CONAN.utils

Classes

get_orbital_elements
supersampling

Functions

CA_08_PCmodel(phi, Fd, C1, D1, C2, D2)	Calculate the phase curve of a planet using the Cowan & Agol 2008 model.
Tdur_to_aR(Tdur, b, Rp, P[, e, w, tra_occ])	convert transit duration to scaled semi-major axis
_get_Tconjunctions(t, t0, per[, ecc, omega, Rstar, ...])	Get the time of conjunctions (transit and eclipse) for the given time array.
aR_to_Tdur(aR, b, Rp, P[, e, w, tra_occ, total])	convert scaled semi-major axis to transit duration in days
aR_to_rho(P, aR[, e, w, qm])	Compute the transit derived stellar density from the planet period and scaled semi major axis.
bin_data(t, f[, err, statistic, bins])	Bin data in time.
bin_data_with_gaps(t, f[, e, statistic, binsize, ...])	split t into chunks with gaps larger than gap_threshold*bin_size
convert_LD(coeff1, coeff2[, conv])	convert quadratic limb darkening coefficients between different parameterizations.
convert_rho(rho[, ecc, w, conv])	convert true stellar density to transit derived density or vice-versa
cosine_atm_variation(phi[, Fd, Fn, delta_deg, ...])	Calculate the phase curve of a planet approximated by a cosine function from Fmin to Fmax
decontaminate(F, contam_frac)	decontaminate flux F following prescription by eq. 8 of kipping & Tinetti https://doi.org/10.1111/j.1365-2966.2010.17094.x
doppler_boosting_signal(phi[, A_db])	Calculate the Doppler boosting signal of a planet as a function of phase angle.
ecc_om_par(ecc, omega[, conv_2_obj, return_tuple])	This function calculates the prior values and limits for the eccentricity and omega parameters,
ellipsoidal_variation_signal(phi[, A_ev, f1_ev, inc_rad])	Calculate the ellipsoidal variation signal of a planet as a function of phase angle.
esolve(M, ecc)	Solve Kepler's equation M = E - ecc.sin(E), returning the eccentric anomaly.
gauss_atm_variation(phi[, A, delta_deg, width_deg])
get_T0s(t, t_ref, P)	get the transit times of a light curve
get_Tconjunctions(t, t0, per[, ecc, omega, Rstar, aR, ...])	Get the time of conjunctions (transit and eclipse) for the given time array.
get_transit_time(t, per, t0)	Get the transit time within a light curve.
impact_parameter(inc, a[, e, w, tra_occ])	Function to convert inclination in degrees to impact parameter b.
inclination(b, a[, e, w, tra_occ])	Function to convert impact parameter b to inclination in degrees.
ingress_duration(aR, b, Rp, P[, e, w, tra_occ])	Compute the ingress duration of transit or occultation in units of P
jitter_estimate(f, e)	Estimate the jitter of a light curve
k_to_Mp(k, P, Ms, i, e[, Mp_unit])	Compute the mass of a planet from the rv semi amplitude following https://iopscience.iop.org/article/10.1086/529429/pdf
lambertian_atm_variation(phi[, Fd, Fn, delta_deg, ...])	Calculate the phase curve of a planet approximated by a lambertian function.
light_travel_time_correction(t, t0, aR, P, inc, Rstar)	Corrects the time array for light travel time effects i.e subtracts the light travel time at each time point
outlier_clipping(x, y[, yerr, clip, width, verbose, ...])	Remove outliers using a running median method. Points > clip*M.A.D are removed
phase_fold(t, per, t0[, phase0])	Phase fold a light curve.
rescale0_1(x)	Rescale an array to the range [0,1].
rescale_minus1_1(x)	Rescale an array to the range [-1,1].
rho_to_aR(rho, P[, e, w, qm])	convert stellar density to semi-major axis of planet with a particular period.
rho_to_tdur(rho, b, Rp, P[, e, w, tra_occ, total])	convert stellar density to transit duration in days https://doi.org/10.1093/mnras/stu318
rms_estimate_LC(f)	Estimate the RMS of a light curve
robust_std(data)	Compute the robust standard deviation using the Median Absolute Deviation (MAD).
sesinw_secosw_to_ecc_omega(sesinw, secosw[, angle_unit])	Convert sesinw and secosw to eccentricity and argument of periastron in angle_unit
sinusoid(x[, A, x0, P, n, trig])	Calculate the sinusoidal function y = A*sin(2*pi*(x-x0)/P) or y = A*cos(2*pi*(x-x0)/P) given the parameters.
split_transits([t, P, t_ref, baseline_amount, ...])	Function to split the transits in the data into individual transits and save them in separate files or to remove a certain amount of data points around the transits while keeping them in the original file.
tdur_to_rho(Tdur, b, Rp, P[, e, w, tra_occ])	convert transit duration to stellar density in g/cm^3 https://doi.org/10.1093/mnras/stu318
transit_depth(RpRs, b)	Calculate the area of overlap between two circles (planet and star) given the impact parameter.