Syntax:
-MandelAgolTransit <bls | blsfixper | P0 T00 r0 a0 <"i" inclination | "b" bimpact> e0 omega0 mconst0> <"quad" | "nonlin"> ldcoeff1_0 ... ldcoeffn_0 fitephem fitr fita fitinclterm fite fitomega fitmconst fitldcoeff1 ... fitldcoeffn fitRV [RVinputfile RVmodeloutfile K0 gamma0 fitK fitgamma] correctlc omodel [model_outdir] Example 1.$ ./vartools -i EXAMPLES/3.transit -oneline \ -BLS q 0.01 0.1 0.5 5.0 20000 200 7 1 0 0 0 \ -MandelAgolTransit bls quad 0.3471 0.3180 \ 1 1 1 1 0 0 1 0 0 0 0 1 EXAMPLES/OUTDIR1 Name = EXAMPLES/3.transit BLS_Period_1_0 = 2.12312625 BLS_Tc_1_0 = 53727.297046247397 BLS_SN_1_0 = 38.39425 BLS_SR_1_0 = 0.00237 BLS_SDE_1_0 = 4.77204 BLS_Depth_1_0 = 0.01136 BLS_Qtran_1_0 = 0.03000 BLS_i1_1_0 = 0.98500 BLS_i2_1_0 = 1.01000 BLS_deltaChi2_1_0 = -24130.93833 BLS_fraconenight_1_0 = 0.42662 BLS_Npointsintransit_1_0 = 146 BLS_Ntransits_1_0 = 4 BLS_Npointsbeforetransit_1_0 = 106 BLS_Npointsaftertransit_1_0 = 120 BLS_Rednoise_1_0 = 0.00156 BLS_Whitenoise_1_0 = 0.00490 BLS_SignaltoPinknoise_1_0 = 12.89679 BLS_Period_invtransit_0 = 1.14599569 BLS_deltaChi2_invtransit_0 = -3289.67397 BLS_MeanMag_0 = 10.16740 MandelAgolTransit_Period_1 = 2.12328176 MandelAgolTransit_T0_1 = 53727.29695831 MandelAgolTransit_r_1 = 0.09789 MandelAgolTransit_a_1 = 9.35954 MandelAgolTransit_bimpact_1 = 0.33094 MandelAgolTransit_inc_1 = 87.97368 MandelAgolTransit_e_1 = 0.00000 MandelAgolTransit_omega_1 = 0.00000 MandelAgolTransit_mconst_1 = 10.16687 MandelAgolTransit_ldcoeff1_1 = 0.34710 MandelAgolTransit_ldcoeff2_1 = 0.31800 MandelAgolTransit_chi2_1 = 27.06054
Use -BLS to identify a transit signal in the light curve EXAMPLES/3.transit and fit a Mandel-Agol transit model to it. For the -MandelAgolTransit command we indicate that the initial parameter values should be determined based on the results from the -BLS command. We use a quadratic limb-darkening law, with parameters 0.3471 and 0.3180. We set flags to vary the ephemeris (P and T0), Rp/R*, a/R* and the impact parameter. We do not vary either the eccentricity or argument of periastron. We vary the mean out-of-transit magnitude, and we do not vary either of the limb-darkening coefficients. We do not fit and RV curve or subtract the best-fit model from the light curve. We output the best-fit model to the directory EXAMPLES/OUTDIR1 (the filename will be EXAMPLES/OUTDIR1/3.transit.mandelagoltransit.model.
Fig 1. Fit of a Mandel-Agol transit model to the light curve in Example 1.