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Optical & Near Infrared Imaging of NGC1275

  • D. H. Hughes (a1), E. I. Robson (a1) and M. J. Ward (a2)

Abstract

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.

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References

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Aaronson, M. 1977. , Harvard University.
Frogel, J.A., Persson, S.E., Aaronson, M., & Matthews, K. 1978. Astrophys. J., 220, 75.
Metik, L.P. & Pronik, I.I. 1984. Astrofizika, 21, 233.
Minkowski, R. 1957. Radio Astronomy, I.A.U. Symp. No. 4, ed. van de Hulst, H.C. (C.U.P.), p.107.

Optical & Near Infrared Imaging of NGC1275

  • D. H. Hughes (a1), E. I. Robson (a1) and M. J. Ward (a2)

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