The innermost dusty structure in active galactic nuclei as probed by 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	Date	Flux (mJy)^a					Magnitude		Host^b	AD	V² corrected	R_ring corr.	R_{τ_K} fit^d


	(UT)	Z	Y	J	H	K	J	K	(%)	fraction^c		(pc)	(pc)

AKN120	2009-12-13	11.7	11.8	16.4	26.6	60.7	12.4	10.1	0.6 ± 0.1	0.17 ± 0.05	0.822 ± 0.117	0.38 ± 0.14	0.15
IC4329A	2010-06-13	15.0	16.0	23.9	41.6	75.5	12.0	9.8	0.9 ± 0.2	0.29 ± 0.09	0.839 ± 0.119	0.21 ± 0.08	0.13
Mrk6^e	1999-02-27	–	–	16.3	29.1	53.6	12.4	10.2	0.2 ± 0.1	0.21 ± 0.05	0.890 ± 0.061	0.18 ± 0.05	0.097
3C273	2010-06-14	29.0	29.1	33.2	45.7	81.9	11.7	9.7	< 0.1	0.28 ± 0.09	0.942 ± 0.047	0.81 ± 0.34	1.1
NGC 4151	2010-06-14	51.1	54.0	81.8	136.	264.	10.7	8.5	0.2 ± 0.1	0.14 ± 0.05	0.912 ± 0.021^f	0.037 ± 0.007^g	0.037

Notes.

^(a)

Flux measurement uncertainty is ~ 5% (see Sect. 3 in Paper I).

^(b)

Host galaxy flux fraction at K-band estimated for the KI’s 50 mas FOV in the AO-corrected images.

^(c)

AD flux fraction of the point source at K-band.

^(d)

R_{τ_K} from UV luminosity using the fit by Suganuma et al. (2006).

^(e)

From 2MASS images.

^(f)

Value for the shortest baseline data.

^(g)

Best-fit value for 2010-05-01 data.

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