Notes. : fraction of non-stellar flux in the K band within an aperture of 1′′ (for most sources); T: temperature of a black body from a fit to the K-band spectrum (for errors on and T, see B15); A_V: extinction towards the hot dust (from B15; error is estimated to be 3 mag, see Sect. 2); N_H: X-ray absorbing column from Ricci et al. (2015). (formal errors are <0.2 dex); N_H variable: full range of other published N_H values for these sources; Seyfert type: for broad-line galaxies (1.0/1.2/1.5) based on the Hβ/[OIII] λ5007 ratio (see reference there) and converted to a Seyfert type according to the Winkler (1992) scheme, Seyfert 1.8/1.9: Osterbrock (1981), 1i: broad hydrogen recombination line(s) detected at infrared wavelengths, 1h: broad hydrogen recombination line(s) detected in polarized optical light; 2: no broad hydrogen recombination line detected. ^⋆ New observations with adaptive optics for NGC 6814 show much hotter dust in this source than in B15. The origin of this discrepancy is unknown and might be related to intrinsic variability. Here we adopt an intermediate value, effectively reducing the adopted A_V from 7.2 to 0.

Reference. X-ray variability: ¹: Risaliti et al. (2002), ²: Walton et al. (2014), ³: Rivers et al. (2014), ⁴: Ricci et al. (in prep.), ⁵: Lamer et al. (2003), ⁶: Markowitz et al. (2014), ⁷: Fedorova et al. (2011), ⁸: Beckmann et al. (2011), ⁹: Guainazzi (2002), ¹⁰: Leighly et al. (1999), ¹¹: Bianchi et al. (2009), ¹²: Kawamuro et al. (2013). Seyfert types and line ratios: