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with the collaboration of Guido Risaliti, Yair Krongold, Fabrizio Nicastro, Chris Reynolds

Reynolds C. Eclipsing in AGN:. X-ray absorption and AGN Structure. Martin Elvis Harvard-Smithsonian Center for Astrophysics. with the collaboration of Guido Risaliti, Yair Krongold, Fabrizio Nicastro, Chris Reynolds and many others…. The Quasar Puzzle.

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with the collaboration of Guido Risaliti, Yair Krongold, Fabrizio Nicastro, Chris Reynolds

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  1. Reynolds C. Eclipsing in AGN: X-ray absorption and AGN Structure Martin Elvis Harvard-Smithsonian Center for Astrophysics with the collaboration of Guido Risaliti, Yair Krongold, Fabrizio Nicastro, Chris Reynolds and many others… Martin Elvis, MIT, 4 March 2008

  2. The Quasar Puzzle Jiang et al., 2007, ApJL, 666, L9, VanDen Berk et al., 2001,AJ,122, 549 Lya CIV MgII • AGN SEDs, spectra same • Over 6 decades of Luminosity • Over 13 Gyr of cosmic time • Unchanging structure • Determined within BH sphere of influence: “The Nucleus” • Complex phenomenology • Non-trivial structure • Answers affect cosmic feedback z~1-3 SDSS template z~6 quasar Z=6.4 SDSS spectrum, SED Martin Elvis, MIT, 4 March 2008

  3. Conical geometry AGN ‘funnel wind’ Structure Elvis 2000 ApJ 545, 63; 2003 astro-ph/0311436; 2009 in preparation Multi-wavelength approach, uniting all atomic physics features in AGNs Thin Wind Pressure balance Martin Elvis, MIT, 4 March 2008

  4. Eclipses in Astronomy “These late eclipses of the sun and moon portend no good to us.”King Lear I:2:98 …but useful in astronomy: earth is a sphere binary stars black hole masses 1st test of GR extrasolar planets… …and for quasars Martin Elvis, MIT, 4 March 2008

  5. X-ray Spectral Variability Scales of Quasar/AGN Components Warm Absorber Compton Wind molecular torus Black Hole inabsorption Rs 105 10 1 1000 X-ray Cont. broad Fe-K BELR Low Ionization MgII, FeII Balmer series High Ionization CIV HeII OVI NIR cont JHK NELR Ha [OIII] Coronal lines Optical/UV continuum Martin Elvis, MIT, 4 March 2008

  6. 100,000 Rg: Cold Obscuring Torus Warm Absorber Compton Wind molecular torus Black Hole Rs 105 10 1 1000 X-ray Cont. broad Fe-K BELR Low Ionization MgII, FeII Balmer series High Ionization CIV HeII OVI NIR cont JHK NELR Ha [OIII] Coronal lines Optical/UV continuum Martin Elvis, MIT, 4 March 2008

  7. 100,000RS The Dusty Molecular Torus • Flattened optical & X-ray obscuring region Lawrence & Elvis 1982 • type1type2 AGN = ‘Unified Scheme’ • Rsub= 1.3x105L0.10.5 M8 0.5 T1500-2.8RS • NH~1024cm-2; H/R~1 • Puffed up by IR on dust? Krolik 2007, Murray 2007 Is this the whole story? Martin Elvis, MIT, 4 March 2008

  8. EPIC-MOS NGC1365: an AGN Structure Laboratory • Face-on barred spiral D~25Mpc • Bright X-ray source fx~1mCrab, logLx=42.2 Ward et al. 1978 MN 223, 788 • LBol~10-3 Ledd(M/M8)-1 • logMBH ~ 7.3 - 7.8 M • M-sbulge, M-K • Obscured: NH>1022.5cm-2 • Highly variable NH: • Key to study of AGN structure Martin Elvis, MIT, 4 March 2008

