A dozen years of hot exoplanet atmospheric investigations. Results from a large HST program. David K. Sing. #acrosshr Cambridge.
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1 A dozen years of hot exoplanet atmospheric investigations Results from a large HST program David K. Sing #acrosshr Cambridge ] 1 Aug 2014
2 Outline Introduction to Transit Spectroscopy Highlight 3 Science Questions 2 Eras of Transiting Atmospheres HST large program hot Jupiters David K. Sing
3 Exoplanet Atmosphere Characterization by Spectra Transits Direct Imaging Close-In Planets Wide-Separations Mpl, Rpl(λ), i, P, a, Fluxpl(λ,Φ) asin(i), Fluxpl(λ) Atmo. Composition Atmo. Composition Clouds/Hazes Clouds/Hazes Thermal profile Temperatures Stratospheres Thermospheres Exospheres Escape Dynamics, Winds Dynamics Photochemistry Chemistry Radial Velocity Bright Targets Kp, Mpl, i Atmo. Composition Stratospheres Dynamics, Winds David K. Sing
4 Transiting Planets 0.05% phase curve 0.3% secondary eclipse Transit 2.5% David K. Sing
5 Exoplanet Spectra Transmission spectrum Albedo Emission spectrum Rpl fpl λ λ f pl ( ) R pl ( ) David K. Sing
6 WASP-12A & b To Scale with Atmosphere Pitfall Instrument Systematics Astrophysical Systematics
7 Hot Jupiter models What might these planets look like? Lodders & Fegley (2006) HD Wasp-12 Fortney et al Early Atmosphere Models Solar Composition Chemical Equilibrium Jupiter Radiative Transfer H2 Na K H2O - Dominant CO - hotter atmospheres CH4 - cooler atmospheres TiO - Thermal Inversion Layers Clouds - likely depending on T-P profiles Brown Dwarf Temperature (K) 7
8 Major Science Q s noninverted inverted Thermal Structure Stratospheres? Day/Night? Composition & Abundances H2O? Chem? Formation? Clouds & Hazes and many more
9 Transiting Exoplanet Atmospheres Timeline STIS STIS & WFC3 cryogenic warm HR Phot MOS # Transiting Planets Spectra for Lisa Nortmann 53 Mercedes Lopez-Morales 209/189 era > survey era > 9 David K. Sing
10 Transiting Exoplanet Atmospheres 209/189 era STIS STIS & WFC3 cryogenic warm HR Phot MOS # Transiting Planets Spectra for /189 era > survey era > 10 David K. Sing
11 Transiting Exoplanet Atmospheres 209/189 era Thermal Inversions? 3.6 & 4.5 µm points Seager & Deming (2010) Major degeneracies in composition & thermal structure and many measurements needed refinement 11 David K. Sing
12 HD b: our first characterised exoplanet Transmission Emission Rayleigh H2 Na TiO/VO? 0.2 solar 2 solar Na, H2O, CO, Rayleigh Low albedo - few % Possible?? Stratosphere Likely Thermosphere Albedo Charbonneau et. al. (2002) Sing et al. ( 08a, 08b) Desert et al. (2009) Agol et al. (2010) Lecavelier et al. (2008) Rowe et al. (2008) 12 Burrows et al. (2008) Crossfield et al. (2012) Knutson et al. ( 07, 08) Deming et al. (2013) Vidal-Madjar (2011) Zellem et al. (2014) Phase Curve David K. Sing
13 HD b: our best characterised exoplanet Transmission Phase Curve Haze Na Albedo Optical Haze blue planet offset Hot Spot - Jets Na, H α, H2O and CO present Efficient heat re-distribution Emission Charbonneau et al. (2008) Grillmair et al. (2007) Knutson et al. ( 07, 09, 12) Pont et al. ( 07, 13) Sing et al. ( 09, 12) de Kok et al. (2013) Birkby et al. (2013) Desert et al. ( 09, 11) Agol et al. (2010) Gibson et al. ( 11, 12) Huitson et al. (2012) ) Evans et al. (2013) Jensen et al. (2012) Redfield et al. (2018) 13 David K. Sing
14 Stellar Activity & HD189733b: haze or spots? Longterm photometric monitoring of ALL stars Spectra Corrected for Occulted & Un-occulted Spots Pont et. (2008,2013) Sing et al. (2009,2011) Huitson et al. (2012) Evidence Against Large Persistent Spot Levels 1 - statistics of observed spot crossing 2 - statistics of spots from CoRot & Kepler studies 3 - absence of spots signatures in the final transmission spectrum 4 - Na line shape, Narrow & Tall McCullough et al. (2014) Oshagh et al. (2014) Arguments For Large Persistant Belt Spots 1 - Spots can explain the Transmission Spectrum 2 - Clear atmo more likely than hazy/cloudy atmo BUT need to be - Persistent over > 5 years & Cover a large fraction - Very Uniform to NOT be detected in Photo & Spect. Monitoring Unlikely by design you need a exoplanetary atmosphere to detect such spots 14 David K. Sing
15 Transiting Exoplanet Atmospheres survey era STIS STIS & WFC3 cryogenic warm # Transiting Planets Spectra for... Revolution Broadband Spectra Optical to near-ir 10 s ppm accuracy HR Phot MOS 209/189 era > survey era > 100 s of known Planets 15 David K. Sing
