Dipoles for everyone: the pseudo-$C_\ell$ approach to directional stacking

TL;DR

This paper introduces a pseudo-$C_ll$ method for directional stacking in astrophysics, enabling efficient reconstruction of signals related to galaxy velocities, shapes, and tidal forces through cross-power spectra with $E$ and $B$ modes.

Contribution

It presents a novel power spectrum approach to reconstruct all directional stacking signals without information loss, improving speed and data analysis in cosmological studies.

Findings

All directional stacking signals can be reconstructed via cross-power spectra.

The approach offers advantages in speed, resolution handling, and data visualization.

Recovered signals may contain information already present in galaxy density cross-spectra.

Abstract

Stacking (i.e. averaging) the value of a given astrophysical field around sources allows us to detect new cosmological signatures, such as the kinematic Sunyaev-Zel'dovich, and gain insight on the astrophysical properties of galaxies and their environment. Further information may be gained by orienting these stacks along preferred axes defined by a local directed field, such as the transverse galaxy velocities, galaxy shapes, or the local tidal forces. Examples of this are searches for the moving lens effect, the detection of dipole signatures, or the study of cosmic filaments. Here we show that all directional stacking signals may be reconstructed, without loss of information, in terms of the cross-power spectrum between the quantity of interest and the $E$ and $B$ modes of the spin field used to define the preferred axes weighted by the local galaxy density. The power spectrum approach has several practical advantages, in terms of speed, finite-resolution effects, data visualisation, and combination with other cosmological probes. We also argue that, in some cases, such as stacking using velocities or tidal forces reconstructed from the density field, the recovered signal may be dominated by information that is already present in the cross-spectrum between the target field and the galaxy overdensity itself.