Black Holes and Revelations

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Black Holes and Revelations
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?p????????
apokálypsis
revelations
Inspired by Apocalypse (Book of revelations)?
Not really
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Ten important questions about AGN?
1) Testing general relativity with AGN 2)
Physical parameters, mechanisms and modulators
driving radio-loudness 3) AGN and environment
reciprocal influence on small and large scales 4)
Unified model what to keep and what to
change 5) Very high energy phenomena in AGN 6)
Missing and elusive AGN identification and
relevance 7) AGN from z0 to high-z 8) SMBH
formation, and galaxy-AGN co-evolution model
predictions vs observational constraints 9)
What triggers, modulates and halts accretion onto
SMBHs 10) AGN and host galaxy separation data,
methods, and measurements Others? Please specify
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Ten important questions about AGN

• SMBH formation, and galaxy-AGN co-evolution
  model predictions vs. observational constraints
  4.13
• 2) What triggers, modulates and halts accretion
  onto SMBHs 3.76
• 3) AGN from z0 to high-z 3.52
• 4) AGN and environment reciprocal influence on
  small and large scales 3.48
• 5) Unified model what to keep and what to
  change 3.25
• Testing general relativity with AGN 3.12
• Physical parameters, mechanisms and modulators
  driving radio-loudness 3.00
• Missing and elusive AGN identification and
  relevance 2.90
• Very high energy phenomena in AGN 2.75
• AGN and host galaxy separation data, methods,
  and measurements 2.66

• Other issues
• X-ray polarimetry ? geometry circumnuclear
  matter
• BL Lacs vs. FSRQs really different?
• Binary BH statistics and model formation a new
  observational constraint?

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Lets start from the bottom the other issues

• Other issues
• X-ray polarimetry ? geometry circumnuclear
  matter
• BL LACs vs. FSRQs really different?
• Binary BH statistics and model formation a NEW
  observational constraint?

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X-ray polarimetry
Geometry of the torus the polarization angle
will give us the orientation of the torus, to be
compared with IR results, and with the ionization
cones
Urry Padovani 1995
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Geometry of the torus the polarization angle
will give us the orientation of the torus, to be
compared with IR results, and with the ionization
cones
Urry Padovani 1995
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Key parameters of future polarimetric missions
NHXM
Polarimeter also onboard IXO
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Polarimetric sensitivity
Soft X-ray channel
Two polarimetric channels (2 10 keV and 10 35
keV) for an effective diagnostic of the emission
mechanisms
2-10 keV channel
6-35 keV channel
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FSRQs vs. BL Lacs
Tavecchios review
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FSRQs a typical AGN jet
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DAmmando
PKS 0537-441 seems to be an outlier (not the
only!) in the blazars divide...why?
PKS 0537-441 is a FSRQ with non-thermal continuum
so strongly enhanced that hides the broad
lines... ...or it is a transitional object
between FSRQs and BL Lac objects with an
intermediate accretion rate?
Ghisellini et al. 2009, MNRAS, 396, L105
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Binary black holes
Colpis review Piconcellis talk Montuori
Farina posters
A NEW observational constrain for models Where
can we search for binary black holes? SDSS ?
sampling the pairing phase? How many? Gas-rich
environment, galaxy type In ULIRGs/disturbed
systems buried AGNSTB?
X-rays able to reveal buried nuclei
Bianchi, Chiab, Piconcelli et al. 2009
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1. SMBH and AGN-galaxy co-evolution
2. What triggers, modulates, and halts accretion
onto SMBHs?
Feedback
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The fact many observational evidencies
Several talks Observations vs. theory and
models What is missing?
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Alexander et al. 2008
QSOs galaxy lags the MBH growth - dominance
Growth BH vs. host galaxy Eddington-limited SF at
high-z (1000 M?/kpc2) LAGNLedd (review by
Maiolino)
SCUBA galaxies MBH lags the stellar growth -
adjustment
Volonteris review
Colpi et al. 2007
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• Progenitors?
• Seed BH masses? Mseed,BH 100 M? vs. 103-5 M?
• Pop III stars? Any chance to observe them?
• High-z QSOs already settled BHs with masses
  comparable with those of local SMBHs ...
• Gas accretion vs. gas consumption by star
  formation (1/3 high-z QSOs) and SN explosions
• Missing population of lower masses BHs at high-z
  Test case for WFXT

