博士论文答辩ppt10.ppt

2004年6月 博士论文答辩 博士论文答辩 Butcher-Oemler (B-O) 效应(1978, 1984) A168研究进展 邻近星系团 z = 0.045; BM: II-III 非统一的光度函数：较平的暗尾(Dressler, A. 1978, ApJ, 223, 765) 双X射线峰，明显的X/光学中心偏离：~10￠ (~540 kpc, H0=75) ?很可能是两个子团碰撞的结果(Ulmer,M.~P., Wirth, G.~D., Kowalski, M.~P. 1992, ApJ, 397, 430) 没有发现与碰撞有关的蓝星系(Tomita et al. 1996 AJ, 111, 42) Appendix I Statistic of velocities Statistic of velocities Statistic of velocities- K-S K-S test results D=0.30 P=6% So, two velocity distribution is significantly different at 94% confidence level. Bubble plot Velocity along the elongation 动力学 K-S检验表明这两个分布有94%的概率来自不同的母分布。 分布的扭曲(skewness) 和拖尾(kurtosis)检验表明他们有本质的区别。 平均视向速度差是：264±142 km/s Appendix II Gravitationally bound Gravitationally bound Mass estimation Gravitationally bound Gravitationally bound Gravitationally bound Probability of binding. GB- probability Appendix III LFs DSF 光度函数1 Schechter Function 光度函数2 Double Schechter Function (DSF) DSF fit (figure) 光度函数 B/FA168N=0.68 B/FA168S=1.37 明显的星系成分差别说明A168N和A168S 很可能有不同的形成与演化的历史。 Appendix IV Density profile Density profile Appendix V Photometric redshift S-P- redshift compare Redshift distribution Appendix VI Eest-west divide LF for EW SP for EW VD for EW Appendix VII X-ray observations Proposal abstract Proposal Title: ABELL 168, A RARE MERGER WITH THE SIMPLEST GEOMETRY ? Proposal Number: Principal Investigator: Maxim Markevitch ? Abstract:?Mergers provide a unique laboratory for studying cluster physics. For example, using the gas temperature and density upstream and downstream of a merger shock, one can determine the shock velocity that defines the merger timescale and energetics. If shock fronts are discernible (with the help of Chandras arcsecond resolution), one can use them to study microscopic properties of the intracluster plasma, including the magnetic field. While many clusters exhibit signs of merging, most have complicated geometries and projections that preclude unambiguous interpretation. We propose to obtain a detailed tem