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Table 2:

Point-source flux from UKIRT imaging data and the KI results corrected for host galaxy and unresolved AD component.

Name
Flux (mJy)   Magnitude Hosta AD V2 corrected $R_{\rm ring}$ corr. $R_{\rm\tau_K}$ fitc
  Z Y J H K   J H K (%) fractionb   (pc) (pc)
NGC 4151 39.7 42.4 59.4 96.3 173.   11.0 10.1 8.9 0.3 $\pm$ 0.1 0.17 $\pm$ 0.06 0.841 $\pm$ 0.024 0.041 $\pm$ 0.004 0.033
NGC 4051 8.88 9.98 14.9 24.8 46.1   12.6 11.6 10.4 1.5 $\pm$ 1.0 0.14 $\pm$ 0.05 0.870 $\pm$ 0.038 0.032 $\pm$ 0.005 0.011
Mrk231 21.0 22.0 33.5 71.6 152.   11.7 10.4 9.1 0.5 $\pm$ 0.1 0.15 $\pm$ 0.05 0.921 $\pm$ 0.033 0.33 $\pm$ 0.07 0.33
IRAS 13349 7.75 8.71 12.6 26.3 62.3   12.7 11.5 10.0 0.4 $\pm$ 0.1 0.14 $\pm$ 0.04 0.856 $\pm$ 0.021 0.92 $\pm$ 0.06 0.49

a Host galaxy flux fraction at K-band estimated for the KI's 50 mas FOV in the AO-corrected images. b AD flux fraction of the point source at K-band. c $R_{\rm\tau_K}$ from UV luminosity using the fit by Suganuma et al. (2006). It has an uncertainty of a factor of $\sim$1.5 based on the scatter of the fit (see text).

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