Butcher-Oemler (B-O) 效应 (1978, 1984)

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Butcher-Oemler (B-O) 效应 (1978, 1984)

Rakos & Schombert 1995 ApJ, 439, 47



A168 研究进展邻近星系团 z z = 0.045; BM: II-III= 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 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)

引言：


A168 的形成与演化的综合研究：


Appendix I

Statistic of velocities


Statistic of velocities


Statistic of velocities- K-S K-S test results

D=0.30P=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

光学数据及其分析：动力学 && 光度函数：


Appendix II

Gravitationally bound



L.O.S.


Mass estimation

1

0

20

P

P

2r

P2r

2

2

d)(1

)5.01(

)1(1

,/12

3

/12

/1 ,3

symmetricly sphetrical

,/1

c

Pzcz

zH

R

R

v

GM

Rrvv

r

vGM



.cos ,sin

where

,cossin2

binding nalgravitatio

for criterion Newtonian The

pr

2p

2r

RRVV

GMRV



).cos1

sin()

2(

),sin()2

(

),cos1(2

2/1

2/13

m

m

m

R

GMV

Rt

RR


Gravitationally bound Probability of binding.

%92

d),()(

vvpvpP


GB- probability

PP=92%=92%



Appendix III

LFs & DSF


光度函数 1

引言：

X-RAY EMISSION FROM CLUSTERS OF GALAXIES - Craig L. Sarazin (198X-RAY EMISSION FROM CLUSTERS OF GALAXIES - Craig L. Sarazin (1988) 8)


Schechter Function


光度函数 2

Trentham & Tully 2002, MNRAS, Trentham & Tully 2002, MNRAS, 335335, 712, 712

引言：


Double Schechter Function (DSF)


DSF fit (figure)


DSF fit (table)


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。

光学数据及其分析：动力学 && 光度函数：


Appendix IV

Density profile


Density profile


Appendix V

Photometric redshift


测光红移


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 SIMP

LEST 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 merger timescale and energetics. If shock fronts are discernible (with the help of Chandra's 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 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.


观测信息 Target Name: A168_OFFSET1 A168_OFFSET

2 Observe data: 2002-01-05 2002-11-01 Released data: 2003-01-10 2003-11-05 Exposure time: 41.12 ks 38.11 ks Observation ID: 3203 3204 Instrument: ACIS-I ACIS-I

Chandra X 射线分析：观测及数据处理：

http://cda.harvard.edu:9011/chaser/viewerImage.do?filetype=loresimg_jpg&obsid=3204


数据处理 ACIS 原始数据处理 :

ciao3.0 http://cxc.harvard.edu/ciao/

二级 (Level-two) 数据文件

Chandra X 射线分析：观测及数据处理：

http://cxc.harvard.edu/ciao/









Appendix of Imaging2After “csmooth”


Appendix of Imaging1

Exposure Map Corrected




Chandra X 射线分析： X 射线谱分析：







Appendix VIII

Eest-west divide



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Butcher-Oemler (B-O) 效应 (1978, 1984)