are observable/resolvable in the mid-IR • disks (dust) vertical structure • dust settling • dust coagulation • disks stratification • search for forming/formed planets signature: • direct detection of forming protoplanet is highly unlikely (brightness peak@accreting phase ?) • embedded massive bodies produce structures in disks: • gaps • bright rims • asymmetries Disks and exoplanets : sciences cases for interferometry

  42. MIRI study of Large Scale Structure ofProtoplanetary Disks

  43. What do we observe in the mid-IR range ? ~1 AU,10 mas • Mainly the thermal emission from heated dust grains • Mainly the inner rim (1500 K) that produces >90% of the total 10 m flux (continuum)  coronagraphic mode is compulsory to avoid detector saturation (Fmax=20 mJy) and decrease photon noise • Once, the inner rim masked/subtracted, the thermal emission produced at the disks' surface (=1), on intermediate distance scales (3-100 AU) • PAH emission (7.7, 8.6, 11.3 m) on larger scales ( Rout) ~100 AU Disks and exoplanets : sciences cases for interferometry

  44. Large Scale Parameters HD97048 8.6 m VLT/VISIR (Lagage et al. 2006) Star measure: • scale height at a given distance • flaring parameter • dust sizes vs distance • dust composition vs distance indirect indications/constraints on: • gas content • turbulence (small grains) • surface density Disks and exoplanets : sciences cases for interferometry

  45. Disks in "transition" phase HD 95881 model sketch Disks and exoplanets : sciences cases for interferometry

  46. Continuum profiles MIRI MIRI In the case of Herbig disks, the PAH emission (8.6, 11.3 m) is brighter and more extended than continuum emission Disks and exoplanets : sciences cases for interferometry

  47. Scattered mid-IR emission Disks and exoplanets : sciences cases for interferometry

  48. MIRI study of Disks Vertical Structure

  49. Disks appareance Disks and exoplanets : sciences cases for interferometry

  50. Disks appareance as a probe of dust settling PAH dominated spectrum Disks and exoplanets : sciences cases for interferometry

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