Black Holes and Revelations
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Transcript of Black Holes and Revelations
Αποκάλυψις = apokálypsis = revelations
Inspired by Apocalypse (Book of revelations)?
Not really …
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 z=0 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…Others? Please specify…
Ten important questions about AGN1) 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 z=0 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
6) Testing general relativity with AGN 3.12
7) 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
Let’s start from the “bottom”: the other issues
Geometry of the torus: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
X-ray polarimetry
Key parameters of future polarimetric missions
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NHXM GEMS
# of Te lescopes 1 3
Energy band (keV)
2 ÷ 35 (2-10 + 6-35)
2 ÷ 10 (+0.5 keV)
Field of View diameter (arcmin) 12 14
Half Power Diameter (arcsec at 30 keV)
20 Non imaging
MDP (1 mCrab, 100 ks 2-10 keV band)
10% 5%
Rotation Not needed Yes (0.1 rpm)
MDP (systematics) << 1% Unknown
Background 0.13 Crab (2-10 keV) 0.4 Crab (6-35 keV) 0.2 mCrab
NHXM
Polarimeter also onboard IXO
Polarimetric sensitivity
Soft X-ray channel
6-35 keV channel
Two polarimetric channels (2 – 10 keV and 10 – 35 keV) for an effective diagnostic of the emission mechanisms
2-10 keV channel
FSRQs vs. BL Lacs
FSRQs: a “typical AGN” + jet
[email protected] 15 AGN 9: BLACK HOLES AND REVELATIONS May 24 2010
Ghisellini et al. 2009, MNRAS, 396, L105
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?
Colpi’s reviewPiconcelli’s talkMontuori & 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 AGN+STB?
Bianchi, Chiab, Piconcelli et al. 2009
X-rays able to reveal buried nuclei
Binary black holes
1. SMBH and AGN-galaxy co-evolution
2. What triggers, modulates, and halts accretion onto SMBHs?
Feedback …
The ‘fact’: many observational evidencies
Several talks …Observations vs. theory and modelsWhat is missing?
Colpi et al. 2007
SCUBA galaxies: MBH lags the stellar growth -
adjustment
QSOs: galaxy lags the MBH growth - dominance
Alexander et al. 2008
Volonteri’s review
Growth BH vs. host galaxyEddington-limited SF at high-z (≈1000 M/kpc2)LAGN≈Ledd (review by Maiolino)
• 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…
Mass function of seed BHsVolonteri+08; Devecchi & Volonteri 09
Gas-dynamical collapse
Pop III remnants Proto-cluster• Eddington ratio behaviour vs. z? (Shankar …)
Γ=MBH/Mstar increases with z by a factor≈7 from z=0 to z=3Large sample, no RLQ/RQQ dichotomy
Decarli’s talk
Semi-analytic model by Lamastra, Menci+able to explain high-z QSOs and SMGs
unobscured
obscured in SMGs
obscuredX-ray selected
z=2
Sarria’s talk
Large-scale outflow?Largely discussed by Maiolino and Polletta
Alexander et al. 2010 – see also Nesvabda et al. 2008
• Energy input required: 1059 erg over 30 Myrs wind radiatively driven by the AGNand/or supernovae winds from intense star formation. • Energy injection required to drivethe 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.
Review talk by PollettaHow many? How much representative?
z=2.07
Halting the accretion through mechanical removal of the gasradio mode?
Giodini’s review
(from Fender et al. 2004; Remillard and McClintock 2007)
LSLS – low/hard stateHS HS – high/soft stateVHS/IS VHS/IS – very high and intermediate states
Shocks during jet production
Data for GX 339-4
Disc-jet coupling in X-ray binaries
Disc-dominated phase
(Lorentz factor)
X-ray hardness
X-r
ay in
tens
ity
jet
corona
disc
track of a simple X-ray transient outburst with a single optically
thin jet production episode
3. AGN from z=0 to high-z
AGN physicsAGN evolution
AGN demography – elusive AGNAGN census at high-z
Fraction of obscured AGNProperties of AGN across cosmic time
Miniutti’s reviewIonized 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 – Nardini’s talk
Luminosity Dependent Density Evolution (LDDE)
(see previous results fromUeda et al. 2003)
Lower luminosity AGNpeak at lower redshifts:DOWNSIZING(see models of galaxy andAGN formations)
LF, Fiore, Comastri+05
Marconi+04
La Franca’s review: LDDE works for X-ray selected AGN, optically selected Type 1 (once faint ones are included)
Downsizing: luminous QSO mostly radiate at z~2, lower-luminosity Seyferts mostly radiate at z<1. At z=2, metals already formed and big BH in place.
