Relativistic reflection within an extended hot plasma geometry

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Volume 704 (December 2025)

A&A, 704 (2025) A129

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Table 2.

Comparison of the lamp post and extended models for ESO 033-G002.

Parameter	Model 1a	Model 1b	Model 2a	Model 2b
TBABS_full
N_H	$1 . 65_{- 0.20}^{+ 0.18}$ $1.65^{+0.18}_{-0.20}$	$1 . 59_{- 0.31}^{+ 0.20}$ $1.59^{+0.20}_{-0.31}$	$1 . 56_{- 0.36}^{+ 0.22}$ $1.56^{+0.22}_{-0.36}$	$1 . 55_{- 0.30}^{+ 0.23}$ $1.55^{+0.23}_{-0.30}$

TBABS_part
N_H	7.8 ± 1.3	$8 . 0_{- 1.6}^{+ 1.0}$ $8.0^{+1.0}_{-1.6}$	$8 . 0_{- 1.9}^{+ 1.3}$ $8.0^{+1.3}_{-1.9}$	$7 . 9_{- 1.6}^{+ 1.2}$ $7.9^{+1.2}_{-1.6}$
C_f	$0 . 791_{- 0.023}^{+ 0.020}$ $0.791^{+0.020}_{-0.023}$	$0 . 792_{- 0.020}^{+ 0.021}$ $0.792^{+0.021}_{-0.020}$	$0 . 786_{- 0.020}^{+ 0.024}$ $0.786^{+0.024}_{-0.020}$	$0 . 790_{- 0.018}^{+ 0.024}$ $0.790^{+0.024}_{-0.018}$

XSTAR
N_H	$5 . 9_{- 1.7}^{+ 2.1}$ $5.9^{+2.1}_{-1.7}$	$5 . 2_{- 2.3}^{+ 2.6}$ $5.2^{+2.6}_{-2.3}$	$4 . 7_{- 2.2}^{+ 2.5}$ $4.7^{+2.5}_{-2.2}$	$4 . 8_{- 2.0}^{+ 2.9}$ $4.8^{+2.9}_{-2.0}$
log ξ	$3 . 45_{- 0.06}^{+ 0.05}$ $3.45^{+0.05}_{-0.06}$	$3 . 45_{- 0.07}^{+ 0.06}$ $3.45^{+0.06}_{-0.07}$	$3 . 44_{- 0.08}^{+ 0.06}$ $3.44^{+0.06}_{-0.08}$	$3 . 44_{- 0.07}^{+ 0.06}$ $3.44^{+0.06}_{-0.07}$
${v_{out}}^{a}$ ${v_{\mathrm{out}}}^{a}$	$4800_{- 900}^{+ 930}$ $4800^{+930}_{-900}$	$4830_{- 900}^{+ 1030}$ $4830^{+1030}_{-900}$	$5010_{- 900}^{+ 930}$ $5010^{+930}_{-900}$	$4830_{- 1200}^{+ 1200}$ $4830^{+1200}_{-1200}$

