The [O III] emission line luminosity function of optically selected type-2 AGN from zCOSMOS
Creators
- Bongiorno, A.1, 2
- Mignoli, M.
- Zamorani, G.
- Lamareille, F.
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Lanzuisi, G.3, 4
- Miyaji, T.5, 6
- Bolzonella, M.
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Carollo, C. M.7
- Contini, T.
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Kneib, J. P.8
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Le Fèvre, O.8
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Lilly, S. J.7
- Mainieri, V.9
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Renzini, A.10
- Scodeggio, M.11
- Bardelli, S.
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Brusa, M.1
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Caputi, K.7
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Civano, F.3
- Coppa, G.12
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Cucciati, O.8
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de la Torre, S.8, 11, 13
- de-Ravel, L.8
- Franzetti, P.11
- Garilli, B.11
- Halliday, C.14
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Hasinger, G.1, 15
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Koekemoer, A. M.16
- Iovino, A.11
- Kampczyk, P.7
- Knobel, C.7
- Kovač, K.7
- Le Borgne, J.-F.
- Le-Brun, V.8
- Maier, C.7
- Merloni, A.1, 17
- Nair, P.
- Pellò, R.
- Peng, Y.7
- Pérez-Montero, E.18
- Ricciardelli, E.19
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Salvato, M.15, 17, 20
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Silverman, J.7
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Tanaka, M.9
- Tasca, L.8, 11
- Tresse, L.8
- Vergani, D.
- Zucca, E.
- Abbas, U.8
- Bottini, D.11
- Cappi, A.
- Cassata, P.8, 21
- Cimatti, A.12
- Guzzo, L.14
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Leauthaud, A.8
- Maccagni, D.11
- Marinoni, C.22
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McCracken, H. J.23, 24
- Memeo, P.11
- Meneux, B.1
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Oesch, P.7
- Porciani, C.7
- Pozzetti, L.
- Scaramella, R.25
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1.
Max Planck Institute for Extraterrestrial Physics
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2.
University of Maryland, Baltimore County
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3.
Harvard-Smithsonian Center for Astrophysics
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4.
Sapienza University of Rome
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5.
National Autonomous University of Mexico
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6.
University of California, San Diego
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7.
ETH Zurich
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8.
Laboratoire d'Astrophysique de Marseille
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9.
European Southern Observatory
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10.
Osservatorio Astronomico di Padova
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11.
Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano
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12.
University of Bologna
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13.
Brera Astronomical Observatory
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14.
Arcetri Astrophysical Observatory
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15.
Max Planck Society
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16.
Space Telescope Science Institute
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17.
Excellence Cluster Universe
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18.
Instituto de Astrofísica de Andalucía
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19.
University of Padua
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20.
California Institute of Technology
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21.
University of Massachusetts Amherst
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22.
Centre de Physique Théorique
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23.
Institut d'Astrophysique de Paris
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24.
Sorbonne University
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25.
Astronomical Observatory of Rome
Abstract
Aims. 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) L_☉ < L_([O III]) < 10^(9.1) L_☉. 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 [O III]λ5007 Å line luminosity function (LF) and we constrain the fraction of obscured AGN as a function of luminosity and redshift. Methods. 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 ([O III]/Hβ versus [N II]/Hα and [O III]/Hβ versus [S II]/Hα) to isolate AGN in the redshift range 0.15 < z < 0.45 and the diagnostic diagram [O III]/Hβ versus [O II]/Hβ to extend the selection to higher redshift (0.5 < z < 0.92). Results. 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.
Additional Information
© ESO 2010. Received 2 September 2009. Accepted 17 November 2009. A.B. wishes to thank the referee for the useful suggestions that significantly improved the manuscript. A.B. also thank H. Netzer for the the stimulating discussion, R. Fassbender for helping to improve the manuscript and S. Savaglio for sharing the expertise. This work is based on the zCOSMOS ESO Large Program Number 175.A-0839 and was supported by an INAF contract PRIN/2007/1.06.10.08, and an ASI grant ASI/COFIS/WP3110 I/026/07/0, Partial support of this work is provided by NASA ADP NNX07AT02G, CONACyT 83564, and PAPIITIN110209. These results are also based in part on observations obtained with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).Attached Files
Published - Bongiorno2010p7476Astron_Astrophys.pdf
Files
Bongiorno2010p7476Astron_Astrophys.pdf
Additional details
Identifiers
- Eprint ID
- 18009
- Resolver ID
- CaltechAUTHORS:20100416-154341585
Funding
- Istituto Nazionale di Astrofisica (INAF)
- PRIN/2007/1.06.10.08
- Agenzia Spaziale Italiana (ASI)
- ASI/COFIS/WP3110 I/026/07/0
- NASA
- NNX07AT02G
- Consejo Nacional de Ciencia y Tecnología (CONACyT)
- 83564
- Dirección General Asuntos del Personal (DGAPA)
- PAPIIT IN 110209
- ESA Member States
Dates
- Created
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2010-04-19Created from EPrint's datestamp field
- Updated
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2021-11-08Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- COSMOS , Infrared Processing and Analysis Center (IPAC)