Evolution of luminous AGN at high-z
• Radio
(Wall+05)
• Soft X-ray (Hasinger+05)
• Soft X-ray (Silverman+04)
• Optical (Fan+01,04)
LX>1045 erg/s
Luminous AGN are found to decline exponentially up to z~4-6. Nothing isknown above z~3 for less luminous AGN, i.e. the bulk of the population
Still many open issues, mergers dominant, missing details? see Brusa’s talkWhat may we expect?
What about the obscured QSOs at high-redshift?
Brusa+09COSMOS; still limited numbers
PSU group results (CV, Steffen, Just, Gibson)+Young+10 – but see earlier
Einstein results
Lusso+10 for X-ray selectedsee poster by Antonucci
Properties of AGN similar at low and high redshift, despite different conditions of the ‘environment’
The fraction of absorbed AGN as function of LX and z
*) Assuming no luminosity and redshift dependences
assumed *)
predicted
DECREASE WITH LUMINOSITYEarlier 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).
INCREASE WITH THE REDSHIFT
LF, Fiore, Comastri+05
- Type 2 fraction a strong function of luminosity a) At high (quasar) luminosity: type 2 <20%; 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
The fraction of absorbed AGN as function of LX and z
Strong support from many works
BUTIs the ‘receding-torus’ model the
right answer?
Support from IR observations
(CF; Maiolino+ 07)
4. AGN and environment reciprocal influence on small and large scales
Feedback through winds
Optical/UV
PG 0946+301 - Arav et al. 2001
Fast (v up to ~ 50000 km/s) winds in BAL QSOs
~15-20% of QSOs (Bruni’s talk)
+ mini-BALs/NALQSOs (Giustini’s talk)
Pounds et al. 2003a,b
Reeves et al. 2003
PDS456 (z=0.18) v~0.1c
2 Energy (keV) 5 7 10
High-velocity (v~0.1c), highly ionized outflowsCommon! (Cappi’s talk; Tombesi et al. 2010)Relevant energy budget (duty cycle…)
X-rays
the longest look at a mini-BAL QSO
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
mini-BAL QSOs
Giustini’s talk
NGC 1365 (Risaliti et al. 2005)
Large scale structure
NGC 5252: Tadhunter & Tsvetanov 1989
[OIII]
Large scale structure
Bianchi et al. 2010
Mrk 573: X-rays/[O III] Mrk 573: X-rays/Radio
AGN ionization confirmed by high-resolution (RGS) spectra (Risaliti’s review)See results for Compton-thick Sey2 Tol0109-383 (Marinucci) and BLRGs (Torresi)
5. Unified models: what to keep and what to change
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)
• Compact (a few pc) tori with a clumpy/filamentary dust distribution (warm disk + geom. thick torus)
• No significant Sey1/Sey2 difference
Tristram+09; (see also Jaffe+04, Meisenheimer+07; Tristram+07)
Tristram+07 - Circinus
Eclipses of the X-ray source are COMMON in nearby AGN:
ΔNH ~ 1023-1024 cm-2
v>103 km/sD ≈ 1013 cm
n ~ 1010-1011 cm-2
X-ray absorber “made” of BLR clouds
Risaliti et al. 200n, n=[6,9]
Inner TORUS: BLR X-ray absorption
NH > 1024 cm-2
hoursNH~1023 cm-2
days
NH~3*1023 cm-2
days NH~1023 cm-2
hours
NGC 1365
NGC 4151
UGC 4203
NGC 7582
Bianchi et al. 2009Risaliti et al. 2010
Risaliti et al. 2009
Puccetti et al. 2007
6. Testing General Relativity with AGN
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)
Iwasawa et al 96
Review by Miniutti
BH spin measurements rely on the id. ISCO ≅ Rin
Fabian et al 02Early results in MCG-6 indicate that Rin < 2 rg
which translates into a BH spin of a > 0.94 Other models (complex absorption; Miller, Turner…) too fine-tuned – problems with
observed variability
Swift J2127.4+5654 with Suzaku
The broadband analysis confirms results from Fe K diagnostics
a ~ 0 is excluded but just at the 3σ level a ~ 0.998 is excluded at more than 5σ
Miniutti et al. 2009
See you at AGN10