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NIRISS René Doyon, Université De Montréal, FGS/NIRISS PI

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NIRISS René Doyon, Université De Montréal, FGS/NIRISS PI Transit Spectroscopy with NIRISS René Doyon, Université de Montréal, FGS/NIRISS PI ExoPAG 9 4 Jan 2014! 1 Collaborators •" David Lafrenière, UdeM (NIRISS exoplanet team lead) •" Loic Abert, UdeM •" Etienne Artigau, UdeM •" Mike Meyer, ETH, Switzerland •" Ray Jayawardhana, Toronto •" …. ExoPAG 9 4 Jan 2014! 2 Outline •" NIRISS overview •" Transit spectroscopy capability •" Simulations •" Performance limitations ExoPAG 9 4 Jan 2014! 3 FGS/NIRISS overview •" Two instruments in one box provided by CSA •" FGS (Fine Guidance Sensor) •" Provides fine guiding to the observatory •" 0.6-5 µm IR camera. No filters, single optical train with two redundant detectors each with a FOV of 2.3’x2.3’ •" Noise equivalent angle (one axis): 3.5 milliarcsec •" 95% sky coverage down to JAB=19.5 •" NIRISS (Near-Infrared Imager and Slitless Spectrograph) •" 0.7-5 µm IR camera. •" Four observing modes •" Main science drivers •" First Light: high-z galaxies •" Exoplanet detection and characterization ExoPAG 9 4 Jan 2014! ExoPAG 9 4 Jan 2014! 5 ExoPAG 9 4 Jan 2014! 6 ExoPAG 9 4 Jan 2014! 7 NIRISS SOSS (Single-Object Slitless Spectroscopy) mode •" Specifically optimized for transit spectroscopy •" Unique features •" Broad simultaneous wavelength range: 0.7-2.5 um •" Built-in weak lens to increase dynamic range and minimize systematic ‘’red noise’’ due to undersampling and flatfield errors. •" Key component is a directly ruled ZnSe grism (manufactured by Bach) combined with a ZnS prism, all AR coated except the ruled surface on the ZnSe grism. •" Two spares were manufactured by LLNL and received October 2012 (after instrument delivery in July 2012) •" Groove quality much better/sharper compared to the flight grism. Measurements and model suggested improved efficiency by > 2x. •" Plan is to swap grism after CV2. ExoPAG 9 4 Jan 2014! 8 SOSS mode implementation Monochromatic PSF measured in the lab! #! 20 pixels! ExoPAG 9 4 Jan 2014! Blaze function – Flight vs Spare ~2x! ~4x! ExoPAG 9 4 Jan 2014! 10 Total throughput – NIRISS vs NIRSpec NIRSpec A1600/PRISM/CLEAR 0.30 0.25 NIRSpec MOS1x3/G140H/F070LP NIRSpec A1600/G140H/F070LP R=30-90! R=1300-3600! NIRISS Spare (LLNL) 0.20 R=430-1350! 0.15 Throughput NIRISS Flight (Bach) 0.10 Kaltenegger & Traub (2009! 0.05 0.00 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 Wavelength (nm) Curves include a conservative margin (~20%) ! ExoPAG 9 4 Jan 2014! 11 Total throughput – NIRISS vs NIRSpec NIRSpec A1600/PRISM/CLEAR 0.30 0.25 NIRSpec MOS1x3/G140H/F070LP NIRSpec A1600/G140H/F070LP R=30-90! R=1300-3600! NIRISS Spare (LLNL) 0.20 R=430-1350! 0.15 Throughput NIRISS Flight (Bach) 0.10 Kaltenegger & Traub (2009! 0.05 0.00 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 Wavelength (nm) Curves include a conservative margin (~20%) ! ExoPAG 9 4 Jan 2014! 