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Optical & Near Infrared Imaging of NGC1275

Published online by Cambridge University Press:  07 August 2017

D. H. Hughes ,
E. I. Robson  and
M. J. Ward
D. H. Hughes
Affiliation:
Physics and Astronomy, Lancashire Polytechnic, Preston PR1 2TQ, U.K.
E. I. Robson
Affiliation:
Physics and Astronomy, Lancashire Polytechnic, Preston PR1 2TQ, U.K.
M. J. Ward
Affiliation:
Institute of Astronomy, Cambridge CB3 OHA, U.K.

Abstract

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We are currently studying a selection of active galaxies using the new IR array camera IRCAM on UKIRT. Our aim is to seperate the underlying stellar emission from that of the active galactic nucleus. Although the optical is the best wavelength region to discriminate between the different populations in the underlying spiral and elliptical galaxies, it is in the infrared that the contrast between the non-thermal central core and the surrounding galaxy is increased. We present reduced data from infrared images taken at 1.25, 1.65 and 2.2 μm with an image scale of 0.6 arcsec/pixel together with optical 0.44 and 0.55 μm CCD images of the Seyfert galaxy NGC1275.

Type
Part 7: Dust, Molecules, Infrared and MM Radiation
Information
Symposium - International Astronomical Union , Volume 134: Active Galactic Nuclei , 1989 , pp. 376 - 378
Copyright
Copyright © Kluwer 1989 

References

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