1 / 19

A time(scales) trip to Mkn478 with XMM-Newton

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),.

zarifa
Download Presentation

A time(scales) trip to Mkn478 with XMM-Newton

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 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. 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. Important timscales for AGN • Light crossing time (MBHM7107 MsunRRg) • lc  200  M7 seconds • Keplerian flow dynamic timescale • K  15 3/2 M7 minutes • Thermal timescale • th  -1 K  hours • Viscous timescale • v  th (r/h)2  days/months • Disk reprocessing/torus reprocessing/diffuse gas ... r h

  4. The Mkn478 monitoring program • Why Mkn478? • Variable • Weak reprocessing features • Low absorption • NH,Gal=1.01020 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) Mkn478 (Leighly 1999) Mkn478 is a micro-cosmos of Narrow Line Seyfert 1 variability

  5. E=6.700.08 keV EW=12080 eV P96% XMM-Newton spectra SOFT BAND HARD BAND Double power-law fits

  6. 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. 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. Expected tracks for a pair-dominated plasma: face-on disk and Tbb = 100 eV (Haardt et al. 1997) (Lack of) spectral correlations hard vs. Fhard soft vs. Fsodt  vs. R RLsoft/Lhard vs. FX

  9. The quest for the “physical driver” Double Comptonization scenario (Titarchuck & Lyubarskij 1994, Hua & Titarchuck 1994) kT0=60 eV 2001: kT0=683 eV 2003: kT0=58.51.9 eV

  10. Variablity on shorter timescales 0.2-1 keV 3-10 keV

  11. The quest for the “typical” variability timescale Structure function: SF() = < [ F(t) - F(t+) ]2 > (Simonetti et al. 1985) 0.6 (Nandra et al. 1997, Edelson et al. 2002, Vaughan et al. 2003) Normalized excess variance 2nxs = (2obs-2exp)/<x>2

  12. R  0.9 same soft same hard Spectral variability between bands Hardness ratio 0.2-1 keV versus 3-10 keV Cross-correlation 0.2-1 keV versus 3-10 keV Jan 7 – 1st half Jan 7 – 2nd half

  13. Spectral variabilty in the soft band

  14. Spectral variability in the hard band “Flares” light curve and HR HR vs count rate correlation probabilities: P  50% P  82% P  95%

  15. 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. End Lunch time

  17. Recent results on Seyfert variability PKS0558-504 NGC7469 IRAS13224-3809 (Gallo et al. 2003) (Gliozzi et al. 2001) (Petrucci et al. 2003) 1H0419-577 (Page et al. 2002)

  18. Multi-blackbody models kT  120 eV kT  250 eV kT  120 eV kT  70 eV kT  1700 eV kT  50 eV kT  200 eV kT  210 eV kT  100 eV kT  75 eV kT  1700 eV kT  50 eV

  19. Narrow-band features OVII E=6.700.09 keV EW=12080 P(F-test)96.7 Photoabsorption edge? In 7-Jan-2003 observation only: the lowest hard X-ray flux ever

More Related