Speaker
Description
The three-dimensional galaxy power spectrum is a powerful probe of primordial non-Gaussianity and additional general relativistic effects, which become important on large scales. At the same time, wide-angle (WA) effects due to differing lines-of-sight (LOS) on the curved sky also become important with large angular separation. In this talk, we present a new way to non-perturbatively model WA and GR effects present in the commonly used power spectrum multipoles (PSM). We accurately model WA and GR effects using the spherical Fourier-Bessel (SFB) formalism, before transforming the result into the PSM. Moreover, for the first time, we can compute the analytical PSM Gaussian covariance on large scales, exactly including WA-induced mode-couplings, without resorting to any plane-parallel approximations.
