Modified gravity below O(10) Mpc in a CPL dynamical dark energy background is required to suppress structure growth at low redshifts while satisfying CMB constraints from ISW and lensing.
Miyatakeet al., Hyper Suprime-Cam Year 3 re- sults: Cosmology from galaxy clustering and weak lensing with HSC and SDSS using the emulator based halo model, Phys
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Baryonic feedback affects galaxy-galaxy, galaxy-shear, and shear-shear three-point correlation functions more strongly than two-point functions on small scales, reaching up to 90 percent suppression depending on redshift and model parameters.
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Signatures of Modified Gravity Below $\mathcal{O}(10)$ Mpc in a Dynamical Dark Energy Background
Modified gravity below O(10) Mpc in a CPL dynamical dark energy background is required to suppress structure growth at low redshifts while satisfying CMB constraints from ISW and lensing.
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$4\times3$ Point Correlation Functions in Galaxy Surveys: Impact of Baryonic Feedback
Baryonic feedback affects galaxy-galaxy, galaxy-shear, and shear-shear three-point correlation functions more strongly than two-point functions on small scales, reaching up to 90 percent suppression depending on redshift and model parameters.