THE DISTRIBUTION OF FAINT SATELLITES AROUND CENTRAL GALAXIES IN THE CANADA–FRANCE–HAWAII TELESCOPE LEGACY SURVEY
THE DISTRIBUTION OF FAINT SATELLITES AROUND CENTRAL GALAXIES IN THE CANADA–FRANCE–HAWAII TELESCOPE LEGACY SURVEY
复制标题
DOI：
10.1088/0004-637x/760/1/16
复制
发表时间：
2012-09
期刊：
影响因子：
--
通讯作者：
Chunyan Jiang;Y. Jing;Cheng Li
中科院分区：
文献类型：
--
作者：
Chunyan Jiang;Y. Jing;Cheng Li
利用加拿大-法国-夏威夷望远镜（CFHT）遗产巡天观测了低红移宇宙中心星系周围暗卫星的径向数密度剖面和丰度分布。我们考虑从Yang等人的Sloan数字巡天星表中选取的三个中心星系样本，其星等分别为Mr = −21、−22和−23。通过将这些星系与CFHT Legacy Survey的测光星表互相关，得到了这些中心星系周围的卫星分布。卫星的投影径向数密度服从幂律形式，最佳拟合对数斜率为-1.05，与中央星系光度和卫星光度无关。中心星系与卫星星系的投影互相关函数随卫星光度的变化呈现出非单调的趋势。这在Mr = −21的中央星系中最为明显，当卫星星系比中央星系暗2等以上时，星系团振幅随卫星星系光度的下降趋势就逆转了。与银河系（MW）和M31的卫星星系光度函数的比较表明，MW/M31系统的卫星星系数量大约是类似光度的典型中央星系的两倍。理论模型的影响进行了简要讨论。
We investigate the radial number density profile and the abundance distribution of faint satellites around central galaxies in the low-redshift universe using the Canada–France–Hawaii Telescope (CFHT) Legacy Survey. We consider three samples of central galaxies with magnitudes of Mr = −21, −22, and −23 selected from the Sloan Digital Sky Survey group catalog of Yang et al. The satellite distribution around these central galaxies is obtained by cross-correlating these galaxies with the photometric catalog of the CFHT Legacy Survey. The projected radial number density of the satellites obeys a power-law form with the best-fit logarithmic slope of −1.05, independent of both the central galaxy luminosity and the satellite luminosity. The projected cross-correlation function between central and satellite galaxies exhibits a non-monotonic trend with satellite luminosity. It is most pronounced for central galaxies with Mr = −21, where the decreasing trend of clustering amplitude with satellite luminosity is reversed when satellites are fainter than central galaxies by more than 2 mag. A comparison with the satellite luminosity functions in the Milky Way (MW) and M31 shows that the MW/M31 system has about twice as many satellites as around a typical central galaxy of similar luminosity. The implications for theoretical models are briefly discussed.