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ACTIVE GALACTIC NUCLEI
http//www.mporzio.astro.it/fiore/agn 1-
Introduction -A first glance to the
monster -A brief history of AGN 2-
Phenomenology -The many appearances of the
beast the blind man and the elephant
-Unification schemes metereology (complexity and
randomness)
or underlying order? 3- Demography -
number density and luminosity functions -
AGN evolution. QSO probes of high z Universe
- supermassive black hole volume density 4-
Metabolics feeding the monster -
energetics - accretion discs - winds
and outflows 5- Ecology the environment -
Active nucleus-host galaxy interplay - the
large scale environment 6- Observation and data
analysis techniques
2
A (rather incomplete)
bibliography More than 12,000 referred published
papers since 1947! Undreds of books! Today rate
2 papers/day Blanford, Netzer, Woltjer, 1991,
AGN, Springer-Verlag Weedman, 1986, Quasar
Astronomy, Cambridge University Press Osterbrock,
1989, Astrophysics of gaseous nebulae and AGN,
Peterson, 1997, AGN, Cambridge University
Press Ribichi Lightman Frank, King, Reine, 1985,
Accretion power in astrophysics, Camb. Univ
P. Supermassive Black Holes in the Distant
Universe", Ed. A. J. Barger, Kluwer Academic
Publishers (astro-ph 2004 search in
comments) Astro-ph/0407273 Moran Distant X-ray
galaxies 0405170 Armitage Theory of disk
accretion 0405144 Mushotzky How are AGN
found 0404504 Natarajan Modeling the accretion
history of SMBH 0403693 Comastri Compton thick
AGN 0403618 Risaliti Elvis Panchromatic view
of AGN 0403225 Haiman Quaetert Formation and
evolution of first SMBH
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Rees 1984, ARAA, 22, 471 (SMBH
paradigma) Pringle, 1981, ARAA, 19, 137
(Accretion disk theory) Begelman, Blandford,
Rees, 1984, Rev. Mod. Phys 56, 255 (theory of
rad. S.) Mushotzky, Done, Pounds, 1993, ARAA,
31, 717 (observations X-ray) Antonucci 1993,
ARAA, 31, 473 (Unification schemes) Urry,
Padovani 1995, PASP, 107, 803 (Unification
schemes) Shields 1999, PASP, astro-ph/9903401
(history of AGN) Hartwick Shade 1990 ARAA (AGN
evolution) Brandt Hasinger ARAA, Vol 43,
astro-ph/0501058 (Deep surveys)
4
bibliography
continue. Elvis, 2000, ApJ, 545, 60
(Unification schemes, AGN atmospheres) Murray
Chang 1995, ApJ, 454, L105 (AGN winds) King
2003, astro-ph/0308342 (AGN winds) Elvis et al.
1994 ApJ (SED) Laor et al. 1997, ApJ, 477, 93
(SED) Risaliti Elvis astro-ph/0403618 (SED)
Elvis et al. 1994, ApJ, 422, 60 (high z
QSOs) Fan et al 2001, AJ, 121, 54 (high z
QSOs) Fan et al. 2003, AJ, 125, 1649 (high z
QSOs) Vignali et al. 2003, AJ, 125, 2876 (high z
QSOs) Cristiani et al. 2003 astro-ph/0309049
(high z QSOs) Haardt Maraschi, 1991, ApJ, 380
L51 (emission mechanisms) Tanaka et al. 1995,
Nature, 375,659 (rel. iron K? line) Fabian et al.
2002, MNRAS, astro-ph/0206095 (rel. iron K?
line) Krongold et al. 2003, ApJ, 597, 832
(ionized absorbers)
5
bibliography continue
Setti Woltjer 1989, AA, 224, L21 (CXB, AGN
synthesis models) Comastri et al. 1995, AA , 296
,1(CXB, AGN synthesis models) Soltan 1982,
MNRAS, 200, 115 (CXB SMBH mass
density) Fabian 1999, MNRAS, 308, L39 (SMBH
obscured growth) Fabian 2003, astro-ph/0304122
(Review CXB and SMBH) Hasinger 2003,
astro-ph/0302574, 0310804 (review X-ray AGN
evolution) Fiore 2003, astro-ph/0309355, 0306556
(X-ray AGN evolution) Comastri, astro-ph/0403693
(Compton thick AGN) Fiore 2006,astro-ph/0603823
(AGN evolution) Gebhardt et al. 2002, ApJ, 543,
L5 (local SMBH mass density) Marconi et al. 2004,
MNRAS, 351, 169 (SMBH mass density)
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The Cosmic X-ray Background
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Co-evolution of galaxies and SMBH

