Code_files functions

Code_files.Comparison_GO3077 module

This module compares the phase curves observed during the JWST GO 3077 program with the simulations.

Code_files.Comparison_GO3077.load_data(filename, key)

Load the data from the .h5 file.

Parameters:

filename (str) – The path to the .h5 file.
key (str) – The key to access the data in the .h5 file.

Returns:

The data loaded from the file.

Return type:

np.ndarray

Code_files.Comparison_GO3077.main()

Code_files.Comparisons_bare_rocks_atm module

This module is to compare the phase curves of TRAPPIST-1 planets with and without thick atmospheres.

Code_files.Comparisons_bare_rocks_atm.Keplerian = True: Set to True to use Keplerian orbital periods, False for periods modified because of TTVs (not working yet)

Code_files.Comparisons_bare_rocks_atm.do_simulation = False: Set to True if the simulation hasn’t been done yet, False if the phase curves were already saved and you don’t want to redo the simulation

Code_files.Comparisons_bare_rocks_atm.filter = 'F1500W': MIRI filter to use

Code_files.Comparisons_bare_rocks_atm.nb_points = 100000: Number of points in the simulation

Code_files.Comparisons_bare_rocks_atm.planets = 'defgh': Planets to simulate

Code_files.Comparisons_bare_rocks_atm.plot_individual_planets = True: Set to True if you want to plot the individual planets as bare rocks to see their phases, False otherwise

Code_files.Comparisons_bare_rocks_atm.run_comparison(): Runs the comparison of TRAPPIST-1 phase curves with and without thick atmospheres following the previous settings.

Code_files.Comparisons_bare_rocks_atm.save_plots = False: Set to True if you want to save the plots, False otherwise

Code_files.Flux_wavelength module

Code_files.Flux_wavelength.Planck_law(wavelength, T)

Determines the spectral radiance of a black body (in W/m^2 m^-1 sr^-1).

Parameters:

wavelength (float) – the wavelength (in m)
T (float) – the temperature (in K)

Returns:

B

Return type:

float

Code_files.Flux_wavelength.conversion_IS_to_mJy(F, wavelength, dist, R)

Converts the flux density (in W/m^2/m) to mJy.

Parameters:

F (float) – the flux density (in W/m^2/m)
wavelength (float) – the wavelength (in m)
dist (float) – the distance of the object (in m)
R (float) – the radius of the object (in m)

Returns:

F_mJy

Return type:

float

Code_files.Flux_wavelength.conversion_mJy_to_IS(F_mJy, wavelength, dist, R)

Converts the flux density (in mJy) to W/m^2/m.

Parameters:

F_mJy (float) – the flux density (in mJy)
wavelength (float) – the wavelength (in m)flux_T1_sphinx_cut *= QE
dist (float) – the distance of the object (in m)
R (float) – the radius of the object (in m)

Returns:

F

Return type:

float

Code_files.Flux_wavelength.filter(filter_name)

Returns the filter band of the specified filter.

Parameters:: filter_name (str) – the name of the filter
Returns:: filter_band
Return type:: np.ndarray

Code_files.Flux_wavelength.flux_Wm2(F_mJy, lambda_min, lambda_max, dist, R)

Compute the flux of an object in W/m^2 over a range of wavelengths.

Parameters:

F_mJy (float) – the flux density (in mJy)
lambda_min (float) – the minimum wavelength (in m)
lambda_max (float) – the maximum wavelength (in m)
dist (float) – the distance of the object (in m)
R (float) – the radius of the object (in m)

Returns:

F

Return type:

float

Code_files.Flux_wavelength.flux_black_body(lambda_min, lambda_max, T)

Determines the flux of a black body (in W/m^2) over a range of wavelentgths.

Parameters:

lambda_min (float) – the minimum wavelength (in m)
lambda_max (float) – the maximum wavelength (in m)
T (float) – the temperature (in K)

Returns:

F

Return type:

float

Code_files.Flux_wavelength.flux_mJy(F, lambda_min, lambda_max, dist, R)

Compute the flux of an object in mJy over a range of wavelengths.

