Suzy Collin-ZahnLUTH, Observatoire de Paris Meudon AGN, MASSIVE BLACK HOLES, ACCRETIONARE AGN FACTORIES OF HIGH ENERGY PARTICLES AND PHOTONS?OR

THE CONTEXTDICHOTOMY RADIO LOUD / RADIO QUIET OBJECTS AND JETS / WINDSSTRONG AND WEAK ACCRETORSCONCLUSION

THE CONTEXTDICHOTOMY RADIO LOUD / RADIO QUIET OBJECTS AND JETS / WINDSSTRONG AND WEAK ACCRETORSCONCLUSION

Active Galactic Nuclei: from quasars (L=1046-48 erg/s) to Seyfert galaxies (L=1043-46 erg/s), and Low Luminosity AGN (L=1040-43 erg/s)RECALL OF SOME WELL-KNOWN FACTS2. Power derived from accretion onto a supermassive black hole3. BH present in ALL NUCLEI of galaxy, M(BH) from L=1010 to 105 M , M(BH) ~ M(Bulge)/10004. Unified Scheme

Black holeAbsorbing torusNarrow line regionBroad line regionAccretion disk(RL or RQ)

(FRI) (FRII)Windradio galaxiesLINERs

MILLIONS OF LIGHT-YEARS Faranoff-Riley, 1974

SOME FIDUCIAL VALUESEddington luminositygravitational radius: =1.5 1013 M8 cm ~10-5 pcbolometric luminositywhere is the accretion ratermaximum radiation efficiency of mass-energy conversion0.057 for a Schwarzschild BH, R(ISCO)=6Rg0.3 for a maximally rotating Kerr BH, R(ISCO)~1Rg= 1.3 1046 M8 erg/s

HOW TO FUEL BLACK HOLES?The angular momentum (GMR)1/2 must be transported outward!Major and minor mergers (quasars)Tidal interactions between galaxies (luminous Seyfert)Bars, bars within bars, nonaxisymmetric potentials (weak Seyfert)Dynamical friction of molecular clouds (LLAGN)1. At large distances ( 100pc)2. At small distances (

THE CONTEXTDICHOTOMY RADIO LOUD / RADIO QUIET OBJECTS AND JETS / WINDSSTRONG AND WEAK ACCRETORSCONSLUSION

In local UniverseLuminous AGN : ~ 1% of all galaxiesLow Luminosity AGN : ~ 40% of all galaxiesThe remainder 60%: dormant BH

ACCRETION DISKS:INFLUENCE OF THE ACCRETION RATE

Spectral distribution of Seyfert and RQQ,no radio or gamma radiation, everything is thermal!synchrotrondustcold accretion diskthermal Compton

hot coronathermal ComptoninverseComptonthermal emissionaccretionA. STRONG ACCRETORSObservations by Sanders et al. 1989

Thin disks, H/R

CONTROVERSY ABOUT THICK DISKS

Do these boulimic accretors exist? MHD simulations seems to show that if m >> 10 at large distance, strong outflows are expelled at smaller distance, and the accretion rate on the BH remains limited at the Eddington value..

NO HARD X-RAYS ARE EXPECTED FROM THESE DISKSproof of the presence of a hot medium emitting the hard X-rays whose emission is reflected by the diskIntensityEnergy in keVMCG _6_30_15Iron K lineRelativistic profile of FeK the disk extends down to ~10Rg, and sometimes to ~1Rg ISCO of a rapidly spinning BHBUTFabian et al. 2006

The reflection model: radiatively coupled disk + coronaDone, Gierlinski , 2004Same radiation coupling, but more realistic model : disk + magnetic flaresCorona Compton-cooled by UV photons

Disk heated by gravitational release AND X-rays

Optically thin, geometrically thick, hot (relativistic) disks, emitting mainly radio and X-rays,Gas falls into the BH before radiating, thus LLAGN, radio galaxies FRI (M87..), Galactic CenterB. WEAK ACCRETORS

Inflated codona, orsuppression of the inner regions of accretion diskThe Big Blue Bump does not exist

CONTROVERSY ABOUT THESE DISKSWhich model for these anorexic accretors? ADAF, ADIOS, CDAF RIAFIs there also a jet?

