1. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 1 XMM-Newton A time(scales) trip to Mkn478 A time(scales) trip to Mkn478 with XMM-Newton Matteo Guainazzi XMM-Newton Science Operations Center Research and Science Support Division of ESA, VILSPA, Spain J.Clavel, N.Loiseau, A.Orr (ESA), F.Fiore (Oss. Monteporzio) K.Mason, E.Puchnarewicz (MSSL), G.Matt, G.C.Perola (Un. Roma Tre),

2. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 2 XMM-Newton Goal Narrow Line Seyfert 1 Galaxies are X-ray variable [talk T.Boller] Their X-ray spectra have two-components, directly related to accretion [posters C.Matsumoto, M.Murashima] XMM-Newton covers the whole 0.1-10 keV with unprecedented sensitivity (RXTE: 2-20 keV) design a specific experiment to probe the spectral variability in NLSy1s on a range of different timescales

3. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 3 XMM-Newton Important timscales for AGN Light crossing time (M BH M 7 10 7 M sun RR g ) – lc  200  M 7 seconds Keplerian flow dynamic timescale – K  15  3/2 M 7 minutes  Thermal timescale – th   -1  K  hours Viscous timescale – v   th (r/h) 2  days/months Disk reprocessing/torus reprocessing/diffuse gas... h r

4. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 4 XMM-Newton The Mkn478 monitoring program Why Mkn478? –Variable –Weak reprocessing features –Low absorption –N H,Gal =1.010 20 cm -2 Which data? –1 ASCA observation (July 1995) –1 BeppoSAX observation (Aug 2000) –1 XMM-N observation (Dec 2001) –3 close XMM-N observations (1, 4, 7 Jan 2003) – –Exposure times: –30 ks (ASCA) –50 ks (BeppoSAX) –20 ks (XMM-N) (Leighly 1999) Mkn478 Mkn478 is a micro-cosmos of Narrow Line Seyfert 1 variability

5. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 5 XMM-Newton XMM-Newton spectra Double power-law fits SOFT BAND HARD BAND E=6.70  0.08 keV EW=120  80 eV P  96%

6. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 6 XMM-Newton The history of the X-ray SED in Mkn478  Flux dynamical ranges: – 2 in soft X-rays – 4 in hard X-rays  Constant soft X-ray spectral shape  Variable hard X-ray spectral shape (1.0) – No correlation with the soft, hard or total X-ray power  Soft/hard X-ray luminosity ratio 0.4-2.5

7. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 7 XMM-Newton The history of the X-ray SED in Mkn478  Flux dynamical ranges: – 2 in soft X-rays – 4 in hard X-rays  Constant soft X-ray spectral shape  Variable hard X-ray spectral shape (1.0) – No correlation with the soft, hard or total X-ray power  Soft/hard X-ray luminosity ratio 0.4-2.5

8. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 8 XMM-Newton (Lack of) spectral correlations  soft vs. F sodt  hard vs. F hard R  L soft /L hard vs. F X  vs. R (Haardt et al. 1997) Expected tracks for a pair-dominated plasma: face-on disk and T bb = 100 eV

9. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 9 XMM-Newton The quest for the “physical driver” kT 0 =60 eV 2001: kT 0 =68  3 eV 2003: kT 0 =58.5  1.9 eV Double Comptonization scenario (Titarchuck & Lyubarskij 1994, Hua & Titarchuck 1994)

10. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 10 XMM-Newton Variablity on shorter timescales 0.2-1 keV 3-10 keV

11. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 11 XMM-Newton The quest for the “typical” variability timescale Structure function: SF(  ) = (Simonetti et al. 1985) Normalized excess variance  2 nxs = (  2 obs -  2 exp )/ 2 (Nandra et al. 1997, Edelson et al. 2002, Vaughan et al. 2003)  0.6

12. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 12 XMM-Newton Spectral variability between bands Cross-correlation 0.2-1 keV versus 3-10 keV Jan 7 – 1 st half Jan 7 – 2 nd half Hardness ratio 0.2-1 keV versus 3-10 keV R  0.9 same  soft same  hard

13. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 13 XMM-Newton Spectral variabilty in the soft band 

14. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 14 XMM-Newton Spectral variability in the hard band HR vs count rate correlation probabilities: P  50% P  82% P  95% “Flares” light curve and HR

15. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 15 XMM-Newton Summary The hard X-ray flux varies achromatically on timescales of fraction of hours The hard X-ray spectrum varies on timescales of days, with no obvious correlation with the X-ray power No unique physical driver for the long-term variability The soft X-ray flux varies almost achromatically on scales of hours to days Soft and hard X-rays are related – by not correlated – on scales of hours  driven by a common physical parameter? –On longer timescales this relation is basically lost The scenario is complex: –careful selection of the energy bands to study is crucial –different timescales mix

16. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 16 XMM-Newton End Lunch time

17. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 17 XMM-Newton Recent results on Seyfert variability (Page et al. 2002) (Gallo et al. 2003) (Gliozzi et al. 2001) (Petrucci et al. 2003) IRAS13224-3809 PKS0558-504 1H0419-577 NGC7469

18. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 18 XMM-Newton Multi-blackbody models kT  70 eV kT  120 eV kT  1700 eV kT  50 eV kT  120 eV kT  250 eV kT  50 eV kT  100 eV kT  200 eV kT  75 eV kT  210 eV kT  1700 eV

19. Matteo Guainazzi Science Operations & Data Systems Division Research & Scientific Support Department “Stellar-mass, intermediate-mass and supermassive black holes” – Kyoto (Japan) – 28-31 October 2003 Page 19 XMM-Newton Narrow-band features OVII In 7-Jan-2003 observation only: lowest hard X-ray flux ever the lowest hard X-ray flux ever E=6.70  0.09 keV EW=120  80 P(F-test)  96.7 Photoabsorption edge?