A XRISM view of the iron line complex in NGC 1068: Rethinking the prototypical Compton-thick AGN

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Volume 710 (June 2026)

A&A, 710 (2026) A274

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Table 1.

Measured parameters of the main emission lines in the XRISM/Resolve spectrum of NGC 1068.

Line	Velocity shift	σ	Flux or ratio
	(km s⁻¹)	(km s⁻¹)	(10⁻⁵ ph cm⁻² s⁻¹)
Fe Kα	−30 ± 12^‡	$155_{- 16}^{+ 18}^{‡}$ $Mathematical equation: $ 155^{+18}_{-16}{^\ddagger} $$	5.8 ± 0.2
Fe Kβ			0.103 ± 0.016^†
Ni Kα			0.066 ± 0.012^†
Fe Kα (broad)	$- 700_{- 300}^{+ 250}$ $Mathematical equation: $ -700^{+250}_{-300} $$	2400 ± 400	0.39 ± 0.06^†

Fe XXV Heα	$- 300_{- 500}^{+ 300}^{‡}$ $Mathematical equation: $ -300^{+300}_{-500}{^{\ddagger}} $$	2400 ± 200^‡	$4 . 4_{- 0.5}^{+ 0.6}$ $Mathematical equation: $ 4.4^{+0.6}_{-0.5} $$
Fe XXVI Lyα		2400 ± 200^‡	$1 . 5_{- 0.4}^{+ 0.6}$ $Mathematical equation: $ 1.5^{+0.6}_{-0.4} $$

Si XIV Lyα	−100 ± 140^‡	$710_{- 120}^{+ 150}^{‡}$ $Mathematical equation: $ 710^{+150}_{-120}{^{\ddagger}} $$	7.1 ± 1.5
S XV Heα			3.2 ± 0.9
S XVI Lyα			1.4 ± 0.3

Notes. The Fe Kα and Kβ lines are modeled with zbfeklor and zbfekblor. The Ni Kα and Lyα lines are modeled as 2:1 Gaussian doublets. The Heα lines are modeled as Gaussian triplets (four components in the case of Fe XXV). In all cases, the reported fluxes refer to the total flux summed over all components (see text for further details). ^( † )Flux ratios relative to the Fe Kα core flux. ^( ‡ )Velocity shift and Gaussian width are tied among lines of the same element or line family.

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