Parameters:

F (float) – the flux density (in W/m^2/m)
lambda_min (float) – the minimum wavelength (in m)
lambda_max (float) – the maximum wavelength (in m)
dist (float) – the distance of the object (in m)
R (float) – the radius of the object (in m)

Returns:

F_mJy

Return type:

float

Code_files.Flux_wavelength.flux_mJy_array(F_array, lambda_vals, lambda_min, lambda_max, dist, R)

Compute the integrated flux of an object in mJy over a given wavelength range.

Parameters:

F_array (array-like) – Array of flux densities (in W/m^2/m)
lambda_vals (array-like) – Corresponding wavelengths for F_array (in m)
lambda_min (float) – Minimum wavelength for integration (in m)
lambda_max (float) – Maximum wavelength for integration (in m)
dist (float) – Distance to the object (in m)
R (float) – Radius of the object (in m)

Returns:

Integrated flux in mJy

Return type:

float

Code_files.Flux_wavelength.flux_model_interp(l, model='sphinx')

Interpolates the flux of TRAPPIST-1 at a given wavelength from the SPHINX or PHOENIX model.

Parameters:

l (float) – the wavelength (in m)
model (str) – the model to use: ‘sphinx’ or ‘phoenix’ (default: ‘sphinx’)

Returns:

F

Return type:

float

Code_files.Flux_wavelength.flux_planet_miri(filter_name, T_planet)

Returns the flux of the planet in the specified MIRI filter band.

Parameters:

filter_name (str) – the name of the filter
T_planet (float) – the temperature of the planet (in K)

Returns:

F_planet_miri

Return type:

float

Code_files.Flux_wavelength.flux_ratio_black_body(R_planet, R_star, T_star, d, lambda_min, lambda_max)

Determines the flux ratio between the planet and the star as black bodies(in ppm).

Parameters:

F_planet (float) – the flux of the planet (in W/m^2)
F_star (float) – the flux of the star (in W/m^2)
R_planet (float) – the radius of the planet (in m)
R_star (float) – the radius of the star (in m)

Returns:

F_ratio

Return type:

float

Code_files.Flux_wavelength.flux_ratio_miri(filter_name, R_planet, R_star, T_planet)

Returns the flux ratio between the planet and the star in the specified MIRI filter band (in ppm).

Parameters:

filter_name (str) – the name of the filter
R_planet (float) – the radius of the planet (in m)
R_star (float) – the radius of the star (in m)
T_planet (float) – the temperature of the planet (in K)

Returns:

F_ratio_miri

Return type:

float

Code_files.Flux_wavelength.flux_star_miri(filter_name)

Returns the flux of the star TRAPPIST-1 in the specified MIRI filter band using the SPHINX model.

Parameters:: filter_name (str) – the name of the filter
Returns:: F_star
Return type:: float

Code_files.Flux_wavelength.integrate_flux_model_mJy(filter_name, model='sphinx')

Integrates the flux (in mJy) of the SPHINX or PHOENIX model over the specified MIRI filter band.

Parameters:

filter_name (str) – the name of the filter
model (str) – the model to use: ‘sphinx’ or ‘phoenix’ (default: ‘sphinx’)

Returns:

F_miri

Return type:

float

Code_files.Flux_wavelength.main()

Code_files.Flux_wavelength.planet_equilibirium_temperature(T_star, R_star, d, albedo=0.0, redistribution=0.0)

Determines the equilibrium temperature of the day side of a tidally locked planet (in K).

Parameters:

T_star (float) – the effective temperature of the star (in K)
R_star (float) – the radius of the star (in m)
d (float) – the distance between the star and the planet (in m)
albedo (float) – the albedo of the planet (default: 0)
redistribution (float) – the redistribution efficiency between the day side and night side (default: 0)

Returns:

T_eq

Return type:

float

Code_files.Flux_wavelength.quantum_efficiency(filter_name, wavelength)

Returns the quantum efficiency of the specified filter at the given wavelength.

