lusee.MonoSkyModels

Functions

B2T(B, f)	Function that returns sky temperature, T, in [K] from brightness, B, in [W/m*2/Hz/sr] and frequency, f, in [MHz]
B2V(B, f, leff, gamma)	Function that returns power spectral density in [V^2/Hz] for a dipole of effective length leff in [m] and preamp coupling efficiency gamma c.f.
B_C(f)	Function that returns sky brightness, B, in [W/m**2/Hz/sr] at frequency, f, in [MHz] according to the model of Cane from MNRAS 189.3 (1979): 465-478.
B_NB(f)	Function that returns sky brightness, B, in [W/m**2/Hz/sr] at a frequency, f, in [MHz] according to the model of Novaco and Brown from ApJ 221 (1978): 114-123
T2B(T, f)	Function that returns sky brightness, B, in [W/m*2/Hz/sr] from temperature, T, in [K] and frequency, f, in [MHz]
T_C(f)	Function that returns sky temperature, T, in [K] at frequency, f, in [MHz] according to the model of Cane from MNRAS 189.3 (1979): 465-478.
T_DarkAges_Scaled(nu[, nu_min, nu_rms, A])	Function that rescales the location, width, and depth of the Dark Ages temperature decrement signal (the Dark Ages "trough"), and interpolates the temperature decrement at the specified frequencies, nuu.
T_J(f)	Function that returns sky temperature, T, in [K] at frequency, f, in [MHz] according to Eq.
T_NB(f)	Function that returns sky temperature, T, in [K] at frequency, f, in [MHz] according to the model of Novaco and Brown from ApJ 221 (1978): 114-123

Classes

BalePlasmaEffects([fname])

Class that loads data from simulations by Stuart Bale modeling plasma effects on observed radio signal, and interpolates the signal at a specified frequency in [MHz].