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XMM-Newton Monitoring of 3C 273

XMM-Newton Monitoring of 3C 273. Orbit Exposure (s) 094 63,000 095 27,000 095 30,000 096 58,000 277 43,000 370 5,000 373 4,900 472 4,900 554 4,500 563 8,500 655 58,000 735 8,500

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XMM-Newton Monitoring of 3C 273

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  1. XMM-Newton Monitoring of 3C 273 Orbit Exposure (s) 094 63,000 095 27,000 095 30,000 096 58,000 277 43,000 370 5,000 373 4,900 472 4,900 554 4,500 563 8,500 655 58,000 735 8,500 835 20,000 835 18,000 Page, K, Turner, M.J.L., Done, C., O’Brien, P.T., Reeves, J.N., Sembay, S., Stuhlinger, M., 2004, MNRAS, 349, 57 Forthcoming Cross-Cal observations: ~July 2005 XMM/Swift/Integral ~Dec 2005 XMM/Astro-E

  2. Major changes to low energy calibration for EPIC cameras planned. (See poster on EPIC cross-calibration…M.P.Esquej et al. this meeting) MOS: For the next SAS release rmfgen will be modified to generate rmfs for the MOS detectors which are epoch AND spatially dependant.

  3. Major changes to low energy calibration for EPIC cameras planned. (See poster on EPIC cross-calibration…M.P.Esquej et al. this meeting) MOS: For the next SAS release rmfgen will be modified to generate rmfs for the MOS detectors which are epoch AND spatially dependant. Relative fluxes from sample of AGN (EPIC: 15-40 arcsec extraction radius)

  4. Major changes to low energy calibration for EPIC cameras planned. (See poster on EPIC cross-calibration…M.P.Esquej et al. this meeting) MOS: For the next SAS release rmfgen will be modified to generate rmfs for the MOS detectors which are epoch AND spatially dependant. Zeta Puppis: Early O-type Supergiant Distance 429 pc, mv=2.25

  5. Major changes to low energy calibration for EPIC cameras planned. (See poster on EPIC cross-calibration…M.P.Esquej et al. this meeting) PN: Shows no significant evolution of the rmf or arfwith time but a change in the absolute rmf is being implemented to improve low energy calibration.

  6. Cross-calibration with (test) MOS rmf and SAS6.1.0 PN rmf:

  7. January 2003 Courvoisier et al. 2003 A&A 411, L343

  8. January 2003 After Renormalisation to PN Data consistent with… Γ ~ 1.74 above 3 keV Courvoisier et al. 2003 A&A 411, L343

  9. The observed JET in 3C 273 HST Chandra Merlin 13” from core LX (jet) ~ 3x1043 ergs s-1 c.f. LX (core) > 1046 ergs s-1 20” from core Marshall et al. 2001, ApJ, 549, L167

  10. EPIC Observed Photon Index (3-10 keV)

  11. EPIC Observed Photon Index (3-10 keV)

  12. Description: kTB ~100 eV and kTBB~ 250 eV Page et al. 2004 MNRAS, 349, 57 Fe EW ~ 0-50 eV Ginga/ASCA/SAX/XMM

  13. “Untangling the Jet and Accretion-Disk Emission” BeppoSAX 1997 BeppoSAX 2001 Grandi, P. and Palumbo, G.G.C., 2004, Science, 306, 998 Analysed 6(9) BeppoSAX observations between 1997 and 2001

  14. Γ = 1.8 i = 18o RC = 0.8 “Seyfert” Spectral Fit with wabs * (zbb + pexrav + zpo) model “Seyfert” “Jet” FSEY = 1.74 + (FBB x 1.64) FJET ~ 1.5 x FSEY

  15. Predicted “Seyfert” and “Jet” high energy fluxes: EPIC

  16. Predicted “Seyfert” and “Jet” high energy fluxes: EPIC + SAX

  17. XMM Obs. In Orbit 563

  18. Photon Index of “Jet” component

  19. Predicted “Seyfert” and “Jet” high energy fluxes: EPIC MCG -6-30-15 Vaughan and Edelson, 2001, ApJ, 548, 694 ΓSEY Softer ?

  20. ΓJET Harder ?

  21. Measuring the Iron Line emission PN < 22 eV MOS < 43 eV PN = 36±19 eV MOS = 57±23 eV PN < 32 eV MOS < 65 eV

  22. Power law fit: χ2 = 1579/1397 dof With Broad Line: χ2 = 1510/1394 dof EFE=6.44±0.11 keV σ = 0.42±0.09 keV EQW=36.4±19 eV F=3.8(1.6)x10-5 phts/cm2/s

  23. EFE=6.44 keV (fixed) σ = 0.42 keV (fixed) EQW=57±23 eV

  24. Power law fit: χ2 = 1036/1060 dof EFE=6.44 keV σ = 0.42 keV EQW < 22 eV

  25. EFE=6.44±0.11 keV σ = 0.42±0.09 keV EQW=36.4±19 eV F=3.8x10-5 phts/cm2/s

  26. PN intermediate Flux State

  27. Summary Major advances in the EPIC low energy cross-calibration soon to be implemented suggest a more robust determination of the spectral shape/model of the soft excess in 3C 273 can be made. The EPIC view of the hard X-ray data suggest that the nonthermal component is dominant over the “accretion” component, probably more so than suggested by the recent published analysis of BeppoSAX results.

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