primary transit observations of the hot jupiter hd189733b
DESCRIPTION
Primary transit observations of the hot Jupiter HD189733b. Jean-Philippe Beaulieu (IAP) Giovanna Tinetti (UCL) Sean Carey (SSC, IPAC) Ignasi Ribas (CSIC-IEEC) Mao-Chang Liang, Yuk Yung (CALTECH) Robert Barber, Jonathan Tennyson (UCL) Nicole Alard, David Sing (IAP) - PowerPoint PPT PresentationTRANSCRIPT
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Primary transit observations of the hot Jupiter HD189733b
Jean-Philippe Beaulieu (IAP)Giovanna Tinetti (UCL)Sean Carey (SSC, IPAC)Ignasi Ribas (CSIC-IEEC) Mao-Chang Liang, Yuk Yung (CALTECH)Robert Barber, Jonathan Tennyson (UCL)Nicole Alard, David Sing (IAP)Franck Selsis (ENS Lyon)
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Primary transit photometry Primary transit photometry
Brillance
Charbonneau et al., 2002; Vidal-Madjar et al., 2003, 2004;Richardson et al., 2006; Ballester, Sing, Herbert, 2007;Knutson et al., 2006, 2007; Beaulieu et al., 2007
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Brillance 1
23
Charbonneau et al., 2002; Vidal-Madjar et al., 2003, 2004;Richardson et al., 2006; Ballester, Sing, Herbert, 2007;Knutson et al., 2006, 2007; Beaulieu et al., 2007
Primary transit photometry Primary transit photometry
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Transmission spectroscopy and emission spectroscopy (primary-secondary transits) are two complementary techniques to probe exoplanetary atmospheres
Primary transits -> molecular abundances, clouds
Secondary transits -> T-P profiles, clouds
Ideally you want to use both!!!
To have a better understanding of the atmospheric processes, we need a broad wavelength range
Hot-Jupiters in transit
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Photochemistry prediction
(Liang et al., 2003,2004)
Tinetti, Liang, et al., ApjL, 2007
CO & H2O
Water and CO in extrasolar planets
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C/O < solar
C/O = solar
C/O > solar
Tinetti, et al., ApjL, 2007
Predicted transmission spectra of HD189733
Predicted difference 3.6-5.8 μm = 0.05 %
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SPITZER OBSERVATIONS
4.5 hours on October 31, 2006 at 3.6 and 5.8 μm33 hours on November 2, 8 μm (Knutson et al., 2007, Nature)
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SPITZER 5.8 μm, (channel 3)
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SPITZER 3.6 μm, (channel 1)
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We must beat down systematics !
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Correcting for pixel phase effects
Morales-Calderon et al., 2006, IRAC handbook
Flux Correction= f(distance to pixel-center)
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Estimating systematic trends from the data
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MODELING THE LIGHT CURVE &
LIMB DARKENING
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3.6 μm, LD-uniform = 0.027 %
5.8 μm, LD-uniform = 0.021 %
3.6 - 5.8 μm = 0.080 % (Uniform)3.6 - 5.8 μm = 0.074 % (LD)
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HD189733, a spotted star
Winn et al., 2007, opticalPont et al., 2007, HST, 0.8 μm
Being a K star T~5000 K, it is not a surprise
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An extreme spotted star model (Ribas)
Star a K star 20 % of the star covered with 1000 K cooler spots
In this extreme case : •Transit depth smaller by 0.58 % in the visible• Transit depth smaller by 0.19 % at 3.6 μm• Transit depth smaller by 0.18 % at 5.8 μm
Differential effect 3.6 – 5.8 μm = 0.01 %Differential effect visible - 3.6 μm = 0.39 %
Spots contribution is critical for optical – IR comparisonSpots contribution is critical for optical – IR comparisonDifferential effects at 3.6 – 5.8 Differential effects at 3.6 – 5.8 μμm are smallm are small
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Measured transit depths at 3.6, 5.8, 8 μm
Knutson et al. 2007 measurement at 8 μm (uniform source) = 2.38 ± 0.02 %
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Trasmission spectrum from the VIS to the far-IR
Na
K
H2-H2
H2O
Tinetti et al., Nature 448, 163
Abs. coeff.:(Allard N.,2006; Barber2006;Borisow et al., )
T-P profileIro et al., 2005Burrows et al., 2006
Richardson et al., 2006
Charbonneau et al., 2002Knuthson et al., 2007a
Knutson et al., 2007
Winn et al., 2007
Beaulieu et al. 2007
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First detection of water vapor
Isotherme à 500 K
Isotherme à 2000 K
TP profils TP with terminator (Burrows et al. 2006)
Tinetti et al., Nature 448, 163
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CONCLUSION• Water vapor has been detected by primary transit observation (3.6, 5.8
and 8 μm)
• In agreement with predictions and photochemistry models
• Possible to do high precision photometry with SPITZER
• HD209458, 20 hours of Spitzer observations scheduled in December (WETWORLD, Tinetti et al.)
Tinetti et al., Nature 448, 163Beaulieu et al., ApJ submitted
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Predicted T-P profiles Predicted T-P profiles for day/night sidesfor day/night sides
Burrows et al., 2006
T (K)
T (K)P (b
ar)
P (b
ar)
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Secondary transit: Secondary transit: simulated emission spectrasimulated emission spectra
Simulated emission spectrum,No clouds
Isothermal profile @ ~ 1800 K
Clouds @ 10-2-10-3 bars
Tinetti et al., Nature, 2007
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