Gas-dynamical collapse
Pop III remnants
Proto- cluster

• Eddington ratio behaviour vs. z? (Shankar )

Mass function of seed BHs Volonteri08 Devecchi
Volonteri 09
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Decarlis talk
GMBH/Mstar increases with z by a factor7 from
z0 to z3 Large sample, no RLQ/RQQ dichotomy
Semi-analytic model by Lamastra, Menci able to
explain high-z QSOs and SMGs
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z2
unobscured
obscured X-ray selected
obscured in SMGs
Sarrias talk
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Large-scale outflow? Largely discussed by
Maiolino and Polletta
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• Energy input required 1059 erg over 30 Myrs
• ? wind radiatively driven by the AGN
• and/or supernovae winds from intense star
  formation.
• Energy injection required to drive
• the outflow is comparable to the estimated
  binding energy of the galaxy spheroid, suggesting
  that it can have a significant impact on the
  evolution of the galaxy.

z2.07
Review talk by Polletta
Alexander et al. 2010 see also Nesvabda et al.
2008
How many? How much representative?
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Halting the accretion through mechanical removal
of the gas radio mode?
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Giodinis review
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Disc-jet coupling in X-ray binaries
LS low/hard state HS high/soft state VHS/IS
very high and intermediate states Shocks during
jet production Data for GX 339-4
jet
disc
(Lorentz factor)
corona
Disc-dominated phase
X-ray intensity
track of a simple X-ray transient outburst with
a single optically thin jet production episode
X-ray hardness
(from Fender et al. 2004 Remillard and
McClintock 2007)
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3. AGN from z0 to high-z
AGN physics AGN evolution AGN demography
elusive AGN AGN census at high-z Fraction of
obscured AGN Properties of AGN across cosmic time
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Miniuttis review Ionized reflection to explain
the soft excess and the broad-band spectrum Need
for IXO to appreciate the features and BH spin
measurements for large samples!
See Ark 120 Nardinis talk
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Luminosity Dependent Density Evolution (LDDE)
La Francas review LDDE works for X-ray selected
AGN, optically selected Type 1 (once faint ones
are included)
(see previous results from Ueda et al. 2003)
Lower luminosity AGN peak at lower
redshifts DOWNSIZING (see models of galaxy
and AGN formations)
LF, Fiore, Comastri05
Downsizing luminous QSO mostly radiate at z2,
lower-luminosity Seyferts mostly radiate at zlt1.
At z2, metals already formed and big BH in place.
Marconi04
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X-ray AGN LF
0.5-2 keV Hasinger, Miyaji, Schmidt 05
See also -Ueda03 (selection effects
included) -Barger05 -Silverman08 -Della
Ceca08 -Ebrero09 (selection effects
included) -Yencho09 -Aird10

• Downsizing of AGN activity
• Quasar density peaks at z2-3
• AGN density peaks at z0.5 - 1
• Most of BH accretion happens in quasars at high-z
• Most of X-ray background in Seyfert 2s at low-z

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LDDE found also for optically selected AGN1 once
the faint end of the LF is probed
Bongiorno, Zamorani08
See also e.g. Fontanot07, Shankar Mathur 07
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Evolution of luminous AGN at high-z
Brusa09 COSMOS still limited numbers
Luminous AGN are found to decline exponentially
up to z4-6. Nothing is known above z3 for less
luminous AGN, i.e. the bulk of the
population Still many open issues, mergers
dominant, missing details? see Brusas talk What
may we expect? What about the obscured QSOs at
high-redshift?
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PSU group results (CV, Steffen, Just,
Gibson)Young10 but see earlier Einstein
results Lusso10 for X-ray selected see poster
by Antonucci
Properties of AGN similar at low and high
redshift, despite different conditions of the
environment
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The fraction of absorbed AGN as function of LX
and z
assumed )
predicted
) Assuming no luminosity and redshift dependences
DECREASE WITH LUMINOSITY Earlier evidences of a
decrease of the fraction of absorbed AGN with
luminosity from Lawrence Elvis (1982) and
Lawrence (1991). Confirmed by Ueda et al. (2003).
LF, Fiore, Comastri05
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The fraction of absorbed AGN as function of LX
and z
Strong support from many works BUT Is the
receding-torus model the right answer? Support
from IR observations (CF Maiolino 07)

