In medio stat virtus: Enrichment history in poor galaxy clusters

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Table 3.

Iron mass diffused in the ICM, stellar masses, and effective iron yields for MKW3s, A2589, and Hydra A.

	$M_{Fe, 500}^{ICM}$ $M_{\mathrm{Fe,500}}^{\mathrm{ICM}}$		$M_{500}^{star}$ $M_{500}^{\mathrm{star}}$		𝒴_Fe, 500

	Best fit	Systematics	Best fit	Systematics	Best fit	Systematics
	(10¹⁰ M_⊙)	(10¹⁰ M_⊙)	(10¹² M_⊙)	(10¹² M_⊙)	(Z_⊙)	(Z_⊙)
MKW3s	1.28 ± 0.06	[ + 0.35, −0.20]	2.86 ± 0.44	[ + 0.00, −1.14]	2.68 ± 0.34	[ + 2.36, −0.33]
A2589	0.92 ± 0.09	[ + 0.55, −0.14]	2.20 ± 0.63	[ + 0.51, −0.51]	2.54 ± 0.64	[ + 2.13, −0.62]
Hydra A	1.25 ± 0.04	[ + 0.46, −0.20]	0.84 ± 0.17	[ + 0.22, −0.00]	7.51 ± 1.47	[ + 0.13, −3.31]

Notes. $M_{Fe, 500}^{ICM}$ $M_{\mathrm{Fe,500}}^{\mathrm{ICM}}$ refers to the iron mass diffused in the ICM, computed within R₅₀₀. The systematic errors associated with these measurements originate from abundance profiles derived using individual XRB modelling, as described in Sect. 5.3.2. The term $M_{500}^{star}$ $M_{500}^{\mathrm{star}}$ refers to stellar mass measurements within R₅₀₀, including both statistical and systematic errors, as detailed in Appendix D. Finally, we report the effective iron yields, combining the best-fit measurements and systematic errors of the previous two quantities, as discussed in Sect. 5.3.3.

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