Flux_wavelength module

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

Flux_wavelength.main()