Parameters:

filter_name (str) – the name of the filter
wavelength (float) – the wavelength (in m)

Returns:

QE

Return type:

float

Code_files.JWST_Obs_plot module

Code_files.JWST_Obs_simu module

Code_files.JWST_Obs_simu.phase_curve_visit(planets, redistribution, filter, model, unit, nb_points=10000, Keplerian=True)

Simulates the phase curves of the TRAPPIST-1 planets during JWST visits.

Parameters:

planets (str) – the planets to simulate
redistribution (float) – the redistribution efficiency between the day side and night side (default: 0)
filter (str) – the MIRI filter to use
model (str) – the model to use for the stellar flux. If ‘sphinx’, the flux is computed using the SPHINX model. If ‘phoenix’, the flux is computed using the PHOENIX model.
unit (str) – the unit of the phase curve. If ‘ppm’, the fluxes of the planets will be computed relatively to the stellar flux in ppm. If ‘mJy’, the planetary fluxes will be computed in absolute value in “mJy”. Will be set automatically to ‘mJy’ if the model is ‘phoenix’.
nb_points (int) – the number of points for the phase curves (default: 10000)
Keplerian (bool) – whether to use the Keplerian periods or not (default: True)

Return type:

None

Code_files.MIRI_filter module

This module is to plot MIRI filters’ quantum efficiency.

Code_files.MIRI_filter.plot_filters(): Load MIRI filter data from CSV and plot the quantum efficiency curves for F1280W and F1500W filters. The plot is saved as ‘MIRI_filters.png’ and also displayed.

Code_files.Orbital_motion module

Code_files.Orbital_motion.compute_true_anomaly(nu_0, e, T, t, t_0=0)

Computes the true anomaly with respect to time.

Parameters:

nu_0 (float) – the initial true anomaly (in rad)
e (float) – the eccentricity
T (float) – the orbital period
t (float) – the time passed
t_0 (float) – the initial time (default value: 0)

Returns:

nu_t

Return type:

float

Code_files.Orbital_motion.kepler_equation(E, M, e)

Returns the Kepler equation: M = E - e sin(E)

Parameters:

E (float) – the eccentric anomaly
M (float) – the mean anomaly
e (float) – the eccentricity

Returns:

E - e*np.sin(E) - M

Return type:

float

Code_files.Orbital_motion.main()

Code_files.Orbital_motion.solve_kepler(M, e)

Solve the Kepler equation to find the eccentric anomaly E.

Parameters:

E (float) – the eccentric anomaly
M (float) – the mean anomaly

Returns:

E

Return type:

float

Code_files.Orbital_motion.true_anomaly(E, e)

Computes the true anomaly from the eccentric anomaly and the eccentricity.

Parameters:

E (float) – the eccentric anomaly
e (float) – the eccentricity

Returns:

nu

Return type:

float

Code_files.Phase_curve_TTV module

Code_files.Phase_curve_TTV.main()

Code_files.Phase_curve_TTV.phase_TTV(P_TTV, t0, t_end, transit_peaks, nb_points)

Computes the phase of the planet taking into account the modification of the period due to TTVs starting from the nearest transit peak from t0

Parameters:

P_TTV (numpy.ndarray) – the modified orbital periods of the planet due to the TTVs (in days)
t0 (float) – the initial time (in BJD_TBD - 2450000)
t_end (float) – the final time (in BJD_TBD - 2450000)
transit_peaks (numpy.ndarray) – the peaks of the transits (in BJD_TBD - 2450000)
nb_points (int) – the number of points for the phase curve

Returns:

phases_TTV, t

Return type:

numpy.ndarray, numpy.ndarray

Code_files.Phase_curve_TTV.phase_curve_simulation(t0, nb_days, nb_points=10000, planets='bcdefgh', redistribution=0, filter=None, model='sphinx', unit='ppm', Keplerian=False, total=True, plot=True, save_plot=False, save_txt=False)

Simulates the phase curves of the planets of TRAPPIST-1 for a given number of days starting from t0 taking into account the modified periods due to TTVs. We assume circular orbits as otherwise the code does not manage to solve the Kepler equation to compute the true anomaly due to the modified periods.

