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Home All issues Volume 705 (January 2026) A&A, 705 (2026) A59 Full HTML
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Table 1.

Properties of the sample.

(1) (2) (3) (4) (5) (6) (7) (8)
Object D log LBAT log P1.4GHz log P4.8 GHz log LH log LIR Sub-samples
[Mpc] [erg/s] [W/Hz] [W/Hz] [erg/s] [erg/s]
Arp220 78.8 – 23.36 23.20 43.19 45.68 SF
Centaurus A 3.1a 42.19 21.71a 21.83a 41.19 43.25 BAT; [MgV]
Cygnus A 240.9 44.98 26.74b 27.15b 43.58 45.79 BAT; RS; [MgV]; IR
ESO137-G034 31.0b 42.43 – – 42.54 44.05 BAT; [MgV]
ESO420-G13 51.0 – 22.30 – 43.06 44.95 [MgV]; IR
IC5063 48.6 43.28 23.73c 23.17c 43.06 45.13 BAT; RS; [MgV]; IR
IIZw96 154.7 – 23.08 22.26d 42.72 45.82 IR
IRAS05189–2524 188.8 43.60 23.07 – 44.13 46.13 BAT; IR
IRAS07251–0248 375.2 – 23.27 – 43.73 45.91 IR
IRAS09022–3615 255.6 – 23.80 – 43.77 45.92 RS; IR
IRAS09111–1007 232.0 – 22.26 – 43.81 45.38 SF
IRAS10565+2448 184.7 – 23.35 – 43.91 45.68 SF
IRAS13120–5453 131.8 – 23.49c 23.12c 43.96 45.91 SF
IRAS14348–1447 352.8 – 23.69 – 43.74 45.00 SF
IRAS15250+3609 236.6 – 22.96 – 43.56 45.89 IR
IRAS19297–0406 367.4 – 23.64 – 43.89 45.85 SF
IRAS19542+1110 278.4 – 23.25 – 43.97 45.72 SF
IRAS20551–4250 184.3 – 23.08e – 43.58 45.85 IR
IRAS22491–1808 333.2 – 22.86 – 43.61 45.78 SF
IRAS23128–5919 191.1 – – – 43.31 45.85 IR
IRASF01364–1042 206.7 – 22.87 22.76 43.26 45.20 IR
IRASF08572+3915NW 249.4 – 22.48 – 43.09 46.07 IR
IRASF14378–3651 289.9 – 23.50 – 43.71 45.68 IR
IRASF23365+3604 276.3 – 23.37 – 43.78 45.81 IR
M81 3.3c 40.42 20.05 20.11 41.80 42.32 BAT
M87 15.8d – 24.64 24.24 42.23 42.79 RS
M94 4.2e – 19.41 20.35 42.09 42.84 SF
M104 8.0f – 20.86 21.08f 42.43 42.37 SF
MCG-05-23-016 36.6 43.52 21.36 – 42.97 44.70 BAT; [MgV]; IR
Mrk231 180.7 – 24.06 24.19 44.81 46.46 RS; IR
Mrk273 160.0 43.18 23.63 23.33 43.73 45.81 BAT; [MgV]; IR
NGC 0253 3.5e – 21.59 21.55h 41.38 44.37 SF
NGC 0424 50.4 42.81 21.84 – 43.23 44.86 BAT; IR
NGC 1052 19.2g 42.14 22.60 23.14f 42.75 43.63 BAT
NGC 1068 10.1h 41.66 22.77 22.29g 42.90 45.23 BAT; [MgV]; IR
NGC 1365 18.3i 42.40 22.18 22.08h 42.00 44.90 BAT; [MgV]
NGC 1566 6.6g 41.01 20.93c 20.72i 41.62 42.71 BAT; [MgV]
NGC 1808 9.5j – 21.76 21.41i 42.21 44.47 SF
NGC 3081 23.8k 42.74 20.56 – 42.30 44.10 BAT; [MgV]
NGC 3256N 40.1 – – – 43.06 45.60 SF
NGC 3256S 40.1 – 23.07c 22.78i 43.17 – IR
NGC 4258 6.8l 41.11 21.44 21.23b 41.80 42.76 BAT
NGC 4395 4.4m 40.81 19.75 18.07i 39.78 41.61 BAT; [MgV]
NGC 5506 23.8n 43.21 22.36 22.09k 42.92 44.57 BAT; [MgV]; IR
NGC 5728 39.0o 43.18 22.10 – 42.86 44.36 BAT; [MgV]
NGC 6240 104.2 43.94 23.73 23.32 43.89 45.66 BAT, RS; [MgV]
NGC 6552 113.7 43.50 22.68 22.70d 43.48 45.25 BAT; [MgV]; IR
NGC 7172 37.4 43.42 21.79 – 42.88 44.20 BAT; [MgV]; IR
NGC 7319 96.5 43.60 22.76 – 43.11 44.59 BAT; [MgV]; IR
NGC 7469 69.7 43.61 23.01 22.60 43.75 45.56 BAT; [MgV]
NGC 7582 23.2 42.72 22.22e 21.68k 43.02 44.77 BAT; [MgV]; IR
UGC05101 168.7 43.37 23.75 23.40 43.88 45.54 BAT, RS; IR
VV114 86.0 – 23.33 22.92f 43.20 45.58 IR
VV340a 144.3 – 23.34 22.81 43.87 45.05 [MgV]