RELXILL
i	$50 . 7_{- 3.4}^{+ 2.9}$ $50.7^{+2.9}_{-3.4}$	$50 . 8_{- 2.5}^{+ 4.0}$ $50.8^{+4.0}_{-2.5}$	$50 . 1_{- 3.1}^{+ 3.0}$ $50.1^{+3.0}_{-3.1}$	$50 . 3_{- 2.3}^{+ 3.0}$ $50.3^{+3.0}_{-2.3}$
a	> 0.97	> 0.94	> 0.93	> 0.93
h	< 2.0	< 3.2	< 2.4	< 3.4
x	0.0	0.0	< 2.1	< 1.8
Γ	1.75 ± 0.08	$1 . 68_{- 0.07}^{+ 0.09}$ $1.68^{+0.09}_{-0.07}$	$1 . 63_{- 0.07}^{+ 0.09}$ $1.63^{+0.09}_{-0.07}$	$1 . 65_{- 0.06}^{+ 0.10}$ $1.65^{+0.10}_{-0.06}$
log ξ	$3 . 10_{- 0.17}^{+ 0.27}$ $3.10^{+0.27}_{-0.17}$	$2 . 5_{- 0.5}^{+ 0.4}$ $2.5^{+0.4}_{-0.5}$	$2 . 93_{- 0.27}^{+ 0.16}$ $2.93^{+0.16}_{-0.27}$	$2 . 81_{- 0.47}^{+ 0.14}$ $2.81^{+0.14}_{-0.47}$
log n	< 17.7	< 18.3	< 19.1	< 18.2
A_Fe	$4 . 0_{- 1.1}^{+ 1.6}$ $4.0^{+1.6}_{-1.1}$	$4 . 7_{- 1.3}^{+ 2.5}$ $4.7^{+2.5}_{-1.3}$	$5 . 2_{- 1.7}^{+ 3.4}$ $5.2^{+3.4}_{-1.7}$	$5 . 1_{- 1.7}^{+ 2.8}$ $5.1^{+2.8}_{-1.7}$
kT_e	$56_{- 13}^{+ 46}$ $56^{+46}_{-13}$	$43_{- 16}^{+ 19}$ $43^{+19}_{-16}$	$50_{- 14}^{+ 29}$ $50^{+29}_{-14}$	$38_{- 9}^{+ 17}$ $38^{+17}_{-9}$
BOOST	$0 . 71_{- 0.26}^{+ 0.73}$ $0.71^{+0.73}_{-0.26}$	> 0.26	> 0.76	1^b
Norm	$9_{- 5}^{+ 10}$ $9^{+10}_{-5}$	$4 . 9_{- 4.8}^{+ 5.9}$ $4.9^{+5.9}_{-4.8}$	$0 . 36_{- 0.18}^{+ 11.78}$ $0.36^{+11.78}_{-0.18}$	$2 . 6_{- 2.3}^{+ 24.8}$ $2.6^{+24.8}_{-2.3}$

XILLVER_CP
Norm	$9 . 6_{- 2.5}^{+ 3.3}$ $9.6^{+3.3}_{-2.5}$	$8 . 1_{- 2.3}^{+ 3.3}$ $8.1^{+3.3}_{-2.3}$	$7 . 3_{- 2.2}^{+ 3.9}$ $7.3^{+3.9}_{-2.2}$	$6 . 9_{- 1.8}^{+ 3.9}$ $6.9^{+3.9}_{-1.8}$

APEC
kT	$0 . 88_{- 0.08}^{+ 0.09}$ $0.88^{+0.09}_{-0.08}$	$0 . 90_{- 0.09}^{+ 0.11}$ $0.90^{+0.11}_{-0.09}$	$0 . 93_{- 0.10}^{+ 0.12}$ $0.93^{+0.12}_{-0.10}$	$0 . 92_{- 0.10}^{+ 0.11}$ $0.92^{+0.11}_{-0.10}$
Norm	$7 . 4_{- 2.0}^{+ 2.2}$ $7.4^{+2.2}_{-2.0}$	$6 . 5_{- 2.0}^{+ 2.1}$ $6.5^{+2.1}_{-2.0}$	$5 . 9_{- 2.0}^{+ 2.3}$ $5.9^{+2.3}_{-2.0}$	$6 . 1_{- 2.0}^{+ 2.4}$ $6.1^{+2.4}_{-2.0}$

NTHCOMP_scat
Norm	$28_{- 6}^{+ 4}$ $28^{+4}_{-6}$	$32_{- 5}^{+ 4}$ $32^{+4}_{-5}$	$34_{- 4}^{+ 3}$ $34^{+3}_{-4}$	$33_{- 5}^{+ 4}$ $33^{+4}_{-5}$

χ²/D.o.F	458.0/401	458.8/401	458.6/400	458.8/401

Notes. Model 1a corresponds to the lamp post model with constant disk density and no returning radiation, Model 1b includes returning radiation and an α-disk density gradient. Model 2a differs from Model 1b by varying the new parameter x, while in Model 2b the BOOST parameter is fixed. All uncertainties are given at 90% confidence. Units of N_H are in 10²² cm⁻², the ionization ξ in erg cm s⁻¹, density n in cm⁻³, inclination i in degrees, height h and radius x in r_g, and model temperatures kT in keV. The normalizations are given in units of 10⁻⁶ cm⁻² s⁻¹ keV⁻¹, Norm_RELXILL is in units of 10⁻⁴ cm⁻² s⁻¹ keV⁻¹. The iron abundance, A_Fe is relative to the interstellar medium abundance of Wilms et al. (2000). a: Outflow velocities are calculated from the redshift parameter z of XSTAR as v_out = (z_cosmological − z)c; b: for Model 2b, the BOOST parameter is fixed.

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