# AY202a Galaxies & Dynamics Lecture 14: Galaxy Centers & Active Galactic Nuclei - PowerPoint PPT Presentation

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AY202a Galaxies & Dynamics Lecture 14: Galaxy Centers & Active Galactic Nuclei. Galaxy Centers. History AGN Discovered way back when --- Fath 1908 Broad lines in NGC1068 Seyfert 1943 Strong central SB correlates with broad lines

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AY202a Galaxies & Dynamics Lecture 14: Galaxy Centers & Active Galactic Nuclei

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## AY202a Galaxies & DynamicsLecture 14:Galaxy Centers &Active Galactic Nuclei

### Galaxy Centers

History

AGN Discovered way back when ---

Fath 1908 Broad lines in NGC1068

Seyfert 1943 Strong central SB

Growing evidence over the years that there was a central engine and that the central engine must be a black hole!

And, what about galaxies that are not AGN?

Masers in NGC4258

microarcsec proper motions with VLBI

### Reverberation Mapping

Blandford & McKee ’82,  Peterson et al.

Assume

1. Continuum comes from a single

central source

2. Light travel time is the most

important timescale τ = r/c

3. There  a simple (not necessarily

linear) relation between the

observed continuum and the

ionizing continuum.

Continuum light curve relative to mean

### L(V,t) = ∫ (V,τ) C(t-τ) dτ

Velocity delay map

N5548

Lag relative to 1350A = 12 days @ Lyα, 26 days @ CIII], 50 days @ MgII

Kaspi et al R vs L

& M vs L

From Reverberation Mapping

Greene & Ho SDSS AGN M● vs σ

Greene

& Ho

Push to low M

Log (M●/M) = 7.96 + 4.02 (σ/200 km/s)

Barth,

Greene

& Ho

BH Mass Function

Greene & Ho ‘07

### Active Galactic Nuclei

1943 Carl Seyfert Sy1 = Broad Balmer lines 104 km/s

Sy2 = Intermediate width lines 103

1950’s Jansky, Ryle detected Radio Sources

Virgo A = M87, Cygnus A, NGC5128, NGC1275

1963 Greenstein & Schmidt identified QSO’s

(3C48 z=0.367, 3C273 z =0.158)

General Properties

Compact central source  energy density high,

dominates host galaxy

Non-thermal spectrum

Optical/UV - general shows strong emission lines from dense and less dense regions. Polarization (1-10%), jets

Radio – jets, lobes, compact sources

X-rays --- Power law spectrum, often into the Mev

Gamma rays --- detection of some sources like BL Lac’s into the TeV

Variability

### Classifications

Sy1/QSO = Type I Broad permitted lines 104+ km/s

narrower forbidden lines 103 km/s, BLRG

Sy2 = Type II narrower lines, all ~ 103 km/s

line ratios indicative of photoionization by a

non-thermal (power law) spectrum, NLRG

BL Lac = Blazar continuum emission only, usually strong radio and/or x-ray source, polarized

LINER = Low ionization nuclear emission line region

OVV = Optically Violent Variable  QSO, Blazar

NGC5940 Sy1

[OIII]

H

ns

NGC4151 Sy1.2

NGC4151 Sy1.2

[NII]

[NII]

[OI] [OI]

[SII]

NGC4388 Sy2

NGC3998 LINER

Peterson

### High S/N UV

LBQS Mean QSO Spectrum

Common Emission Lines in AGN

### Spectral Classification by Line Ratio

Seyferts/QSOs

Baldwin,

Terlevich

& Phillips

(based on

Osterbrock)

Star Forming

LINER

Electron Density from Line Ratios

Intensity ratio changes as

collisional depopulation

begins to dominate

collisional

[SII] doublet

6717 &6731A

collisional

Peterson, Pogge based on Osterbrock

Temperature from Line Ratios

Relative population of states depends on temperature

[OIII] 4363 and the 4959+5007 doublet

Peterson, Pogge based on Osterbrock

Real or Memorex?

Classification can

depend on how you

look --- total vs

polarized.

(Miller et al.)

looks a lot like a Sy1!

### Fanaroff-Riley Classification

Fanaroff & Riley (1974) noted that radio source structure was correlated source luminosity

FR I – weak sources, bright centers decreasing

surface brightness to the

edge

FR II – have limb brightened

regions of enhanced emission

1400 Mhz vs MB from

Owen & Ledlow ‘94

FR I

(3C449,

Perley et al ’79)

FR II

(3C47,

Bridle et al. ’94)

David W. Hogg, Michael R. Blanton, and the Sloan Digital Sky Survey Collaboration

David W. Hogg, Michael R. Blanton, and the Sloan Digital Sky Survey Collaboration

Cen A

Chandra

Optical

X-ray

Comp

### Superluminal Motions

3C279 (NRAO)

VLBI

Keel

Consider two blobs, one stationary and one moving away from it at a velocity c at an angle of  to the line-of-sight. Apparent transverse velocity is

v =

which has a maximum at

v ~ c  = 1/(1-2)1/2

c sin()

1-  cos()

### Basic Models

1959 Woltjer’s argument --- (1) centers of AGN very small, r < 100 pc, (2) typical line widths are v > 1000 km/s, so by

GM/r ~ v2  M > 1010 (r/100pc) M

So either M is really big, implying a very high mass density inside r, or r is much smaller, implying a very high energy density at the center - or both.

Continuum Spectrum best described as

Synchrotron-Self Compton + thermal emission from an accretion disk + dust & stars, + lines from the gas.

SSC  Synchrotron spectrum with a low frequency turnover due to self absorption and a high frequency break due to Compton losses and an x-ray-HE spectrum from inverse Compton scattering from the relativistic electrons

### Synchrotron Spectrum

Depends on the energy spectrum of the electrons, e.g. for

n(E) = N E–S /4 = W(E/mc2)–S /4

where E/mc2 is usually abbreviated as γ

the power, P, emitted per unit volume is

dP/dV = 1.7x1021 N a(S) B(4.3x106 B/)(S-1)/2

(volume emissivity) ergs/s/cm3/Hz

B = magnetic field in Gauss, a(s) ~0.1 for 1.5<S<5

power law spectrum slope is related to energy spectrum slope ~ (S-1)/2

See Ginzburg & Syrovatskii 1964, Sov AJ 9, 683

1965, AR 3, 297, 1969 AR 7, 375

Blumenthal & Gould 1970 Rev Mod Phys 42, 237

Synchrotron Peak

@ m  B1/5 F2/5 -4/5

Synchrotron Peak

SSC Model

fit to Mk501

spectrum

(Konopelko 2003)

Self-Compton

High and

Low γ-ray

states

M. Boettcher

### Accretion Disks

To first order, assume it radiates as a black body

F() =

where T(r) is the disk temperature at radius r

2h2 1

c2 eh/kT(r) -1

Malkan 1983

### References

B. Peterson, An Introduction to Active Galactic Nuclei (Cambridge 1997)

J. Krolik, Active Galactic Nuclei (Princeton 1999)