The XMM-Newton and NuSTAR view of IRASF11119+3257 - I. Detection of multiple ultra fast outflow components and a very cold corona

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Volume 689 (September 2024)

A&A, 689 (2024) A247

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Table 3.

Continuum and XSTAR absorption table best-fit parameters.

Component	Parameter		Units
`pexrav`	Γ	2.05 ± 0.06	–
	R	< 0.35	–
	E_cut	$25 . 4_{- 5.0}^{+ 9.5}$ $25.4_{-5.0}^{+9.5}$	keV
	f_scat	1.2 ± 0.4%	–
`WA`	log(N_H)	$22 . 43_{- 0.04}^{+ 0.06}$ $22.43_{-0.04}^{+0.06}$	cm⁻²
	log(ξ)	$0 . 05_{- 0.17}^{+ 0.25}$ $0.05_{-0.17}^{+0.25}$	erg cm/s
	v_turb	300 ^( * )	km/s
	v_out	< 2500	km/s
`UFO`_L	log(N_H)	$21 . 54_{- 0.23}^{+ 0.26}$ $21.54_{-0.23}^{+0.26}$	cm⁻²
	log(ξ)	$2 . 57_{- 0.17}^{+ 0.26}$ $2.57_{-0.17}^{+0.26}$	erg cm/s
	v_turb	1000 ^( * )	km/s
	v_out	0.30 ± 0.01	v/c
`UFO`_H	log(N_H)	> 23.99	cm⁻²
	log(ξ)	$4 . 95_{- 0.45}^{+ 0.43}$ $4.95_{-0.45}^{+0.43}$	erg cm/s
	v_turb	3000 ^( * )	km/s
	v_out	0.27 ± 0.01	v/c

	𝒞−stat/ν	389.3/369	–
	L_{2 − 10 keV}	1.3 × 10⁴⁴	erg s⁻¹

Notes. One XSTAR table with v_turb = 300 km s⁻¹ is used for the WA component, one with v_turb = 1000 km s⁻¹ for the soft UFO component, and one with v_turb = 3000 km s⁻¹ for the hard UFO component. pexrav parameters are defined as in Table 1; log(N_H), log(ξ), v_turb and v_out for WA, UFO_L and UFO_H components are defined as in Table 1; 𝒞−stat/ν is the fit statistic over the number of degrees of freedom; L_{2 − 10 keV} is the absorption-corrected luminosity in the 2–10 keV rest frame band; ^( * )fixed parameters.

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