NGC 7592 = VV 731 = MCG-01-59-017 is a system of close interacting galaxies. Two main galactic bodies are present in the CCD R-band image taken at the 1.8m, F/9 telescope of the Asiago Observatory and shown in Figure 1:

• a north-western (NW) component (≡VV 731B), whose starlike nucleus (A) shows a Seyfert-type spectrum (Archipova et al., 1981). A is surrounded by a nearly spheroidal envelope, with an extension in the west at P.A. = 290° detected up to a distance from A of ≈ 9 arcsec, which corresponds to ≈ 2.5h-1kpc of projected linear distance (1 arcsec ≈ .35 h-1kpc at the redshift z = 0.0244; H0 = 100 h km s-1Mpc-1). This extension seems to bend in the northern direction and to join a bright wing, detected up to « 22 arcsec from A, which turns to east and resembles a spiral arm or a tidal tail.

• The envelope around A is connected (over ~ 20 arcsec 7h-1kpc) to a second galactic body (SE) located in the south-east of it. Its nucleus (B), identified by Markarian and Lipovetskii (1976) as the nucleus of Mkn 928, is located at dAB ~ 11 arcsec(~ 4h-1kpc) from A at P.A. = 100°. The morphology of this component is highly peculiar. In the central region, B is linked to two fainter knots which extend up to d″ ~ 4 arcsec at P.A. — 90°. This structure gives to the region surrounding B an elongated and distorted shape. Moreover, a bar-like structure is detected on either sides of B. The north-eastern side of the bar (P.A. = 40°) joins a slightly distorted loop of condensations, which can be traced from P.A. = 335° (at a distance from B«6 arcsec % 2.1 h-1kpc) to P.A. = 100° and from P.A. = 200° to P.A. = 240°, but not in corrispondence of the contact region between the two galaxies. This structure seems to be drained and distorted in the direction of a third condensation C at dBC ≈ 11.7 arcsec (≈ 4.1 h-1kpc) from B at P.A. — 212°. A faint plume bent in a direction opposite to that expected for spiral arms of the SE galaxy appears to extend from the west side of C.