Detecting the polarization induced by scattering of the microwave background quadrupole in galaxy clusters

TL;DR

This paper assesses the feasibility of detecting CMB polarization caused by scattering in galaxy clusters, proposing optimal estimators and forecasting detection prospects for future CMB surveys, highlighting the challenges and potential scientific gains.

Contribution

It introduces linear and quadratic maximum-likelihood estimators for detecting cluster-induced CMB polarization and forecasts their effectiveness for upcoming surveys.

Findings

Detection is challenging with current surveys without dedicated polarization follow-up.

An r.m.s. noise of about 1 μK-arcmin is needed for a 2-sigma detection with ~550 clusters.

Next-generation CMB missions could measure this effect with high signal-to-noise.

Abstract

We analyse the feasibility of detecting the polarization of the CMB caused by scattering of the remote temperature quadrupole by galaxy clusters with forthcoming CMB polarization surveys. For low-redshift clusters, the signal is strongly correlated with the local large-scale temperature and polarization anisotropies, and the best prospect for detecting the cluster signal is via cross-correlation. For high-redshift clusters, the correlation with the local temperature is weaker and the power in the uncorrelated component of the cluster polarization can be used to enhance detection. We derive linear and quadratic maximum-likelihood estimators for these cases, and forecast signal-to-noise values for the SZ surveys of a Planck-like mission and SPTPol. Our estimators represent an optimal `stacking' analysis of the polarization from clusters. We find that the detectability of the effect is sensitive to the cluster gas density distribution, as well as the telescope resolution, cluster redshift distribution, and sky coverage. We find that the effect is too small to be detected in current and near-future SZ surveys without dedicated polarization follow-up, and that an r.m.s. noise on the Stokes parameters of roughly 1 uK-arcmin for each cluster field is required for a 2-sigma detection, assuming roughly 550 clusters are observed. We discuss and quantify potential biases from the kinetic part of the signal caused by the relative motion of the cluster with respect to the CMB, and from the background CMB polarization behind the cluster, discussing ways in which these biases might be mitigated. Our formalism should be important for next-generation CMB polarization missions, which we argue will be able to measure this effect with high signal-to-noise. This will allow for an important consistency test of the LCDM model on scales that are inaccessible to other probes.