16 HST Exoplanet Surveys Cycle 18 WFC3 Cycle 19 STIS+WFC3 Cycle 20 WFC3 Cycle 21 WFC3 Cycle 22 STIS+WFC3 16 HJs Deming HJs Sing SE Bean HJs Bean SEs Benneke David K. Sing
17 HST Exoplanet Surveys Cycle 18 WFC3 Cycle 19 STIS+WFC3 Cycle 20 WFC3 Cycle 21 WFC3 Cycle 22 STIS+WFC3 17 HJs Deming HJs Sing SE Bean Bean HJs Bean SEs Benneke David K. Sing
18 Small Exoplanets & Clouds they re everywhere? GJ3470b HD97658b Ehrenreich et al. (2014) Knutson et al. (2014a,b) Kreidberg et al. (2014) Clouds covering features in Super-Earths / hot Neptunes GJ1214b 18 GJ436b
19 HST Exoplanet Surveys Cycle 18 Cycle 19 Cycle 20 Cycle 21 Cycle 22 WFC3 STIS+WFC3 WFC3 WFC3 STIS+WFC3 19 HJs Deming Deming HJs Sing SE Bean HJs Bean SEs Benneke David K. Sing
20 HST WFC3 Hot Jupiter Survey P.I. Deming Mandell et al. (2014) Deming et al. (2013) Line et al. (2013) HAT-P-12b H2O Detected & Spectral Resolved Variety of Amplitudes Clouds? Hazes? Low Abundances? 20 David K. Sing
21 Broadband Optical + near-ir+spitzer Science Goals - Directly Identify Stratosphere TiO - Clouds & Hazes Large HST Transmission Spectra Program PI SING Results published for Wasp-19b, Wasp-12b, Hat-P-1b, 2 more submitted
22 Wasp%12b) Wasp%12b) Wasp-12b TiO Muted 1.4 μm water- band absorp5on (already known; Swain et al. 2013) Op5cal shows no agreement with CLEAR, solar abundance atmospheric models TiO ruled out Sing et al. (2013) 22
23 Wasp%12b) Wasp-12b Best fits Mie scanering Al 2 O 3 T= K Rayleigh scanering good fit - but needs a low Temp of 880 K Variety of cloudy/hazy models are acceptable fits - Aerosols needed for Transmission (Sub-micron) - Helps explain Modest albedo (AB=25%) - Helps explain black body emission spectrum Sing et al. (2013) 23
24 WASP-31b: Cloudy Hazy & Potassium A heavily Clouded but not flat exoplanet Sing et al. (2014, submitted) 24 Rayleigh ScaNering by a Haze (4- σ) Cloud- Deck Covers H 2 O Detect Potassium (4- σ) but not Na 10 mbar - no alkali press broad. 1 mbar - No H 2 O Na/K < 1? ln[na/k] = - 3.3±2.8 solar is +3
25 WASP-31b: Cloudy Hazy & Potassium Can Clouds/Hazes be sustained at high altitudes?? WASP-31b g=4.56 m/s 2 Pressure (bars) Particle radius (µm) e 05 (m/s) Downward settling velocity for silicates requires: Kzz~10-4 m 2 s -1 at 10 mbar Kzz~10-5 m 2 s -1 at 1 mbar 10 mbar - no alkali broad. 1 mbar - No H 2 O ~1 micron size Parmen5er et al. (2013) 3D simula5ons of HD b WASP- 31 similar Temp es5mates effec5ve diffusivity Kzz~10-5 m 2 s -1 at 10 mbar Kzz~10-6 m 2 s -1 at 1 mbar Sing et al. (2014, submitted) It appears physically plausible that the circulation will be sufficiently strong to mix particles upward to 1 10 mbar 25
26 Hazy vs Clear Hot Jupiter Atmospheres haze scattering Na K Narrow Alkali lines Hazy Clear H 2 O H 2 O H 2 O H 2 O Wide Pressure Broadened Alkali lines
27 Comparative Exoplanet Spectroscopy A Family of hazy/cloudy exoplanets R ~ 50 S/N ~ µm Common Scale Scattering haze for non-active stars too 27 Cloudy Signatures - Opt IR - Obscured H2O - Opt Scattering - Flat Spectra - K?
28 Comparative Exoplanet Spectroscopy A Family of clear atmo. exoplanets Clear Signatures - Strong H2O - IR often > Opt - Strong Na - Pressurebroad Alkali 28
29 Large HST Transmission Spectra Program HST Large Transmission Spectra Program Results All 10 Hot Jupiters Have Detected Atmospheric Features Comparative Exoplanet Atmospheric Studies 1/2 are published (Wasp-12, Wasp-19, Hat-P-1, HD189733) others well in progress* Largest & Widest Comparison of Exoplanet spectra Ever Assembled Clouds/Hazes, Na, H2O are all very common across HJ parameter space BUT NOT UNIVERSAL 29 * This information is subject to change without notice. Some assembly required. Any rebroadcast, reproduction, or other use of the pictures and accounts of this game without the express written consent of Major League Baseball is prohibited.
30 Comparative Exoplanet Spectroscopy Clouds/Hazes a major distinguishing Characteristic of Hot Jupiters But Why? Cloud haze physics from cloudy HJs Condensation Chem.?? Photochemistry?? Abundances easier for clear atmosphere HJs Chemistry Formation
31 Conclusions jwst.nasa.gov Now in an Exciting Era of Comparative Exoplanetology Clouds could be important Spectral Classification for Gas Giant Exoplanets Next Revolution: JWST is coming SOON David K. Sing
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