Cosmology and source redshift constraints from galaxy clustering and tomographic weak lensing with HSC Y3 and SDSS using the point-mass correction model

The combination of galaxy clustering and weak lensing is a powerful probe of the cosmology model. We present a joint analysis of galaxy clustering and weak lensing cosmology using Sloan Digital Sky Survey (SDSS) data as the tracer of dark matter (lens sample) and the Hyper Suprime-Cam year-3 (HSC Y3) dataset as source galaxies. The analysis divides HSC Y3 galaxies into four tomographic bins for both galaxy-galaxy lensing and cosmic shear measurements and employs a point-mass correction model to utilize galaxy-galaxy lensing signals down to 2 h − 1 Mpc , extending up to 70 h − 1 Mpc . These strategies enhance the signal-to-noise ratio of the galaxy-galaxy lensing data vector. Using a flat Λ CDM model, we find S 8 = 0.78 0 − 0.030 + 0.029 , and using a w CDM model, we obtain S 8 = 0.75 6 − 0.036 + 0.038 with w = − 1.17 6 − 0.346 + 0.310 . We apply uninformative priors on the redshift mean-shift parameters for the third and fourth tomographic bins. Leveraging the self-calibration power of tomographic weak lensing, we measure Δ z 3 = − 0.11 2 − 0.049 + 0.046 and Δ z 4 = − 0.18 5 − 0.081 + 0.071 , in agreement with previous HSC Y3 results. This demonstrates that weak lensing self-calibration can achieve redshift constraints comparable to other methods such as photometric and clustering redshift calibration.