跳到主要內容

臺灣博碩士論文加值系統

(44.200.86.95) 您好!臺灣時間:2024/05/22 14:47
字體大小: 字級放大   字級縮小   預設字形  
回查詢結果 :::

詳目顯示

: 
twitterline
研究生:侯冠州
研究生(外文):Hou, Kuan-Chou
論文名稱:次毫米波星系的環境研究
論文名稱(外文):Environment of submillimeter galaxies
指導教授:陳林文
指導教授(外文):Chen, Lin-Wen
學位類別:碩士
校院名稱:國立臺灣師範大學
系所名稱:地球科學系
學門:自然科學學門
學類:地球科學學類
論文種類:學術論文
論文出版年:2011
畢業學年度:100
語文別:英文
論文頁數:56
中文關鍵詞:高紅移星系次毫米波星系
外文關鍵詞:Galaxies: high-redshiftsubmillimetre: galaxies
相關次數:
  • 被引用被引用:0
  • 點閱點閱:188
  • 評分評分:
  • 下載下載:10
  • 收藏至我的研究室書目清單書目收藏:0
次毫米波星系是一種位於高紅移的星系,它的大質量和非常高的恆星形成率,一般相信是由星系合併所產生的結果。本篇論文主要研究次毫米波星系的性質以及它們在大尺度結構中所扮演的角色。 研究方法是計算次毫米波星系周圍的可見光星系密度,以及藉由關聯性方程式這種統計方法來分析次毫米波星系與萊曼α發射星系的關係。主要研究的範圍是COSMOS和ECDF-S天區。在ECDF-S天區中,LABOCA和AzTEC儀器所觀測到的次毫米波星系有紅位移的估計,可以有效減少天空中投影的效應。我們取半徑為1-2個百萬秒差距計算次毫米波星系周圍的星系密度,結果顯示在紅移2.5和3.5的地方有些微的訊號,不過還是需要注意紅移的誤差造成的不確定性。我們更進一步使用B、z 、K三個濾鏡選取出BzK星系,它們可以區分出星系是否還有恆星生成。我們發現在一個百萬秒差距內,低恆星生成率的BzK星系與次毫米星系有較高的關聯性。另一方面,使用關聯性方程式分析次毫米波星系與萊曼α發射星系,結果沒有顯示任何訊號,亦即兩種星係可能沒有空間上的關連性。最後我們討論了次毫米波星系所在的大尺度結構的性質以及次毫米波星系與其他高紅移星系之間的交互關係。

