Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 413, Issue 3, Pages 1687-1699Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2011.18244.x
Keywords
galaxies: active; galaxies: evolution; galaxies: statistics; galaxies: stellar content
Categories
Funding
- CNPq
- CAPES
- France-Brazil CAPES-COFECUB
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy
- National Aeronautics and Space Administration
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- University of Cambridge
- Case Western Reserve University
- University of Chicago
- Drexel University
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max-Planck-Institute for Astronomy (MPIA)
- Max-Planck-Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
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We use the W-H alpha versus [N ii]/H alpha (WHAN) diagram introduced by us in previous work to provide a comprehensive emission-line classification of Sloan Digital Sky Survey galaxies. This classification is able to cope with the large population of weak line galaxies that do not appear in traditional diagrams due to a lack of some of the diagnostic lines. A further advantage of the WHAN diagram is to allow the differentiation between two very distinct classes that overlap in the low-ionization nuclear emission-line region (LINER) region of traditional diagnostic diagrams. These are galaxies hosting a weakly active galactic nucleus (wAGN) and 'retired galaxies' (RGs), i.e. galaxies that have stopped forming stars and are ionized by their hot low-mass evolved stars. A useful criterion to distinguish true from fake AGN (i.e. the RGs) is the value of xi, which measures the ratio of the extinction-corrected H alpha luminosity with respect to the H alpha luminosity expected from photoionization by stellar populations older than 108 yr. We find that xi follows a markedly bimodal distribution, with a xi 1 population composed by systems undergoing star formation and/or nuclear activity, and a peak at xi similar to 1 corresponding to the prediction of the RG model. We base our classification scheme not on xi but on a more readily available and model-independent quantity which provides an excellent observational proxy for xi: the equivalent width of H alpha. Based on the bimodal distribution of W-H alpha, we set the practical division between wAGN and RGs at W-H alpha = 3 A. Five classes of galaxies are identified within the WHAN diagram: pure star-forming galaxies: and W-H alpha > 3 A; strong AGN (i.e. Seyferts): and W-H alpha > 6 A; weak AGN: and W-H alpha between 3 and 6 A; RGs (i.e. fake AGN): W-H alpha < 3 A; passive galaxies (actually, lineless galaxies): W-H alpha and W-[N ii] < 0.5 A. A comparative analysis of star formation histories and of other physical and observational properties in these different classes of galaxies corroborates our proposed differentiation between RGs and wAGN in the LINER-like family. This analysis also shows similarities between strong and weak AGN on the one hand, and retired and passive galaxies on the other.
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