A comprehensive classification of galaxies in the Sloan Digital Sky Survey: how to tell true from fake AGN?
Article first published online: 1 MAR 2011
© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS
Monthly Notices of the Royal Astronomical Society
Volume 413, Issue 3, pages 1687–1699, May 2011
How to Cite
Cid Fernandes, R., Stasińska, G., Mateus, A. and Vale Asari, N. (2011), A comprehensive classification of galaxies in the Sloan Digital Sky Survey: how to tell true from fake AGN?. Monthly Notices of the Royal Astronomical Society, 413: 1687–1699. doi: 10.1111/j.1365-2966.2011.18244.x
- Issue published online: 11 MAY 2011
- Article first published online: 1 MAR 2011
- Accepted 2010 December 20. Received 2010 December 15; in original form 2010 August 11
- galaxies: active;
- galaxies: evolution;
- galaxies: statistics;
- galaxies: stellar content
We use the WHα versus [N ii]/Hα (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 ξ, which measures the ratio of the extinction-corrected Hα luminosity with respect to the Hα luminosity expected from photoionization by stellar populations older than 108 yr. We find that ξ follows a markedly bimodal distribution, with a ξ≫ 1 population composed by systems undergoing star formation and/or nuclear activity, and a peak at ξ∼ 1 corresponding to the prediction of the RG model. We base our classification scheme not on ξ but on a more readily available and model-independent quantity which provides an excellent observational proxy for ξ: the equivalent width of Hα. Based on the bimodal distribution of WHα, we set the practical division between wAGN and RGs at WHα= 3 Å.
Five classes of galaxies are identified within the WHAN diagram:
- (i) pure star-forming galaxies: and WHα > 3 Å;
- (ii) strong AGN (i.e. Seyferts): and WHα > 6 Å;
- (iii) weak AGN: and WHα between 3 and 6 Å;
- (iv) RGs (i.e. fake AGN): WHα < 3 Å;
- (v) passive galaxies (actually, lineless galaxies): WHα and W[N ii] < 0.5 Å.
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.