CONAN._classes.load_lightcurves.phasecurve

CONAN._classes.load_lightcurves.phasecurve#

CONAN._classes.load_lightcurves.phasecurve(D_occ=0, Fn=None, ph_off=None, A_ev=0, f1_ev=0, A_db=0, pc_model='cosine', verbose=True)#

Setup phase curve parameters for each unique filter in loaded lightcurve. use ._filnames attribute to see the unique filter order. Fn and ph_off are set to None by default which means the planet’s phase variation is not included in the model (so we have just the occultation model if Docc is given). setting Fn and ph_off to a value, even if fixed to zero turns on the phase variation model.

Parameters:

  • D_occ (float, tuple, list;) – Observed occultation depth in ppm. This may be different from the total dayside flux due to inclination. Default is 0.

  • Fn (float, tuple, list,None;) – Planet Nightside flux in ppm. Default is None which implies that a phase curve model is not included

  • ph_off (float, tuple,list;) – Offset of the hotspot in degrees. Default is None.

  • A_ev (float, tuple, list;) – semi-amplitude of ellipsoidal variation in ppm. Default is 0.

  • f1_ev (float, tuple, list;) – fractional constant of the ellipsoidal variation signal. values should range between 0 and 1. see eq.8 of Esteves 2013 (https://iopscience.iop.org/article/10.1088/0004-637X/772/1/51)

  • A_db (float, tuple, list;) – semi-amplitude of Doppler boosting in ppm. Default is 0.

  • pc_model (str;) – select the function form for the planet phase variation. can be either “cosine” for a pure cosine function or “lambert” for a lambertian function.

  • verbose (bool;) – print output. Default is True.

_model_phasevar#

list of bools indicating whether the phase variation model is included for each filter.

Type:

list;

_PC_dict#

dictionary of phase curve parameters for each filter.

Type:

dict;

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