Closed wmorning closed 7 years ago
Model will be tested on Kepler 36b/c, as we have a signal from those.
Functions now exist to both optimize for the TTV parameters, as well as to perform inference on these parameters, while marginalizing over all Transit parameters such as limb darkening.
These parameters are the results of DE after running for 400 steps (constrainable parameters are constrained to within 0.0001), so these can be given to an MCMC. The product of the transit models from 36b and 36c can still be fit to the data, to constrain all parameters simultaneously. We can decide if we want to do this or not.
Kepler 36b TTV model parameters: [ 2.43553689e+00 1.62320789e+01 1.86189482e-02 1.22919833e+01 9.10712940e+01 2.37060456e-01 9.08356010e+01 2.97214034e-01 1.06218302e+00 8.36455895e-02 2.76683559e+01 5.12695478e+00]
Kepler 36c TTV model parameters: [ 7.35239232e+00 1.38488717e+01 8.75890594e-03 2.33701260e+01 9.01098174e+01 -1.66380149e-03 8.93217198e+01 1.16790294e+00 -2.08614380e+00 -1.23818107e-01 3.24483290e+01 5.15539155e+00]
Write code to model TTV signal.