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Mass and Motion, Tension and Concordance: What Are Tensions in Current Data Telling Us About Dark Energy?
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Gravity Observation and Dark energy Detection Explorer in the Solar System (GODDESS)
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Insights into Dark Matter and Dark Energy... Using Strong Gravitational Lensing Observations of Galaxies, Quasars, and Supernovae
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Gravity Observation and Dark Energy Detection Explorer in the Solar System (GODDESS)
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Gravity Observation and Dark Energy Detection Explorer in the Solar System (GODDESS) -- a Mission Concept
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Exploiting non-linear scales in galaxy–galaxy lensing and galaxy clustering: A forecast for the dark energy survey
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Photometric Properties of Jupiter Trojans Detected by the Dark Energy Survey
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Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey. I. Evidence for Thermal Energy Anisotropy Using Oriented Stacking
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Linear systematics mitigation in galaxy clustering in the Dark Energy Survey Year 1 Data
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Cold dark energy constraints from the abundance of galaxy clusters
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Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data
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Dark Energy Survey Year 3 Results: Multi-Probe Modeling Strategy and Validation
This paper details the modeling pipeline and validates the baseline analysis choices of the DES Year 3 joint analysis of galaxy clustering and weak lensing (a so-called "3$\times$2pt" analysis). These analysis choices include the specific combination of cosmological probes, priors on cosmological and systematics parameters, model parameterizations for systematic effects and related approximations, and angular scales where the model assumptions are validated. We run a large number of simulated likelihood analyses using synthetic data vectors to test the robustness of our baseline analysis. We demonstrate that the DES Year 3 modeling pipeline, including the calibrated scale cuts, is sufficiently accurate relative to the constraining power of the DES Year 3 analyses. Our systematics mitigation strategy accounts for astrophysical systematics, such as galaxy bias, intrinsic alignments, source and lens magnification, baryonic effects, and source clustering, as well as for uncertainties in modeling the matter power spectrum, reduced shear, and estimator effects. We further demonstrate excellent agreement between two independently-developed modeling pipelines, and thus rule out any residual uncertainties due to the numerical implementation.