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

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

Rees 1984, ARA&A, 22, 471 (SMBH paradigma) Pringle, 1981, ARA&A, 19, 137 (Accretion disk theory) Begelman, Blandford, Rees, 1984, Rev. Mod. Phys 56, 255 (theory of rad. S.) Mushotzky, Done, Pounds, 1993, ARA&A, 31, 717 (observations X-ray) Antonucci 1993, ARA&A, 31, 473 (Unification schemes) Urry, Padovani 1995, PASP, 107, 803 (Unification schemes) Shields 1999, PASP, astro-ph/9903401 (history of AGN) Hartwick & Shade 1990 ARA&A (AGN evolution) Brandt & Hasinger ARAA, Vol 43, astro-ph/0501058 (Deep surveys)

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)

bibliography … continue …

Setti & Woltjer 1989, A&A, 224, L21 (CXB, AGN synthesis models) Comastri et al. 1995, A&A , 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)

The Cosmic X-ray Background

Co-evolution of galaxies and SMBH

1.

2.

Two seminal results:

The discovery of SMBH in the most local bulges;

steep and tight correlation

between M BH 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

Black hole mass density

A ~ 5x10

39

erg s

-1

Mpc

-3 

.

BH

A (1-



) L

Bol

~ ——————



c

2

L

X 

=0.1 L

Bol

/L

X

=40

.

 BH  BH

~ 3x10

-5

M

Θ

Yr

-1

Mpc

-3

~ 4x10

5

M

Θ

Mpc

-3

A first glance to the monster

Activity manifest on scales … as large as galaxy correlation lenght (5-10 Mpc i.e. 3 as small as light travel time of 10-100 sec i.e 10 11 -10  12 10 25 cm cm) or even larger if we consider the effect of ionization of IGM...

Broad band spectral energy distribution from 10-100 MHz to GeV-TeV

… a first glance to the monster

...a first glance to the monster

Luminosity 10 41 - 10 48 erg/s  - >> Lgal Variability seconds - years  t d Size R  ct d 10 12 -10 18 Mass M < c 3 t d cm << Rgal R=nm = n GM/c 2 /G (m/R)  2  10 8 t d /1000 (m/R) M O Eddington Luminosity L edd = 4  GMm p c/  T = 1.38  L acc Critical accr. M c = 1.38  = 1.38  = L edd /c 2 10 10 46 46 = 4 M M  8 8 10 = 4 M erg/s (L acc /L edd ) erg/s L acc 8 -8 10 38 M/M O (M/M O ) M O /yr M O /yr if  =0.057

=  Mc 2 Radiation pressure = force of gravity Radiation pressure = momentum per unit surface

S c

 4

L



T



R

2

c



GmM R

2 L Edd  4 

cGMm



T S

 

T c



 t cooling  Energy rate a which Energy is released

P Sync

  2 

T U mag U mag



B

2 8 

P Comp

  2 

T U rad U rad



L cR

2

t Sync

  2 

m e c

2 

T U mag



B

 2   1 5  10 8

s Equipartition



U rad



U mag



B E t Comp

  2 

m e c

2 

T U rad



m e c

2

R

2

L



T

  4  10 4

M

8  1/ 2

Gauss m e m p

  1

R g c

 0.3

M

8   1

s

Synchrotron and Compton cooling times are small, <

…a first glance to the monster: spinning holes

a= specific angular momentum S/M = spin angular momentum per unit mass = ac = 5  10 23 (a/m) M 8 where a E S =5  10 61 M 8 erg for a spinning hole M-M irr  5  10 61 M 8 (a/m) 2 erg L em  10 45 M 8 2 (a/m) 2 B 4 2 erg/s

…a first glance to the monster

Supermassive black hole paradigma M bh =10 6  10 9 M O - variability ---> efficiency of conversion of rest mass into radiation - jets and superluminal expansion - central velocity dispersions - relativistic iron K  lines



… variability



L in



t



E M

 

L

 

t

  4 3 

R

3

nm p



Mc

2  4  3

R

2

m p

 

T E

 

c

2 4 

R

2

m p

 3 

T

 1  

t

  1   

R c



L



t

;

n

  

c

4 4 

m p

3 

T



R



T

 8.5

 10 42 

erg

/

s t d

 if

t d L X



L

/ 

t

  1000

s

and

L X

   8

L X

8.5

 10 42  10 43 1

td

 0.01

NO termonuclear reactions!

Strong support for SMBH paradigma



l x



L x



T



Rm e c

3 

l x



2 3



L L Edd

3

R S R m p m e

4000 if

L



L EDD



1 in most cases

...compactness

L Edd

 4 

GMm p c



T

;

R S

 2

GM c

2    

n



T R n



L R

2

m e c

3

L



T m e c

3

R

  1 

l

1

MeV

 1

l x



m e c

2

h



x

  -rays to escape the

Galactic center

The BH at the Galactic centre

NIR NIR X-rays QuickTime™ e un decompressore Codec YUV420 sono necess ari per visualizzare quest'immagine.

QuickTime™ e un decompressore Codec YUV420 sono necessari per visualizzare quest'immagine.

Black Holes: detecting the horizon

QuickTime™ e un decompressore Codec YUV420 sono necessari per visualizzare quest'immagine.

mmVLBI

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.

Relativistic iron lines MCG-6-30-15

Tanaka et al. 1995, Fabian et al. 2002

Black holes in nearby bulges

Ferrarese&Merrit, Gebhardt et al.

