The Galaxy Luminosity Function at Z=0

博尔特博士正在测量附近宇宙中星系的光度函数（GLF）；换句话说，通过光度来确定星系的分布。他正在使用非常宽视场的ccd成像两个邻近星系群中的单个成员星系：狮子座和彗发I.一旦我们可以定义当前的GLF，我们就可以更好地解释各种宇宙学。所有从早期宇宙重组后的密度波动中形成星系的宇宙学都预测了初始GLF。要解释宇宙演化中不同时期的数据，就需要了解当前宇宙中星系的光度和质量分布。他正在对GLF进行成像，使其亮度接近本星系群中最低的矮球状星系（绝对星等在-9.5的r波段）。他正在验证进入GLF的每个星系的成员性，并用蒙特卡罗实验评估计数的完整性

Dr. Bolte is measuring the luminosity function of galaxies (GLF) in the nearby Universe; in other words, determine the distribution of galaxies by luminosity. He is using very wide field CCDs to image individual member galaxies in two nearby galaxy groups: Leo and Coma I. Once we can define the current GLF we can better interpret various cosmologies. All cosmologies that forma galaxies from post-recombination density fluctuations in the early Universe predict an initial GLF. Knowledge of the distribution of galaxies by luminosity and mass in the current day Universe is required to interpret the data at different epochs in the evolution of the Universe. He is imaging the GLF to luminosities near those of the lowest dwarf spheroidal galaxies (with absolute magnitudes in the R-band of -9.5) in the Local Group. He is verifying the membership of each galaxy that goes into the GLF and evaluating the counting completeness with Monte Carlo experiments.***