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HD 209458 B Shows No Evidence of Tio That Could Potentially Cause an Inversion Layer

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Exoplanet Atmospheres at High Spectral Resolution Jayne Birkby Sagan Fellow, Harvard-Smithsonian Centre for Astrophysics [email protected] http://www.cfa.harvard.edu/~jbirkby @jaynebirkby Detecting molecules with transmission spectroscopy Starlight filtering through an atmosphere during transit is imprinted with the planet’s spectrum 2 Transit depth ~ (Rp/Rs) Relative flux Relative Time Credit: Deming (Nature) Transit depth Transit Wavelength Transmission spectra with HST/WFC3 reveal water in hot Jupiters Deming et al. 2013 Huitson et al. 2013 H2O Wakeford et al. 2013 Deming et al. 2013 McCullough et al. 2014 Kreidberg et al. 2015 Mandell et al. 2013 Kreidberg et al. 2014 Benneke 2015 Transmission spectra with HST/WFC3 reveal water and clouds in warm Neptunes Fraine et al. 2014 Water detected (5σ) in dust-free atmosphere HAT-P-11 b Transit depth (ppm) Transit Warm Neptune Flux variations -4 at 10 level Solar-metallicity, cloud-free Knutson et al. 2014 Hydrogen-poor solar model are important Solar-metallicity, thick clouds GJ 436 b Warm Neptune Flat featureless spectrum in cloudy/hazy atmosphere 60 orbits with HST/WFC3 revealed a featureless (cloudy) spectrum for super-Earth GJ 1214 b ) -6 Relative transit depth (x10 depth transit Relative Kreidberg et al. 2014 Even space telescopes suffer systematics >> planet signal Even space telescopes suffer systematics >> planet signal XO-1 b HST/NICMOS Hot Jupiter HST/WFC3 Deming et al. (2013) Even space telescopes suffer systematics >> planet signal XO-1 b HST/NICMOS Hot Jupiter HST/WFC3 Deming et al. (2013) Instruments must be stable Ground-based observations and well-characterized with require similarly bright repeatable results reference stars ! “The nearest transiting potentially habitable planet is ~11 pc away.” ! “The nearest [non-transiting] potentially habitable planet is ~2.5 pc away.” ! (Dressing & Charbonneau 2015) Detecting molecules with High Dispersion Spectroscopy (HDS) A CRIRES/VLT survey of hot Jupiter atmospheres • CRIRES: CRyogenic high-resolution InfraRed Echelle Spectrograph • R=100,000 spectrograph, 8.2 m mirror • 155hrs • 5 brightest host stars visible from Paranal, Chile (K ~ 4 – 6 mag): HD 209458 b, HD 189733 b, 51 Peg b, ! Boo b, HD 179499 b HDS detects the radial velocity shift of the planetary spectrum Dayside Nightside 5 Relativeline depth 10 x τ Boötis b ModelModel COCO lineslines R~100,000 HDS detects the radial velocity shift of the planetary spectrum 0.8 Toy model of CO lines Blue-shifted Dayside Planet 0.6 Nightside Red-shifted 0.4 Phase 5 0.2 0.0 Relativeline depth 10 x Telluric τ Boötis b ModelModel COCO lineslines R~100,000 -0.2 2.309 2.310 2.311 2.312 2.313 Wavelength / μm Telluric features eliminated by removing common modes in time SNR~200 per resolution element Phase Wavelength CRIRES pipeline output after alignment SYSREM - Treats pixel channels as light curves Mean-subtracted spectra as input to Sysrem (1024 light curves per detector) - PCA-like algorithm identifies trends as a function of time After first Sysrem iteration, airmass-like trend removed - Data are self-calibrating Standard deviation ~ 5x10-4 After optimal Sysrem iterations Combine signal from individual lines via Birkby et al. 2013 10x nominal model injected cross-correlation HDS detects carbon monoxide RV trail in a transiting hot Jupiter atmosphere 0.8 Toy model of CO lines 0.6 Secondary eclipse 0.4 OrbitalPhase Phase 0.2 RV - Vsys (km/s) Snellen et al. 2010 0.0 Transit CO detected at 5.6σ at 2.3 µm in HD 209458 b during transit with 5 hrs on CRIRES/VLT -0.2 2.309 2.310 2.311 2.312 2.313 Wavelength / μm HDS detects carbon monoxide RV trail in a transiting hot Jupiter atmosphere 0.8 Toy model of CO lines Kp = 150 km/s 0.6 Secondary eclipse 0.4 OrbitalPhase Phase 0.2 RV - Vsys (km/s) Snellen et al. 2010 0.0 Transit CO detected at 5.6σ at 2.3 µm in HD 209458 b during transit with 5 hrs on CRIRES/VLT -0.2 2.309 2.310 2.311 2.312 2.313 Non-transiting planet = spectroscopic binary Wavelength / μm HDS detects carbon monoxide RV trail in a non-transiting hot Jupiter atmosphere 0.8 Toy model of CO lines Planet rest frame Observed (Kp=110 km/s) 0.6 0.4 Phase 0.2 Brogi et al. 2012 0.0 CO detected at 6σ at 2.3 µm in τ Boo b on the dayside hemisphere (non-transiting) -0.2 2.309 2.310 2.311 2.312 2.313 with CRIRES/VLT Wavelength / μm