cosmicpy.spectra – Clustering and lensing power spectra¶

 spectra(cosmo, surv[, lmax]) Computes and stores all the window functions
class cosmicpy.spectra.spectra(cosmo, surv, lmax=1000, **kwargs)[source]

Bases: object

Computes and stores all the window functions

W(l, k1=None, k2=None, evol=True, fid_cosmo=None, kmax=0.25)[source]

Computes the Spherical Fourier-Bessel window function for the survey

Parameters: l (int) – Order of the Bessel functions. k1 (array_like, optional) – Value of the scale at which to evaluate the window function in h/Mpc. If None is provided, the window function is evaluated at discrete points defined by the zeroes of the Bessel functions up to the kmax parameter (def : None). k2 (array_like, optional) – Value of the scale at which to evaluate the window function in h/Mpc. If None is provided, a symmetric Bessel window is computed $$W_l(k1, k1)$$ (def : None). evol (boolean, optional) – Flag to include the time dependent linear bias and growth in the computation of the window function (def : True). fid_cosmo (Cosmology, optional) – Fiducial cosmology to use for the computation of redshift to comoving distance in the case of a real survey. If None is provided, the true cosmology is used (def : None). kmax (float, optional) – Maximum scale at which to compute the window if k1 is not provided. This is usefull to avoid computing the window at non linear scales which would be cut afterwards (def : 0.25).

Notes

:math:: W_l (k1,k2) = int k1 phi(r)
j_l(k1 r) j_l(k2 r) r^2 dr
cl_gg(i, j, l, shotNoise=False, linear=True, **kwargs)[source]

galaxy-galaxy angular power spectrum in the Limber approximation

g(i, l, z)[source]

galaxy clustering window function