Parameters:

t0 (float) – the initial time (in BJD_TBD - 2450000)
nb_days (int) – the number of days to simulate
nb_points (int) – the number of points for the phase curves (default: 10000)
planets (str) – the planets to simulate (default: ‘bcdefgh’)
redistribution (float) – the redistribution efficiency between the day side and night side (default: 0)
filter (str or None) – the filter to use (default: None). If None, the bolometric fluxes, expressed in ppm, are used relatively to the stellar flux with the planets considered as bare rocks.
model (str) – the model to use for the stellar flux (default: ‘sphinx’). If ‘sphinx’, the flux is computed using the SPHINX model. If ‘phoenix’, the flux is computed using the PHOENIX model.
unit (str) – the unit of the phase curve (default: ‘ppm’). If ‘ppm’, the fluxes of the planets will be computed relatively to the stellar flux in ppm. If ‘mJy’, the planetary fluxes will be computed in absolute value in “mJy”. Will be set automatically to ‘mJy’ if the model is ‘phoenix’.
Keplerian (bool) – whether to use the Keplerian periods or not (default: False)
total (bool) – whether to plot the total phase curve or not (default: True)
plot (bool) – whether to plot the phase curves or not (default: True)
save_plot (bool) – whether to save the plot or not (default: False)
save_txt (bool) – whether to save the phase curves as txt files or not (default: False)

Returns:

None

Code_files.Phase_curve_v1 module

Code_files.Phase_curve_v1.flux_planet(F_star)

Determines the flux reemitted by a planet (in W/m^2) from the one it receives from its star considering the planet is a black body.

Parameters:: F_star (float) – the flux received by the planet from its star (in W/m^2)
Returns:: F_planet
Return type:: float

Code_files.Phase_curve_v1.flux_star(L, d)

Determines the flux received from a star (in W/m^2) at a distance d.

Parameters:

L (float) – the star luminosity (in W)
d (float) – the distance (in m)

Returns:

F

Return type:

float

Code_files.Phase_curve_v1.luminosity_planet_dayside(F_planet, R_planet)

Determines the luminosity of the dayside of a planet from the flux it reemits and its radius.

Parameters:

F_planet (float) – the flux reemitted by the planet’s dayside (in W/m^2)
R_planet (float) – the planet radius (in m)

Returns:

L_planet

Return type:

float

Code_files.Phase_curve_v1.main()

Code_files.Phase_curve_v1.phase_angle(omega, nu, i)

Determines the phase angle of a planet from its orbital parameters (in rad).

Parameters:

omega (float) – the argument of pericentre (in rad)
nu (float) – the true anomaly (in rad)
i (float) – the inclination (in rad)

Returns:

alpha

Return type:

float

Code_files.Phase_curve_v1.phase_curve(L_star, L_planet, R_star, R_planet, phase_planet, eclipse)

Determines the phase curve of a planet from its luminosity, its star’s luminosity and its phase function expressed as the ratio between the planet and star’s luminosities in ppm.

Parameters:

L_star (float) – the star luminosity (in W)
L_planet (float) – the planet luminosity (in W)
R_star (float) – the star radius (in m)
R_planet (float) – the planet radius (in m)
phase_planet (float) – the phase function of the planet
eclipse (bool) – True if the planet is in eclipse, False otherwise

Returns:

curve

Return type:

float

Code_files.Phase_curve_v1.phase_function(alpha)

Determines the phase function of a Lambert sphere.

Parameters:: alpha (float) – the phase angle (in rad)
Returns:: g
Return type:: float

Code_files.Phase_curve_v1.phase_planet(t, P, t0=0)

Determines the phase of a planet at a given time.

