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Table 1.

Properties of the 16 radio-loud AGN in our sample.

Object Class z B Fmid − IR F6 cm R i MBH Gal NH Fsoft Fhard LX Lbol λ
(1) (2) (a) (3) (a) (4) (a) (5) (6) (7) (k) (8) (9) (10) (ah) (11) (k) (12) (k) (13) (k) (14) (k) (15) (k)
1H 0323+342 S1n 0.063 15.72 n/a 0.30 (d) 130 13 (l) 0.36 (v) 21.7 0.53 0.81 0.278 2.08 0.46
3C 59 S1.8 0.111 16.80 n/a 0.02 (d) 22 n/a 7.94 (w) 6.59 0.36 0.86 0.538 3.88 0.04
3C 120 S1.5 0.033 15.72 0.54 (b) 0.36 (e) 154 21 (m) 0.69 (x) 19.4 3.03 5.27 0.309 2.33 0.27
3C 273 S1.0 0.158 13.05 0.60 (b) 38.4 (f) 1407 20 (n) 65.9 (y) 1.77 5.34 7.93 9.16 97.4 0.12
3C 382 S1.0 0.058 16.50 0.09 (b) 0.15 (d) 128 40 (o) 11.5 (z) 8.96 2.03 3.44 0.544 4.07 0.03
3C 390.3 S1.5 0.056 16.06 0.22 (b) 0.12 (e) 70 33 (o) 2.87 (aa) 4.41 2.10 3.48 0.459 3.36 0.09
4C +31.63 S1.0 0.298 15.85 0.07 (b) 1.40 (d) 676 10 (p) 20.0 (ab) 12.0 0.28 0.45 3.28 29.0 0.11
4C +34.47 S1.0 0.206 15.58 0.05 (b) 0.37 (d) 139 35 (q) 3.16 (ac) 3.36 0.70 0.86 2.19 16.4 0.41
4C +74.26 S1.0 0.104 15.13 0.14 (b) 0.32 (g) 79 40 (r) 41.7 (ad) 23.1 0.85 2.46 1.41 10.4 0.02
ESO 075-G041 S1 0.028 14.78 0.12 (c) 13.4 (h) 2416 10 (s) n/a 2.90 0.49 0.67 0.023 0.31 n/a
III Zw 2 S1.2 0.089 15.96 0.13 (b) 0.43 (d) 233 21 (q) 0.72 (x) 7.13 0.39 0.72 0.251 1.94 0.21
Mrk 6 S1.5 0.019 15.16 0.55 (b) 0.10 (d) 26 9 (t) 1.80 (ae) 9.80 0.17 1.51 0.026 0.23 0.01
Mrk 896 S1n 0.027 15.27 0.13 (c) 0.04 (i) 11 24 (u) 0.12 (af) 4.03 0.54 0.37 0.021 0.15 0.10
PKS 0405–12 S1.2 0.574 15.09 0.09 (b) 1.99 (j) 477 n/a 29.5 (ad) 4.16 0.39 0.43 13.4 112 0.30
PKS 0921–213 S1 0.053 16.50 n/a 0.42 (h) 369 n/a 0.79 (w) 5.75 0.41 0.68 0.083 0.67 0.07
PKS 2135–14 S1.5 0.200 15.63 0.11 (b) 1.33 (h) 525 n/a 44.7 (ag) 5.22 0.36 0.60 1.21 10.2 0.02

Notes. (1) Name of the AGN. (2) Spectral classification. (3) Cosmological redshift. (4) B magnitude. (5) Mid-IR (MIPS 24 μm or IRAS 25 μm) flux in Jy. (6) 6 cm (5 GHz) flux in Jy. (7) Radio-loudness parameter R. (8) Inclination angle of the radio jet axis relative to our line of sight in degrees. (9) Mass of the SMBH in 108 M⊙. (10) Milky Way neutral NH in our line of sight in 1020 cm−2. (11) Soft X-ray (0.3–2 keV) observed flux in 10−11 erg cm−2 s−1 derived from our XMM-Newton spectral modelling. (12) Hard X-ray (2–10 keV) observed flux in 10−11 erg cm−2 s−1 derived from our XMM-Newton spectral modelling. (13) Intrinsic X-ray luminosity over 0.3–10 keV in 1045 erg s−1 derived from our XMM-Newton spectral modelling. (14) Intrinsic bolometric luminosity of the AGN in 1045 erg s−1. (15) The Eddington ratio λ = Lbol/LEdd.

References. (a)Véron-Cetty & Véron (2010). (b)Spitzer MIPS 24 μm from IRSA. (c)IRAS 25 μm from Moshir et al. (1990). (d)Laurent-Muehleisen et al. (1997). (e)Dodson et al. (2008). (f)Gear et al. (1994). (g)Kuehr et al. (1981). (h)Wright & Otrupcek (1990). (i)Bicay et al. (1995). (j)Shimmins & Bolton (1972). (k)Calculated in this paper. (l)Karamanavis (2015). (m)Jorstad et al. (2005). (n)Stawarz (2004). (o)Giovannini et al. (2001). (p)Hogan et al. (2011). (q)Rokaki et al. (2003). (r)Ballantyne & Fabian (2005). (s)Worrall et al. (2012). (t)Kharb et al. (2006). (u)Page et al. (2003). (v)Foschini et al. (2015). (w)Sikora et al. (2007). (x)Grier et al. (2017). (y)Paltani & Türler (2005). (z)Marchesini et al. (2004). (aa)Peterson et al. (2004). (ab)Veilleux et al. (2009). (ac)Vasudevan & Fabian (2007). (ad)Woo & Urry (2002). (ae)Doroshenko et al. (2012). (af)Piotrovich et al. (2015). (ag)Mingo et al. (2014). (ah)Willingale et al. (2013).

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