# The squeezed matter bispectrum covariance with responses

## TL;DR

This paper develops a response-based analytical method to accurately compute the squeezed matter bispectrum covariance, including super-sample effects, which is essential for precise cosmological analyses involving large-scale structure.

## Contribution

It introduces a response function approach to calculate the squeezed matter bispectrum covariance, providing a complete, noise-free, and predictive analytical framework.

## Key findings

- Response-type mode-coupling terms dominate the covariance
- Super-sample covariance contribution is negligible
- Method is applicable to galaxy clustering and weak-lensing analyses

## Abstract

We present a calculation of the angle-averaged squeezed matter bispectrum covariance ${\rm Cov}\left(B_{m}(k_1, k_1', s_1), B_{m}(k_2, k_2', s_2)\right)$, $s_i \ll k_i,k_i'$ ($i=1,2$), that uses matter power spectrum responses to describe the coupling of large- to short-scale modes in the nonlinear regime. The covariance is given by a certain configuration of the 6-point function, which we show is dominated by response-type mode-coupling terms in the squeezed bispectrum limit. The terms that are not captured by responses are small, effectively rendering our calculation complete and predictive for linear $s_1,s_2$ values and any nonlinear values of $k_1,k_1',k_2,k_2'$. Our numerical results show that the squeezed bispectrum super-sample covariance is only a negligible contribution. We also compute the power spectrum-bispectrum cross-covariance using responses. Our derivation for the squeezed matter bispectrum is the starting point to calculate analytical covariances for more realistic galaxy clustering and weak-lensing applications. It can also be used in cross-checks of numerical ensemble estimates of the general bispectrum covariance, given that it is effectively noise-free and complete in the squeezed limit.