Environmental dependence of the presence of active galactic nuclei (AGNs) in the volume-limited Main galaxy samples of SDSS DR6
Corresponding Author
X.-F. Deng
School of Science, Nanchang University, Jiangxi, China, 330031
School of Science, Nanchang University, Jiangxi, China, 330031Search for more papers by this authorY. Xin
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorP. Wu
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorP. Jiang
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorY.-P. Ding
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorX.-P. Qi
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorCorresponding Author
X.-F. Deng
School of Science, Nanchang University, Jiangxi, China, 330031
School of Science, Nanchang University, Jiangxi, China, 330031Search for more papers by this authorY. Xin
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorP. Wu
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorP. Jiang
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorY.-P. Ding
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorX.-P. Qi
School of Science, Nanchang University, Jiangxi, China, 330031
Search for more papers by this authorAbstract
Using two volume-limited Main galaxy samples of the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) above and below the value of M∗︁r, we have explored the environmental dependence of the AGN fraction. It is found that the fraction of AGNs declines substantially with increasing local density in the luminous volume-limited sample, but in the faint volume-limited sample this change is very weak. We also note that the presence of AGNs is not correlated with the stellar mass (© 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
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