Parameters:

t (float) – the time (in days)
P (float) – the orbital period (in days)
t0 (float) – the reference time (in days)

Returns:

phase

Return type:

float

Code_files.Phase_curve_v1.star_planet_separation(a, e, nu)

Determines the distance between a planet and its star using its orbital parameters.

Parameters:

a (float) – the semimajor axis (in m)
e (float) – the eccentricity
nu (float) – the true anomaly (in rad)

Returns:

r

Return type:

float

Code_files.Phase_curve_v1.surface_sphere(R)

Determines the surface of a sphere of radius R.

Parameters:: R (float) – the radius (in m)
Returns:: S
Return type:: float

Code_files.Phase_curves_comparison module

Code_files.Phoenix module

PHOENIX Spectrum Generation for star TRAPPIST-1 using pysynphot

Code_files.Phoenix.Ms = 1.5959799999999999e+32: Stellar mass in g

Code_files.Phoenix.P = 1.510826: days orbital period b planet from Agol et al. 2021

Code_files.Phoenix.Rp = 711784800.0000001: cm b planet from Agol et al. 2021

Code_files.Phoenix.Rs = 8292744000.0: Stellar radius planet from Agol et al. 2021 in cm

Code_files.Phoenix.T14 = 1944.0000000000002: transit duration (36 min x 0.9 eff)

Code_files.Phoenix.Teff = 2566: Teff = 2566 +/- 26 K from Agol et al. 2021

Code_files.Phoenix.a = 172638400000.0: cm b planet from Agol et al. 2021

Code_files.Phoenix.dist = 3.8473162e+19: stellar distance in pc, converted to cm

Code_files.Phoenix.e = 0.001: Wang et al. 2017 K2 (Note Luger et al. 2017 K2 data give e = 0.001)

Code_files.Phoenix.generate_phoenix_model()

Generate and save the PHOENIX model spectrum for TRAPPIST-1 using pysynphot.

Creates a PHOENIX stellar model for TRAPPIST-1 with specified parameters.
Normalizes the model to the observed J-band magnitude.
Converts the spectrum to wavelength in microns and flux in mJy (for JWST ETC).
Saves the spectrum to ‘TRAPPIST1_Phoenix_model.txt’.
Plots the spectrum between 10 and 20 microns.

Code_files.Phoenix.logg = 5.189952052020907: cgs

Code_files.Solar_System_constants module

This module contains some constants from Solar System bodies commonly used in exoplanetology.

Code_files.Solar_System_constants.L_Sun = 3.83e+26: Solar luminosity in watts (from Wikipedia)

Code_files.Solar_System_constants.M_Earth = 5.9722e+24: Earth mass in kilograms (from Wikipedia)

Code_files.Solar_System_constants.M_Jupiter = 1.8986e+27: Jupiter mass in kilograms (from Wikipedia)

Code_files.Solar_System_constants.M_Sun = 1.9885e+30: Solar mass in kilograms (from Wikipedia)

Code_files.Solar_System_constants.R_Earth = 6378137.0: Earth equatorial radius in meters (from Wikipedia)

Code_files.Solar_System_constants.R_Jupiter = 71492000.0: Jupiter equatorial radius in meters (from Wikipedia)

Code_files.Solar_System_constants.R_Sun = 696342000.0: Solar equatorial radius in meters (from Wikipedia)

Code_files.TRAPPIST1_parameters module

This module contains some parameters for the planets of the TRAPPIST-1 system.

