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The Chandra view of Mrk 279

The Chandra view of Mrk 279. Elisa Costantini SRON, National Institute for Space Research Astronomical Institute Utrecht. Outline. Mrk 279 Chandra-LETGS observation Emission spectrum Broad lines UV– X-rays modeling Absorption components Warm absorber Redshift zero absorption

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The Chandra view of Mrk 279

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  1. The Chandra view of Mrk 279 Elisa Costantini SRON, National Institute for Space Research Astronomical Institute Utrecht

  2. Outline Mrk 279 Chandra-LETGS observation Emission spectrum • Broad lines • UV– X-rays modeling Absorption components • Warm absorber • Redshift zero absorption Conclusions Warsaw warm absorber workshop

  3. Mrk 279 previous study • z = 0.0306 • ASCA (Weaver et al. 2001) • Variable iron line at 6.4 keV • On the line of sight of ionized gas at z=0 (Savage et al. 2003) • HTS+FUSE+Chandra HETGS (Scott et al. 2004) • 4 absorption systems from the host galaxy • 1 warm absorber Warsaw warm absorber workshop

  4. LETGS observation of Mrk 279 - 10-20th May 2003 - 7 shots (30-100 ks) - Total exposure: 355 ks • - FUSE (91 ks) + HST (41.3 ks) • Arav et al. 2004, 2005 • Gabel et al. 2005 Warsaw warm absorber workshop

  5. The first fit • Complex oxygen region: • Narrow emission lines (OVII f, OVIII Ly α) • Absorption lines  OI-OVIII • Broad emission features OVII, OVIII Warsaw warm absorber workshop

  6. X-rays broad lines in Sy 1 NGC 5548 Broad emission lines  Iron K α 6.4 keV (Tanaka 1995) OVII triplet (21.5-22.09 Å) (ngc5548 Steenbrugge et al. 2005) OVIII Ly α (18.96 Å) (ngc4051 Ogle et al. 2004, Fenovcik et al. 2005) Warsaw warm absorber workshop

  7. X-rays broad lines in Sy 1 Broad emission lines  Iron K α 6.4 keV (Tanaka 1995) OVII triplet (21.5-22.09 Å) (ngc5548 Steenbrugge et al. 2005) OVIII Ly α (18.96 Å) (ngc4051 Ogle et al. 2004, Fenovcik et al. 2005) Relativistic broadening Warsaw warm absorber workshop

  8. UV broad lines Gabel et al. 2005 FWHM=11000 km/s Warsaw warm absorber workshop

  9. The LOC method • One component of ionized emitting gas is inadequate to describe emission.  BLR as a distribution of clouds with different density, distance, column density, and covering factor. (Baldwin et al. 1995, Ferland et al.) The Locally Optimally emitting Cloud (LOC)  Successfully applied to NGC 5548 (Korista & Goad 2000) Warsaw warm absorber workshop

  10. Reflected Transmitted The LOC method (2) Ingredients for the BLR: Log NH=23 cm-2 Cf =0.5 Log n = 8-12.5 cm-3 Log r = 15.2-17.5 cm Warsaw warm absorber workshop

  11. FUSE+HST best fit:  = 0.89 • = 0.97 X-ray line luminosity ! Warsaw warm absorber workshop

  12. Where are the lines produced? BLR size: 6-17 ldays (Santos-Lleo et al. 2001) Warsaw warm absorber workshop

  13. No strong evidence of : • highly ionized skin of the BLR • relativistically broadened profile of OVIII Warsaw warm absorber workshop

  14. Warm absorber: the models • SPEX (Kaastra 2001) • SLAB: transmission from a thin layer. Parameters: ionic column densities, outflow velocity, line broadening • XABS: fit with a pre-calculated grid of NH and ξ, gi ven a SED relies on XSTAR or Cloudy Parameters: NH, ξ, outflow velocity, line broadening • WARM: a continuos distribution of XABS Parameters: outflow velocity, sigma, ξlowξhigh Warsaw warm absorber workshop

  15. Warm absorber: variability • Difficult issue because: • High S/N • High resolution • Sufficient flux amplitude variation • Long time scale variation: e.g. ngc 3516 (Turner et al.2005) ngc 4151 (Kraemer et al. 2005) • Short time scale variation: No ngc 5548 (Steenbrugge et al. 2005) ngc 3783 (Netzer et al. 2003) Yes ngc 4051 (Krongold et al. 2005) 0 days 10 Warsaw warm absorber workshop

  16. warm absorber variability Logξ 2.5 0.46 NH • Large error bars • Large scatter in the ionization parameter Warsaw warm absorber workshop

  17. The warm absorber (2) 3 ionized warm absorbers intrinsic to Mrk 279 2 absorbers in the Milky Way Warsaw warm absorber workshop

  18. The nature of the wa in mrk 279 No pressure equilibrium  continuous distribution ? Warsaw warm absorber workshop

  19. Continuous vs clumpy wa • Phases in pressure equilibrium • NGC 3783 (Netzer et al. 2003, • Krongold et al. 2003) • Prompt reaction to flux variation • Continuous distribution • NGC 4051 (Ogle et al. 2004) • NGC 5548 (Steenbrugge et al. 2005) NGC5548 Warsaw warm absorber workshop

  20. The Milky way ionized absorber Blue wing v= - 87 km/s σ = 80 km/s (Kaastra et al in prep.) Warsaw warm absorber workshop

  21. Z=0 absorber: interpretation • predicted EW(OVI)X =0.74 mÅ, consistent with non detection • if OVII were connected with the narrow UV component •  deep OVII edge which is not observed Global UV-X model: collisionally ionized absorber Winning interpretation:HVC complex C/K v= -(100-55) km/s solar metallicity Warsaw warm absorber workshop

  22. Conclusions • Broad lines: HST + FUSE  BLR lines in X-rays  independent constraints to the X-ray spectral fit. No strong evidence of a highly ionized skin of the BLR No strong evidence of relativistic profiles • Warm absorbers: 3 main components, not variable, possibly in a continuous outflow z=0 absorption: most likely in the Milky Way Warsaw warm absorber workshop

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