銀河物理学特論 IG l ti A t h i IGalactic Astrophysics I

II-2: Active Galactic Nuclei and Super Massive Black Holes

2015/06/22

Stellar Mass Black Hole candidates星質量ブラックホール候補天体星質量ブラックホ ル候補天体

Blackhole binary scalesBlackhole binary scalesMcClintock et al. 2011, arXiv:1101.0811

Black hole effective potentialブラックホールの有効ポテンシャルブラックホ ルの有効ポテンシャル

• Different from Newtonian potential.

Frolov 2003

Accretion disk around black holesブラックホールまわりの降着円盤ブラックホ ルまわりの降着円盤

• Schwarzschild radius: rs=2GM/c^2• The innermost stable circular orbit

f t ti BH 3of non-rotating BH : 3 rs• The radiation energy from

Schwarzschild black hole is 6% of the rest mass energy of accretingthe rest mass energy of accreting matter. 0.06 mdot c^2

• Viscosity transfer angular

Non-rotating Innermost Stable Circular Orbit (3Rs)

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).

McClintock et al. 2011, arXiv:1101.0811

Radiation from accretion disk : stellar mass black hole降着円盤からの放射: 星質量ブラックホールの場合降着円盤からの放射 星質量ブラックホ ルの場合

• Standard accretion disk with geometrically-thin optically-thickgeometrically-thin, optically-thick disk.

• For stellar mass black holes, the black body radiation from the innerblack 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 photons originate y p gfrom 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ールの場合降着円盤からの放射 超大質量ブラックホ ルの場合

• For SMBHs the black body radiation ffrom 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 in the p psurface of the disks.

Kawaguchi et al. 2001, ApJ, 546, 966

Spectral Energy Distribution of AGNsAGN 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 AGNsAGN 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 di tiradiation energy.

Richards et al. 2006, ApJS, 166, 470, p , ,

UV/optical spectra of AGNs紫外線/可視光のスペクトル紫外線/可視光の クトル

• UV/Optical average SEDs of SDSS QSOs

Richards et al 2003 ApJ 126 1131Richards et al. 2003, ApJ, 126, 1131

Two types of AGNs: type-1 / type-22 種類の AGN: type-1 / type-2種類の yp / 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, because the gas density of (禁制線) p , g ythe 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 1 Seyfert 2y

Permitted lines: broad+narrow-line

Forbidden lines: narrow-line

y

Permitted lines: only narrow-line

Forbidden lines: narrow-line

Size of Broad-line RegionBroad-line 領域のサイズ領域のサイズ

• “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 blacklines. The time lag corresponds to the typical distance between the black 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-line regionvirialized condition of the broad line region.

Peterson et al. 2004, ApJ, 613, 682

Size of Broad-line RegionBroad-line 領域のサイズ領域のサイズ

• 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 ofaround 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 regionBroad-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-polarimetricobservation Dust torus structure around the nuclei hide the broad-line region ofobservation. Dust torus structure around the nuclei hide the broad-line region of 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 regionBroad-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 Narrow-line 領域ダ トト ラ と 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 X 線放射ダ トト ラ と 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 AGNsAGN の統一モデルの統 デル

• Luminous AGN: QSOs,

• Less-luminous AGN: SeyfertLess 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ダストトーラスのサイズダ トト ラ 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 i i i il t th t i f th b d li isize is similar to the outer size of the broad-line region.

Suganuma et al. 2006, ApJ, 639, 46

Fraction of obscured AGNs隠された AGN の割合隠された 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 領域を持つ AGN隠された 領域を持

• Seyfert 2 galaxies with Hidden-broad-line region (HBLR: Revealed by spectro-polarimetry) show “hot” MIR-FIR spectra similar to Seyfert 1

l i (N HBLR S f t 2 l i h i il F25/F60 t HII igalaxies. (Non-HBLR Seyfert 2 galaxies show similar F25/F60 to HII-region, 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 narrow-line AGN の選択ライン比を用 た 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 variationType-1 から Type-2 への遷移yp から yp の遷移

• Changing AGN type from type-1 to type-1.9 in ~ a few 10 years time scale.

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 BLR サイズの測定反響 ッ ング法による サイズの測定

• BLR size, velocity and mass M = f (R sigma^2 / G)

Peterson 2006

BLR size, velocity and mass M f (R sigma 2 / G)• “f” represents the kinematics and geometry of BLR. Isotoropic: f=3.

“f”-factor“f” 係数係数

• BLR size, velocity and mass M = f (R sigma^2 / G)M f (R sigma 2 / G)

• “f” represents the ki i dkinematics and geometry of BLR. Isotropic sphere: f=3.

• “f” is determined to match MBH sigma relation forMBH-sigma relation for non-active galaxies.

Onken et al. 2004, ApJ, 615, 645

“f”-factor“f” 係数係数

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