我們使用疊加分析來探討在低紅移之六十一個星系團內的星系光度函數及其環境影響。
由X-ray光度函數所定義的豐富度，對於藍色或是紅色的光度函數形狀沒有影響。這可能是因為我們的光度函數不是分割於高亮度端和或是低亮度端。在藍色波段(如g波段)，低紅位移的星系團比高紅位移的相比，顯示出較為明亮的M*值。我們認為在低紅移星系團內內部有更明亮的星系，這與解釋不一致，且不符合結構演化的分層情景（Kauffmann等，2003）。結果可能來自Malmquist 偏差。在藍色波段中顯示出來，星系團內的外圍則顯示較低的α值。這實驗結果與我們認為在星系團內的外圍有更多的微弱的藍色星系，而藍色矮星星通常分布在遠離中心的地方（Papaderos等，1996）是一致的。

We investigate the environment effects of the galaxy luminosity function inside the sixty-one clusters of galaxies at low Redshift using stacking analysis.
The richness of cluster, defined by X-ray luminosity function, shows no effect on the shape of the luminosity function both in blue and red band. This maybe due to the fact that our luminosity function cut is not high and low end. At low redshift, clusters show brighter M* compared to high redshift clusters in blue band (i.e. g band). This is not consistent with interpretation that we have more bright galaxies inside low redshift clusters, and in disagreement with hieratical scenario of structure formation (Kauffmann et al., 2003). The result maybe comes from Malmquist bias. Outskirts of clusters show lower α, again most vividly shown in the blue band. This is consistent with interpretation that we have more faint blue galaxies at outskirt in the clusters. And the blue dwarf galaxies often are distributed far to the center (Papaderos et al., 1996).

Alam et al., 2015, APJs, 219, 12
Barrena et al., 2012, A&A, 540, 90
Baum, W. A., 1962, in IAU Symp. 15, Problems of Extra-Galactic Research, ed. G. C. McVittie (New York: MacMillan), 390
Blanton et al., 2003, Apj, 592, 189
Beck et al., 2016, MNRAS, 460, 1371
Chilingarian et al., 2010, MNRAS, 405, 1409
De Filippis et al., 2011, MNRAS, 414, 2771
De Propris et al., 1995, APJ, 450, 534
Gal et al., 2009, AJ, 137, 2981
Goto, T et al., 2002, PASJ...54..515G
Gunn et al., 2006, APJ, 131, 2332
Hansen et al., 2009, APJ, 699, 1333
Hashimoto et al., 2007, A&A, 467, 485
Hashimoto et al., 2007, A&A, 468, 25
Hashimoto et al., 2008, MNRAS, 390,1562
Ilbert et al., 2009, APJ, 690, 1236
Koester et al., 2007, APJ, 660, 221
Lin et al., 1999, ApJ, 518, 533
Loveday et al., 2015, MNRAS, 451, 1540
Lawrence et al., 2007, MNRAS, 379, 1599
Lumsden et al., 1997, MNRAS, 290, 119
Moretti et al., 2015, A&A, 581, A11
Mehrtens et al., 2012, MNRAS, 423, 1024
Paolillo et al., 2001, A&A, 367, 59
Papaderos et al., 1996, A&A, 314, 59
Popesso et al., 2006, A&A, 445, 29
Schecheter, 1976, APJ, 203, 297
Schmidt et al., 1968, APJ, 151, 393
Smith et al., 2009, MNRAS, 397, 868
Strauss et al., 2002, APJ, 124, 1810
Trentham and Tully, 2002, MNRAS, 335, 712
Valloto et al., 1997, APJ, 479, 90
Valloto et al., 2001, APJ, 546, 157
Von Kuhlmann, 2002PhDT..1V
Willson, 1997, MNRAS, 284, 915
Yagi et al., 2002, APJ, 123, 87