transit analysis package zach gazak john tonry john johnson
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Transit Analysis Package
Zach Gazak
John Tonry
John Johnson
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Extrasolar Planets
1992: First discovered (pulsar timing variations)
1995: First orbiting Main Sequence star (radial velocity)
1999: First photometric transit light curve:
(Charbonneau et al. 2000)
Transiting Extrasolar Planets
~80 transiting exoplanets
Transits give us access to the geometry of the system
(Charbonneau et al. 2000)
NASA
Modeling Transit Photometry
Analytic light curve of (Mandel & Agol 2002)
Period, Inclination, Rp, a, Rs, e, ω, Tmid, limb darkening
Inclination, Rp/Rs, a/Rs:
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Parameter Statistics: MCMC
Markov Chain Monte Carlo
Gives access to Bayesian probability distribution
model x0
trial state x’
Likelihood: –χ
‾2~exp[ ]
ℒ’
ℒ’
ℒ0
⎯
meets Jump probability?
Parameter Statistics: MCMC
Markov Chain Monte Carlo
Gives access to Bayesian probability distribution
model x0trial state x’
More likely states always selected, but MCMC can explore.
. . . xN
Is the “Classic” MCMC Enough?
Most light curves show correlated “red” noise:
But “classic” MCMC is not able to compensate.
Red Noise FilteringHow “Likely” is the noise described by a (σwhite, σred) pair?
(Carter & Winn 2009)
Maximize that “Wavelet Likelihood”:
Wavelet Basis MCMC
Wavelet decompose residuals (data - model fit)
Use wavelet likelihood instead of “Classic”
Wavelet Basis MCMC
For contaminated data, “Classic” MCMC is insufficient!
Severely underestimates probability distributions.
“True” value Classic
Wavelet