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 4.

Best-fit parameters of the model where a DISK-WIND grid was used to replace the XSTAR table to model the UFO_H features.

Component	Parameter		Units
`pexrav`	Γ	2.05 ± 0.05	–
	R	< 0.35	–
	E_cut	$24 . 3_{- 4.6}^{+ 2.6}$ $24.3_{-4.6}^{+2.6}$	keV
	f_scat	0.45 ± 0.4%	–
`WA`	log(N_H)	$22 . 54_{- 0.07}^{+ 0.02}$ $22.54_{-0.07}^{+0.02}$	cm⁻²
	log(ξ)	$- 0 . 03_{- 0.19}^{+ 0.27}$ $-0.03_{-0.19}^{+0.27}$	erg cm/s
	v_turb	300 ^( * )	km/s
	v_out	< 2500	km/s
`UFO`_L	log(N_H)	$21 . 60_{- 0.25}^{+ 0.23}$ $21.60_{-0.25}^{+0.23}$	cm⁻²
	log(ξ)	$2 . 57_{- 0.24}^{+ 0.19}$ $2.57_{-0.24}^{+0.19}$	erg cm/s
	v_turb	1000 ^( * )	km/s
	v_out	0.30 ± 0.01	v/c
DISK-WIND	f_v	$1 . 53_{- 0.11}^{+ 0.07}$ $1.53_{-0.11}^{+0.07}$ (1.5^a)	–
	(v_∞)	(0.38 ± 0.02)	v/c
	μ = cos θ	$0 . 53_{- 0.02}^{+ 0.03}$ $0.53_{-0.02}^{+0.03}$ (0.525^a)	–
	${\dot{M}}_{w}$ $\mathcal{\dot M}_{\mathrm{w}}$	$0 . 99_{- 0.17}^{+ 0.26}$ $0.99_{-0.17}^{+0.26}$	( $\frac{{\dot{M}}_{out}}{{\dot{M}}_{Edd}}$ $\frac{{\dot{M}}_{\mathrm{out}}}{{\dot M_{\mathrm{Edd}}}}$ )
	ℒ_X	> 1.72%	( $\frac{L_{2 - 10 keV}}{L_{Edd}}$ $\frac{L_\mathrm{2-10\,\mathrm{keV}}}{L_{\mathrm{Edd}}}$ )

	𝒞−stat/ν	390/370	–
	$L_{2 - 10 keV}^{b}$ $L_{\mathrm{2-10\,keV}}^{\mathbf{b}}$	5.4 × 10⁴⁴	erg s⁻¹

Notes.pexrav parameters are defined as in Table 1; log(N_H), log(ξ), v_turb and v_out for WA, and UFO_L components are defined as in Table 1; For the DISK-WIND component f_v is the velocity parameter defined as f_v = v_∞/v_esc; v_∞ is the corresponding terminal velocity for v_esc = 0.25; μ is the cosine of the inclination angle; ${\dot{M}}_{w}$ $\mathcal{\dot M}_{\mathrm{w}}$ is the mass outflow rate in Ṁ_Edd units; ℒ_X is the ionizing luminosity in L_Edd units. 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; ^af_v and μ closest grid points used to derive more reliable constraints on ${\dot{M}}_{w}$ $\mathcal{\dot M}_{\mathrm{w}}$ and ℒ_X. ^( * )fixed parameter.

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