  9. Constant E<2keV Thermal component Constant flux narrow Fe-K component NGC1365: Compton thick/Thin Transitions • Compton thickthin transitions are rare: • 4/30 Matt et al. 2003 • 1/11 Guainazzi et al. 2005 • NGC1365 transitions reliably often: • ~7/13 observations Compton-thin • NGC1365 is a special object log NH~23.5 log NH~23.7 log NH>24.2 Martin Elvis, MIT, 4 March 2008

  10. NGC1365: Fairly Rapid Compton thin/thick transitions Risaliti et al., 2005a, ApJL, 623, L93 • DNH>~1024cm-2in 3 weeks: • requires R<104Rs <4.5x1017cm, • ne>109 cm-3 • What is changing? • fx(intrinsic)? • c.f. disk cooling time > 30R201/2d • ionization? • Dx (ionization) ~ 103 • NH • Hard to reconcile with standard torus 23 days 2002Dec 24, t= 0 d 2003Jan 16, t=23 d 185 days 2003Feb 09, t=47 d 2003Aug13, t=232d Martin Elvis, MIT, 4 March 2008

  11. NGC1365: Really Rapid Compton thin/thick transitions Risaliti et al., 2007, ApJL, 659, L111 • Chandra: Compton ThinThickThin in4 days • DNH>~1024cm-2in 2 days • ne>109 cm-3 • R(NH) < few 1000 Rs • Inconsistent with standard torus 2 days 2 days Martin Elvis, MIT, 4 March 2008

  12. 3000RsA More Compact Torus Elvis et al., 2004, ApJL, 615, L25;Risaliti et al., 2005a, ApJL, 623, L93 • Need another ‘torus’ location near BELR • Accretion disk wind? • Also toroidal • Large H/R natural • No support problem • Dust radiation pressure driven? • dust survives in disk toR>~2000 Rs (Tdisk<1000 K) • Magnetic support? Kartje, Königl & Elitzur, 1999 ApJ 513, 180 Should see fluorescent Fe-K from other parts of torus Martin Elvis, MIT, 4 March 2008

  13. ct 3ct 2ct 3000Rs Where is the narrow Fe-K? Suzaku Cycle 2: Elvis (PI) et al. Suzaku/NGC5548: Fe-K • Suzaku 2-month monitoring of NGC5548 • High S/N 240 ksec spectrum • Fe-K narrow core: FWHM = 5500 km/s s = 50+/-15eV R~3000Rg= Obscuring material? I.e. Rs ~23 l-dMBH = 6.7x107 M • Butfactor ~4 in ~30days • Fe-K core = constant • Larger than 3000 Rs? • Non-Keplerian motions? • Light travel time smearing? • Not a worry yet. Martin Elvis, MIT, 4 March 2008

  14. Dusty Wind Moving inwards: Warm Absorbers Warm Absorber Compton Wind molecular torus Black Hole Rs 105 10 1 1000 X-ray Cont. broad Fe-K BELR Low Ionization MgII, FeII Balmer series High Ionization CIV HeII OVI NIR cont JHK NELR Ha [OIII] Coronal lines Optical/UV continuum Martin Elvis, MIT, 4 March 2008

  15. 3000Rs Where are the Warm Absorbers? Kaspi et al. 2002, ApJ, 574, 643 • Highly ionized, blueshifted (~1000km/s): Wind • Common: ~50% of all AGNs and quasars • Location? Factor 106 in radius proposed • NELR to HiBELR • Mass loss rate uncertain by factor 106 • Is AGN feedback important to galaxy evolution or not? Chandra HETG: 900ksec NGC3783 Martin Elvis, MIT, 4 March 2008

  16. Step function change Gradual WA response How to Measure the Warm Absorber Location Nicastro et al., 1999, ApJ, 512, 184 WA response to continuum is not instantaneous: • ‘Ionization time’ and ‘Recombination time’  measure ne • UX ~ 4p LX/R2 • WA measures Ux • hence radius, R Martin Elvis, MIT, 4 March 2008

