AGNs: A Review Th. Boller Max-Planck-Institut fr extraterestrische - PowerPoint PPT Presentation

AGNs: A Review Th. Boller Max-Planck-Institut für extraterestrische Physik, Garching Accreting black holes Fe K α GR effects Fe K α GR dynamics BH spin measurements 1H0707-495: spectral template and time lags The relativistic RM model: strong and weak field limit results 1

Accreting BHs Open questions: ESA CV 2015-2025 YB writing - how does matter behave in the strong GR field regime? - does it always obey GR predictions? - what are the processes near the event horizon? (accretion/ejection) - how does the spin affect the emission/jet processes? - how are BH spins distributed? (BH birth/growth) 2

Fe K α GR effects previous Fe K α line measurements Nandra 2006, Fabian 2002 MCG-6-30-15 MCG-6-30-15 NGC 3516 NGC 4151 NGC 4051 NGC 2992 NGC 3783 Mrk 766 MGC 52316 the accretion disc line interpretation for broad relativistic Fe K α lines is robust in 8 AGNs robust against other models which can mimic a red wing (Reeves 2004) - absorption by high column density - high ionization warm absorbers - continuum uncertainties 3

Fe K α GR dynamics I. Fe K α time resolved and mean spectra dynamics mean spectrum Iwasawa 04 data NGC 3516 model emission from a single orbiting spot 4

Fe K α GR dynamics II. Fe K α on-phase, off-phase statistics Variations of the red feature 5

Fe K α GR dynamics III. Predictions ESA CV 2015-2025 YB strong gravity section 6

BH spin measurements Why do we care about the BH spin? - stellar mass BHs: - dynamics of BH formation in supernovae - supermassive BHs: - propagate vs. retrograde accretion - relative importance of mergers and accretion modes 7

BH spin: GR predictions relativistic line profile ISCO = f(spin) BH spin measurements rely on the ISCO ≅ R in 8

BH spin measurements Fabian 02 Early results in MCG-6 indicate that R in < 2 R g which translates into a BH spin of a > 0.94 9

Relativistic X-ray reflection and BH spin Ross, Fabian 05 Miniutti 09 Swift J2127.4+5654 with Suzaku The relativistic Fe K line should be associated with a full X-ray reflection spectrum which shows up at > 10 keV (Compton hump) 10

Relativistic X-ray reflection and BH spin Miniutti 09 Swift J2127.4+5654 The relativistic RM accounts for the whole broadband spectrum to delivers the BH spin 11

Relativistic X-ray reflection and BH spin Swift J2127.4+5654 (Miniutti 09 ) Broad band relativistic RM analysis a ~ 0 is excluded but just at the 3 σ level a ~ 0.998 is excluded at more than 5 σ intermediate spin due to a recent major merger? 12

The special case of 1H 0707-495 I. The extreme This is an AGN belonging to the class of NLS1 galaxies (Puchnarewicz 1992 , Boller 96 , Fabian 09 ) it is remarkable in the X-rays: large amplitude and fast X-ray variability(Gallo 04 ,Blustin 09 ) huge soft X-ray excess extreme spectral curvature at Fe energies (Boller 02 ) all these properties are observed in almost all (unobscured) AGN to a much lesser extent and therefore much more difficult to interpret presently 13

The special case of 1H 0707-495 II. spectral properties Fabian 09 orbit by orbit time-averaged Fe K Fe L - ratios of the data to a simple power law + BB model - two unambiguous features appear between 0.6-1 keV and 4-7 keV and they can be interpreted as broad Fe L and K lines coming from the same medium with huge reflection fraction and high Fe abundance 14

The special case of 1H 0707-495 III. Time lags Fabian 09 primary PL comes first followed by reflection component 30 min 30 seconds fast variations (< 20 min) Looking for time lags between lines and continuum: the most crucial result supporting the relativistic RM 15

The special case of 1H 0707-495 III. Time lags The observed lag means that: - the soft X-ray spectrum (Fe L) has to be reprocessed emission - if it was the same continuum the lag would be in the opposite direction - the magnitude of the lag (~ 30s) is dictated by light travel time: - the X-ray corona is very close to the BH (few R G ) - the BH mass is likely 3-5 x 10 6 M sun 16

The special case of 1H 0707-495 IV. Why is reflection so strong? Miniutti,Fabian 03 GR light bending R G,Z R G,X 0 It is a natural consequence of having a X-ray corona close to the BH as demonstrated by the ~30s lag 17

The special case of 1H 0707-495 V: There is another template: IRAS 13224-3809 Pointi 10 Also negative time lag detected but with lower statistics 18

Do we have a spectral template ? What a standard one would look like In the standard situation and with normal exposures we are unable to detect all these features except for the soft excess (which is indeed ubiquitously) detected 19

The special case of 1H 0707-495 VI. The relativistic RM for soft broad X-ray lines O VII/VIII blend Ross, Fabian 05 Boller 10 Refl Refl+ kdblur ξ σ σ (erg cm s -1 ) (eV) (eV) EF E [keV cm -2 s -1 ] 5000 ~400 ~650 2000 200 400 1000 30 100 500 10 60 200 5 20 O VIII blend 100 4 15 Energy [keV] 20

1H0707 strong and weaker field GR limit results Boller 10 reflection: strong GR field limit Index=6.3+-0.4, R in (G)=3.3+-0.1, ξ =1000+-260 emission from the innermost stable orbit strong Compton broadening FWHM ~ 1/3c additional soft broad line blends: weaker GR field limit emission from a few 1000 R G FWHM ~ 0.03 – 0.08c 21

Ark 564 strong and weaker field GR limit results Boller 10 RM parameters: Reflection: strong GR field Index=3.4+-0.6 R in (G)=3.6+-0.4 ξ =6000+-900 E=0.60 σ =85 eV FWHM~1/3c E=0.95 keV σ =150 eV FWHM~1/3c FWHM 18000 km/s =0.06c 12000 km/s =0.04c Additional blends: weaker GR field 22

Mrk 110 strong and weaker field GR limit results Boller 10 Reflection: strong GR field Index=3.1+-3.0 R in (G)=3.4+-0.9 ξ =1400+-1000 E=0.53 σ =60 eV E=0.90 FWHM~0.1c σ =70 eV FWHM~0.08c FWHM Additional blend: 10000 km/s =0.003c weaker GR field 23

Predictions for IXO Müller 06 gravitational redshift z G g f � i i g = core f � i distance R G line profile measurements provide values for g core which deliver the z G and R G 1. this allows to test GR prediction via IXO measurements 2. the strong gravity Fe K α measurements can be extended to the weaker field limit by studying relativistic soft X-ray lines 24

The Future satellites: eROSITA, ASTRO-H, ELT, LISA, IXO…..(Planck, Herschel) important impact on multifrequency observations and physics 25

(Future) Great Observatories Maiolino 08 IR JWST Radio SKA mm ALMA IXO X-ray NIR Opt. EELT 26

New science goals with MWL future Arnaud et al. 08 , Nandra 10 , ESA CV YB 10 Are the GR prediction correct? First light: What is the nature of the earliest galaxies? What is the nature of the host galaxies of super-massive black holes and gamma ray bursts? What sources are responsible for reionisation? What is the metal enrichment history of galaxies and the IGM? How many types of matter exist? What is dark matter? types? What is dark energy? Does it evolve? How many types are there? 27