• Two seminal results
• The discovery of SMBH in the most local bulges
  steep and tight correlation between MBH and bulge
  properties.
• The BH mass density obtained integrating the AGN
  L.-F. and the CXB that obtained from local
  bulges

? most BH mass accreted during luminous AGN
phases! Most bulges passed a phase of
activity Need to understand AGN physics and
evolution to fully understand galaxy evolution
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Black hole mass density

• A 5x1039 erg s-1Mpc-3
• A (1-?) LBol
• ?BH
• ? c2 LX
• ?0.1 LBol/LX40
• ?BH 3x10-5 MT Yr-1 Mpc-3
• ?BH 4x105 MT Mpc-3

.
.
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A first glance to the
monster Activity manifest on scales as
large as galaxy correlation lenght (5-10 Mpc i.e.
3?1025cm) or even larger if we consider the
effect of ionization of IGM... as small as
light travel time of 10-100 sec i.e 1011-1012
cm Broad band spectral energy distribution from
10-100 MHz to GeV-TeV
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a first glance to the monster
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...a first glance to the
monster Luminosity 1041 - 1048
erg/s ? - gtgt Lgal Variability
seconds - years ? td Size
R ? ctd 1012-1018 cm ltlt Rgal Rnm n
GM/c2 Mass M lt c3 td /G
(m/R) ? 2?108 td/1000 (m/R) MO Eddington
Luminosity Ledd 4?GMmpc/?T 1.38 ? 1038 M/MO
1.38 ?
1046 M8 erg/s
Lacc 1.38 ? 1046 M8 (Lacc/Ledd) erg/s Lacc
?Mc2 Critical accr. Mc Ledd/c2
4 ? 10-8 (M/MO) MO/yr
4 M8 MO/yr if
?0.057
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Synchrotron and Compton cooling times are small,
ltltRg/c, therefore the radiating particles must be
continuously injected or reaccelerated in the
source volume
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a first glance to the monster spinning
holes a specific angular momentum S/M spin
angular momentum per unit mass ac 5?1023
(a/m) M8 cm2/s where altm for a black
hole S/M ltlt specific angular momentum of ISM in
the surrounding galaxy Total energy stored in a
spinning BH M-Mirr lt 0.29M ---gt ES5?1061 M8
erg for a spinning hole M-Mirr ? 5?1061 M8
(a/m)2 erg Lem ? 1045 M82 (a/m)2 B42 erg/s
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a first glance to the
monster Supermassive black hole paradigma
Mbh106?109 MO - variability ---gt efficiency
of conversion of rest mass into radiation
- jets and superluminal expansion - central
velocity dispersions - relativistic iron K?
lines
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variability
NO termonuclear reactions! Strong support for
SMBH paradigma
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...compactness
If lx is big it will not possible for ?-rays to
escape the source without creating pairs
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Galactic center
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The BH at the Galactic centre
NIR NIR
X-rays
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Black Holes detecting the horizon
mmVLBI
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BH and strong field GR effects spectroscopy and
polarimetry

• Line profiles emitted by matter around a
  rotating BH are relativistically distorted if the
  line emission is produced by a hot spot' on the
  accretion disc then the BH mass (and spin!) can
  be estimated, assuming Keplerian disc rotation.
• X-ray polarimetry can also be used to probe
  strong-field GR effects. In AGN a rotation with
  time of the polarization angle of the Compton
  Reflection component is expected.
• In presence of a hard surface (such as that of a
  neutron star), the internal energy stored in the
  flow is inevitably released and radiated away at
  the star surface. On the contrary, if the
  accretion flow crosses an event horizon the
  internal energy is carried into the black hole
  and hardly radiated away. The expected spectra
  are different.

