| |
 |
| Paper: |
AMIGA Project: Nuclear Activity in a Complete Sample of Isolated Galaxies |
| Volume: |
421, Galaxies in Isolation: Exploring Nature Versus Nurture |
| Page: |
57 |
| Authors: |
Sabater, J.; Leon, S.; Verdes-Montenegro, L.; Lisenfeld, U.; Sulentic, J.; Verley, S. |
| Abstract: |
The project AMIGA (Analysis of the interstellar Medium of Isolated GAlaxies) provides a statistically significant sample of the most isolated galaxies in the northern sky. Such a control sample is necessary to understand the role of the environment in evolution and galaxy properties like the interstellar medium (ISM), star formation and nuclear activity. The data is publicly released under a VO interface at http://amiga.iaa.es/. One of our main goals is the study of nuclear activity in non-interacting galaxies using different methods. We focus on the well known radiocontinuum-far infrared (FIR) correlation in order to find radio-excess galaxies which are candidates to host an active galactic nucleus (AGN) and FIR colours to find obscured AGN candidates. We looked for the existing information on nuclear activity in the Véron-Cetty catalogue and in the NASA Extragalactic Database (NED). We also used the nuclear spectra from the Sloan Digital Sky Survey which allow us to determine the possible presence of an AGN and to study the properties of the underlying stellar populations. We produced a final catalogue of AGN-candidate galaxies which will provide a baseline for the study of the nuclear activity depending on the environment. We find that the fraction of FIR selected AGN-candidates ranges between 7% and 20%. There are no radio-excess galaxies in our sample above a factor 5 of radio excess which is the lowest rate found in comparison with other samples in denser environments. Finally, we obtained a fraction of about 22% of AGN using the optical spectra, a significant fraction for a sample of isolated galaxies. We conclude that the environment plays a crucial and direct role in triggering radio nuclear activity and not only via the density-morphology or the density-luminosity relations. |
|
|
|
|
|
