Speaker
Description
The angular power spectrum of redshift fluctuations is a novel observable that involves a specific kind of weighting of the galaxy number counts, meant to recover complementary information, using the redshift distribution along the line of sight. This has been shown to be generally effective in improving constraining power when combined with the conventional angular power spectrum, and was recently used with Quaia data to provide the tightest constraint on $f_{\rm NL}$ from large scale structure 2-point statistics, second only to the DESI DR1 3D power spectrum analysis. Using data from DESI, there is an opportunity to use this technique to further improve these constraints. I will briefly review the theoretical framework of angular redshift fluctuations, discuss results from forecasts, in anticipation of future work using DESI, and compare to the current results.