On the relation of optical obscuration and X-ray absorption in Seyfert galaxies

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Table 1

Sample properties.

ID		T	A_V	log N_H	log N_H	Seyfert	[OIII] λ5007 / Hβ
				BAT	variable	type
		[K]	[mag]	[cm^-2]

Circinus galaxy	0.77	691	27.2	24.4	–	1h^a	–
ESO 137-G034	<0.1	–	–	24.3	–	2^b	–
ESO 548-G081	0.87	1236	1.6	<20.0	–	1.0	5.5^c
IC 5063	0.56	947	11.3	23.6	23.3¹−23.4¹	1h^d	–
MCG -05-23-16	0.86	1207	2.3	22.2	22.1¹−22.7¹	1.9	0.07^e
NGC 1052	0.24	1239	1.5	23.0	–	1h^f	–
NGC 1068	0.92	723	24.6	25.0	–	1h^g	–
NGC 1365	0.94	1282	0.4	22.2	22.0²−25.0¹	1.8	0.08^e
NGC 1566	0.57	1479	0.0	<20.1	< 20.1⁴−21.9¹²	1.5	0.91^h
NGC 2110	0.81	967	10.5	23.0	22.5³−22.9⁴	1h^s	–
NGC 2992	0.61	1111	5.1	21.7	21.6¹−22.2¹	1.8	0.09^e
NGC 3081	0.37	977	10.0	23.9	23.7¹−23.8¹	1hⁱ	–
NGC 3227	0.67	1543	0.0	21.0	21.0⁴−23.4⁵	1.5	0.37^j
NGC 3281	0.83	732	23.9	23.9	–	2^k	–
NGC 3783	0.99	1244	1.3	20.5	20.5⁴−23.0⁶	1.5	1.07^e
NGC 4051	0.64	1305	0.0	<19.6	–	1.5	1.1^l
NGC 4388	0.78	887	14.2	23.5	23.3⁷−23.8⁷	1h^m	–
NGC 4593	0.88	1292	0.2	<19.2	–	1.5	1.85^e
NGC 5128	0.82	796	19.4	23.1	22.8⁸−23.2⁸	2ⁿ	–
NGC 5506	0.99	1223	1.9	22.4	22.3¹−22.7¹	1i^o	–
NGC 5643	<0.1	–	–	25.4	–	2^k	–
NGC 5728	<0.1	–	–	24.2	–	2^k	–
NGC 6300	0.53	677	28.4	23.3	23.3^1,9−25.0¹⁰	2^k	–
NGC 6814	0.58	1500^⋆	0.0	21.0	–	1.5	0.55^h
NGC 7130	<0.1	–	–	24.0	–	1.9^p	–
NGC 7172	0.7	822	17.8	22.9	22.9¹−23.0¹	1i^q	–
NGC 7213	0.81	1181	3.0	<20.4	–	1.5	0.79^h
NGC 7469	0.88	1355	0.0	20.5	–	1.0	6.5^r
NGC 7582	0.89	1082	6.1	24.2	22.7¹−24.1¹¹	1i^s	–

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:

^(a)

Oliva et al. (1998);

^(b)

Véron-Cetty & Véron (2010);

^(c)

Koss et al., in prep.;

^(d)

Lumsden et al. (2004);

^(e)

Schnorr-Müller et al., in prep.;

^(f)

Barth et al. (1999);

^(g)

Antonucci & Miller (1985);

^(h)

Winkler (1992);

⁽ⁱ⁾

Moran et al. (2000);

^(j)

Smith et al. (2004);

^(k)

Phillips et al. (1983);

^(l)

Grupe et al. (2004);

^(m)

Shields & Filippenko (1996);

⁽ⁿ⁾

Tadhunter et al. (1993);

^(o)

Nagar et al. (2002);

^(p)

Storchi-Bergmann et al. (1990);

^(q)

Smajić et al. (2012);

^(r)

Kim et al. (1995);

^(s)

Reunanen et al. (2003).

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