1、1,博士論文答辯,Butcher-Oemler (B-O) 效應(yīng)(1978, 1984),Rakos BM: II-III 非統(tǒng)一的光度函數(shù)：較平的暗尾(Dressler, A. 1978, ApJ, 223, 765) 雙X射線峰，明顯的X/光學(xué)中心偏離：10 (540 kpc, H0=75) 很可能是兩個(gè)子團(tuán)碰撞的結(jié)果(Ulmer,M.P., Wirth, G.D., & Kowalski, M.P. 1992, ApJ, 397, 430) 沒有發(fā)現(xiàn)與碰撞有關(guān)的藍(lán)星系(Tomita et al. 1996 AJ, 111, 42),引言：,4,博士論文答辯,A168的形成與演化的綜合研究

2、：,5,博士論文答辯,Appendix I,Statistic of velocities,6,博士論文答辯,Statistic of velocities,7,博士論文答辯,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.,8,博士論文答辯,Bubble plot,9,博士論文答辯,Velocity along the elongation,10,博士論文答辯,動(dòng)力

3、學(xué),K-S檢驗(yàn)表明這兩個(gè)分布有94%的概率來自不同的母分布。 分布的扭曲(skewness) 和拖尾(kurtosis)檢驗(yàn)表明他們有本質(zhì)的區(qū)別。 平均視向速度差是：264142 km/s,光學(xué)數(shù)據(jù)及其分析：動(dòng)力學(xué) & 光度函數(shù)：,11,博士論文答辯,Appendix II,Gravitationally bound,12,博士論文答辯,Gravitationally bound,13,博士論文答辯,Mass estimation,14,博士論文答辯,Gravitationally bound,15,博士論文答辯,Gravitationally bound,16,博士論文答辯,Gravitat

4、ionally bound,Probability of binding.,17,博士論文答辯,GB- probability,P=92%,18,博士論文答辯,19,博士論文答辯,Appendix III,LFs & DSF,20,博士論文答辯,光度函數(shù)1,引言：,X-RAY EMISSION FROM CLUSTERS OF GALAXIES - Craig L. Sarazin (1988),21,博士論文答辯,Schechter Function,22,博士論文答辯,光度函數(shù)2,Trentham & Tully 2002, MNRAS, 335, 712,引言：,23,博士論文答辯,Do

5、uble Schechter Function (DSF),24,博士論文答辯,DSF fit (figure),25,博士論文答辯,DSF fit (table),26,博士論文答辯,光度函數(shù),B/FA168N=0.68 B/FA168S=1.37 明顯的星系成分差別說明A168N和A168S 很可能有不同的形成與演化的歷史。,光學(xué)數(shù)據(jù)及其分析：動(dòng)力學(xué) & 光度函數(shù)：,27,博士論文答辯,Appendix IV,Density profile,28,博士論文答辯,Density profile,29,博士論文答辯,Appendix V,Photometric redshift,30,博士論文

6、答辯,測(cè)光紅移,31,博士論文答辯,S-P- redshift compare,32,博士論文答辯,Redshift distribution,33,博士論文答辯,Appendix VI,Eest-west divide,34,博士論文答辯,LF for EW,35,博士論文答辯,SP for EW,36,博士論文答辯,VD for EW,37,博士論文答辯,Appendix VII,X-ray observations,38,博士論文答辯,Proposal abstract,Proposal Title: ABELL 168, A RARE MERGER WITH THE SIMPLEST

7、GEOMETRY Proposal Number: 03800125 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 m

8、erger 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

9、and projections that preclude unambiguous interpretation. We propose to obtain a detailed temperature map of A168 whose image suggests a head-on collision of two similar cool subclusters occurring in the plane of the sky - the simplest possible merger scenario.,39,博士論文答辯,觀測(cè)信息,Target Name:A168_OFFSET

10、1A168_OFFSET2 Observe data:2002-01-05 2002-11-01 Released data:2003-01-10 2003-11-05 Exposure time:41.12 ks38.11 ks Observation ID: 32033204 Instrument: ACIS-IACIS-I,Chandra X 射線分析：觀測(cè)及數(shù)據(jù)處理：,40,博士論文答辯,數(shù)據(jù)處理,ACIS 原始數(shù)據(jù)處理: ciao3.0 /ciao/ 二級(jí) (Level-two) 數(shù)據(jù)文件,Chandra X 射線分析：觀測(cè)及數(shù)據(jù)處理：,41,博士論文答辯,42,博士論文答辯,Appendix of Imaging2,After “csmooth”,43,博士論文答辯,Appendix of Imaging1,Exposure Map Corrected,44,博士論文答辯,45,博士論文答辯,46,博士論