Post-Born lensing¶
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isitgr.postborn.
get_field_rotation_BB
(params, lmax=None, acc=1, CMB_unit='muK', raw_cl=False, spline=True)[source]¶ Get the B-mode power spectrum from field post-born field rotation, based on perturbative and Limber approximations. See arXiv:1605.05662.
Parameters: - params –
model.CAMBparams
instance with cosmological parameters etc. - lmax – maximum \(\ell\)
- acc – accuracy
- CMB_unit – units for CMB output relative to dimensionless
- raw_cl – return \(C_\ell\) rather than \(\ell(\ell+1)C_\ell/2\pi\)
- spline – return InterpolatedUnivariateSpline, otherwise return tuple of lists of \(\ell\) and \(C_\ell\)
Returns: InterpolatedUnivariateSpline (or arrays of sampled \(\ell\) and) \(\ell^2 C_\ell^{BB}/(2 \pi)\) (unless raw_cl, in which case just \(C_\ell^{BB}\))
- params –
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isitgr.postborn.
get_field_rotation_power
(params, kmax=100, lmax=20000, non_linear=True, z_source=None, k_per_logint=None, acc=1, lsamp=None)[source]¶ Get field rotation power spectrum, \(C_L^{\omega\omega}\), following arXiv:1605.05662. Uses lowest Limber approximation.
Parameters: - params –
model.CAMBparams
instance with cosmological parameters etc. - kmax – maximum k (in \({\rm Mpc}^{-1}\) units)
- lmax – maximum L
- non_linear – include non-linear corrections
- z_source – redshift of source. If None, use peak of CMB visibility for CMB lensing
- k_per_logint – sampling to use in k
- acc – accuracy setting, increase to test stability
- lsamp – array of L values to compute output at. If not set, set to sampling good for interpolation
Returns: \(L\), \(C_L^{\omega\omega}\): the L sample values and corresponding rotation power
- params –