NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-06-17 T18:52:48 PDT
Help | Comment | NED Home

For refcode 1994MNRAS.270..580S:
Retrieve 1 NED object in this reference.
Please click here for ADS abstract

NED Abstract

Copyright by Royal Astronomical Society. 1994MNRAS.270..580S Multifrequency monitoring of the Seyfert 1 galaxy NGC 4593 - I. Isolating the nuclear emission M. Santos-Lleo, J. Clavel, P. Barr, I, S. Glass, D. Pelat, B. M. Peterson and G. Reichert Observatoire de Paris, DAEC 92195 Meudon Cedex, France ESA IUE Observatory, PO Box 5072728080 Madrid Spain ISO Observatory, Code SAI ESTEC, Postbus 299,2200 AG Noordwijk, The Netherlands South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape, South Africa Department of Astronomy, Ohio State University, 174 W. 18th Avenue, Columbus, OH 4321 0, USA NASA -Goddard Space Flight Center Code 684.9, Building 21, Greenbelt, MD 20771, USA Accepted 1994 May 3. Received 1994 April 28; in original form 1994 January 20 ABSTRACT We present data obtained within a Campaign to monitor spectral variations in the low-luminosity Seyfert 1 galaxy NGC 4593, at X-ray, ultraviolet, optical and near-IR (J, H, K and L) frequencies. The different `parasitic' contributions that contaminate the pure nuclear continuous emission have been isolated and modelled. The light from the composite stellar population and the dust in the bulge and disc of the underlying galaxy are characterized by a spectral energy distribution similar to that of the Sb spiral M31. Its surface brightness profile is modelled with two components and provides the luminosity through any given aperture. Stars are responsible for as much as 70-85 per cent of the 5600-A flux through a 4 X 4 arcsec^2^ square aperture. The `small bump' which characterizes the spectral energy distribution of active nuclei in the 2000-4000 A range is well accounted for by many blended broad Fe II lines plus Balmer continuum emission. On average ~64 per cent of the total 2710-A flux is due to Fe II plus Balmer emission. Almost half of the broad-line cooling is due to FeII line emission. The pattern of variability of the pure nuclear continuum, as well as the broad lines and their implications, is discussed in an accompanying paper. Key words: galaxies: individual: NGC 4593 - galaxies: nuclei - galaxies: Seyfert - infrared: galaxies - ultraviolet: galaxies - X-rays: galaxies.
Retrieve 1 NED object in this reference.
Please click here for ADS abstract

Back to NED Home