The properties of the obscuring material of a sample of active galactic nuclei from mid-IR and X-ray simultaneous fitting

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Table 3.

General information of the sample.

Objname	z	N_{H_Gal}	L_{X_{(2 − 10 KeV)}}	L_bol	log(M_BH)	L/L_edd	mid-IR
		[cm⁻²]	[erg s⁻¹]	[erg s⁻¹]	[M_⊙]		model
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
			Seyfert 1

Mrk590	0.0213	0.040	42.57 $\pm_{0.02}^{0.02}$ $\pm_{0.02}^{0.02}$	43.36	7.57 ⁽¹⁾	–2.32	`Clumpy`
PG0804+761	0.1000	0.038	42.55 $\pm_{0.01}^{0.01}$ $\pm_{0.01}^{0.01}$	45.30	8.73 ⁽¹⁾	–1.54	`Two-Phases`
I11119+3257	0.1890	0.024	44.12 $\pm_{0.08}^{0.06}$ $\pm_{0.08}^{0.06}$	45.17	7.30 ⁽²⁾	–0.24	`Two-Phases`
Mrk231	0.0422	0.010	42.78 $\pm_{0.04}^{0.04}$ $\pm_{0.04}^{0.04}$	43.6	8.40 ⁽³⁾	–2.91	`Two-Phases`
Mrk1383	0.0866	0.035	44.30 $\pm_{0.01}^{0.01}$ $\pm_{0.01}^{0.01}$	45.23	9.01 ⁽¹⁾	–1.89	`Two-Phases`
Mrk1392	0.0361	0.050	43.18 $\pm_{0.02}^{0.02}$ $\pm_{0.02}^{0.02}$	44.09	7.87 ⁽¹⁾	–1.89	`Clumpy`
ESO141-G055	0.0371	0.118	43.94 $\pm_{0.01}^{0.01}$ $\pm_{0.01}^{0.01}$	44.91	7.99 ⁽¹⁾	–1.19	`Two-Phases`
NGC7213	0.0051	0.017	41.98 $\pm_{0.01}^{0.01}$ $\pm_{0.01}^{0.01}$	42.80	7.13 ⁽¹⁾	–2.44	`Clumpy`

			Seyfert 2

UM146	0.0144	0.079	41.84 $\pm_{0.07}^{0.06}$ $\pm_{0.07}^{0.06}$	42.82	6.83 ⁽⁴⁾	–2.12	`Clumpy`
NGC788	0.0136	0.029	42.43 $\pm_{0.07}^{0.06}$ $\pm_{0.07}^{0.06}$	43.41	8.18 ⁽¹⁾	–2.88	`Clumpy`
NGC1052	0.0048	0.029	41.74 $\pm_{0.01}^{0.01}$ $\pm_{0.01}^{0.01}$	42.55	8.82 ⁽¹⁾	–4.38	`Clumpy`
NGC1358	0.0134	0.066	42.38 $\pm_{0.03}^{0.02}$ $\pm_{0.03}^{0.02}$	43.83	8.10 ⁽³⁾	–2.38	`Clumpy`
J05081967+1721483	0.0175	0.383	42.97 $\pm_{0.02}^{0.02}$ $\pm_{0.02}^{0.02}$	43.83	8.35 ⁽¹⁾	–2.63	`Two-Phases`
Mrk78	0.0371	0.038	43.11 $\pm_{0.05}^{0.05}$ $\pm_{0.05}^{0.05}$	44.05	8.53 ⁽¹⁾	–2.59	`Clumpy`
Mrk1210	0.0135	0.033	44.63 $\pm_{0.02}^{0.02}$ $\pm_{0.02}^{0.02}$	43.78	6.86 ⁽¹⁾	–1.19	`Two-Phases`
J10594361+6504063	0.0836	0.028	43.66 $\pm_{0.02}^{0.02}$ $\pm_{0.02}^{0.02}$	44.63	8.25 ⁽¹⁾	–1.73	`Smooth`
NGC4507	0.0118	0.105	43.17 $\pm_{0.01}^{0.01}$ $\pm_{0.01}^{0.01}$	44.21	7.81 ⁽¹⁾	–1.71	`Clumpy`
NGC4939	0.0085	0.044	42.0 $\pm_{0.04}^{0.04}$ $\pm_{0.04}^{0.04}$	43.00	7.75 ⁽¹⁾	–2.86	`Two-Phases`
IC4518W	0.0162	0.170	42.68 $\pm_{0.06}^{0.05}$ $\pm_{0.06}^{0.05}$	43.61	7.64 ⁽¹⁾	–2.14	`Two-Phases`
ESO138-G1	0.0091	0.217	42.43 $\pm_{0.04}^{0.04}$ $\pm_{0.04}^{0.04}$	42.57	6.57 ⁽¹⁾	–2.11	`Clumpy`
NGC6300	0.0029	0.105	41.86 $\pm_{0.01}^{0.01}$ $\pm_{0.01}^{0.01}$	42.69	6.77 ⁽¹⁾	–2.19	`Two-Phases`
ESO103-G35	0.0133	0.082	43.23 $\pm_{0.01}^{0.01}$ $\pm_{0.01}^{0.01}$	44.15	7.37 ⁽¹⁾	–1.33	`Clumpy`
IC5063	0.0088	0.067	42.55 $\pm_{0.02}^{0.01}$ $\pm_{0.02}^{0.01}$	43.47	8.24 ⁽¹⁾	–2.88	`Clumpy`
PKS2356-61	0.0963	0.015	43.96 $\pm_{0.04}^{0.04}$ $\pm_{0.04}^{0.04}$	45.15	8.55 ⁽¹⁾	–1.51	`Clumpy`

Notes. Columns from 1 to 8 correspond to the object name, redshift, galactic column density (obtained by the N_H tool within HEASOFT), intrinsic (not absorbed) X-ray luminosity (obtained through the clumin tool from Xspec), black hole mass, Eddington ratio, and the best mid-IR model obtained from individual fits, respectively. The bolometric luminosity is computed from the X-ray luminosities reported in Col. 5 of this table and using the relationship L_bol = kL_X(2 − 10 keV), where the bolometric correction (k) is determined by a fourth-order polynomial dependent on L(2 − 10 keV) (Marconi et al. 2004). Superscript numbers (1) to (4) next to the M_BH values indicate the references used for the black hole mass estimates: (1) Koss et al. (2022), (2) Yang et al. (2020), (3) Osorio-Clavijo et al. (2022), and (4) van den Bosch (2016).

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