KiDS-SBI: Simulation-based inference analysis of KiDS-1000 cosmic shear

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Volume 694 (February 2025)

A&A, 694 (2025) A223

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Table 1.

Parameters used to sample galaxies and their shapes in line with the expectations for the KiDS-1000 gold sample for each tomographic bin (from S1 to S5).

Bin	${\bar{n}}_{eff}$ $\overline{n}_{\mathrm{eff}}$	${\bar{σ}}_{ϵ} / \sqrt{2}$ $\overline{\sigma}_{\epsilon}/\sqrt{2}$	a_{n_eff}	b_{n_eff}	a_{σ_ϵ}	b_{σ_ϵ}
	[arcmin⁻²]				×10³
S1	0.62	0.27	−0.035	0.72	1.81	0.267
S2	1.18	0.26	−0.042	1.30	1.30	0.257
S3	1.85	0.28	−0.243	2.58	−0.86	0.280
S4	1.26	0.25	−0.250	2.01	−0.62	0.255
S5	1.31	0.27	−0.416	2.56	2.39	0.261

Notes. ${\bar{n}}_{eff}$ $\overline{n}_{\mathrm{eff}}$ is the mean galaxy number density for a given tomographic bin, ${\bar{σ}}_{ϵ} / \sqrt{2}$ $\overline{\sigma}_{\epsilon}/\sqrt{2}$ is the mean per-component shape dispersion, a_{n_eff} and b_{n_eff} are the slope and y-intercept, respectively, for the linear interpolation of the galaxy density as a function of the root-mean-square of the background noise in the KiDS catalogue, σ_rms, according to Eq. (28), while a_{σ_ϵ} and b_{σ_ϵ} are the parameters to linearly interpolate σ_ϵ from σ_rms according to Eq. (29).

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