HDS provides unambiguous detections of CO in hot Jupiter atmospheres 51 Peg b τ Boo b HD 189733 b Non-transiting Non-transiting Transiting [email protected]µm [email protected]µm Brogi et al. 2013 Brogi et al. 2012 [email protected]µm de Kok et al. 2013 Other molecules are more complex and appear at different wavelengths Model CO lines Model H2O lines 5 Relativeline depth 10 x Model CO lines Model CO2 lines Model CH4 lines Other molecules are more complex and appear at different wavelengths Model CO lines Model H2O lines 5 Greater uncertainty Relativeline depth 10 x Model CO lines in line positions at high temperatures Model CO2! lines Model CH4 lines More telluric contamination Spectral time-series @ 2.3μm Time Wavelength Spectral time-series @ 3.2μm Time 2000K Wavelength HDS provides unambiguous detections of Boo b - CO complex51 Peg b - COmolecules + H O in hot Jupiter atmospheres 2 90 140 70 90 140 70 60 120 ) ) ° 60 ° 120 50 ) ) -1 -1 50 100 (km s 40 (km s P 100 P K K 40 Orbital inclination ( Orbital inclination ( 80 30 80 51 Peg b τ Boo b HD 189733 b Non-transiting Non-transiting 30 Transiting 60 [email protected]µm 20 60 [email protected]µm [email protected]µm -40 -20 0 20 40 -80 -60 -40 -20 0 20 Brogi et al. 2013 -1 -1Brogi et al. 2012 de Kok et al. 2013 Vsys (km s ) Vsys (km s ) Significance () Significance () -2.7 -1.6 -0.5 0.6 1.7 2.8 3.9 5.0 -3.8 -2.6 -1.4 -0.2 1.0 2.2 3.4 4.6 HD 189733b - CO HD 179949b - CO + H2O 180 160 160 90 90 70 ) ) 70 ° 140 ° 140 60 ) ) -1 60 -1 120 50 (km s 120 (km s P 50 P K K HD 189733 b 51 Peg b 100 Orbital inclination ( HD 179949 b 40 Orbital inclination ( 100 40 Transiting Non-transiting Non-transiting [email protected]µm [email protected]µm 80 80 [email protected]µm Birkby et al. 2013 30 30 Birkby et al. in prep Brogi et al. 2014 -60 -40 -20 0 20 40 60 -60 -40 -20 0 20 40 -1 -1 Vsys (km s ) Vsys (km s ) Significance () Significance () -4.5 -3.0 -1.5 0.0 1.5 3.0 4.5 -3.0 -1.5 0.0 1.5 3.0 4.5 6.0 See also Rodler et al. 2012; 2013 (CO in τ Boo b & HD 189733 b); Lockwood et al. 2014 (H2O in τ Boo b) Exoplanet atmospheres as fossil records? C/O ratio could reveal where and how a planet formed in its protoplanetary disk Oberg et al. (2011) Helling et al. (2014) C/O ratio could reveal where and how a planet formed in its protoplanetary disk Oberg et al. (2011) Helling et al. (2014) Marois et al. (2010) For HR 8799 planets: i) Super-stellar C/O: core accretion at location ii) Stellar C/O: gas collapse at location Barman et al. 2015, Teske et al. 2014 HR 8799 bcde Simulations identify 3.5µm as spectral ‘sweet spot’ for measuring C/O ratio Simulation of CRIRES sensitivity de Kok, Birkby et al. (2014) RelativeCorrelation Wavelength / μm Simulations identify 3.5µm as spectral ‘sweet spot’ for measuring C/O ratio Simulation of CRIRES sensitivity de Kok, Birkby et al. (2014) H2O! HD 209458 b CH4! τ Boo b CO2 (Birkby et al. in prep.) CO! HD 179949 b C/O<1 (Brogi et al. 2014) H2O! CH4 RelativeCorrelation H2O! CO2! CH4 H2O! CO2 Wavelength / μm Accurate line lists are essential for HDS HD 209458 b shows no evidence of TiO that could could that TiO evidence HD of 209458 no shows b potentially cause an inversion layercause inversion an potentially Hoeijmakers Observed , de Kok, Snellen, Brogi, Birkby, Schwarz, 2014 deSnellen, Kok, , Brogi, Birkby, Injected -11 -10 -9 -8 -7 VMRTiO=10 VMRTiO=10 VMRTiO=10 VMRTiO=10 VMRTiO=10 HD 209458 b shows no evidence of TiO that could could that TiO evidence HD of 209458 no shows b potentially cause an inversion layercause inversion an potentially Hoeijmakers Observed , de Kok, Snellen, Brogi, Birkby, Schwarz, 2014 deSnellen, Kok, , Brogi, Birkby, Injected -11 -10 -9 -8 -7 VMRTiO=10 VMRTiO=10 VMRTiO=10 VMRTiO=10 VMRTiO=10 Stellarmodel atmospheres observations M-dwarf HD 209458 b shows no evidence of TiO that could could that TiO evidence HD of 209458 no shows b potentially cause an inversion layercause inversion an potentially Hoeijmakers Observed , de Kok, Snellen, Brogi, Birkby, Schwarz, 2014 deSnellen, Kok, , Brogi, Birkby, Injected -11 -10 -9 -8 -7 VMRTiO=10 VMRTiO=10 VMRTiO=10 VMRTiO=10 VMRTiO=10 for the high resolution technique resolution high the for Data cross-correlated with Barnard’s star (M-dwarf) Datacross-correlated Barnard’s with Accurate Stellarmodel atmospheres line lists arelists crucial line observations M-dwarf Monitoring atmospheric dynamics with HDS Nightside features are deeper and Dayside potentially easier to detect Night side Reveals heat circulation de Kok, Birkby et al.
