Accuracy requirements on intrinsic alignments for Stage-IV cosmic shear

Abstract

In the context of cosmological weak lensing studies, intrinsic alignments (IAs) are one the most complicated astrophysical systematic to model, given the poor understanding of the physical processes that cause them. A number of modelling frameworks for IAs have been proposed in the literature, both purely phenomenological or grounded on a perturbative treatment of symmetry-based arguments. However, the accuracy with which any of these approaches is able to describe the impact of IAs on cosmic shear data, particularly on the comparatively small scales ($k\simeq 1{\mathrm{Mpc}}^{-1}$) to which this observable is sensitive, is not clear. Here we quantify the level of disagreement between the true underlying intrinsic alignments and the theoretical model used to describe them that can be allowed in the context of cosmic shear analyses with future Stage-IV surveys. We consider various models describing this "IA residual", covering both physics-based approaches, as well as completely agnostic prescriptions. The same qualitative results are recovered in all cases explored: for a Stage-IV cosmic shear survey, a mis-modelling of the IA contribution at the $\sim 10\%$ level produces shifts of $\lesssim 0.5\sigma$ on the final cosmological parameter constraints. Current and future IA models should therefore aim to achieve this level of accuracy, a prospect that is not unfeasible for models with sufficient flexibility.

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• Cosmic shear with small scales: DES-Y3, KiDS-1000 and HSC-DR1
• HYMALAIA: A Hybrid Lagrangian Model for Intrinsic Alignments
• Intrinsic galaxy alignments in the KiDS-1000 bright sample: dependence on colour, luminosity, morphology, and galaxy scale
• Prospects for disentangling dark matter with weak lensing
• Calibrating baryonic effects in cosmic shear with external data in the LSST era
• Non-linear infusion of intrinsic alignment and source clustering: impact on non-Gaussian cosmic shear statistics