Investigating the consistency of the shape and flux of X-ray reflection spectra in the hard state with an accretion disk reaching close to the black hole

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Volume 691 (November 2024)

A&A, 691 (2024) A85

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Table 1.

Best-fit model parameters with consistent flux and shape for model B and B.1.

Component	Parameter	Model B	Model B.1
Interstellar absorption	N_H (10²² cm⁻²)	0.14(f)	0.14(f)

	Γ	1.385 $_{- 0.005}^{+ 0.009}$ $_{-0.005}^{+0.009}$	1.371 $_{- 0.006}^{+ 0.004}$ $_{-0.006}^{+0.004}$
Power law	cut-off (keV)	300(f)	300(f)
	Norm	0.649 $_{- 0.009}^{+ 0.007}$ $_{-0.009}^{+0.007}$	0.622 $_{- 0.015}^{+ 0.013}$ $_{-0.015}^{+0.013}$
	Flux	4.97 × 10⁻⁸	5.06 × 10⁻⁸
	r_in (R_g)	2.11 $_{- 0.15}^{+ 0.23}$ $_{-0.15}^{+0.23}$	1.79 $_{- 0.04}^{+ 0.58}$ $_{-0.04}^{+0.58}$
	r_out (R_g)	1000(f) ^(a)	1000(f)^a
	L (L_Edd)	2.81 $_{- 0.07}^{+ 0.09} \times 10^{- 4}$ $_{-0.07}^{+0.09}\times10^{-4}$	2.52 $_{- 0.03}^{+ 0.04} \times 10^{- 3}$ $_{-0.03}^{+0.04}\times10^{-3}$
Inner	ξ_in	1.06 × 10⁵	1.14 × 10⁶
reflection	n (10¹⁵ cm⁻³)	1.24 $_{- 0.29}^{+ 0.32} \times 10^{4}$ $_{-0.29}^{+0.32}\times10^{4}$	1.49 $_{- 0.25}^{+ 0.46} \times 10^{4}$ $_{-0.25}^{+0.46}\times10^{4}$
	Norm	1.11 × 10⁵ (f)	1.11 × 10⁴(f)
	Flux	6.24 × 10⁻⁹	5.36 × 10⁻⁹

	r_in (R_g)	671 $_{- 74}^{+ 71}$ $_{-74}^{+71}$	669 $_{- 78}^{+ 76}$ $_{-78}^{+76}$
	r_out (R_g)	1000(f)	1000(f)
	L (L_Edd)	1.18 $_{- 0.02}^{+ 0.02} \times 10^{- 3}$ $_{-0.02}^{+0.02}\times10^{-3}$	1.14 $_{- 0.03}^{+ 0.01} \times 10^{- 3}$ $_{-0.03}^{+0.01}\times10^{-3}$
Outer	ξ_in	107	107
reflection	n (10¹⁵ cm⁻³)	1.55 $_{- 0.10}^{+ 0.11} \times 10^{3}$ $_{-0.10}^{+0.11}\times10^3$	1.55 $_{- 0.10}^{+ 0.13} \times 10^{3}$ $_{-0.10}^{+0.13}\times10^3$
	Norm	1.11 × 10⁵(f)	1.11 × 10⁵(f)
	Flux	2.58 × 10⁻⁸	2.60 × 10⁻⁸

	χ²/ν	2158/1866	2146/1866

Notes. In model B, the reflection is modeled by kynrefionx(reflionx_hd) and its normalization parameter is fixed according to the distance of the source. Model B.1 is model B with modification in the normalization of inner reflection, introduced in the last paragraph of Section 4.2. Given errors represent 1 σ range of fitted parameters. Luminosity (L) is a free parameter within kynrefionx, representing the luminosity in units of Eddington luminosity (L_Edd) from the extended corona at inclination 66° in 2–10 keV energy range illuminating the disk to give rise to the RS. ξ(r) is computed inside the model and its value at the inner radius (ξ_in) is presented. The tabulated flux is the unabsorbed one in units of ergs cm⁻² s⁻¹, calculated from XSPEC within energy range 1 eV–1 MeV. The frozen parameters during fitting are indicated as (f). We assume emissivity index q = 3 and no radial variation of density. However, keeping q to be free or assuming the radial variation of density to be the same as that of the Keplerian disk leads to very similar best fitted parameters.

^(a)

Setting r_out of inner reflection = r_in of outer reflection leads to very similar best fitted results.

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