The dust-gas AGN torus as constrained from X-ray and mid-infrared observations

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Volume 651 (July 2021)

A&A, 651 (2021) A91

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Table 2.

General properties of the sample.

Object	Coordinates		Type ^( * )	z	L_X	M_BH ^( * )	Obsid	Exptime	N_H
	RA	Dec			log(L_{2 − 10 KeV})	log(M/M_⊙)		(ks)	variability
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)
Mrk 1018	02 06 15.98	−00 17 29.22	Sy1.8	0.0424		8.03⁽¹⁾	60301022003	43.3	N¹
Mrk 590	02 14 33.56	−00 46 00.18	Sy1.2	0.0213		7.20⁽²⁾	90201043002	51.0	N²
PG 0804+761	08 10 58.66	+76 02 42.45	Sy1	0.1000		8.73⁽¹⁾	60160322002	17.3	N³
RBS 0770	09 23 43.00	+22 54 32.57	Sy1.2	0.0323		7.34⁽¹⁾	60061092002	18.8	–
I 11119+3257	11 14 38.89	+32 41 33.48	Sy1	0.1890		8.4⁽³⁾	60101045002	10.4	Y⁴
PG 1211+143	12 14 17.67	+14 03 13.18	Sy1	0.0904		7.49⁽²⁾	60001100007	74.8	N⁵
RBS 1125	12 32 03.62	+20 09 29.49	Sy1	0.0630		7.76⁽¹⁾	60061229002	19.9	–
Mrk 231	12 56 14.23	+56 52 25.24	Sy1	0.0422		8.39⁽³⁾	80302608002	82.0	N⁶
Mrk 1383	14 29 06.57	+01 17 06.15	Sy1	0.0866		8.65⁽³⁾	60061254002	32.4	N⁷
Mrk 1392	15 05 56.55	+03 42 26.34	Sy1.8	0.0361		8.17⁽¹³⁾	60160605002	21.0	–
Mrk 1393	15 08 53.95	−00 11 48.99	Sy1.5	0.0543		7.87⁽¹⁾	60376005002	30.8	Y⁸
PG 1535+547	15 36 38.40	+54 33 33.21	Sy1	0.0451		7.19⁽⁴⁾	60201023004	82.1	N⁹
ESO 141-G055	19 21 14.15	−58 40 12.98	Sy1.2	0.0371		−	60201042002	93.0	–
NGC 7213	22 09 16.21	−47 10 00.08	Sy1.5	0.0051		7.99⁽²⁾	60001031002	10.1	N¹⁰
MCG+01-57-016	22 40 17.06	+08 03 13.52	Sy1.8	0.0249		7.20⁽¹³⁾	60061343002	21.3	–

UM 146	01 55 22.02	+06 36 42.42	Sy2	0.0144	41.84	6.23⁽¹³⁾	60465002002	28.4	–
NGC 788	02 01 06.46	−06 48 57.15	Sy2	0.0136	42.43	7.51⁽²⁾	60061018002	15.4	N¹²
NGC 1052	02 41 04.79	−08 15 20.75	Sy2	0.0048	41.74	8.19⁽²⁾	60201056002	59.6	Y¹³
NGC 1358	03 33 39.68	−05 05 22.23	Sy2	0.0134	42.38	7.88⁽²⁾	60301026002	49.8	–
J05081967+1721483	05 08 19.71	+17 21 48.09	Sy2	0.0175	42.97	−	60006011002	15.5	–
Mrk 3	06 15 36.45	+71 02 15.24	Sy2	0.0143	43.53	8.65⁽²⁾	60002048004	33.4	N¹⁴
ESO 428-G014	07 16 31.21	−29 19 28.89	Sy2	0.0054	39.83	7.3⁽⁵⁾	60001152002	40.2	–
Mrk 78	07 42 41.70	+65 10 37.43	Sy2	0.0371	43.11	7.87⁽²⁾	60061336002	24.1	–
Mrk 1210	08 04 05.86	+05 06 49.81	Sy2	0.0135	44.63	7.1⁽⁶⁾	60061078002	15.4	Y¹⁴
J10594361+6504063	10 59 43.62	+65 04 06.37	Sy2	0.0836	43.66	−	60061207002	25.9	–
NGC 4388	12 25 46.82	+12 39 43.45	Sy2	0.0045	41.87	8.54⁽⁷⁾	60061228002	21.3	N¹¹
NGC 4507	12 35 36.63	−39 54 33.66	Sy2	0.0118	43.17	8.25⁽⁷⁾	60102051004	34.4	Y¹¹
NGC 4939	13 04 14.33	−10 20 22.32	Sy2	0.0085	42.0	−	60002036002	22.0	Y¹⁶
ESO 097-G013	14 13 09.91	−65 20 20.47	Sy2	0.0009	40.78	7.95⁽⁸⁾	60002039002	53.8	N¹⁴
IC 4518W	14 57 40.50	−43 07 54.00	Sy2	0.0162	42.68	−	60061260002	7.78	–
ESO 138-G1	16 51 20.27	−59 14 04.28	Sy2	0.0091	42.43	6.7⁽⁹⁾	60201040002	45.6	N¹⁴
NGC 6300	17 16 59.47	−62 49 13.98	Sy2	0.0029	41.86	5.45⁽¹⁰⁾	60261001004	23.5	N¹⁴
ESO 103-G35	18 38 20.32	−65 25 39.14	Sy2	0.0133	43.23	7.0⁽¹¹⁾	60301004002	43.7	–
MCG+07-41-03	19 59 28.36	+40 44 02.09	Sy2	0.0561	44.61	−	60001083002	43.6	Y¹⁵
IC 5063	20 52 02.33	−57 04 07.60	Sy2	0.0088	42.55	7.74⁽²⁾	60061302002	18.4	Y¹⁰
PKS 2356−61	23 59 04.36	−60 54 59.41	Sy2	0.0963	43.96	8.96⁽¹²⁾	60061330002	23.0	N¹⁷

Notes. ^( * )Classification obtained from NASA/IPAC Extragalactic Database (NED) (https://ned.ipac.caltech.edu/). Note that UM 146 is classified as Sy2. However, its classification is controversial; It is also classified as Sy1.9 according to NED. The intrinsic (not absorbed) X-ray luminosity obtained through clumin tool from Xspec. References M_BH: (1) Kamraj et al. (2018); (2) Woo & Urry (2002); (3) Sani et al. (2010); (4) Vestergaard & Peterson (2006); (5) Fabbiano et al. (2019); (6) Clouse et al. (2011); (7) Nicastro et al. (2003); (8) Walton et al. (2013b); (9) Piconcelli et al. (2011); (10) Awaki et al. (2005); (11) Wilkes et al. (2001); (12) Ursini et al. (2018); and (13) mass calculated using the M_BH ∝ σ relationship, using the σ values reported in the hyperleda database (http://leda.univ-lyon1.fr) (Makarov et al. 2014). References for the N_H variability: (1) Krumpe et al. (2017); (2) Denney et al. (2014); (3) Papadakis et al. (2003); (4) Tombesi et al. (2017); (5) Reeves et al. (2018); (6) Teng et al. (2014); (7) Scott et al. (2004); (8) Wang et al. (2009); (9) Ballo et al. (2008); (10) Burtscher et al. (2016); (11) Risaliti et al. (2002); (12) Hernández-García et al. (2015); (13) Osorio-Clavijo et al. (2020); (14) Hernández-García et al. (2016); (15) Laha et al. (2020); (16) Guainazzi et al. (2005); and (17) Ursini et al. (2018).

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