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Relativistic iron lines MCG-6-30-15 Tanaka et al.
1995, Fabian et al. 2002
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Black holes in nearby bulges FerrareseMerrit,
Gebhardt et al.
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The accretion disk of
NGC4258 This is seen nearly edge on, so that OH-
maser emission at 1.3cm points toward us. VLBA
observations with resoslution of 0.6-0.3?10-3
arcsec allows to measure accurately radial
velocity as a function of the distance from the
centrum. The rotation curve is perfectly
Keplerian down to 4?10-3 arcsec, or 0.13pc from
the centrum. The mass within this radius is
3.6?107 MO.
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• A brief history of AGN
• Emission line in galaxies 1900-1940
• Emission lines in spirals (1068, 1275, 3516,
  4051,4151, 7469) Seyfert 1943
• broader (1000-10000 km/s) than that of normal
  spirals (a few 100km/s)

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• Breakthrough from Radio astronomy!! A new
  technique interferometry!
• Bolton 1948-1949 RyleSmith 1948
• CenA, VirA identified with NCG5128, M87, two
  large ellipticals
• Baade Minkowsky 1954 identified CygA with a
  tiny, distorted, emission
• line galaxy (redshift of 16,830 km/s). H0540
  (!!!) km/s put the source
• at 31Mpc gt huge luminosity!! ? 1043 erg/s.
• Ryle Faint radio sources are distributed
  uniformly on the sky
• either very close or very far away! Nearby
  radio-stars seems the obvious choice
• Ryle builds new interferometers. He manages
  technology, observation and theory. Nearly
  impossible today

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• Ryle Faint radio sources are distributed
  uniformly on the sky
• either very close or very far away! Nearby
  radio-stars seems the obvious choice
• Ryle builds new interferometers. He manages
  technology, observation and theory. Nearly
  impossible today
• Ryle 1958 distance of radio sources is unknown,
  but assume that the weaker sources are on average
  farther away.
• number of faint sources much higher than expected
  based on euclidean
• Universe EVOLUTION!! It seemed as we were in
  the middle of a big sphere, with a much higher
  concentration of radio sources near the surface
  of the sphere than in the centre.
• Ryle conjectured that galaxies were more prone to
  undergo radio outbursts when they were young,
  billions years ago.
• Strongly against stady-state Universe!!! Where
  sources must belong to similar population all
  time.
• Despite this new argument the controversy took
  many years to die down.
• During the 60 some of Ryle radio sources were
  identified with distant quasars. Quasars proved
  to be more common at high-z, evolution was
  confirmed.

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• a brief history of AGN
• Radio emission interpreted as synchroton emission
  (Ginzburg among others)
• huge energies up to 1060 ergs
• 1960 Minkowski identifies 3C295 with the central
  galaxy of a cluster at
• z0.46
• Sandage takes images and spectra of 3C48
• it looks like a quasi stellar object, no galaxy
  around!
• Faint broad lines at unfamiliar wavelength
• WHAT IS IT? A peculiar nearby star?
• 1963 M. Schmidt understands the spectrum of
  3C273, identifies the
• Balmer series and the MgII line gt z0.16! And
  no galaxy around..
• The optical luminosity is 10-100 times that of
  a giant elliptical..
• And still the flux is variable! Small sizes,
  huge luminosities..
• 1964 Salpeter and Zeldovich (independently)
  suggests the idea of QSO
• energy production as accretion onto a SMBH,
  which grows in mass
• 1969 Lynden-Bell SMBH should be common in
  galaxies thermal radiation
• from accretion disk, which lead to
  photoionization and broad line em.
• different BH masses can explain Seyferts, QSOs,
  even cosmic rays!

