Source code for lezargus.library.atmosphere

"""Atmospheric functions and other operations.

This file keeps track of all of the functions and computations which deal
with the atmosphere.
"""

import astropy.modeling
import numpy as np

from lezargus import library
from lezargus.library import hint
from lezargus.library import logging


[docs]def airmass(zenith_angle: float | hint.ndarray) -> float | hint.ndarray: """Calculate the airmass from the zenith angle. This function calculates the airmass provided a zenith angle. For most cases the plane-parallel atmosphere method works, and it is what this function uses. However, we also use a more accurate formula for airmass at higher zenith angles (>80 degree), namely from DOI:10.1364/AO.28.004735. We use a weighted average between 75 < z < 80 degrees to allow for a smooth transition. Parameters ---------- zenith_angle : float or ndarray The zenith angle, in radians. Returns ------- airmass_ : float or ndarray The airmass. The variable name is to avoid name conflicts. """ # The bounds of the spline region. low_spline_deg = 75 high_spline_deg = 80 # For the Kasten Young 1989 equation, we need the zenith angle in degrees. zenith_angle_degree = np.rad2deg(zenith_angle) # We either use the faster secant version for zenith angles. secant_airmass = 1 / np.cos(zenith_angle) kasten_young_airmass = 1 / ( np.cos(zenith_angle) + 0.50572 * (6.07995 + 90 - zenith_angle_degree) ** (-1.6364) ) # The two modes of calculation. airmass_ = np.where( zenith_angle_degree <= high_spline_deg, secant_airmass, kasten_young_airmass, ) # Creating the average splice between the two regions. splice_index = (zenith_angle_degree >= low_spline_deg) & ( zenith_angle_degree <= high_spline_deg ) kasten_young_weights = ( zenith_angle_degree[splice_index] - low_spline_deg ) / 5.0 secant_weights = 1 - kasten_young_weights airmass_[splice_index] = (secant_airmass[splice_index] * secant_weights) + ( kasten_young_airmass[splice_index] * kasten_young_weights ) # All done. return airmass_
[docs]def index_of_refraction_ideal_air(wavelength: hint.ndarray) -> hint.ndarray: """Calculate the ideal refraction of air over wavelength. The index of refraction of air depends slightly on wavelength, we use the updated Edlen equations found in DOI: 10.1088/0026-1394/30/3/004. Parameters ---------- wavelength : ndarray The wavelength that we are calculating the index of refraction over. This must in microns. Returns ------- ior_ideal_air : ndarray The ideal air index of refraction. """ # The wave number is actually used more in these equations. wavenumber = 1 / wavelength # Calculating the index of refraction, left hand then right hand side of # the equation. ior_ideal_air = ( 8342.54 + 2406147 / (130 - wavenumber**2) + 15998 / (38.9 - wavenumber**2) ) ior_ideal_air = ior_ideal_air / 1e8 + 1 return ior_ideal_air
[docs]def index_of_refraction_dry_air( wavelength: hint.ndarray, pressure: float, temperature: float, ) -> hint.ndarray: """Calculate the refraction of air of pressured warm dry air. The index of refraction depends on wavelength, pressure and temperature, we use the updated Edlén equations found in DOI: 10.1088/0026-1394/30/3/004. Parameters ---------- wavelength : ndarray The wavelength that we are calculating the index of refraction over. This must in microns. pressure : float The pressure of the atmosphere, in Pascals. temperature : float The temperature of the atmosphere, in Kelvin. Returns ------- ior_dry_air : ndarray The dry air index of refraction. """ # We need the ideal air case first. ior_ideal_air = index_of_refraction_ideal_air(wavelength=wavelength) # The Edlén equations use Celsius as the temperature unit, we need to # convert from the standard Kelvin. temperature = temperature - 273.15 if temperature < 0: logging.warning( warning_type=logging.AccuracyWarning, message=( "The temperature specified for the Edlén equation for the index" " of refraction is lower than 0 C. The applicability is of this" " temperature is unknown." ), ) # Calculating the pressure and temperature term. pt_factor = (pressure / 96095.43) * ( (1 + pressure * (0.601 - 0.009723 * temperature) * 1e-8) / (1 + 0.003661 * temperature) ) # Calculating the index of refraction of dry air. ior_dry_air = (ior_ideal_air - 1) * pt_factor ior_dry_air = ior_dry_air + 1 return ior_dry_air
[docs]def index_of_refraction_moist_air( wavelength: hint.ndarray, temperature: float, pressure: float, water_pressure: float, ) -> hint.ndarray: """Calculate the refraction of air of pressured warm moist air. The index of refraction depends on wavelength, pressure, temperature, and humidity, we use the updated Edlen equations found in DOI: 10.1088/0026-1394/30/3/004. We use the partial pressure of water in the atmosphere as opposed to actual humidity. Parameters ---------- wavelength : ndarray The wavelength that we are calculating the index of refraction over. This must in microns. temperature : float The temperature of the atmosphere, in Kelvin. pressure : float The pressure of the atmosphere, in Pascals. water_pressure : float The partial pressure of water in the atmosphere, Pascals. Returns ------- ior_moist_air : ndarray The moist air index of refraction. """ # The wave number is actually used more in these equations. wavenumber = 1 / wavelength # We need the dry air case first. ior_dry_air = index_of_refraction_dry_air( wavelength=wavelength, pressure=pressure, temperature=temperature, ) # Calculating the water vapor factor. wv_factor = ( -1 * water_pressure * (3.7345 - 0.0401 * wavenumber**2) * 1e-10 ) # Computing the moist air index of refraction. ior_moist_air = ior_dry_air + wv_factor return ior_moist_air
