The [OIII] emission line luminosity function of optically selected type-2 AGN from zCOSMOS
Abstract
We present a catalog of 213 type-2 AGN selected from the zCOSMOS survey. The selected sample covers a wide redshift range (0.15<z<0.92) and is deeper than any other previous study, encompassing the luminosity range 10^{5.5} < Lsun< L[OIII] < 10^{9.1} Lsun. We explore the intrinsic properties of these AGN and the relation to their X-ray emission (derived from the XMM-COSMOS observations). We study their evolution by computing the [OIII]5007A line luminosity function (LF) and we constrain the fraction of obscured AGN as a function of luminosity and redshift. The sample was selected on the basis of the optical emission line ratios, after applying a cut to the signal-to-noise ratio (S/N) of the relevant lines. We used the standard diagnostic diagrams [OIII]/Hbeta versus [NII]/Halpha and ([OIII]/Hbeta versus [SII]/Halpha) to isolate AGN in the redshift range 0.15<z<0.45 and the diagnostic diagram [OIII]/Hbeta versus [OII]/Hbeta to extend the selection to higher redshift (0.5<z<0.92). Combining our sample with one drawn from SDSS, we found that the best description of the evolution of type-2 AGN is a luminosity-dependent density evolution model. Moreover, using the type-1 AGN LF we were able to constrain the fraction of type-2 AGN to the total (type-1 + type-2) AGN population. We found that the type-2 fraction decreases with luminosity, in agreement with the most recent results, and shows signs of a slight increase with redshift. However, the trend with luminosity is visible only after combining the SDSS+zCOSMOS samples. From the COSMOS data points alone, the type-2 fraction seems to be quite constant with luminosity.
Keywords
Cite
@article{arxiv.0911.3914,
title = {The [OIII] emission line luminosity function of optically selected type-2 AGN from zCOSMOS},
author = {A. Bongiorno and M. Mignoli and G. Zamorani and F. Lamareille and G. Lanzuisi and T. Miyaji and M. Bolzonella and C. M. Carollo and T. Contini and J. P. Kneib and O. Le Fevre and S. J. Lilly and V. Mainieri and A. Renzini and M. Scodeggio and S. Bardelli and M. Brusa and K. Caputi and F. Civano and G. Coppa and O. Cucciati and S. de la Torre and L. de Ravel and P. Franzetti and B. Garilli and C. Halliday and G. Hasinger and A. M. Koekemoer and A. Iovino and P. Kampczyk and C. Knobel and K. Kovac and J. -F. Le Borgne and V. Le Brun and C. Maier and A. Merloni and P. Nair and R. Pello and Y. Peng and E. Perez Montero and E. Ricciardelli and M. Salvato and J. Silverman and M. Tanaka and L. Tasca and L. Tresse and D. Vergani and E. Zucca and U. Abbas and D. Bottini and A. Cappi and P. Cassata and A. Cimatti and L. Guzzo and A. Leauthaud and D. Maccagni and C. Marinoni and H. J. McCracken and P. Memeo and B. Meneux and P. Oesch and C. Porciani and L. Pozzetti and R. Scaramella},
journal= {arXiv preprint arXiv:0911.3914},
year = {2015}
}
Comments
20 pages, 11 figures, accepted for publication in Astronomy and Astrophysics