Exploring the inner region of type 1 AGNs with the Keck interferometer

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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			Host^a	AD	V² corrected	$R_{\rm ring}$ corr.	$R_{\rm\tau_K}$ fit^c
	Z	Y	J	H	K	J	H	K	(%)	fraction^b		(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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