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Weak gravitational lensing convergence peaks, the local maxima in weaklensing convergence maps, have been shown to contain valuable cosmologicalinformation complementary to commonly used two-point statistics. To exploit thefull power of weak lensing for cosmology, we must model baryonic feedbackprocesses because these reshape the matter distribution on non-linear andmildly non-linear scales. We study the impact of baryonic physics on the numberdensity of weak lensing peaks using the FLAMINGO cosmological hydrodynamicalsimulation suite. We generate ray-traced full-sky convergence maps mimickingthe characteristics of a Stage IV weak lensing survey. We compare the numberdensities of peaks in simulations that have been calibrated to reproduce theobserved galaxy mass function and cluster gas fraction or to match a shiftedversion of these, and that use either thermally driven or jet AGN feedback. Weshow that the differences induced by realistic baryonic feedback prescriptions(typically $5-30$% for $\kappa = 0.1-0.4$) are smaller than those induced byreasonable variations in cosmological parameters ($20-60$% for $\kappa =0.1-0.4$) but must be modeled carefully to obtain unbiased results. The reasonsbehind these differences can be understood by considering the impact offeedback on halo masses, or by considering the impact of different cosmologicalparameters on the halo mass function. Our analysis demonstrates that thebaryonic suppression is insensitive to changes in cosmology up to $\kappa\approx 0.4$ and that the higher $\kappa$ regime is dominated by Poisson noiseand cosmic variance.

The FLAMINGO project: Baryonic impact on weak gravitational lensing convergence peak counts