1 / 35

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.

koen
Download Presentation

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

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. 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

More Related