Imitating intrinsic alignments: A bias to the CMB lensing-galaxy shape cross-correlation power spectrum induced by the large-scale structure bispectrum

TL;DR

This paper analyzes how nonlinear large-scale structure growth biases the CMB lensing-galaxy shape cross-correlation, potentially mimicking intrinsic alignments and affecting cosmological parameter estimates.

Contribution

It provides a theoretical calculation of the bias induced by the large-scale structure bispectrum on the CMB lensing-galaxy shape cross-correlation, highlighting its significance for future surveys.

Findings

Bias is negative on most scales, mimicking intrinsic alignments.

Bias becomes significant at small scales ($  2500$) for Euclid-like data.

Uncorrected bias can cause 2-3 sigma errors in intrinsic alignment amplitude estimates.

Abstract

Cross-correlating the lensing signals of galaxies and comic microwave background (CMB) fluctuations is expected to provide valuable cosmological information. In particular it may help tighten constraints on parameters describing the properties of intrinsically aligned galaxies at high redshift. To access the information conveyed by the cross-correlation signal its accurate theoretical description is required. We compute the bias to CMB lensing-galaxy shape cross-correlation measurements induced by nonlinear structure growth. Using tree-level perturbation theory for the large-scale structure bispectrum we find that the bias is negative on most angular scales, therefore mimicking the signal of intrinsic alignments. Combining Euclid-like galaxy lensing data with a CMB experiment comparable to the Planck satellite mission the bias becomes significant only on smallest scales ($\ell\gtrsim 2500$). For improved CMB observations, however, the corrections amount to 10-15 per cent of the CMB lensing-intrinsic alignment signal over a wide multipole range ($10 \lesssim \ell \lesssim 2000$). Accordingly the power spectrum bias, if uncorrected, translates into $2\sigma$ and $3\sigma$ errors in the determination of the intrinsic alignment amplitude in case of CMB stage III and stage IV experiments, respectively.