Code_files.TRAPPIST1_parameters.L_star = 2.104741546874703e+23: Luminosity of star TRAPPIST-1 in Watts (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.M_star = 1.785673e+29: Mass of star TRAPPIST-1 in kilograms (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.P_b = 1.51088432: Orbital period of TRAPPIST-1 b in days (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.P_c = 2.42179346: Orbital period of TRAPPIST-1 c in days (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.P_d = 4.04978035: Orbital period of TRAPPIST-1 d in days (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.P_e = 6.09956479: Orbital period of TRAPPIST-1 e in days (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.P_f = 9.20659399: Orbital period of TRAPPIST-1 f in days (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.P_g = 12.3535557: Orbital period of TRAPPIST-1 g in days (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.P_h = 18.7672745: Orbital period of TRAPPIST-1 h in days (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.R_b = 7118000.892000001: Radius of TRAPPIST-1 b in meters (Agol et al. 2021)

Code_files.TRAPPIST1_parameters.R_c = 6996816.289: Radius of TRAPPIST-1 c in meters (Agol et al. 2021)

Code_files.TRAPPIST1_parameters.R_d = 5025971.956: Radius of TRAPPIST-1 d in meters (Agol et al. 2021)

Code_files.TRAPPIST1_parameters.R_e = 5867886.04: Radius of TRAPPIST-1 e in meters (Agol et al. 2021)

Code_files.TRAPPIST1_parameters.R_f = 6665153.164999999: Radius of TRAPPIST-1 f in meters (Agol et al. 2021)

Code_files.TRAPPIST1_parameters.R_g = 7200916.673: Radius of TRAPPIST-1 g in meters (Agol et al. 2021)

Code_files.TRAPPIST1_parameters.R_h = 4815493.435: Radius of TRAPPIST-1 h in meters (Agol et al. 2021)

Code_files.TRAPPIST1_parameters.R_star = 83003966.4: Radius of star TRAPPIST-1 in meters (Agol et al. 2021)

Code_files.TRAPPIST1_parameters.T_eff_star = 2566: Effective temperature of star TRAPPIST-1 in Kelvin (Agol et al. 2021)

Code_files.TRAPPIST1_parameters.a_b = 1670869843.632: Semi-major axis of TRAPPIST-1 b in meters (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.a_c = 2288419353.6480002: Semi-major axis of TRAPPIST-1 c in meters (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.a_d = 3224704094.6400003: Semi-major axis of TRAPPIST-1 d in meters (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.a_e = 4233202286.4: Semi-major axis of TRAPPIST-1 e in meters (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.a_f = 5569566145.44: Semi-major axis of TRAPPIST-1 f in meters (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.a_g = 6781424054.880001: Semi-major axis of TRAPPIST-1 g in meters (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.a_h = 8956127974.560001: Semi-major axis of TRAPPIST-1 h in meters (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.dist_system = 3.8358636856984774e+17: Distance between the TRAPPIST-1 system and the Solar system in meters (from NASA Exoplanet Archive)

Code_files.TRAPPIST1_parameters.e_b = 0.00622: Orbital eccentricity of TRAPPIST-1 b (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.e_c = 0.00654: Orbital eccentricity of TRAPPIST-1 c (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.e_d = 0.00837: Orbital eccentricity of TRAPPIST-1 d (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.e_e = 0.00051: Orbital eccentricity of TRAPPIST-1 e (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.e_f = 0.01007: Orbital eccentricity of TRAPPIST-1 f (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.e_g = 0.00208: Orbital eccentricity of TRAPPIST-1 g (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.e_h = 0.00567: Orbital eccentricity of TRAPPIST-1 h (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.flux_T1_phoenix_mJy = array([5.23820679e-107, 5.24895784e-107, 5.25973095e-107, ..., 1.21781009e-001, 1.16229755e-001, 1.13663120e-001]): Stellar flux of TRAPPIST-1 in mJy from the PHOENIX spectrum model

Code_files.TRAPPIST1_parameters.flux_T1_sphinx = array([3.90774100e+10, 4.77147922e+10, 5.01808734e+10, ..., 5.52572215e+07, 5.43826188e+07, 0.00000000e+00]): Wavelengths (m) and flux from SPHINX model spectrum of star TRAPPIST-1

