\mathrm{FoM} \propto \dfrac{1}{\sqrt{ \det (\mathbf{C}_{\rm marg} )}}

θ~10arcmin/l=1024

θ~20arcmin/l=540

Zu ̈rcher+ (2023)

(l1-norm)

Bias as function of survey area

BNT transform

When we observe shear, contributions come from mass at different redshifts.
BNT Transform: method to “null” contributions from unwanted redshift ranges.
It reorganizes weak-lensing data so that only specific redshift ranges contribute to the signal.
BNT aligns angular (ℓ) and physical (k) scales.
This could help mitigate baryonic effects by optimally removing sensitivity to poorly modeled small scales and controlling scale leakage.

no BNT

BNT

Power Spectrum

l1-norm

* This could help mitigate baryonic effects by optimally removing sensitivity to poorly modeled small scales and controlling scale leakage?

Loss of power compared to contours without cuts

Loss of power compared to contours with cuts

Conclusions

Part 2

Unmodeled baryonic effects can lead to significant bias in cosmological parameters.
To remove the bias from baryons, stringent scale cuts are required (ℓ~500 ).
Even after scale cut at ℓ~500, HOS maintain significantly increased constraining power, compared to the PS.
The BNT transform, while offering more physical scale cuts, leads to a significant inflation in contour size.

Part 1

Mass mapping can have a significant impact on cosmological contours
With a state-of-the-art mass-mapping method (MCALens) we managed to get 2.6x improvement in FoM over KS.

By Andreas Tersenov