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Astron. Astrophys. 338, 8-14 (1998)

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7. Discussion

We have observed the Seyfert galaxy WKK 6092 at different wavelengths. The resulting data are summarized in Table 2.

WKK 6092 and its neighbour are both members of ACO 3627. They have similar redshifts but show no indications of interaction. The morphology of both galaxies do not seem distorted (cf., Fig. 1). The Seyfert has a very blue nucleus, a distinct bar and a ring superimposed on an otherwise smooth disk.

An upper limit for the Galactic foreground extinction in the line of sight of the Seyfert galaxy can be set at [FORMULA] = 1.6 mag. This was determined by three different methods, the Balmer decrement in the optical spectrum, the fitting of an absorbed power low to the X-ray spectrum and the Galactic H I column densities. All give a consistent value of the foreground extinction. A minor fraction of the extinction is intrinsic to the galaxy.

The extinction corrected near-infrared colours of WKK 6092 are typical of a Seyfert 1 and are in agreement with well known Seyfert 1's such as NGC 1566 (Glass & Moorwood 1985). The X-ray spectrum is also consistent with the standard expectation for this object.

At the adopted cluster distance of R = 93 [FORMULA] Mpc, the absolute magnitude (corrected for the galactic extincton) is [FORMULA]. The H I and total mass is [FORMULA] and [FORMULA], respectively. The Seyfert is at a projected distance of 0.8 [FORMULA] Mpc from the cluster centre and the H I content of the galaxy might be influenced by interactions with the Inter Cluster Medium due to processes like ram pressure stripping (Cayatte et al. 1990). The H I content is in fact quite low. This is, however, not inconsistent with the expectation for a barred early-type spiral.

Despite the difficulties in analysing data of an object deep within the Milky Way, all data concerning the here investigated Seyfert galaxy WKK 6092 at 30 arcmin from the centre of the rich cluster ACO 3627 correspond to the standard characteristics of a Seyfert 1 galaxy.

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© European Southern Observatory (ESO) 1998

Online publication: September 8, 1998
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