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a brief history of AGN
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• a brief history of AGN
• 1965 Sandage discovers of a large population of
  radio-quiet QSOs
• UV excesses z1.24 ---gt cosmological tools!
• 1965 Gunn Peterson effect
• 1967 Lynds PHL5200 Broad Absoption Line QSO
  outflows at 0.1c
• 1965 Radio superluminal motion using VLBI
  (recording signals on tapes and
• then correlating them by analog means!)
• 1962 Giacconi Rossi discover the Cosmic X-ray
  Background

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• 1967-1970 X-rays from M87 3C273 and CenA
• 1970-1973 Uhuru! First X-ray satellite. X-rays
  from NGC4151 NGC1275
• 1975 Ariel V X-rays are common from Seyferts
  (Elvis, Pounds, Maccacaro, Perola)
• 1977-1979 HEAO1 first all sky survey, about 100
  AGN, ?E 0.7 with little dispersion, Mushotzky
  et al.
• 1979 - 1980 Einstein first X-ray imaging
  satellite thousands of AGNs.
• 20-30 of 0.5-3.5 keV CXB resolved in sources,
  EMSS survey Maccacaro Gioia

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Fourth UHURU Catalog 339 X-ray sources
detected binaries, SNR, Seyfert galaxies and
cluster of galaxies
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Ariel V Launch October 15 1974 from S.
Marco in Kenya. USA UK collaboration. End of
Operation March 14 1980 0.3-40 keV
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Payload Experiments aligned with the spin axis.
Rotation Modulation Collimator (RMC) (0.3-30
keV). High resolution proportional counter
spectrometer. Polarimeter/spectrometer.
Scintillation telescope. All-Sky Monitor (ASM)
a small (1 cm2) pinhole camera (3-6 keV). Sky
Survey Instrument (SSI) composite of two
proportional counters with 290 cm2 effective area
each (1.5-20 keV).
Long-term monitoring of numerous X-ray
sources. Discovery of several long period
(minutes) X-ray pulsars. Discovery of several
bright X-ray transients probably containing a
Black Hole (e.g. A0620-00Nova Mon
1975). Establishing that Seyfert I galaxies (AGN)
are a class of X-ray emitters. Discovery of iron
line emission in extragalactic sources.
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COS-B
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Lifetime August 1975 - April 1982 Energy
Range 20 MeV - 1 GeV Payload32-level wire
spark-chamber aligned with satellite spin axis
(20 MeV-1 GeV), eff. area 540 cm2 Observations
of gamma-ray pulsars, binary systems. Gamma-ray
map of the Galaxy. Detailed observations of the
GEMINGA gamma-ray pulsar.
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Esperiment A-2 Cosmic X-Ray Detector 6 collimated
proportional counters with thin windows, energy
range 0.2 - 60 keV. LED 0.15-3.0 keV, eff. area 2
detectors of 400 cm2 each. MED 1.5-20 keV, eff.
area 1 detector at 800 cm2.HED 2.5-60 keV, eff.
area 3 detectors at 800 cm2 each. MED and HEDs
had various FOV settings, 1.5 x 3, 3 x 3 and
3 x 6 PI Elihu Boldt GSFC NASA
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A3 - Modulation Collimator (MC) 0.9-13.3 keV,
eff. area 2 collimators 400 cm2 (MC1) 300 cm2
(MC2), FOV 4 X 4 A4 - Hard X-Ray / Low Energy
Gamma Ray Experiment seven inorganic phoswich
scintillator detectors Low Energy Detectors
15-200 keV, eff. area 2 detectors 100 cm2 each,
FOV 1.7 x 20 Medium Energy Detectors 80 keV -
2 MeV, eff. area 4 detectors 45 cm2 each, FOV
17 High Energy Detector 120 keV - 10 MeV, eff.
area 1 detector 100 cm2, FOV 37
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HEAO-2, later renamed Einstein, first X-ray
telescope to produce images
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First high resolution spectroscopy and
morphological studies of supernova remnants.
Recognized that coronal emissions in normal
stars are stronger than expected. Resolved
numerous X-ray sources in the Andromeda Galaxy
and the Magellanic Clouds. First study of the
X-ray emitting gas in galaxies and clusters of
galaxies revealing cooling inflow and cluster
evolution. Detected X-ray jets from Cen A and
M87 aligned with radio jets. First medium and
Deep X-ray surveys Discovery of thousands of
"serendipitous" sources
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• 1978 IUE lauched, a window to the AGN UV
  continuum and lines

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• 1983 IRAS launched, first 10-100 ?m AGN
  observations
• non thermal continuum or dust reprocessed
  radiation?