12 Saturatiom limits – NIRISS & NIRSPec 4 Unsaturated m=2, partial saturation in m=1" 55 Cnc e (256-pixel sub-arrray) " 0.9-2.5 !m , m=1 only" 6 HD 189733 b (80-pixel sub-array)" HD 209458 b 0.7-2.5 μm , m=1, m=2" GJ 436 b (256-pixel sub-array) " 8 Educated guess of M dwarfs yield from TESS. " GJ 1214 b 10 CoRoT-7 b J-band magnitude 12 Assumes 4-amp read-out mode or high-gain mode " NIRSPEC/F070LP/G140H/H NIRSPEC/F170LP/G235H/H 14 NIRISS/ORDER 1/80P NIRISS/ORDER 1/256P KNOWN TRANSITS NIRISS/ORDER 2/256P TESS (M DWARFS ONLY) NIRSPEC/CLEAR/PRISM 16 4.0 3.9 3.8 3.7 3.6 3.5 Log Teff ExoPAG 9 4 Jan 2014! 13 Saturation limit vs wavelength 4 630 - 1050 420 - 1310 500 - 2000 6 420 - 1310 1900 - 3600 1900 - 3600 700 - 1300 1300 - 2300 1900 - 3600 700 - 1300 NIRSPEC/CLEAR/PRISM 8 NIRSPEC/F070LP/G140/M 500 - 850 700 - 1300 NIRSPEC/F100LP/G140/M NIRSPEC/F170LP/G235/M NIRSPEC/F290LP/G395/M NIRISS/ORDER 1/80P NIRISS/ORDER 1/256P J-band saturation magnitude NIRISS/ORDER 2/256P NIRCAM/F277W NIRCAM/F322W2 NIRCAM/F356W 10 NIRCAM/F410M NIRCAM/F444W 30 - 300 12 1 2 3 4 5 Wavelength (microns) ExoPAG 9 4 Jan 2014! 14 NIRISS First Light with the GR700 grism (GSFC, October 2013) ExoPAG 9 4 Jan 2014! 15 MIRI & FGS into ISIM ExoPAG 9 4 Jan 2014! Real data vs simulation CV1RR (October 2013)! Simulation! Excellent correlation between data and simulations.! ExoPAG 9 4 Jan 2014! 17 GR700XD Monochromatic PSFs 0.64 um! 0.64 um! 0.64 um! Monochromatic PSF Tilt at 0.64 µm Order 1 order 1! order 2! order 3! 1619 1618 1617 Y position (pixel) 1616 Tilt = -1.0° 1615 330 340 350 360 370 380 X position (pixel) 1.06 um! 1.06 um! order 1! order 2! NIRISS grism is designed to have a PSF slanted by ~2° to mitigate undersampling problems.! ExoPAG 9 4 Jan 2014! 18 NIRISS Transit Spectroscopy Simulations (photon-noise limited) ExoPAG 9 4 Jan 2014! 19 GJ1214b Charbonneau et al 2009, Nature, 462, 17 ! What’s the nature of GJ1214b?" GJ1214b Earth Neptune o" An ice giant (a mini Neptune) ? ! o" A water world ?! Mass 6.5 1.0 17 Radius 2.7 1.0 4.0 Temperature 400-600 300 55 (Kelvin) Density 1.9 5.5 1.7 (g/cm3) ExoPAG 9 4 Jan 2014! 20 Current observations of GJ1214b HST/WFC3" At R=50" σ=230 ppm in 10 hr" Berta et al. 2012! Ground & space combined" Limited by aperture, platform stability, detector and instrument systematics and atmosphere ExoPAG 9 4 Jan 2014! 21 The same observations with JWST/NIRISS Water rich atmosphere ("Water world") GJ 1214b H2O rich atmosphere" 0.9868 R = 165" 0.9866 6.8 hr total" 0.9864 σ = 70 ppm" Flux(in)/Flux(out) 0.9862 170 ppm! JWST/NIRISS GJ1214b (M4.5V) J=9.8 τ=6.8 h (5 visits) R=165 at 1.25 µm 1.0 1.5 2.0 2.5 Wavelength (µm) ∆f R H(λ) 10 p f ⇡ R2 ✓ ◆atmo ? Same$ H = kT/µg model! µ 18 ⇠ Credit: D. Lafrenière ! Model from Miller-Ricci et al. 2010! ExoPAG 9 4 Jan 2014! 22 A more challenging observation… An Earth analog around an M dwarf (R~100) Feature Strength (ppm) H20 5-15 Broad ozone CH4 ~10 feature ! CO2 5-30 O2 <5 JWST/NIRISS, ROSS238 (M5.5V), 3.2 pc! O3 ~30 J=6.9 138 hrs (50 transits) ! Model from Kaltenegger et al. 2009! ExoPAG 9 4 Jan 2014! 