The Galaxy Luminosity Function at Z=0

Z=0 处的星系光度函数

• 批准号: 9901256
• 负责人: Michael Bolte
• 金额: $ 28.18万
• 依托单位: University of California-Santa Cruz
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1999
• 资助国家: 美国
• 起止时间: 1999-06-15 至 2005-05-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9901256&HistoricalAwards=false
• 关键词: Galaxy; Luminosity; Function; Z=0

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.***

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，根据光度来确定星系的分布。他正在使用非常宽的视场ccd成像附近两个星系群中的单个成员星系：狮子座和彗星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。所有从早期宇宙复合后密度涨落形成星系的宇宙学都预示着最初的GLF。要解释宇宙演化中不同时期的数据，需要了解星系在当今宇宙中的光度和质量分布。他正在将GLF成像到局部群中最低的矮小球状星系(绝对星等在-9.5的R波段)附近的光度。他正在验证进入GLF的每个星系的成员资格，并用蒙特卡罗实验评估计数的完整性。