Color Variabilities of QSOs at z = 0.3 - 1.2

以作者查詢圖書館館藏

、以作者查詢臺灣博碩士

、以作者查詢全國書目

、勘誤回報

、線上人數：39

、訪客IP：3.145.59.187

姓名

陸勇志(Loke, Young Tzee) 查詢紙本館藏

畢業系所

天文研究所

論文名稱

(Color Variabilities of QSOs at z = 0.3 - 1.2)

相關論文

★ 亮紅外線星系ARP 55的CO(J=2-1)和CO(J=1-0)之譜線研究	★ 合併中之明亮紅外線星系的次毫米波段觀測
★ 后髮座星系團內相對論性電子能譜的數值計算	★ 萊曼α吸收雲的運動學SZ效應所引起之宇宙背景輻射非均向性
★ 類星體-星系對 0248+430 中的原子與分子氣體	★ 亮紅外星系 NGC 6090 中分子氣體之研究
★ X射線背景輻射對星系團質量-溫度關係之限制	★ AM CVn系統之可見光觀測
★ 利用電波與近紅外線觀測資料研究活躍星系核的性質	★ 具有偏極化寬譜線與不具有偏極化寬譜線的西佛二型星系之塵埃型態
★ On the Origin of the Radio Emission of Ultraluminous Infrared Galaxies	★ 使用近紅外波段搜尋高質量X射線雙星的光學對應體
★ 窄線西佛I型星系之電波及紅外線性質	★ 合併星系的快速搜尋法
★ 活躍星系中分子雲之物理特性	★ 伽瑪射線爆周圍環境探討

檔案

[Endnote RIS 格式]

[Bibtex 格式]

[相關文章]

[文章引用]

[完整記錄]

[館藏目錄]

[檢視]

[下載]

本電子論文使用權限為同意立即開放。
已達開放權限電子全文僅授權使用者為學術研究之目的，進行個人非營利性質之檢索、閱讀、列印。
請遵守中華民國著作權法之相關規定，切勿任意重製、散佈、改作、轉貼、播送，以免觸法。

摘要(中)

我們研究了類星體的顏色變化的特性。我們交叉比對史隆數位化巡 (SDSS) 所釋出的第七版資料 (DR 7) 和第十二版資料 (DR 12) 的類星體目錄，選出 608 個在兩個版本都有觀測資料且紅移在 0.3 到 1.2 之間的類星體。我們選用在靜止坐標系下 3000 埃與 4000 埃的光通量密度比值來定義顏色值。我們透過比較兩個版本類星體的顏色值來定義顏色變化。我們發現在靜止坐標系下，類星體的顏色變化分佈類似常態分佈，但部分類星體在數年的時間尺度下有著明顯的顏色變化。另外，我們還發現了八個類星體的光譜變化可以被塵埃紅化現象來解釋。我們的結果也顯示了類星體的顏色變化可能存在多個物理機制。

摘要(英)

We investigate the color variabilities of QSOs at z = 0.3 – 1.2. We selected the sample of 608 QSOs, which have multi-epoch spectra in both the Sloan Digital Sky Survey (SDSS) Data Released 7 (DR7) and Data Released 12 (DR12). We defined the spectral color ofthe QSOs by the ratio of flux densities of 3000 Å to 4000 Å in the rest frame. In each sample, the color variability is defined by the differences of color in DR7 and DR12.We find that the color variabilities show a Gaussian distribution with some QSOs displaying significant color changes within the timescale of a few years. We find that the spectral variabilities of eight color-change QSOs could be explained by dust reddening. Our results also show that the color variabilities of QSOs might originate from more than one physics mechanisms.

關鍵字(中)

★ 類星體
★ 活躍星系核
★ 星系

關鍵字(英)

★ QSO
★ AGN
★ Galaxy

論文目次

摘要 vii
Abstract ix
Contents xi
List of Figures xiii
1 Introduction 1
1.1 Active Galactic Nucleus....................................................... 1
1.2 Unification model ............................................................. 2
1.3 Subclass of QSOs.............................................................. 3
1.4 Red QSOs ..................................................................... 4
1.5 Variabilities of QSOs.......................................................... 4
2 Sample Selection 7
2.1 Spectroscopic Data............................................................ 7
2.2 Sample Selection and Defi nition of the Color ................................ 8
2.3 Defi nition of Color-change QSOs ............................................. 9
3 Results 11
3.1 Redshift Distribution of Color-change QSOs ................................. 11
3.2 Time Distribution of Color-change QSOs .................................... 13
3.3 Color of QSOs................................................................. 14
4 Discussions 25
4.1 Host Galaxy Contamination .................................................. 25
4.2 Dust reddening of the QSOs continuum...................................... 26
4.3 The intrinsic variabilities of QSOs............................................ 33
5 Conclusion 35
Bibliography 37
A Information of the selected QSOs 39
B Spectra of the color-change QSOs 61
C Example spectra of the controlled QSOs 69

