  On-going or soon to come cosmological large-scale structure surveys such as
DESI, SPHEREx, Euclid, or the High-Latitude Spectroscopic Survey of the Nancy
Grace Roman Space Telescope promise unprecedented measurement of the clustering
of galaxies on large scales. When quantified with the Cartesian Fourier basis,
the measurement of these large scales requires the introduction of so-called
wide-angle corrections. By contrast, the measurement of the power spectrum in a
spherical Fourier Bessel (SFB) basis does not require such corrections and
naturally accounts for the spherical survey geometries. Here, we develop and
implement a fast code to construct the SFB power spectrum and investigate how
line of sight effects, physics such as non-Gaussianity, and differing survey
geometries affect SFB power spectrum estimates. We then leverage our program to
predict the tightness of cosmological constraints from realistic survey
specifications using a Fisher matrix formalism.
