Position-dependent correlation function of weak-lensing convergence

We provide a systematic study of the position-dependent correlation function in weak-lensing convergence maps and its relation to squeezed limit three-point (3PCF) using state-of-the-art numerical simulations. relate harmonic counterpart, i.e., power spectrum or equivalently integrated bispectrum (IB). use recently proposed improved fitting function, BiHalofit, for compute theoretical predictions as source redshifts. In addition low redshift results (${z}_{s}=1.0--2.0$) we also inferred from lensing cosmic microwave background (CMB), ${z}_{s}=1100$. include Euclid-type realistic survey mask noise. agreement with recent studies on spectrum, find that simulations are consistent expectations when appropriate corrections included. Performing rough estimate, signal-to-noise (S/N) detection ${f}_{\mathrm{sky}}=0.35$, can range between 6--12 depending value intrinsic ellipticity distribution parameter ${\ensuremath{\sigma}}_{\ensuremath{\epsilon}}=0.3--1.0$. For reconstructed $\ensuremath{\kappa}$ an ideal CMB $\mathrm{S}/\mathrm{N}\ensuremath{\approx}1.8$. found 10% deviation ${\ensuremath{\sigma}}_{8}$ be detected IB optimistic case ${\ensuremath{\sigma}}_{\ensuremath{\epsilon}}=0.3$ $\mathrm{S}/\mathrm{N}\ensuremath{\approx}5$. The S/N such ${\mathrm{\ensuremath{\Omega}}}_{M}$ is lower.