Notes. (1) Galaxy name; (2) Distances were taken from the literature when available; otherwise, they were estimated from the redshift, assuming a cosmology with h = 0.7, Ωm = 0.3, and ΩΛ = 0.7. Superscript letters indicate the corresponding references: a: Majaess et al. (2008), b: Willick et al. (1997), c: Gerke et al. (2011), d: Oldham & Auger (2016), e: Radburn-Smith et al. (2011), f: Spitler et al. (2006), g: Tully et al. (2013), h: Nasonova et al. (2011), i: Riess et al. (2016), j: Tully et al. (2016), k: Bottinelli et al. (1984), l: Hoffmann & Macri (2015), m: Sabbi et al. (2018), n: Karachentsev et al. (2014), o: Rest et al. (2014); (3) Hard X-ray (14–195 keV) luminosity from Oh et al. (2018); (4) 1.4 GHz power taken from the NRAO VLA Sky Survey (NVSS; Condon et al. 1998), and supplemented with additional data from the literature (indicated by superscripts): a: Tingay et al. (2003), b: Steenbrugge et al. (2010), c: Allison et al. (2014), d: Brown et al. (2017), e: Condon et al. (1996); (5) 4.8 GHz radio power taken from the Green Bank 4.85 GHz survey (Gregory et al. 1996), with additional data from the literature (indicated by superscripts): a: Tingay et al. (2003), b: Becker et al. (1991), c: Wright et al. (1994), d: Gregory & Condon (1991), e: Baan & Klöckner (2006), f: Griffith et al. (1994), g: Sajina et al. (2011), h: Stil et al. (2009), i: Wright et al. (1994), j: Nagar et al. (2005), k: Orienti & Prieto (2010). (6) H-band luminosity from The Two Micron All Sky Survey (2MASS; Skrutskie et al. 2006); (7) IR luminosity obtained from the WISE W4 luminosity (Wright et al. 2010) using the relation from Cluver et al. (2017). The northern nucleus of NGC 3256 is an order of magnitude brighter in IR than the southern nucleus (Bohn et al. 2024); thus, we quote LIR only for the northern nucleus. High-resolution IR data reveal an AGN in the southern nucleus (Ohyama et al. 2015), which is included in our IR AGN sample. For IRAS 13120-5453, LIR was estimated from the 25 μm IRAS flux, as WISE magnitudes are unavailable; (8) The sub-samples to which each object belongs.

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