[docs]def absolute_atmospheric_refraction_function( wavelength: hint.ndarray, zenith_angle: float, temperature: float, pressure: float, water_pressure: float, ) -> hint.Callable[[hint.ndarray], hint.ndarray]: """Compute the absolute atmospheric refraction function. The absolute atmospheric refraction is not as useful as the relative atmospheric refraction function. To calculate how the atmosphere refracts one's object, use that function instead. Parameters ---------- wavelength : ndarray The wavelength over which the absolute atmospheric refraction is being computed over, in microns. zenith_angle : float The zenith angle of the sight line, in radians. temperature : float The temperature of the atmosphere, in Kelvin. pressure : float The pressure of the atmosphere, in Pascals. water_pressure : float The partial pressure of water in the atmosphere, Pascals. Returns ------- abs_atm_refr_func : Callable The absolute atmospheric refraction function, as an actual callable function. """ # We need to determine the index of refraction for moist air. ior_moist_air = index_of_refraction_moist_air( wavelength=wavelength, pressure=pressure, temperature=temperature, water_pressure=water_pressure, ) # The constant of refraction. const_of_refr = (ior_moist_air**2 - 1) / (2 * ior_moist_air**2) # Incorporating the zenith angle. abs_atm_refr = const_of_refr * np.tan(zenith_angle) # Creating the function itself. abs_atm_refr_func = library.wrapper.cubic_1d_interpolate_factory( x=wavelength, y=abs_atm_refr, ) return abs_atm_refr_func
[docs]def relative_atmospheric_refraction_function( wavelength: hint.ndarray, reference_wavelength: float, zenith_angle: float, temperature: float, pressure: float, water_pressure: float, ) -> hint.Callable[[hint.ndarray], hint.ndarray]: """Compute the relative atmospheric refraction function. The relative refraction function is the same as the absolute refraction function, however, it is all relative to some specific wavelength. Parameters ---------- wavelength : ndarray The wavelength over which the absolute atmospheric refraction is being computed over, in microns. reference_wavelength : float The reference wavelength which the relative refraction is computed against, in microns. zenith_angle : float The zenith angle of the sight line, in radians. temperature : float The temperature of the atmosphere, in Kelvin. pressure : float The pressure of the atmosphere, in Pascals. water_pressure : float The partial pressure of water in the atmosphere, Pascals. Returns ------- rel_atm_refr_func : Callable The absolute atmospheric refraction function, as an actual callable function. """ # We need the absolute refraction function first. abs_atm_refr_func = absolute_atmospheric_refraction_function( wavelength=wavelength, zenith_angle=zenith_angle, pressure=pressure, temperature=temperature, water_pressure=water_pressure, ) # The refraction at the reference wavelength. ref_abs_refr = abs_atm_refr_func(reference_wavelength) def rel_atm_refr_func(wave: hint.ndarray) -> hint.ndarray: """Relative refraction function. Parameters ---------- wave : ndarray The input wavelength for computation. Returns ------- rel_atm_refr : ndarray The relative atmospheric refraction. """ rel_atm_refr = abs_atm_refr_func(wave) - ref_abs_refr return rel_atm_refr # All done. return rel_atm_refr_func
[docs]def gaussian_psf_kernel( shape: tuple, x_stddev: float, y_stddev: float, rotation: float, ) -> hint.ndarray: """Return a 2D Gaussian point spread function convolution kernel. We normalize the point spread function via the amplitude of the Gaussian function as a whole for maximal precision: volume = 1. We require the input of the shape of the kernel to allow for `x_stddev` and `y_stddev` to be expressed in pixels to keep it general. By definition, the center of the Gaussian kernel is in the center of the array. Parameters ---------- shape : tuple The shape of the 2D kernel, in pixels. x_stddev : float The standard deviation of the Gaussian in the x direction, in pixels. y_stddev : float The standard deviation of the Gaussian in the y direction, in pixels. rotation : float The rotation angle, increasing counterclockwise, in radians. Returns ------- gaussian_kernel : ndarray The discrete kernel array. """ # The center of the array given by the shape is defined as just the center # of it. However, we need to take into account off-by-one errors. nrow, ncol = shape cen_row = (nrow - 1) / 2 cen_col = (ncol - 1) / 2 # The normalization constant is provided as amplitude itself. norm_constant = 1 / (2 * np.pi * x_stddev * y_stddev) # The mesh grid used to evaluate the Gaussian function to derive the kernel. xx, yy = np.meshgrid(np.arange(ncol), np.arange(nrow)) # Deriving the kernel and computing it. gaussian2d = astropy.modeling.models.Gaussian2D( amplitude=norm_constant, x_mean=cen_col, y_mean=cen_row, x_stddev=x_stddev, y_stddev=y_stddev, theta=rotation, ) gaussian_kernel = gaussian2d(xx, yy) return gaussian_kernel