Part I: broad line spectra
(1)宽线区离黑洞很近，处于引力与辐射压力的平衡
(2)吸收吸积盘的连续谱
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宽线区光致电离模型的证据
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•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
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Dong et al. 2011
2796 & 2803
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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
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Hu et al. 2008
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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
Lya/Hb(obs) = 5-15 (>= 30)
Ha/Hb(obs) = 4-6 (~2.8)
Reference: Baker & Menzel (1938)
Osterbrock (1989)
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Part II: basic parameter
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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
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Line Diagnostics: Density
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Location of BLR
From light curve: the location of the BLR is several light days from the central BH.
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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
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Gas mass in BLR (with temperature and density in hand)
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Covering factor and filling factor
Filling factor: (4/3πl3N)/(4/3πr3)
Covering factor:how much of the continuum is
absorbed by BLR: Ω/4π
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Line Variability of BLR
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Line Variability of BLR
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Part III: Photoionization of BLR
宽线区分层结构的一个证据
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Ionization parameter--U
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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）
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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
o
o
+ 0
平谱扩展的部分光致电离区 （PIZ）H /H ~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
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Part IV: Broad line profile
研究线的轮廓的用处
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Double peaked
emission lines

Disk parameters
Eracleous, M. 1994
Strateva, I. 2003
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Evidence for an Intermediate-Line Region?
Inflow?
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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
BAL QSO
Outflow: driven by AGN?
Gibson, R.
2009
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Outflow
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Estimate MBH
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Estimate MBH
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Part V: Reverberation Mapping
Peterson B.M. 1993 Rewiew paper
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Ψ描述了发射线对于δ函数的连续谱的反应
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Ψ描述了发射线对于δ函数的连续谱的反应
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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
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Also found:
(1)Broadest lines vary fastest
(2)Higher ionization lines vary fastest
BLR has a stratified ionization structure
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L—R relation (这个关系非常重要并且被广泛应用)
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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
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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
(1)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
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gravitation dominated!
Peterson et al. 2000
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gravitation dominated!
Peterson et al. 2000
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平均谱
RMS谱
（root mean square）
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how to measure line width and time lag
Peterson
2004
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Open question: What is BLR?
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What is BLR? I
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What is BLR? II
宽线区云块的性质
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宽线区云块的性质
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What is BLR? III
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Outflow/wind
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Outflow/wind
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Elvis
2000
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发射线和连续谱的相关
Indication:
(1)支持光致电离模型
(2)不同源发射线的等值宽
度基本一样
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Baldwin效应
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Baldwin效应
如果Baldwin效应准确，测量CIV高红移类星体的光度
光度距离宇宙学参数
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Baldwin效应
导致该效应的可能原因：
（1）电离参数U随光度的增加下降
（2）覆盖因子随光度的增加下降
（3）盘的倾角
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Torus （Elitzur, M）
Rdust = 1.3L461/2T15002.8pc
(石墨的升华半径)
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