• - Type 2 fraction a strong function of
  luminosity
• a) At high (quasar) luminosity type 2 lt20
  optical color selection is highly complete since
  all are type 1s, and includes most of luminosity
  AGN population emitted in the Universe
• b) At low (Seyfert) luminosity type 2 80
  optical color selection miss most of the AGNs in
  the Universe in terms of number

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4. AGN and environment reciprocal influence on
small and large scales
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Feedback through winds
PG 0946301 - Arav et al. 2001
Fast (v up to 50000 km/s) winds in BAL
QSOs 15-20 of QSOs (Brunis talk)
mini-BALs/NALQSOs (Giustinis talk)
Optical/UV
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X-rays
Pounds et al. 2003a,b
High-velocity (v0.1c), highly ionized
outflows Common! (Cappis talk Tombesi et al.
2010) Relevant energy budget (duty cycle)
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Giustinis talk
the longest look at a mini-BAL QSO
mini-BAL QSOs
narrow absorption line with E 7.0 keV narrow
absorption line with E 7.3 keV
Fe XXV K? blueshifted by 0.05c Fe XXVI K?
blueshifted by 0.05c
X-ray wind velocity 3x UV wind velocity
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NGC 1365 (Risaliti et al. 2005)
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Large scale structure
OIII
NGC 5252 Tadhunter Tsvetanov 1989
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Large scale structure
Mrk 573 X-rays/O III
Mrk 573 X-rays/Radio
Bianchi et al. 2010
AGN ionization confirmed by high-resolution (RGS)
spectra (Risalitis review) See results for
Compton-thick Sey2 Tol0109-383 (Marinucci) and
BLRGs (Torresi)
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5. Unified models what to keep and what to
change
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Unified model Pro easy to understand,
although with many components Con needs some
adjustment based on recent observations Absorber
putative torus not supported by recent
high-resolution observations X-ray spectra ?
probably compact and clumpy Review talks by
Fritz (torus still a good approximation for
photometric points SED fitting) - Risaliti
absorption by dust lanes (Matt 2000) BLR
issues (number, shape, properties, true Sey2,
naked QSOs) Review by Risaliti (see also
Hawkins 04, Bianchi, Panessa Nicastro from the
theoretical side)
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• Compact (a few pc) tori with a
  clumpy/filamentary dust distribution (warm disk
  geom. thick torus)
• No significant Sey1/Sey2 difference

Tristram09 (see also Jaffe04,
Meisenheimer07 Tristram07)
Tristram07 - Circinus
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Eclipses of the X-ray source are COMMON in nearby
AGN ?NH 1023-1024 cm-2
vgt103 km/s D 1013 cm n 1010-1011 cm-2
X-ray absorber made of BLR clouds
Risaliti et al. 200n, n6,9
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Inner TORUS BLR X-ray absorption
NGC 1365
NGC 4151
DNH gt 1024 cm-2 DT10 hours
Puccetti et al. 2007
Risaliti et al. 2009
UGC 4203
NGC 7582
Risaliti et al. 2010
Bianchi et al. 2009
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6. Testing General Relativity with AGN
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The usual suspect MCG-6-30-15
First clear detection of relativistic Fe K line
(Tanaka et al 95) and first evidences for a
rapidly spinning Kerr BH (Iwasawa et al 96, 99)
Review by Miniutti
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BH spin measurements rely on the id. ISCO ? Rin
Early results in MCG-6 indicate that Rin lt 2
rg which translates into a BH spin of a gt 0.94
Fabian et al 02
Other models (complex absorption Miller,
Turner) too fine-tuned problems with observed
variability
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Swift J2127.45654 with Suzaku
The broadband analysis confirms results from Fe K
diagnostics a 0 is excluded but just
at the 3s level a 0.998 is excluded at
more than 5s
Miniutti et al. 2009
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See you at AGN10