Table 2
Multiwavelength properties of the different LINER 1s in our sample.
| Galaxy name | E(B − V)Gal | α ox | log (L2500 Å) | log (L5 GHz) | R X | log (LEdd) | log (LX,crit/LEdd) | log (Lbol) | κ 2−10 keV |
| (erg s-1 Hz-1) | (erg s-1 Hz-1) | (erg s-1) | (erg s-1) | ||||||
|
|
|||||||||
| NGC 266 | 0.069 | (...) | (...) | 28.08 | –2.99 | 46.54 | –6.79 | (...) | (...) |
| NGC 315 | 0.065 | −1.15 ± 0.05 | 26.50 | 30.39 | –1.54 | 47.16 | –6.90 | 42.56 | 15.4 |
| NGC 2681 | 0.023 | (...) | (...) | (...) | (...) | 44.88 | –6.51 | (...) | (...) |
| NGC 2787 | 0.131 | (...) | (...) | 26.89 | –1.97 | 46.25 | –6.74 | (...) | (...) |
| NGC 3226 | 0.023 | −1.13 ± 0.04 | 25.60 | 27.50 | –3.49 | 46.16 | –6.73 | 41.70 | 8.3 |
| NGC 3718 | 0.014 | >−1.27 | <25.98 | 27.39 | –3.81 | 45.71 | –6.65 | 41.73 | 9.8 |
| NGC 3998 | 0.016 | −1.05 ± 0.01 | 26.24 | 28.82 | –2.79 | 47.17 | –6.90 | 42.17 | 5.8 |
| NGC 4143 | 0.013 | −1.37 ± 0.02 | 25.84 | 27.42 | –2.80 | 46.28 | –6.75 | 41.54 | 36.3 |
| NGC 4203 | 0.012 | (...) | (...) | 27.39 | –3.50 | 45.83 | –6.67 | (...) | (...) |
| NGC 4278 | 0.029 | (...) | (...) | 28.60 | –2.04 | 46.82 | –6.84 | 41.25 | 22.24 |
| 0.029 | −1.18 ± 0.02 | 25.99 | 28.60 | –2.04 | 46.82 | –6.84 | 41.83 | 11.25 | |
| NGC 4750 | 0.020 | (...) | (...) | (...) | (...) | 45.37 | –6.59 | (...) | (...) |
| NGC 4772 | 0.027 | (...) | (...) | 26.76 | –3.39 | 45.56 | –6.62 | (...) | (...) |
| NGC 5005 | 0.014 | (...) | (...) | 27.64 | –2.74 | 45.89 | –6.68 | (...) | (...) |
Notes. Columns represent: (1) the galaxy name, (2) the Galactic extinction taken from NED, used to correct the infrared, optical and UV data, (3) the αox derived for the six LINER 1s with simultaneous UV and X-ray fluxes, (4) the 2500 Å luminosity calculated from either the UVM2 or the UVW2 XMM-Newton-OM filters in erg s-1 Hz-1, (5) the core 5 GHz radio luminosity in erg s-1 Hz-1, (6) the radio loudness parameter RX, (7) the Eddington luminosity, (8) log LX,crit/LEdd = −5.356−0.17log (M/M⊙) which represents the critical 2–10 keV luminosity above which the broad-band spectrum of a given AGN is thought to become jet-dominated (Yuan & Cui 2005, see Eq. (3)), (9) the bolometric luminosity Lbol derived from the SED integration for each of the six LINER 1s with reliable SEDs, and finally (10) the bolometric, hard X-ray, correction κ2−10 keV. Two bolometric luminosities were calculated in the case of NGC 4278 corresponding to the low and high state X-ray flux level. See text for details.
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