What makes a galaxy radio-loud?
Abstract
We compare the Spectral Energy Distribution (SED) of radio-loud and radio-quiet AGNs in three different samples observed with SDSS: radio-loud AGNs (RLAGNs), Low Luminosity AGNs (LLAGNs) and AGNs in isolated galaxies (IG-AGNs). All these galaxies have similar optical spectral characteristics. The median SED of the RLAGNs is consistent with the characteristic SED of quasars, while that of the LLAGNs and IG-AGNs are consistent with the SED of LINERs, with a lower luminosity in the IG-AGNs than in the LLAGNs. We infer the masses of the black holes (BHs) from the bulge masses. These increase from the IG-AGNs to the LLAGNs and are highest for the RLAGNs. All these AGNs show accretion rates near or slightly below 10% of the Eddington limit, the differences in luminosity being solely due to different BH masses. Our results suggests there are two types of AGNs, radio quiet and radio loud, differing only by the mass of their bulges or BHs.
Cite
@article{arxiv.1201.4401,
title = {What makes a galaxy radio-loud?},
author = {R. A. Ortega-Minakata and J. P. Torres-Papaqui and H. Andernach and R. Coziol and J. M. Islas-Islas and I. Plauchu-Frayn and D. M. Neri-Larios and M. del C. Rojas-Granados},
journal= {arXiv preprint arXiv:1201.4401},
year = {2015}
}
Comments
3 pages, 3 figures; to appear in Proceedings of IAU Symposium No. 284, The Spectral Energy Distribution of Galaxies (SED2011), Preston, UK, 5-9 sep. 2011