  17. High State High StateHS Low StateLS ~30 ksec Low State Small RWA in NGC4051: XMM/RGS Krongold et al., 2007, ApJ, 659, 1022 • 4X flux increase in ~30 ksec • WA changes! • Not continuous U(r) • WA is dense & compact • Not NELR Martin Elvis, MIT, 4 March 2008

  18. Small RWA in NGC4051: XMM/EPIC Krongold et al., 2007, ApJ, 659, 1022 XMM EPIC Light Curve • Two Warm Absorber components stay close to photo-ionization equilibrium log Ux(t), measured log Ux(t), predicted from photoionization equilibrium Martin Elvis, MIT, 4 March 2008

  19. Small RWA in NGC4051: XMM/EPIC Krongold et al., 2007, ApJ, 659, 1022 • Low Ionization (LIP) R<3.5 l-d • High Ionization (HIP) R=0.5-1.0 l-d Martin Elvis, MIT, 4 March 2008

  20. Dust sublimation radius ~HeII BELR Hb BELR Dusty molecular torus LIP HIP light-days 5 10 15 NGC4051: An Accretion Disk Scale Warm Absorber Krongold et al., 2007, ApJ, 659, 1022 • Rules out Narrow Emission Line Region(kpc scale) • Rules out Obscuring molecular torus(Krolik & Kriss, 2001) • Minimum dust radius, rsubl(NGC4051) ~ 12-170 light-days • Rules out Low Ionization (Hb) broad emission line region(BELR); R(Hb) = 5.9 light-days (Peterson et al. 2000)= disk? • Co-located with High Ionization BELR?: HeII = wind? • Driven by UV absorption lines, as in O-star winds? Murray et al.1995 Warm Absorber Martin Elvis, MIT, 4 March 2008

  21. Dusty Wind 50Rs NarrowFe-K Absorption Warm Absorber Compton Wind molecular torus Black Hole Rs 105 10 1 1000 X-ray Cont. broad Fe-K BELR Low Ionization MgII, FeII Balmer series High Ionization CIV HeII OVI NIR cont JHK NELR Ha [OIII] Coronal lines Optical/UV continuum Martin Elvis, MIT, 4 March 2008

  22. EPIC-MOS Curves of growth High Vt High Vt EW mos Ka/Kb observed pn Log NH Log NH 23 24 EW observed 50Rs NGC1365: Compton Wind Risaliti et al., 2005, ApJL, 630, L129 • 4 strong absorption lines: FeXXV, FeXXVI K-a, K-b • EW~100eV • Broad: vturb~500-1000 km/s • Ka/Kb small - saturated: • High NH>1023.5 Compton thick • Super-High Ionization WA: • logUX~0, R ~ 50(M/M8)-1Rs • Blueshifted • 2500  5000 km/s in 18mo. • acceleration? Martin Elvis, MIT, 4 March 2008

  23. X-ray continuum source 50Rs NGC1365: Failed Compton Wind Risaliti et al., 2005, ApJL, 630, L129 • V(Fe-K) << Vesc ~50,000(M/M8)-1 km/s • high U • L/LEdd ~ 10-3 • ‘failed wind’? or transverse = ‘hitchhiking gas’ ?Murray & Chiang • Filters X-ray continuum from outer gas… • Lowers ionization state… • Enabling UV line driven acceleration (as in O-star winds) • Disk geometry essential Martin Elvis, MIT, 4 March 2008

  24. Dusty Wind 4.<30 RSX-ray Continuum Eclipses Warm Absorber Compton Wind Black Hole Rs 105 10 1 1000 X-ray Cont. broad Fe-K BELR Low Ionization MgII, FeII Balmer series High Ionization CIV HeII OVI NIR cont JHK NELR Ha [OIII] Coronal lines Optical/UV continuum Martin Elvis, MIT, 4 March 2008

  25. NGC1365: Rapid X-ray Continuum Eclipses Risaliti et al., 2007, ApJL, 659, L111 • Compton ThinThickThin in 4 days • Now consider constraints on X-ray Continuum source 2 days 2 days Martin Elvis, MIT, 4 March 2008

