cosmology

The following seminar work of Hernquist details a light profile called the Hernquist profile:

https://ui.adsabs.harvard.edu/abs/1990ApJ...356..359H/abstract

The intensity calculation for a spherical model is given by equations (32-35):

It would be good to implement this light

It was noted in the review for our JOSS paper that the keyword argument noise for the function redshifts_from_comoving_density has a misleading name. See the review comment here. They suggested renaming to fixed_N. My own suggestion would be shot_noise (or perhaps poisson). Since this would require a break

Currently, the canvas.cut_mask() method takes in the healpix map of an experiment footprint. It would be nice to allow the user to apply such cuts using experiment footprints. For example

canvas.cut_mask("CMB-S4", inplace=True) 
canvas.cut_mask("DESI", inplace=True) 

would limit the catalog to the common footprint between S4 and DESI.

TODO: Add masks from [cmb x galax

• pixell version: 0.12.1
• Python version: 3.9.5
• Operating System: Ubuntu 20.04

Description

Currently enmap.read_map flips the U component of an ndmap in an opaque way, depending on the contents of the fits header. The fits header needs to have specific cards/values for the introspection to flip the component. These conditions (all evaluated in enmap.get_stokes_flips) should be

Multiple error cases are not accounted for in the unit tests, hence we should add some new tests at some point.