參考文獻

[1] Alam, S., Albareti, F. D., Allende, P. C., et al. 2015, ApJS, 219, 12
[2] Bian, W.-H., Zhang, L., Green, R., & Hu, C. 2012, ApJ, 759, 88B
[3] Chen, I.-C. and Hwang, C.-Y. and Kaiser, N., et al. 2018, ApJ, 885, 66C
[4] Fynbo, J. P. U., Krogager, J.-K., Venemans, B., et al. 2013, ApJS, 204, 6
[5] Giveon, U., Maoz, D., Kaspi, S., Netzer, H., & Smith, P. S. 1999, MNRAS, 306, 637
[6] Glikman, E., Gregg, M. D., Lacy, M., et al. 2004, ApJ, 607, 60
[7] Glikman, E., Helfand, D. J., White, R. L., et al. 2007, ApJ, 667, 673
[8] Glikman, E., Urrutia, T., Lacy, M., et al. 2012, ApJ, 757, 51
[9] Glikman, E., Urrutia, T., Lacy, M., et al. 2013, ApJ, 778, 127
[10] Gunn, J. E., Siegmund, W. A., Mannery, E. J., et al. 2006, AJ, 131, 2332
[11] Heckman, T. M. 1980, A&A, 87, 152H
[12] Ho, L. C., Filippenko, A. V., & Sargent, W. L. W. 1997, ApJS, 112, 315
[13] Kelly, B. C., Bechtold, J., & Siemiginowska, A. 2009, ApJ, 698, 895
[14] LaMassa, S. M., Cales, S., Moran, E. C., et al. 2015, ApJ, 800, 144
[15] MacLeod, C. L., Ivezi ć , Ž ., Sesar, B., et al. 2012, ApJ, 753, 106
[16] MacLeod, C. L., Ross, N. P., Lawrence, A., et al. 2016, MNRAS, 457, 389
[17] Pâris, I., Petitjean, P., Ross, N. P., et al. 2017, A&A, 597, A79
[18] Pei, Y. C. 1992, ApJ, 395, 130
[19] Richards, G. T., Fan, X., Newberg, H. J., et al. 2002, AJ, 123, 2945
[20] Richards, G. T., Hall, P. B., Vanden Berk, D. E., et al. 2003, AJ, 126, 1131
[21] Ross, N. P., Myers, A. D., Sheldon, E. S., et al. 2012, ApJS, 199, 3
[22] Ruan, J. J., Anderson, S. F., Dexter, J., & Agol, E. 2014, ApJ, 783, 105
[23] Schneider, D. P., Richards, G. T., Hall, P. B., et al. 2010, AJ, 139, 2360
[24] Shields, J. C. 1992, APJ, 399L, 27S
[25] Stoughton, C., Lupton, R. H., Bernardi, M., et al. 2002, AJ, 123, 485
[26] Sun, Y.-H., Wang, J.-X., Chen, X.-Y., & Zheng, Z.-Y. 2014, ApJ, 792, 54
[27] Tsai, A.-L., & Hwang, C.-Y. 2017, ApJ, 842, 57
[28] Ulrich, M.-H., Maraschi, L., & Urry, C. M. 1997, ARA&A, 35, 445
[29] Urrutia, T., Becker, R. H., White, R. L., et al. 2009, ApJ, 698, 1095
[30] Urry, C. M., & Padovani, P., 1995, PASP, 107, 803
[31] Vanden Berk, D. E., Wilhite, B. C., Kron, R. G., et al. 2004, ApJ, 601, 692
[32] Webster, R. L., Francis, P. J., Petersont, B. A., Drinkwater, M. J., & Masci, F. J. 1995,
Nature, 375, 469
[33] Whiting, M. T., Webster, R. L., & Francis, P. J. 2001, MNRAS, 323, 718

指導教授

黃崇源(Chorng-Yuan Hwang)

審核日期

2019-8-19

推文