A normalizing flow approach for the inference of star cluster properties from unresolved broadband photometry - I. Comparison to spectral energy distribution fitting

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Table 1

Inlier percentages for cINN and PHANGS estimates.

	log₁₀(t)	log₁₀(m)	E_B–V
Q_0.16 < θ < Q_0.84	71.0%	61.1%	75.4%
θ − 1σ < $\bar{θ}$ $\[\bar{\theta}\]$ < θ + 1σ	65.4%	52.0%	68.4%
θ − 1σ < $Q_{\frac{1}{2}}$ $\[Q_{\frac{1}{2}}\]$ < θ + 1σ	73.3%	59.8%	77.8%
θ − 1σ < θ_MAP < θ + 1σ	76.3%	64.3%	80.5%

Notes. The top row shows how often the PHANGS estimates (θ) are enclosed by the 16%- to 84%-quantiles of the cINN posterior. Rows two, three and four show how often the cINN posterior mean ( $\bar{θ}$ $\[\bar{\theta}\]$ ), median ( $Q_{\frac{1}{2}}$ $\[Q_{\frac{1}{2}}\]$ ), and MAP estimates (θ_MAP) are contained in the ± 1σ-range of the PHANGS estimates.

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