Active Galactic Nuclei and Super Massive Black Holes

銀河物理学特論 I
G l ti Astrophysics
Galactic
A t
h i I
II-2: Active Galactic Nuclei and
Super Massive Black Holes
2015/06/22
Stellar Mass Black Hole candidates
星質量ブラックホル候補天体
星質量ブラックホール候補天体
Blackhole binary scales
McClintock et al. 2011,
arXiv:1101.0811
Black hole effective potential
ブラックホルの有効ポテンシャル
ブラックホールの有効ポテンシャル
•
Different from Newtonian potential.
Frolov 2003
Accretion disk around black holes
ブラックホルまわりの降着円盤
ブラックホールまわりの降着円盤
•
•
•
Schwarzschild radius: rs=2GM/c^2
The innermost stable circular orbit
off non-rotating
t ti BH : 3 rs
The radiation energy from
Schwarzschild black hole is 6% of
the rest mass energy of accreting
matter. 0.06 mdot c^2
•
Viscosity transfer angular
momentum outside, and heat up
the accretion disk. The disk emits
black body radiation.
•
Stellar-mass black holes
‒ X-ray emission
•
Super massive black holes
‒ UV emission (hard to observe
due to hydrogen absorption).
Non-rotating Innermost Stable Circular Orbit (3Rs)
McClintock et al. 2011, arXiv:1101.0811
Radiation from accretion disk : stellar mass black hole
降着円盤からの放射: 星質量ブラックホ
降着円盤からの放射
星質量ブラックホールの場合
ルの場合
•
•
Standard accretion disk with
geometrically-thin optically-thick
geometrically-thin,
disk.
For stellar mass black holes, the
black body radiation from the inner
most stable circular orbits is in the
X-ray wavelength range.
•
•
Rmax=49/12 rs
Tmax proportional to Mdot^1/4
and M^(-1/2)
•
The hard X-ray
y photons
p
originate
g
from inverse Compton scattering
process in the hot plasma in the
surface of the disks.
Gou et al. 2001, ApJ, 742, 85
Radiation from accretion disk : super massive black hole
降着円盤からの放射: 超大質量ブラックホ
降着円盤からの放射
超大質量ブラックホールの場合
ルの場合
•
For SMBHs the black body radiation
from the inner most stable circular
orbit is in the UV wavelength range.
•
The hard X-ray photons originate
from inverse Compton scattering
process in the hot plasma
p
p
in the
surface of the disks.
Kawaguchi et al. 2001, ApJ, 546, 966
Spectral Energy Distribution of AGNs
AGN のスペクトルエネルギー分布
の
クトルネルギ分布
•
QSO SEDs from radio to X-ray
Richards et al. 2006, ApJS, 166, 470
Spectral Energy Distribution of AGNs
AGN のスペクトルエネルギー分布
の
クトルネルギ分布
•
Conversion factor to the bolometric luminosity (total integrated
luminosity). The UV and IR wavelength range radiation dominates the
radiation
di ti energy.
Richards et al. 2006,, ApJS,
p , 166,, 470
UV/optical spectra of AGNs
紫外線/可視光の
紫外線/可視光のスペクトル
クトル
•
UV/Optical average SEDs of SDSS QSOs
Richards et al.
al 2003,
2003 ApJ,
ApJ 126,
126 1131
Two types of AGNs: type-1 / type-2
2 種類の AGN: type-1
yp
/ type-2
yp
•
Permitted emission lines (Ha,Hb,MgII,CIII],CIV,NV,Lya etc) of Seyfert 1 galaxies show
broad component with FWHM of 2000-10000km/s (broad-lines). Forbidden
transition lines (禁制線) does not have broad component,
p
, because the g
gas density
y of
the broad-line region is higher than the critical density ( 6x10^5cm-3 for [OIII]5007)
of the forbidden transitions. Forbidden emission lines as well as permitted ones
show narrow emission with FWHM 100-1000km/s (narrow-lines).
Seyfert
y
1
Seyfert
y
2
Permitted lines: broad+narrow-line
Permitted lines: only narrow-line
Forbidden lines: narrow-line
Forbidden lines: narrow-line
Size of Broad-line Region
Broad-line 領域のサイズ
•
reverberation mapping observations measure the time-lag between the
time-variation of the fluxes of the nuclear continuum and broad emission
lines The time lag corresponds to the typical distance between the black
lines.
hole and the line emitting region. The black hole masses can be estimated
with the distance and the line width. The lag-velocity diagram suggests the
virialized condition of the broad
broad-line
line region.
region
Peterson et al. 2004, ApJ, 613, 682
Size of Broad-line Region
Broad-line 領域のサイズ
•
Size of the broad-line region is proportional to the square of the luminosity.