Code_files.TRAPPIST1_parameters.i_b = 1.5582299561805375: Orbital inclination of TRAPPIST-1 b in radians (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.i_c = 1.5615460817593265: Orbital inclination of TRAPPIST-1 c in radians (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.i_d = 1.5646876744129166: Orbital inclination of TRAPPIST-1 d in radians (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.i_e = 1.5649145672156757: Orbital inclination of TRAPPIST-1 e in radians (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.i_f = 1.5649669270932354: Orbital inclination of TRAPPIST-1 f in radians (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.i_g = 1.5655254324538737: Orbital inclination of TRAPPIST-1 g in radians (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.i_h = 1.5666598964676701: Orbital inclination of TRAPPIST-1 h in radians (Ducrot et al. 2020)

Code_files.TRAPPIST1_parameters.omega_b = 5.879316118268099: Argument of periastron of TRAPPIST-1 b in radians (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.omega_c = 4.9296824722579835: Argument of periastron of TRAPPIST-1 c in radians (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.omega_d = -0.15236724369910498: Argument of periastron of TRAPPIST-1 d in radians (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.omega_e = 1.891413310386255: Argument of periastron of TRAPPIST-1 e in radians (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.omega_f = 6.436948814280287: Argument of periastron of TRAPPIST-1 f in radians (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.omega_g = 3.33951299076595: Argument of periastron of TRAPPIST-1 g in radians (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.omega_h = 5.915269900859182: Argument of periastron of TRAPPIST-1 h in radians (Grimm et al. 2018)

Code_files.TRAPPIST1_parameters.wavelengths_T1_phoenix = array([1.25892541e-09, 1.26021668e-09, 1.26150927e-09, ..., 7.76142810e-05, 7.76194962e-05, 7.76247117e-05]): Wavelengths from the PHOENIX model spectrum of star TRAPPIST-1 in meters

Code_files.TRAPPIST1_parameters.wavelengths_T1_sphinx = array([4.00000509e-07, 4.00008509e-07, 4.00016509e-07, ..., 3.00285286e-05, 3.00291291e-05, 3.00297297e-05]): Wavelengths from the SPHINX model spectrum of star TRAPPIST-1 in meters

Code_files.TTV module

Code_files.TTV.main()

Code_files.TTV.period_TTV(P, transit_start, transit_end)

Computes the modified orbital periods (in days) of the planet due to the TTVs

Parameters:

P (float) – the initial period of the planet without TTVs (in days)
transit_start (numpy.ndarray) – the start of the transit (in days)
transit_end (numpy.ndarray) – the end of the transit (in days)

Returns:

P_TTV

Return type:

numpy.ndarray

Code_files.TTV.transit_peak(transit_start, transit_end)

Computes the peak of the transit (in days)

Parameters:

transit_start (numpy.ndarray) – the start of the transit (in days)
transit_end (numpy.ndarray) – the end of the transit (in days)

Returns:

transit_peak

Return type:

numpy.ndarray

Code_files.Transits module

Code_files.Transits.eclipse(P, a, R_star, R_planet, i, phase, e, omega, b)

Determines if an exoplanet is in eclipse or not at a given phase.

Parameters:

P (float) – the orbital period (in s)
a (float) – the semimajor axis (in m)
R_star (float) – the radius of the star (in m)
R_planet (float) – the radius of the planet (in m)
i (float) – the inclination (in rad)
phase (float) – the phase of the exoplanet (in rad)
e (float) – the eccentricity
omega (float) – the argument of pericentre (in rad)
b (float) – the impact parameter

Returns:

in_eclipse

Return type:

bool

Code_files.Transits.eclipse_impact_parameter(a, i, e, R_star, omega)

Determines the impact parameter of an exoplanet eclipse.

Parameters:

a (float) – the semimajor axis (in m)
i (float) – the inclination (in rad)
e (float) – the eccentricity
R_star (float) – the radius of the star (in m)
omega (float) – the argument of pericentre (in rad)

Returns:

b

Return type:

float

Code_files.Transits.eclipse_phase(P, a, R_star, R_planet, i, e, omega, b)

Determines the phases of an exoplanet for which its secondary eclipse starts and ends (centered at 0 or 1).