23 A more challenging observation… An Earth analog around an M dwarf (R~100) Feature Strength (ppm) H20 5-15 Broad ozone CH4 ~10 feature ! CO2 5-30 O2 <5 JWST/NIRISS, ROSS238 (M5.5V), 3.2 pc! O3 ~30 J=6.9 138 hrs (50 transits) ! Model from Kaltenegger et al. 2009! ExoPAG 9 4 Jan 2014! 24 Performance limitations 5 ppm is about the noise level needed for minimal characterization of super-Earths. What will prevent reaching the photon-noise limit at this level? " Instrumental « red noise » " Already well-known from SPITZER and HST experience " Detector-related issues " Undersampling + jitter (may be okay with NIRISS) " Persistence " Long term stability (thermal instability) " Could probably be mitigated if noise is well characterized " Detailed simulations needed along with flight-like simulator testbed investigations. "Astrophysical « red noise » " Intrinsic variability (e.g. spots on M dwarfs) ExoPAG 9 4 Jan 2014! 25 The NIRISS Optical Simulator concept ExoPAG 9 4 Jan 2014! 26 Astrophysical noise associated with star spots ExoPAG 9 4 Jan 2014! 27 GJ1214b: are we seeing star spots? •" If GJ1214 is spotted over 5% of its surface and GJ1214b happens to transit a spot-free area … ! •" Out-of-transit spectrum : 95% star, 5% spots! •" In-transit spectrum: 93.6% star, 5% spots! •" Spot spectra, 500 K cooler than photosphere, has significantly deeper water bands and a redder overall SED.! •" In-transit/out-of-transit spectrum will contain significant spectral structures at a level comparable to that induced by an exoplanet’s atmosphere! 2 Rp/Rs=0.116, (χ r= 1.25) 0.124 2 Starspots, η=5%, Teff=3000K, ∆T=500K, (χ r= 1.03) 2 Solar, (χ r= 10.72) 2 No CH4, (χ r= 7.12) 2 H2O, (χ r= 1.30) 0.122 Berta et al. 2012 Bean et al. 2011 0.120 Star spot-induced transit s /R spectrum fits data better than p R 0.118 any planet atmosphere model!! 0.116 0.114 Artigau et al, in prep.! 1.0 1.5 2.0 2.5 Wavelength (µm) ExoPAG 9 4 Jan 2014! 28 Spectrum blueward of 1 µm may be key for discriminating between star spots and water vapor from the exoplanet. 1.005 TiO! 1.005 TiO! p p H2O! 1.000 1.000 NaI! Normalized R Normalized R H2O! 0.995 0.995 Starspots Starspots Water−world Water−world Correlation : −7% Correlation : 84% 0.6 0.7 0.8 0.9 1.0 1.2 1.4 1.6 1.8 2.0 2.2 2.4 Wavelength (µm) Wavelength (µm) •" TiO, NaI, FeH dominate the star spot- induced spectrum.! •" In near-IR domain, both star spots and exoplanets induce very similar signals, Water absorption dominates the •" both dominated by deep water features. planetary features.! Slight difference in the shape spectra arise •" Good spectral resolution needed to from the important difference in detect some features (e.g. NaI, KI)! temperature (2500 K versus 500 K).! ExoPAG 9 4 Jan 2014! 29 Summary •" NIRISS will be a powerful capability for high-precision transit spectroscopy work •" Pros •" Broad simultaneous wavelength coverage (0.7-2.5 µm) •" Medium resolving power (~700).
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