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• a brief history of AGN
• Mid 80 - mid 90 detailed AGN SEDs from Radio
  to X-rays
• Edelson Malkan, Sanders, Elvis et al. ,
  Laor et al.
• 1978 Blandford Rees proposed that BlLacs are
  radio galaxies viewed
• down the axis of the relativistic jet first
  unification scheme!
• 1977 Rowan-Robinson proposes that Sy2 BLR is
  obscured by dust
• 1985 Antonucci Miller observe the BLR of the
  archetipal Sy2 NGC1068
• in polarized light! Unification schemes for
  radio-quiet AGN
• Mid 80 - mid 90 reverberation mapping, Peterson
  et al.
• The BLR is stratified, lower ion. lines are
  emitted farther away from
• the nucleus. BLR radius increases with the L.
  Line em. gas is orbitating.

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Hakucho (Swan) Energy Range 0.1 - 100
keV Discovery of soft X-ray transient Cen X-4
and Apl X-1 Discovery of many burst sources
Long-term monitoring of X-ray pulsar (e.g. Vela
X-1) Discovery of 2 Hz variability in the Rapid
Burster later named Quasi Period Oscillation
TENMA (Pegasus) 0.1 keV - 60 keV Discovery of
the Iron helium-like emission from the galactic
ridge Iron line discovery and/or study in many
LMXRB, HMXRB and AGN Discovery of an absorption
line at 4 keV in the X1636-536 Burst spectra
Discovery of first QPO
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EXOSAT ESA launch 26 may 1983 End 9 april
1986 Very eccentric orbit duration 90 h Energy
range 0.05-2 keV 1-50keV Discovery of the
Quasi Period Oscillations in LMXRB and X-ray
Pulsars Comprehensive study of AGN variability
Observing LMXRB and CV over many orbital
periods Measuring iron line in galactic and
extra galactic sources Obtaining low-energy
high-resolution spectra
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SIGMA aboard GRANAT The precursor
First space coded mask telescope in operation
from 1990 to 1997
Energy range 35 keV - 1.3 MeV Source location
accuracy 30 - 5
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The Ginga Satellite
Large Area Proportional Counter (LAC) 1.5-37
keVEff. area 4000 cm2, FOV 0.8 x
1.7 Discovery of transient Black Hole Candidates
and study of their spectral evolution. Discovery
of weak transients in the galactic ridge.
Detection of cyclotron features in 3 X-ray
pulsars Evidence for emission and absorption Fe
feature in Seyfert probing reprocessing by cold
matter. Thick obscuration in Sy2
galaxies Discovery of intense 6-7 keV iron line
emission from the galactic center region.
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ROSAT The Roentgen Satellite An X-ray
telescope used in conjunction with one of the
following instruments (0.1-2.5 keV) Position
Sensitive Proportional Counter (PSPC) 2 units
detector B, used for the pointed phase,
detector C ,used for the survey FOV 2 diameter
eff area 240 cm2 at 1 keV energy resolution of
deltaE/E0.43 (E/0.93)-0.5 High Resolution
Imager (HRI) FOV 38 ' square eff area 80 cm2 at
1 keV 2 arcsec spatial resolution (FWHM)
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X-ray all-sky survey catalog, more than 150000
objects XUV all-sky survey catalog (479
objects) Source catalogs from the pointed phase
(PSPC and HRI) containing 100000 serendipitous
sources Detailed morphology of supernova
remnants and clusters of galaxies. Detection of
shadowing of diffuse X-ray emission by molecular
clouds. Detection (Finally!) of pulsations from
Geminga. Detection of isolated neutron stars.
Discovery of X-ray emission from comets.
Observation of X-ray emission from the
collision of Comet Shoemaker-Levy with Jupiter
