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Part I: broad line spectra

Part I: broad line spectra. 宽线区离黑洞很近，处于引力与辐射压力的平衡 吸收吸积盘的连续谱. 宽线区光致电离模型的证据. 速度 轮廓 logarithmic F λ (v)~ － ln(v) Blended （如小蓝包） 光变 （宽线区的云块光学厚） 分层结构. Dong et al. 2011. 2796 & 2803. Dong et al. 2011. Doppler broadened FWHM (500~10000km/s with a typical value of 5000km/s)

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Part I: broad line spectra

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  1. Part I: broad line spectra • 宽线区离黑洞很近，处于引力与辐射压力的平衡 • 吸收吸积盘的连续谱

  2. 宽线区光致电离模型的证据

  3. 速度 • 轮廓 logarithmic Fλ(v)~ －ln(v) • Blended （如小蓝包） • 光变（宽线区的云块光学厚） • 分层结构

  4. Dong et al. 2011 2796 & 2803

  5. Dong et al. 2011 Doppler broadened FWHM (500~10000km/s with a typical value of 5000km/s) FWZI （full width at zero intensity）:true range of line of sight velocity

  6. Hu et al. 2008

  7. Assumption: pure hydrogen nebula --Case A: All of the lines are assumed to be optical thin --Case B: Lyman-series lines are all optical thick Reference: Baker & Menzel (1938) Osterbrock (1989) Lya/Hb(obs) = 5-15 (>= 30) Ha/Hb(obs) = 4-6 (~2.8)

  8. Part II: basic parameter

  9. Temperature and density More detailed analyses show CIII] to originate in region different from Lyα or CIV emitting region, typical densities can be as high as 1011 cm-3

  10. Line Diagnostics: Density

  11. Location of BLR From light curve: the location of the BLR is several light days from the central BH.

  12. 发射线的轮廓（对数轮廓） 径向运动方程 电离平衡方程 质量连续性方程

  13. Gas mass in BLR (with temperature and density in hand)

  14. Covering factor and filling factor • Filling factor: (4/3πl3N)/(4/3πr3) • Covering factor:how much of the continuum is • absorbed by BLR: Ω/4π

  15. Line Variability of BLR

  16. Line Variability of BLR

  17. Part III: Photoionization of BLR 宽线区分层结构的一个证据

  18. Ionization parameter--U

  19. 光致电离模型 1 电离连续谱的形状 2 元素丰度（如太阳丰度） 3 云块中的粒子密度（NH） 4 云块的柱密度（源于观测） 5 电离参数 （G. Ferland  Cloudy）

  20. 斯特龙根深度（Stromgren depth） Q(H) = L/hγ U = Q(H)/(4πr2cne) 单位时间内达到云块上的光子数： AcQ(H)/(4πr2) = AcUcne 单位时间内的复合数： ne2αBVc = AcUcne R = Uc/neαB ~ 0.7Rsun • 平谱扩展的部分光致电离区（PIZ）H+/H0~0.1 • Lyman alpha光子被PIZ区捕获，导致n=2态的氢原子增多Lya/Ha小于caseB的预言

  21. Part IV: Broad line profile 研究线的轮廓的用处

  22. Double peaked emission lines  Disk parameters Eracleous, M. 1994 Strateva, I. 2003

  23. Evidence for an Intermediate-Line Region? Inflow?

  24. BAL Quasars: normal quasars viewed at • angle along the l.o.s. of intervening, fast-moving material • High-ionization (HIBAL): Ly, NV, SiIV, CIV • Low-ionization (LOBAL): AlIII, MgII SDSS BALQSOs from Trump et al. 2006

  25. BAL QSO Outflow: driven by AGN? Gibson, R. 2009

  26. Outflow

  27. Estimate MBH

  28. Estimate MBH

  29. Part V: Reverberation Mapping Peterson B.M. 1993 Rewiew paper

  30. Ψ描述了发射线对于δ函数的连续谱的反应

  31. Ψ描述了发射线对于δ函数的连续谱的反应

  32. CCF has a peak at the lag for which C(t) and L(t) match bestbased on CCF we can measure the size of BLR NGC5548 Delay：～22days

  33. Also found: • Broadest lines vary fastest • Higher ionization lines vary fastest • BLR has a stratified ionization structure

  34. L—R relation (这个关系非常重要并且被广泛应用)

  35. Final Part: the assumptions and details used in estimating MBH based on mapping technique • Assumption : • the geometry of BLR? • gravitation dominated • Detail – how to measure line width and time lag

  36. geometry of BLR • MBH = f × RV2/G • f is a scale factor of order unity that depends on the structure, kinematics, and inclination of the BLR • BLR as a flared disk? H/R > 0.1 • (2) BLR as a warped disk • (3) A two component BLR: a disk and a wind Collin et al. 2006

  37. gravitation dominated! Peterson et al. 2000

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