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The Complex Nature of the Seyfert Galaxy NGC 7592

Published online by Cambridge University Press:  12 April 2016

Piero Rafanelli  and
Paolo Marziani
Piero Rafanelli
Affiliation:
Department of Astronomy, University of Padova, Italy
Paolo Marziani
Affiliation:
International School for Advanced Studies, Trieste, Italy

Extract

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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.

Type
III. Observations of Related Objects
Information
International Astronomical Union Colloquium , Volume 124: Paired and Interacting Galaxies , 1990 , pp. 169 - 173
Copyright
Copyright © NASA 1990

References

Archipova, V.P. et al: 1981, Soviet Astron. 25, 277 Google Scholar
Baldwin, J.A., Phillips, M.M., Terlevich, R.: 1981, P.A.S.P. 93, 5 CrossRefGoogle Scholar
Kennicutt, R.C., Keel, W.C., Blaha, C.A.: 1989, Astron. J. 97, 1022 Google Scholar
Markarian, B.E., Lipovetskii, V.A., Stefanian, D.A.: 1977, Astrofisica 13, 225 Google Scholar
Veilleux, S., Osterbrock, D.E.: 1987, Astroph. J. Suppl. 63, 295CrossRefGoogle Scholar
Toomre, A., Toomre, J.: 1972, Astroph. J., 178, 623 CrossRefGoogle Scholar