  26. Ds X-ray source DC VK Eclipsing matter <30 RS X-ray Continuum Eclipses Risaliti et al., 2007, ApJL, 659, L111 • Dimensions of X-ray source: • Ds = Vc x Tecl • If Vc ~ 104 km/s Ds ~ 1014 cm • Can’t be much higher (to avoid overionization, from iron line width) • If lower, even smaller X-ray source • Black hole mass in NGC 1365: • Log MBH/M= 7.3 (0.3,0.3)M-(Ferrarese et al. 2005) • Log MBH/M= 7.86 (0.15,0.3)M-LK(Marconi & Hunt 2003) • X-ray source size < 33 RG Martin Elvis, MIT, 4 March 2008

  27. Schwartzschild eclipse profile Kerr eclipse profile Future Continuum Eclipses Resolving Eclipse profile: • Size/shape/1-D emissivity map • Kerr/Schwartzschild? C.Reynolds • Close to resolving? • Suzaku cycle 3 propoal Martin Elvis, MIT, 4 March 2008

  28. Dusty Wind <30 RSX-ray Relativistic Fe-K Eclipses Warm Absorber Compton Wind Black Hole Rs 105 10 1 1000 X-ray Cont. broad Fe-K BELR Low Ionization MgII, FeII Balmer series High Ionization CIV HeII OVI NIR cont JHK NELR Ha [OIII] Coronal lines Optical/UV continuum Martin Elvis, MIT, 4 March 2008

  29. <30 RS Broad Fe-K Eclipses Risaliti et al., 2007, ApJL, 659, L111 • Red wing on Fe-K is 1% over continuum. Ambiguous. • NGC1365 has strong red wing & strong Fe-K absorption lines  High Fe abundance? • Gone in Compton-thick spectrum. • DFe-K < 1014 cm, <33 RS Martin Elvis, MIT, 4 March 2008

  30. Red wing occulted Blue wing occulted <30 RS Future: Tomography of Fe-K Reynolds, Risaliti, Elvis, … Apply Binary physics • Ingress, egress successively cover/uncover red-/blue- shifted Fe-K • Clean, definitive experiment • Establish • Fe-K • Rotation • z(R) • Goal of Suzaku Cycle 3 proposal • More sensitive mission could probe metric in detail Martin Elvis, MIT, 4 March 2008

  31. 5m 40 Mission for Future Eclipse Mapping of AGNs Elvis, Astro-ph/0403554; 2004, Nucl. Phys. B 134, p.78-80 • Weeks-long observations of each source - not an observatory-class mission • 10 x S/N of Chandra in ~1hour vs. 4 hours -large area, high count rate • Better spectral resolution • Only ~1 arcmin spatial resolution (HPD) Extreme Physics Explorer Martin Elvis, MIT, 4 March 2008

  32. WA NAL HiBEL Dusty Obscurer Compton (failed) Wind 10 1000 100 10000 X-ray Eclipses and AGNs • Several techniques probe scales from 105- 10 Rs • A simpler, physically driven picture of AGN Structure • Makes quasar puzzle of uniformity semi-understandable X-ray Cont. Broad Fe-K Narrow Fe-K rg Martin Elvis, MIT, 4 March 2008

  33. Eclipse results confirm & extend ‘funnel wind’ model Elvis 2000 ApJ 545, 63; 2003 astro-ph/0311436 Becoming a secure basis for physical wind models: will allow extrapolation Martin Elvis, MIT, 4 March 2008

  34. 10 1000 100 10000 The Restless AGN Accretion Disk Dust driven Wind Line driven Wind Compton driven Wind • Replace observational with physical names • Active Disk ‘atmosphere’ at all radii • mechanism must work at all radii • Not standard ‘hot corona’ • More like Solar Corona failed Wind failed Wind L<LEdd UV Cont. X-ray Cont. Broad Fe-K WARM COLD HOT Narrow Fe-K rg Martin Elvis, MIT, 4 March 2008

  35. Reynolds C. AGN X-ray Eclipses …give new views of AGN structure Martin Elvis, MIT, 4 March 2008

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