Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.266..953k&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Vol. 266, NO. 4/FEB15, P. 953, 1994
Astronomy and Astrophysics
Astronomy
65
Scientific paper
This paper is part of a series in which we study a hard-X-ray-selected sample of AGN, mainly optically classified as Seyfert 1 nuclei. In this paper, we use our optical and infrared imaging data of the sample to study the properties of the host galaxies. We separate the non-stellar and stellar components of the nuclear light, on the basis of the results from Papers I and III. The stellar colours in the nucleus are generally much redder in B - V and V - K indices than normal spiral galaxy bulges, and can be reproduced Using stellar evolution models modified by ~1 mag of reddening in A_v_ and/or reradiation from hot dust. The J - H colour is normal, but H - K is usually very red, indicating that the near- infrared (NIR) colours are affected by dust reradiation within the K band, either heated by the active nucleus or by young stars in H II regions associated with enhanced star formation around the nucleus. The NIR colours are similar to those observed in a sample of starburst/LINER galaxies. The B - V, V - K and J - K colours have red gradients towards the nucleus, although there is considerable scatter. The B - V and J - K colour gradients are not correlated, and are therefore likely to be caused by different mechanisms. The colour gradients are in good agreement with those seen in normal spiral galaxies. We present luminosity distributions of the host galaxies in B, V, J and K. There is a strong correlation between the AGN and the host galaxy luminosity, in the sense that the more powerful AGN reside in more luminous host galaxies. The luminosities of the host galaxies for our sample fall between those of normal spiral galaxies and the hosts of quasars. The central surface brightnesses and the length scales of the discs are not well determined from the decomposition fits, but on average they are consistent with values found in previous studies.
Kotilainen Jari K.
Ward Martin J.
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