The accretion disk of NGC4258

This is seen nearly edge on, so that OH 4  10 -3 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 arcsec, or 0.13pc from the centrum. The mass within this radius is 3.6

 10 7 M O .

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)

•Breakthrough from Radio astronomy!! A new technique: interferometry!

•Bolton 1948-1949 Ryle&Smith 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). H 0 =540 (!!!) km/s put the source at 31Mpc ===> huge luminosity!!  10 43 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

•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.

others) z=0.46

… a brief history of AGN

•Radio emission interpreted as synchroton emission (Ginzburg among huge energies up to 10 60 ergs •1960 Minkowski identifies 3C295 with the central galaxy of a cluster at • 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 => z=0.16! 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!

… a brief history of AGN

… a brief history of AGN

•1965 Sandage discovers of a large population of radio-quiet QSOs UV excesses: z=1.24 ---> 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

•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

Fourth UHURU Catalog: 339 X-ray sources detected: binaries, SNR, Seyfert galaxies and cluster of galaxies

Ariel V

Launch October 15 1974 from S. Marco in Kenya. USA UK collaboration. End of Operation March 14 1980 0.3-40 keV

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 cm 290 cm

2 2

) pinhole camera (3-6 keV). Sky Survey Instrument (SSI) composite of two proportional counters with 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. A0620-00=Nova Mon 1975).

Establishing that Seyfert I galaxies (AGN) are a class of X-ray emitters. Discovery of iron line emission in extragalactic sources.

COS-B

Lifetime

: August 1975 - April 1982

Energy Range

: 20 MeV - 1 GeV

Payload

:32-level wire spark-chamber aligned with satellite spin axis (20 MeV-1 GeV), eff. area 540 cm

2

Observations of gamma-ray pulsars, binary systems. Gamma-ray map of the Galaxy. Detailed observations of the GEMINGA gamma-ray pulsar.

Gursky Bradt McDonald Giacconi Lewin Boldt Koch Miramond NASA High Energy Astronomical Observatories (HEAO) Scientists

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 cm

2

each. MED 1.5-20 keV, eff. area 1 detector at 800 cm

2

.HED 2.5-60 keV, eff. area 3 detectors at 800 cm

2

each. MED and HEDs had various FOV settings, 1.5° x 3°, 3° x 3° and 3° x 6° PI: Elihu Boldt GSFC NASA

A3 - Modulation Collimator (MC) : 0.9-13.3 keV, eff. area 2 collimators 400 cm2 (MC1) & 300 cm

2

(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 cm

2

each, FOV 1.7° x 20° Medium Energy Detectors 80 keV - 2 MeV, eff. area 4 detectors 45 cm

2

each, FOV 17° High Energy Detector 120 keV - 10 MeV, eff. area 1 detector 100 cm

2

, FOV 37°

HEAO-2, later renamed Einstein, first X-ray telescope to produce images

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

•1978 IUE lauched, a window to the AGN UV continuum and lines

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

… 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.

Hakucho (Swan)

Energy Range and Apl X-1 Vela X-1) Oscillation : 0.1 - 100 keV Discovery of soft X-ray transient Cen X-4 Discovery of many burst sources Long-term monitoring of X-ray pulsar (e.g. Discovery of 2 Hz variability in the Rapid Burster later named Quasi Period

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

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

SIGMA aboard GRANAT: The precursor

First space coded mask telescope in operation from 1990 to 1997 Energy range: Source location accuracy: 35 keV - 1.3 MeV 30” - 5’

It works!

observation transmission deconvolution

The Ginga Satellite

Large Area Proportional Counter (LAC) 1.5-37 keV Eff. area = 4000 cm

2

, 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.

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 cm

2

at 1 keV energy resolution of deltaE/E=0.43 (E/0.93)-0.5 High Resolution Imager (HRI) FOV 38 ' square ; eff area 80 cm

2

at 1 keV ~ 2 arcsec spatial resolution (FWHM)

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

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 ASCA First X-ray mission to combine imaging capability with broad pass band, good spectral resolution, and a large effective area Four X-ray telescopes each composed of 120 nested gold-coated aluminum foil sufaces (total eff area 1,300 cm diameter, FOV 24´ @ 1 keV) Proportional Counters (IGSPC) keV,Eff area (GIS+XRT) 50 cm

2 2

@ 1 keV, spatial resolution 3´ half power Gas Imaging Spectrometer (GIS; 0.8-12 keV) Two Imaging Gas Scintillation FOV 50´, spatial resolution ~0.5' at 5.9 keV,and energy resolution of 8 % at 5.9 @ 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 (SIS+XRT) 105 cm

2

Giuseppe “Beppo” Occhialini

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 cm

2

@ 0.28 keV, FOV 37´ diameter, angular resolution 9.7´ FWHM @ 0.28 keV. Medium Energy Concentrator Spectrometer (MECS) (three units) 1.3-10 keV, eff area total 150 cm keV, eff area 240 cm

2

@ 30 keV

2

@ 6 keV, FOV 56´ diameter, angular resolution for 50% total signal radius 75" @ 6 keV. High pressure Gas Scintillator Proportional Counter (HPGSPC) 4-120 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 cm

2

@ 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 cm

2

.

… 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 highly obscured!  lines and Compton refl. Component. Sy2 are •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.

… 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 z=6.5.

•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.