To study the environment of high-redshift star-forming galaxy — submillime- ter galaxies (SMGs) — and their role during large-scale structure formation, we have estimated the galaxy number density fluctuations around SMGs, and analyzed their cross correlation functions with lyman alpha emitters (LAEs), and optically-selected galaxies with photometric redshift in the COSMOS and ECDFS fields. We first measured the galaxy density around SMGs based on SMGs with photometric redshift zSMG compiled from data obtained by LABOCA and AzTEC in the ECDFS field. The number density of surrounding galaxies within projected radius of 1–2 Mpc and zSMG ± 0.1 suggests a marginal signal of excess galaxy count at z ∼ 2.5 and ∼ 3.5, although the uncertainty of redshift estimate is still large. We have further investigated the density of passive and starforming BzK galaxies at similar redshift around SMGs and find that BzKs have overdensity around LABOCA-SMGs at radius smaller than 1 Mpc, espe- cially passive BzKs. On the other hand, our second task, the cross correlation functions between SMGs and LAEs, detects no correlation signal between the two populations, even after the exclusion of the SMGs with redshift significantly far from that of LAEs. Finally we discuss the property of the large scale struc- ture where SMGs are located and the interconnection between SMGs and other high-redshift galaxy populations.
1 Introduction 5
2 Data 12
2.1 SMGs ....................................... 13
2.1.1 photometricredshift ........................... 13
2.2 Galaxysamples.................................. 16
2.2.1 BzKs.................................... 16
2.2.2 LAEs.................................... 18
3Galaxy density 20
3.1 Opticalgalaxydensity .............................. 21
3.1.1 MonteCarlotest ............................. 23
3.2 BzKs........................................ 26
3.2.1 Randompositionstest .......................... 29
4Correlation function analysis 31
4.1 LAE-SMGcross-correlationfunction ...................... 33
4.2 Backgroundandforegroundcontamination................... 36
4.2.1 MonteCarlotestofCCF......................... 37
4.3 Correlationlength................................. 38
5 Discussion 39
6 Summary 42
Reference 43
7 Appendix 48
7.1 GalaxydensityaroundSMGswithoutredshift . . . . . . . . . . . . . . . . . 48
7.2 LAErestframeUVcolor............................. 50
7.2.1 Red/blueLAEs? ............................. 50
7.2.2 IdentificationofLAEopticalcounterparts . . . . . . . . . . . . . . . 50
7.2.3 CCFofSMGsandred/blueLAEs.................... 50
7.2.4 Bright/FaintLAEs ............................ 51
7.3 SMGsfluxratio.................................. 55
Aretxaga I. et al., 2011, MNRAS, 415, 3831
Austermann J. E. et al., 2010, MNRAS, 401, 160
Barger A. J., Cowie L. L., Sanders D. B., Fulton E., Taniguchi Y., Sato Y., Kawara K., Okuda H., 1998, Nature, 394, 248
Beelen A. et al., 2008, A&;A, 485, 645
Blain A. W., Chapman S. C., Smail I., Ivison R., 2004, ApJ, 611, 725
Blain A. W., Longair M. S., 1993, MNRAS, 264, 509
Blain A. W., Smail I., Ivison R. J., Kneib J.-P., Frayer D. T., 2002, Phys. Rep., 369, 111
Cardamone C. N. et al., 2010, ApJS, 189, 270
Chapin E. L. et al., 2009, MNRAS, 398, 1793
Chapman S. C., Blain A., Ibata R., Ivison R. J., Smail I., Morrison G., 2009, ApJ, 691, 560
Chapman S. C., Blain A. W., Smail I., Ivison R. J., 2005, ApJ, 622, 772
Condon J. J., 1992, ARA&;A, 30, 575
Cowie L. L., Hu E. M., 1998, AJ, 115, 1319
Daddi E., Cimatti A., Renzini A., Fontana A., Mignoli M., Pozzetti L., Tozzi P., Zamorani G., 2004, ApJ, 617, 746
Daddi E. et al., 2009, ApJ, 694, 1517 Daddi E. et al., 2005, ApJ, 626, 680
Downes T. P., Welch D., Scott K. S., Austermann J., Wilson G. W., Yun M. S., 2012, MNRAS, 423, 529
Finkelstein S. L., Rhoads J. E., Malhotra S., Grogin N., 2009, ApJ, 691, 465
Francis P. J., Palunas P., Teplitz H. I., Williger G. M., Woodgate B. E., 2004, ApJ, 614, 75
Francis P. J., Woodgate B. E., Danks A. C., 1997, ApJ, 482, L25
Francis P. J. et al., 1996, ApJ, 457, 490
Gawiser E. et al., 2007, ApJ, 671, 278
Gear W. K., Lilly S. J., Stevens J. A., Clements D. L., Webb T. M., Eales S. A., Dunne L., 2000, MNRAS, 316, L51
Gronwall C. et al., 2007, ApJ, 667, 79
Guaita L. et al., 2010, ApJ, 714, 255
Gu ̈sten R., Nyman L. ̊A., Schilke P., Menten K., Cesarsky C., Booth R., 2006, A&;A, 454, L13
Hatsukade B. et al., 2009, in Astronomical Society of the Pacific Conference Series, Vol. 418, AKARI, a Light to Illuminate the Misty Universe, Onaka T., White G. J., Nakagawa T., Yamamura I., eds., p. 307
Hayashino T. et al., 2004, AJ, 128, 2073 Hughes D. H. et al., 1998, Nature, 394, 241 Ilbert O. et al., 2009, ApJ, 690, 1236 Kong X. et al., 2006, ApJ, 638, 72
Lai K. et al., 2008, ApJ, 674, 70
– 45 –
Landy S. D., Szalay A. S., 1993, ApJ, 412, 64
Lin L. et al., 2011, ArXiv e-prints
Magliocchetti M., Maddox S. J., 1999, MNRAS, 306, 988
Magnelli B. et al., 2012, A&;A, 539, A155
Matsuda Y. et al., 2005, ApJ, 634, L125
McCracken H. J. et al., 2010, ApJ, 708, 202
Murayama T. et al., 2007, ApJS, 172, 523
Nilsson K. K., Møller P., 2009, A&;A, 508, L21
Nilsson K. K., Møller P., 2011, A&;A, 527, L7
Nilsson K. K. et al., 2007, A&;A, 471, 71
Nilsson K. K., O ̈stlin G., Møller P., Mo ̈ller-Nilsson O., Tapken C., Freudling W., Fynbo J. P. U., 2011, A&;A, 529, A9
Nilsson K. K., Tapken C., Møller P., Freudling W., Fynbo J. P. U., Meisenheimer K., LaursenP.,O ̈stlinG.,2009,A&;A,498,13
Ono Y. et al., 2010, MNRAS, 402, 1580 Ouchi M. et al., 2009, ApJ, 706, 1136 Ouchi M. et al., 2008, ApJS, 176, 301 Ouchi M. et al., 2003, ApJ, 582, 60
Ouchi M. et al., 2010, ApJ, 723, 869
– 46 –
Palunas P., Teplitz H. I., Francis P. J., Williger G. M., Woodgate B. E., 2004, ApJ, 602, 545
Partridge R. B., Peebles P. J. E., 1967, ApJ, 147, 868
Peebles P. J. E., 1980, The large-scale structure of the universe, Peebles, P. J. E., ed.
Perera T. A. et al., 2008, MNRAS, 391, 1227
Pirzkal N., Malhotra S., Rhoads J. E., Xu C., 2007, ApJ, 667, 49
Scott K. S. et al., 2008, MNRAS, 385, 2225
Scott K. S. et al., 2010, MNRAS, 405, 2260
Scott S. E. et al., 2002, MNRAS, 331, 817
Shioya Y. et al., 2009, ApJ, 696, 546
Siringo G. et al., 2009, A&;A, 497, 945
Smail I., Ivison R. J., Blain A. W., 1997, ApJ, 490, L5
Steidel C. C., Adelberger K. L., Shapley A. E., Pettini M., Dickinson M., Giavalisco M., 2000, ApJ, 532, 170
Tacconi L. J. et al., 2008, ApJ, 680, 246 Tamura Y. et al., 2009, Nature, 459, 61 Wardlow J. L. et al., 2011, MNRAS, 415, 1479 Weiß A. et al., 2009, ApJ, 707, 1201
Wilson G. W. et al., 2008, MNRAS, 386, 807
Yun M. S. et al., 2012, MNRAS, 420, 957
連結至畢業學校之論文網頁點我開啟連結
註: 此連結為研究生畢業學校所提供,不一定有電子全文可供下載,若連結有誤,請點選上方之〝勘誤回報〞功能,我們會盡快修正,謝謝!
QRCODE
 
 
 
 
 
                                                                                                                                                                                                                                                                                                                                                                                                               
第一頁 上一頁 下一頁 最後一頁 top