Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 392, Issue 1, Pages 125-134Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2008.13893.x
Keywords
galaxies: active; galaxies: evolution; galaxies: high-redshift; galaxies: statistics; large-scale structure of Universe
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Funding
- Ministerio de Educacion y Ciencia of the Spanish Government [AYA2005-07789]
- NSF [AST-0071048, AST-0071198, AST-0507428, AST-0507483]
- NASA [HF-01182.01-A, NAS 5-26555]
- Space Telescope Science Institute
- NASA through the Spitzer Space Telescope Fellowship Program
- ADMD [PNAYA2005-07789]
- Hubble Space Telescope (HST) [HSTAR10947]
- W. M. Keck Foundation
- Alfred P. Sloan Foundation
- USA Department of Energy
- Japanese Monbukagakusho
- Max Planck Society
- Direct For Mathematical & Physical Scien [0806732] Funding Source: National Science Foundation
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We measure the dependence of the active galactic nuclei (AGN) fraction on local environment at z similar to 1, using spectroscopic data taken from the DEEP2 Galaxy Redshift Survey, and Chandra X-ray data from the All-Wavelength Extended Groth Strip International Survey (AEGIS). To provide a clean sample of AGN, we restrict our analysis to the red sequence population; this also reduces additional colour-environment correlations. We find evidence that high-redshift LINERs in DEEP2 tend to favour higher density environments relative to the red population from which they are drawn. In contrast, Seyferts and X-ray selected AGN at z similar to 1 show little (or no) environmental dependencies within the same underlying population. We compare these results with a sample of local AGN drawn from the Sloan Digital Sky Survey (SDSS). Contrary to the high-redshift behaviour, we find that both LINERs and Seyferts in the SDSS show a slowly declining red sequence AGN fraction towards high-density environments. Interestingly, at z similar to 1 red sequence Seyferts and LINERs are approximately equally abundant. By z similar to 0, however, the red Seyfert population has declined relative to the LINER population by over a factor of similar to 4.5. We speculate on possible interpretations of our results.
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