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ASCA First X-ray mission to combine imaging
capability with broad pass band, good spectral
resolution, and a large effective areaFour X-ray
telescopes each composed of 120 nested
gold-coated aluminum foil sufaces (total eff area
1,300 cm2 _at_ 1 keV, spatial resolution 3 half
power diameter, FOV 24 _at_ 1 keV) Gas Imaging
Spectrometer (GIS 0.8-12 keV) Two Imaging Gas
Scintillation Proportional Counters (IGSPC)FOV
50, spatial resolution 0.5' at 5.9 keV,and
energy resolution of 8 at 5.9 keV,Eff area
(GISXRT) 50 cm2 _at_ 1 keV Solid-state Imaging
Spectrometer (SIS 0.4-12 keV) Two CCD arrays of
four 420 X 422 pix chips, FOV 22 X 22,Spatial
resolution 30", energy resolution of 2 at 5.9
keV , Eff area (SISXRT) 105 cm2
Broad Fe lines from AGN, probing the strong
gravity near the central engine Lower than solar
Fe abundance in the coronae of active
stars Non-thermal X-rays from SN 1006, a site of
Cosmic Ray acceleration Abundances of heavy
elements in clusters of galaxies, consistent with
type II supernova origin
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Payload The Narrow field Instruments (NFI)
Four Xray telescopes working in conjnction with
one of the following detectors Low Energy
Concentrator Spectrometer (LECS) (one unit)
0.1-10 keV, eff area 22 cm2 _at_ 0.28 keV, FOV 37
diameter, angular resolution 9.7 FWHM _at_ 0.28
keV. Medium Energy Concentrator Spectrometer
(MECS) (three units) 1.3-10 keV, eff area total
150 cm2 _at_ 6 keV, FOV 56 diameter, angular
resolution for 50 total signal radius 75" _at_ 6
keV. High pressure Gas Scintillator Proportional
Counter (HPGSPC) 4-120 keV, eff area 240 cm2 _at_ 30
keV Phoswich Detection System (PDS) 15-300 keV.
The lateral shields of the PDS are used as
gamma-ray burst monitor in the range of 60-600
keV. Eff area 600 cm2 _at_ 80 keV Wide Field
Camera (2 units) 2-30 keV with a field of view 20
deg X 20 deg. The WFC are perpendicular to the
axis of the NFI and point in opposite directions
to each other. Eff area 140 cm2.
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• a brief history of AGN
• 1983 EXOSAT launched. AGN long looks, detailed
  variability studies.
• Iron K? line in several Sy1 and Sy2, NGC1068
  only the line is seen!
• 1987 Ginga launched. Iron K? lines and Compton
  refl. Component. Sy2 are
• highly obscured!
• 1989 Setti Woltjer suggest that the CXB shape
  is due to the superposition of obscured and
  unobscured AGNs.
• 1990 ROSAT launched. All sky survey 0.5-2 keV.
  Thousands of AGN
• observed. Deep surveys, Lockman Hole,
  Hasinger, Schmidt et al.
• 70-80 of the 0.5-keV CXB resolved in sources.
  Most are type1 AGN
• Spectral paradox. First systematic X-ray
  observations of high z quasars
• 1993 ASCA launched, first imaging observations
  above 2 keV. Tanaka et al.
• Relativistic iron K? line in MCG-6-30-15
• 1996 BeppoSAX launched. Compton thick Sy2, first
  sensitive survey in the
• 5-10 keV band 20-30 of the CXB resolved in
  sources, most are
• obscured AGN. Cutoffs and compton reflection
  in Sy1.

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• a brief history of AGN
• End 90 2DF survey, Boyle et al. optical AGN
  follows pure luminosity
• evolution
• End 90-present SDSS survey, discovery of QSO up
  to z6.5.
• End 90 Blazars detected up to a few TeV!
• 1999 Chandra and XMM launched. First sensitive
  high resolution imaging
• and spectroscopic observations in the 0.3-10
  keV band. Most CXB
• resolved in sources. Differential evolution of
  luminosity function for
• Sy and QSO. AGN density 10 times higher than
  in optical surveys.
• Outflows and highly ionized winds in low and
  high z AGN.