Joudaki, ShahabBlake, ChrisJohnson, AndrewAmon, AlexandraAsgari, M.Choi, AErben, ThomasGlazebrook, KarlHarnois-Deraps, JoachimHeymans, CatherineWolf, Christian2025-12-112025-12-110035-8711https://hdl.handle.net/1885/733794737We perform a combined analysis of cosmic shear tomography, galaxy-galaxy lensing tomography, and redshift-space multipole power spectra (monopole and quadrupole) using 450 deg2 of imaging data by the Kilo Degree Survey (KiDS-450) overlapping with two spectroscopic surveys: the 2-degree Field Lensing Survey (2dFLenS) and the Baryon Oscillation Spectroscopic Survey (BOSS). We restrict the galaxy-galaxy lensing and multipole power spectrum measurements to the overlapping regions with KiDS, and self-consistently compute the full covariance between the different observables using a large suite of N-body simulations. We methodically analyse different combinations of the observables, finding that the galaxy-galaxy lensing measurements are particularly useful in improving the constraint on the intrinsic alignment amplitude, while the multipole power spectra are useful in tightening the constraints along the lensing degeneracy direction. The fully combined constraint on S8 = σ8 √ωm/0.3 = 0.742 ± 0.035, which is an improvement by 20 per cent compared to KiDS alone, corresponds to a 2.6s discordance with Planck, and is not significantly affected by fitting to a more conservative set of scales. Given the tightening of the parameter space, we are unable to resolve the discordance with an extended cosmology that is simultaneously favoured in a model selection sense, including the sum of neutrino masses, curvature, evolving dark energy and modified gravity. The complementarity of our observables allows for constraints on modified gravity degrees of freedom that are not simultaneously bounded with either probe alone, and up to a factor of three improvement in the S8 constraint in the extended cosmology compared to KiDS alone.We acknowledge the use of CAMBand COSMOMCpackages (Lewis et al. 2000; Lewis & Bridle 2002). This work was supported by resources awarded under Astronomy Australia Ltd.’s merit allocation scheme on the gSTAR national facility at Swinburne University of Technology and on the National Computational Infrastructure. gSTAR is funded by Swinburne and the Australian Government’s Education Investment Fund. This work was supported by computational resources provided by the Australian Government through the Pawsey Supercomputing Centre under the National Computational Merit Allocation Scheme. This work was supported by the Flagship Allocation Scheme of the NCI National Facility at the ANU. Computations for the N-body simulations were performed in part on the Orcinus supercomputer at the WestGrid HPC consortium (www.westgrid.ca), in part on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research FundResearch Excellence; and the University of Toronto. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. SJ acknowledges support from the Beecroft Trust and ERC 693024. CB and DP acknowledge the support of the Australian Research Council through the awards of Future Fellowships. M A and C H acknowledge support from the European Research Council under grant number 647112. JHD acknowledge support from the European Commission under a Marie-Skłodwoska-Curie European Fellowship (EU project 656869). HHi is supported by an Emmy Noether grant (No. Hi 1495/2-1) of the Deutsche Forschungsgemeinschaft. HHo acknowledges support from the European Research Council under FP7 grant number 279396. DK and PS are supported by the Deutsche Forschungsgemeinschaft in the framework of the TR33 ‘The Dark Universe’. KK acknowledges support by the Alexander von Humboldt Foundation. AM acknowledges support from a CITA National Fellowship. LM is supported by STFC grant ST/N000919/1. MV acknowledges support from the European Research Council under P7 grant number 279396 and the Netherlands Organisation for Scientific Research (NWO) through grants 614.001.103. CW was supported by Australian Research Council Laureate Grant FL0992131. KiDS is based on data from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017 and 177.A-3018. 2dFLenS is based on data acquired through the Australian Astronomical Observatory under programme A/2014B/008. It would not have been possible without the dedicated work of the staff of the AAO in the development and support of the 2dF-AAOmega system and the running of the AAT.application/pdfen-AU© 2017 The Author(s)201710.1093/mnras/stx282010.25911/0EGR-HH862023-10-22