Parameters:

P (float) – the orbital period (in s)
a (float) – the semimajor axis (in m)
R_star (float) – the radius of the star (in m)
R_planet (float) – the radius of the planet (in m)
i (float) – the inclination (in rad)
e (float) – the eccentricity
omega (float) – the argument of pericentre (in rad)
b (float) – the impact parameter

Returns:

phase_eclipse_start, phase_eclipse_end

Return type:

float

Code_files.Transits.flat_eclipse_duration(P, a, R_star, R_planet, i, e, omega, b)

Determines the flat duration of an exoplanet eclipse (in s).

Parameters:

P (float) – the orbital period (in s)
a (float) – the semimajor axis (in m)
R_star (float) – the radius of the star (in m)
R_planet (float) – the radius of the planet (in m)
i (float) – the inclination (in rad)
e (float) – the eccentricity
omega (float) – the argument of pericentre (in rad)
b (float) – the eclipse impact parameter

Returns:

t_flat

Return type:

float

Code_files.Transits.flat_transit_duration(P, a, R_star, R_planet, i, e, omega, b)

Determines the flat duration of an exoplanet transit (in s).

Parameters:

P (float) – the orbital period (in s)
a (float) – the semimajor axis (in m)
R_star (float) – the radius of the star (in m)
R_planet (float) – the radius of the planet (in m)
i (float) – the inclination (in rad)
e (float) – the eccentricity
omega (float) – the argument of pericentre (in rad)
b (float) – the transit impact parameter

Returns:

t_flat

Return type:

float

Code_files.Transits.main()

Code_files.Transits.total_eclipse_duration(P, a, R_star, R_planet, i, e, omega, b)

Determines the total duration of an exoplanet eclipse (in s).

Parameters:

P (float) – the orbital period (in s)
a (float) – the semimajor axis (in m)
R_star (float) – the radius of the star (in m)
R_planet (float) – the radius of the planet (in m)
i (float) – the inclination (in rad)
e (float) – the eccentricity
omega (float) – the argument of pericentre (in rad)
b (float) – the eclipse impact parameter

Returns:

t_total

Return type:

float

Code_files.Transits.total_transit_duration(P, a, R_star, R_planet, i, e, omega, b)

Determines the total duration of an exoplanet transit (in s).

Parameters:

P (float) – the orbital period (in s)
a (float) – the semimajor axis (in m)
R_star (float) – the radius of the star (in m)
R_planet (float) – the radius of the planet (in m)
i (float) – the inclination (in rad)
e (float) – the eccentricity
omega (float) – the argument of pericentre (in rad)
b (float) – the transit impact parameter

Returns:

t_total

Return type:

float

Code_files.Transits.transit(P, a, R_star, R_planet, i, phase, e, omega, b, t)

Determines if an exoplanet is in transit or not at a given phase.

Parameters:

P (float) – the orbital period (in s)
a (float) – the semimajor axis (in m)
R_star (float) – the radius of the star (in m)
R_planet (float) – the radius of the planet (in m)
i (float) – the inclination (in rad)
phase (function) – the phase of the exoplanet (in rad)
e (float) – the eccentricity
omega (float) – the argument of pericentre (in rad)
b (float) – the impact parameter
t (float) – time (in days)

Returns:

in_transit

Return type:

bool

Code_files.Transits.transit_depth(R_planet, R_star)

Determines the depth of an exoplanet transit.

Parameters:

R_planet – the radius of the planet (in m)
R_star (float) – the radius of the star (in m)

Returns:

delta_F

Return type:

float

Code_files.Transits.transit_impact_parameter(a, i, e, R_star, omega)

Determines the impact parameter of an exoplanet transit.

Parameters:

a (float) – the semimajor axis (in m)
i (float) – the inclination (in rad)
e (float) – the eccentricity
R_star (float) – the radius of the star (in m)
omega (float) – the argument of pericentre (in rad)

Returns:

b

Return type:

float