It is consistent with the relation expected if (1) the gas density distribution
around nucleus is similar in various AGNs and (2) ionization parameter of
the broad-line region is constant.
Kaspi et al. 2005, ApJ, 629, 61
Dusty-torus around Broad-line region
Broad-line 領域の周りのダストトーラス構造
領域の周りのダトトラ構造
•
Unified model of Seyfert 1 and 2 galaxies is proposed by Antonucci and Miller
(1985, ApJ, 297, 621) based on the data obtained by spectro-polarimetric
observation Dust torus structure around the nuclei hide the broad-line region of
observation.
Seyfert 2 galaxies. Emission from the broad-line can be observed through
scattered light (though electron or dust scattering).
Miller and Antonucci 1983, ApJL, 271, 7
Dusty-torus around Broad-line region
Broad-line 領域の周りのダストトーラス構造
領域の周りのダトトラ構造
Antonucci and Miller, 1985, ApJ, 297, 621
Dusty-torus and narrow-line region
ダストトーラスと
ダ
トトラと Narrow-line 領域
NGC5252 Morse et al.
1998, ApJ 505, 159
Dusty torus structure and X-ray emission
ダストトーラスと
ダ
トトラと X 線放射
•
X-ray emission from the center of narrow-line AGNs show photo-electric
absorption.
Awaki et al. 1991,PASJ, 43, 195
Unified model of AGNs
AGN の統一モデル
の統
デル
•
Luminous AGN: QSOs,
•
Less-luminous
Less
luminous AGN: Seyfert
•
Radio-loud: Radio-loud QSOs,
radio galaxies
•
Radio-quiet:Radio-quiet QSOs,
Seyferts
From www.cv.nrao.edu/course/astr534/ExtraGalactic.html
Size of the dusty torus
ダトトラのサイズ
ダストトーラスのサイズ
•
Size of the inner surface of the dusty torus derived with the time-delay
between the UV and IR radiation. 10 light days = 8.5 mpc = 1700 AU. The
size
i iis similar
i il tto th
the outer
t size
i off th
the b
broad-line
d li region.
i
Suganuma et al. 2006, ApJ, 639, 46
Fraction of obscured AGNs
隠された AGN の割合
•
Fraction of the obscured AGNs determined with the X-ray selected AGNs.
Hasinger 2008, A&A, 490, 905
AGNs with hidden-broad-line region
隠された broad-line 領域を持
領域を持つ AGN
•
Seyfert 2 galaxies with Hidden-broad-line region (HBLR: Revealed by
spectro-polarimetry) show hot MIR-FIR spectra similar to Seyfert 1
galaxies.
l i (Non-HBLR
(N
HBLR Seyfert
S f t 2 galaxies
l i show
h
similar
i il F25/F60 tto HII
HII-region,
i
LINER, Starbursts (HLS). Non-HBLRs have lower intrinsic luminosity).
Tran 2003, ApJ, 583, 632
Narrow-line AGNs selected with line ratio diagram
ライン比を用いた
ライン比を用
た narrow-line AGN の選択
AGNs tend to have stronger highly
ionized emission lines, like [OIII]
Solid line ：selection line by Kewly et al.
(2001) model calculation, Dashed line :
empirical line.
Kauffmann et al. 2003, MNRAS, 346, 1055
Type1-Type2 variation
Type-1
yp
から Type-2
yp
への遷移
の遷移
•
Changing AGN type from type-1 to type-1.9 in
scale.
a few 10 years time
Mrk 590
Denney et al. 2014
arXiv:1404.4879
BLR size with reverberation mapping
反響マッピング法による
反響
ッング法による BLR サイズの測定
Peterson 2006
•
•
BLR size, velocity and mass M = f (R sigma
sigma^2
2 / G)
f represents the kinematics and geometry of BLR. Isotoropic: f=3.
f -factor
f 係数
Onken et al. 2004, ApJ, 615, 645
•
BLR size, velocity and mass
M = f (R sigma
sigma^2
2 / G)
•
f represents the
ki
kinematics
i and
d geometry
of BLR. Isotropic sphere:
f=3.
•
f is determined to match
MBH sigma relation for
MBH-sigma
non-active galaxies.
f -factor
f 係数
Woo et al. 2010, ApJ, 716, 269
f -factor
f -係数
係数
•
Dependence on bar properties ?
Graham et al. 2011, MNRAS, 412, 2211

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