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    Atmospheres of hot alien Worlds Atmospheres of hot alien Worlds Proefschrift ter verkrijging van de graad van Doctor aan de Universiteit Leiden, op gezag van Rector Magnificus prof.mr. C.J.J.M. Stolker, volgens besluit van het College voor Promoties te verdedigen op donderdag 5 juni 2014 klokke 10.00 uur door Matteo Brogi geboren te Grosseto, Italië in 1983 Promotiecommissie Promotors: Prof. dr. I. A. G. Snellen Prof. dr. C. U. Keller Overige leden: Prof. dr. C. Dominik University of Amsterdam Prof. dr. K. Heng University of Bern Prof. dr. E. F. van Dishoeck Dr. M. A. Kenworthy Prof. dr. H. J. A. Röttgering Ai miei genitori, per aver creduto in me, permettendomi di realizzare un sogno Contents 1 Introduction 1 1.1 Planet properties from transits and radial velocities . 2 1.2 Atmospheric characterization of exoplanets . 4 1.2.1 Atmospheres of transiting planets . 4 1.2.2 Challenges of space- and ground-based observations . 7 1.2.3 Ground-based, high resolution spectroscopy . 8 1.2.4 A novel data analysis . 10 1.3 Close-in planets and their environment . 10 1.3.1 From atmospheric escape to catastrophic evaporation . 12 1.4 This thesis . 12 2 The orbital trail of the giant planet t Boötis b 17 2.1 The CRIRES observations . 18 2.2 Data reduction and analysis . 19 2.2.1 Initial data reduction . 19 2.2.2 Removal of telluric line contamination . 19 2.2.3 Cross correlation and signal extraction . 21 2.3 The CO detection and the planet velocity trail .
  • Extrasolar Planets

    Extrasolar Planets

    Extrasolar Planets Dieter Schmitt Lecture Max Planck Institute for Introduction to Solar System Research Solar System Physics KatlenburgLindau Uni Göttingen, 8 June 2009 Outline • Historical Overview • Detection Methods • Planet Statistics • Formation of Planets • Physical Properties • Habitability Historical overview • 1989: planet / brown dwarf orbiting HD 114762 (Latham et al.) • 1992: two planets orbiting pulsar PSR B1257+12 (Wolszczan & Frail) • 1995: first planet around a solarlike star 51 Peg b (Mayor & Queloz) • 1999: first multiple planetary system with three planets Ups And (Edgar et al.) • 2000: first planet by transit method HD 209458 b (Charbonneau et al.) • 2001: atmosphere of HD 209458 b (Charbonneau et al.) • 2002: astrometry applied to Gliese 876 (Benedict et al.) • 2005: first planet by direct imaging GQ Lupi b (Neuhäuser et al.) • 2006: Earthlike planet by gravitational microlensing (Beaulieu et al.) • 2007: Gliese 581d, small exoplanet near habitability zone (Selsis et al.) • 2009: Gliese 581e, smallest exoplanet with 1.9 Earth masses (Mayor et al.) • As of 7 June 2009: 349 exoplanets in 296 systems (25 systems with 2 planets, 9 with 3, 2 with 4 and 1 with 5) www.exoplanet.eu Our Solar System 1047 MJ 0.39 AU 0.00314 MJ 1 MJ 0.30 MJ 0.046 MJ 0.054 MJ 1 AU 5.2 AU 9.6 AU 19 AU 30 AU 1 yr 11.9 yr 29.5 yr 84 yr 165 yr Definition Planet IAU 2006: • in orbit around the Sun / star • nearly spherical shape / sufficient mass for hydrostatic equilib. • cleared neighbourhood around its orbit Pluto: dwarf planet, as Ceres Brown