Yuan, Quataert, Narayan, 2003Synchrotron and Inverse Compton by thermal electronsSynchrotron and Inverse Compton by non-thermal electrons(jet or ADAF?)bremsstrahlungADAF+JET FOR A QUIESCENT BH: THE GALACTIC CENTERmeasured M~3 10-6 Mo /yr L (for ~0.1) should be ~ 1041 erg/s quiescentflaring.BUT measured L~ 1036 erg/s L/LEdd ~ 3 10-9, ~ 10-6

a Sgr A* Jet?F. Baganoff et al. 2003

ADAF+JET MODEL FOR A FRI GALAXYL/LEdd ~ 3 10-4ADAFJetWu, Yuan, Cao, 2008

CONCLUSION:

BOTH STRONG AND WEAK ACCRETORS ARE RADIATIVELY INEFFICIENTDISKS MUST PRODUCE OUTFLOWS TO EVACUATE THEIR ENERGY

THE CONTEXTDICHOTOMY RADIO LOUD / RADIO QUIET OBJECTS AND JETS / WINDSSTRONG AND WEAK ACCRETORSCONCLUSION

AGN are divided in Radio Loud (RL) and Radio Quiet (RQ)Sikora, Stawarz, Lasota, 2007BLRGLINERSRQQRLQSEYFERTSFRI

Mc Lure, Dunlop 2004With a complete sample of quasars (SDSS)Number of RLQ are less than 10% of RQQR = Lradio(5GHz) / Lopt

Log(L/Ledd)LINERSRQQSEYFERTSRADIO LOUDNESS DEPENDS ON THE EDDINGTON FACTORBLRGRLQFRI

LINERS, SEYFERTSRQQRADIO LOUDNESS DEPENDS ON M(BH)BLRGRLQFRI

1. Locally RL are exclusively in elliptical galaxies, RQ in spiral galaxies DIFFERENCES BETWEEN RL AND RQ objects2. RLs are associated with non-thermal relativistic collimated jets,RQs seem associated with thermal non-collimated winds (detected by Broad Absorption Lines and X-ray absorbers)3. Several more subtile properties, not understood (i.e. intense FeII lines only in RQs)I. HIGH LUMINOSITY AGNWHY?

JETS VERSUS WINDSJets are launched at R 1000 Rg (VLBI)Winds are launched at R 10000RgOBSERVATIONS Jets have relativistic bulk velocities and are made of relativistic particlesWinds have velocities from few hundreds km/s to c/10 and consist of warm (105-6 K) thermal gas

Magnetic field is indispensable to explain extended jet acceleration:

1. Centrifugally driven flow

2. Extraction of the rotational energy of the BH: field connects the BH to the disk(Blandford-Znajek, 1977) JET DRIVING MECHANISMJets might be linked with the spin of the BH

BLACK HOLE SPIN1. Even RQ AGN have spinning BH (FeK line)2. Cosmological evolution of AGN requires large fraction of spinning BHs (mass-conversion efficiency must be > 0.06)Measured by dimensionless angular momentum a = J/Jmax = cJ/GM24. It is expected that a increases with accretion AND with merger of two BHs3. Power of the jet must increase with a 5. BHs increase with galaxy bulges, and a fraction of elliptical galaxies (large bulges) are due to the merger of spirals Elliptical galaxies favor high spin, therefore jets

But it does not explain all:Other mechanisms must be at workEnvironnement can play a role:spiral galaxies contain cold gas, ellipticals contain and are surrounded by hot gas2. Geometry of the inner disk can play a role: thick or thin3. Density profile of the circumnuclear regions can play a role: cusp or coreetc etc

DO THEY HAVE JETS? YES! Falcke et al; 2000A sample of Low Luminosity AGNCompact jet structure with flat spectra observed in 40% of LLAGN(bulge)large M(BH)small M(BH)II. LOW LUMINOSITY AGN but no detailed mechanism proposed so far

FINALLY IS THE SOLUTION THIS ONE?Radio Loud AGNRadio Quiet AGN

Hawley, Balbus, 2002OR ARE THE WIND AND THE JET COEXISTING?inner jets can be undetected in luminous AGNWINDJET

CONCLUSION3. BAD NEWS: Only a small proportion of luminous AGN have relativistic jets and non-thermal radiation1. jets or high energy mechanisms can escape detection, if they are quenched close to the BH4. GOOD NEWS: In low luminosity AGN (and basically all galaxies), jets and high energy processes take place close to the central BH2. Jets in radio loud high luminosity AGN are likely driven by spinning black holes, but other mechanisms must play a role AND FINALLY, VERY LITTLE IS YET UNDERSTOOD!

An exemple of a strong accretor (Ton S 180) modeled by a thick disk, M(BH)=6 106 Mo, m=60 Kawaguchi, Pirens, Hur, 2003

Caution: one defines sometimes

Wind driving mechanismradiation pressure driven from the diskbut shielding of the central source necessarycentrifugally driven from disks threated by an open magnetic field- thermally or hydrodynamically driven from the hot coronasketch of a disk wind, centrifugally and/or radiatively accelerated