Tomographic weak lensing surveys contain intrinsic symmetries that depend solely on the geometric structure of the Universe. These symmetries can be revealed through null tests and verifying their validity provides constraints on cosmological parameters that govern the background evolution—particularly the redshift dependence of the angular diameter distance. This forms the foundation of the tomographic cosmic shear nulling test introduced in this work. We describe how this test can be implemented, what aspects of cosmology it can constrain, and its specific efficiency in doing so. We also assess its sensitivity to astrophysical effects—such as magnification bias and reduced shear corrections—as well as to observational systematics, including errors in the mean redshift of source bins. Our results show that, in a survey configuration comparable to that of Euclid, this null test can yield complementary constraints on key cosmological parameters such as ${\mathrm{\Omega }}_{\mathrm{m}},{\mathrm{w}}_0$. However, due to its subdominant constraining power compared to standard $3\times 2\mathrm{pt}$ analysis and through the identification of a required precision of order ${10}^{-3}$ on the mean redshift of the bins, we conclude that nulling would better be used as a photometric redshift calibration probe or consistency check. In combination with standard weak lensing and galaxy clustering analysis, it would then offer a promising route to better control systematics and improve the precision of future cosmological measurements.

Close

PrevNext

View figure in article

• Cosmological parameters
• Cosmology
• Dark energy
• Large scale structure of the Universe