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Quasar Structure: Why the details matter for Co-evolution

Quasar Structure: Why the details matter for Co-evolution. Martin Elvis Harvard-Smithsonian Center for Astrophysics. Simulation. Bimodal galaxy colors. Data. AGN & Galaxy Evolution. Example: AGN winds, radiation inhibit star formation? Bimodal galaxy colors in GOODS

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Quasar Structure: Why the details matter for Co-evolution

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  1. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Quasar Structure:Why the details matter for Co-evolution Martin Elvis Harvard-Smithsonian Center for Astrophysics

  2. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Simulation Bimodal galaxy colors Data AGN & Galaxy Evolution • Example: • AGN winds, radiation inhibit star formation? • Bimodal galaxy colors in GOODS • need to turn off star formation in massive galaxies (R. Somerville) mbulge > 2x1010 Msol • AGN turns off star formation by ejecting gas by either gas or radiation pressure? (never re-accreted) R. Somerville: CfA lunch talk, March 2005

  3. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 3 Pathways for AGN Feedback • Radiation • Heat, ionize ISM: inhibit star formation • Universal in AGN, but AGN rare • Jets • Prevent cooling flows from cooling or flowing • Rare: 10% radio loud at any moment, • Do quiescent BH have ’dark’ jets? [see G. Fabbiano talk] • Winds • Less explored role • Common, even universal?

  4. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Murray, Chiang, Grossman & Voit 1995 20% Winds, Tori and Feedback • Winds: • Location: mass, KE, mv, Z rates • Geometry: fc, vescape, escape route • Torus: blocks 80% feedback to ISM 3.Host disk torus: larger - ISM directly 4.Disk Wind torus: smaller - mdot dependent?

  5. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Winds

  6. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 AGN Wind Basics Winds clearly present in >~50% of AGN, quasars Probably present in all AGN, quasars Provide mass/energy/metals to host galaxy, IGM:

  7. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Influence of AGN Winds Quantitative results hampered by lack of numbers for winds Most papers assume: • Mdotacc=MdotEdd, • Mdotout = 0.1 Mdotacc • All of wind escapes Need: • examples to give reality check • theoretical understanding to extrapolate to quasar population: • Dependence on full range of M, Mdot, Z, z

  8. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 mass/energy/metals ejection by AGN Winds Rates depend heavily on Location and Geometry • covering factor, equatorial vs conical vs polar • blocking by torus, host ISM Estimates of location span factor 106 in radiuskpc to 1000Rg • Mdot = 75 Msol/yr at 0.2pc Netzer et al. 2003 • Unsustainable: Mdot (out)>>Mdot(acc) Paradox Unified Model: 80% of lines of sight blocked by torus • Produces 4:1 ratio of type2:type1 AGN • Most AGN radiation, wind does not reach host galaxy  AGN feedback NOT important?

  9. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Chandra HETG: 900ksec NGC3783 X-ray Warm Absorbers and UV NALs = Wind Narrow UV lines: NAL ‘Warm Absorber’ Narrow X-ray lines Narrow UV lines Narrow X-ray lines Same Outflow ~1000 km s-1 Outflow ~1000 km s-1 Seen in same 50% of quasars Seen in 50% of quasars High ionization OVII, OVIII High ionization CIV, OVI Same outflow

  10. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 1. Wind Location

  11. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Breakthrough Result:A measured WA radius in NGC4051

  12. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Time Evolving Photoionization measures R Response is not instantaneous: ‘Ionization time’ and ‘Recombination time’ measure ne independent of Ux and so measures R Nicastro et al. (1999) Step function change Gradual WA response

  13. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 XMM EPIC Light Curve NGC 4051:Two Warm Absorber Components in Photoionization Equilibrium Krongold et al., 2005, Nature, submitted High Ionization phase log Ux(t), measured log Ux(t), predicted from photoionization equilibrium Low Ionization phase  Both WA components are DENSE and COMPACT

  14. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Lower limit on LIP ne and hence R • Low Ionization Phase, LIP in photoionizatin equilibrium at all times  teq(LIP) < tl,m = 3 ks  ne(LIP) > 8.1 107 cm-3 But (neR2)LIP = 6.6 1039 cm-1  R(LIP) < 8.9 x 1015 cm < 0.0029 pc < 3.5 light days

  15. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Measurement of HIP ne and hence R • At extremes (high and low) HIP is out of photoionization equilibrium teqi,j+k(HIP) > tj+k = 10 ks • HIP is in eq. at moderate fluxes  teql,m(HIP) < tl,m = 3 ks  ne(HIP)=(0.6-2.1)x 107 cm-3  R(HIP) = (1.3- 2.6)x 1015 cm = (0.5-1.0) light days

  16. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Warm Absorber (wind) Location: outer Dust sublimation radius ~HeII BELR Hb BELR Dusty molecular torus • RHIP ~ 0.5-1.0 light-day = (1.3-2.6) x 1015 cm • RLIP < 3.5 light-day: consistent • 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 Hb broad emission line region (BELR) • R(Hb) = 5.9 light-days (Peterson et al. 2000) LIP HIP light-days 5 10 15

  17. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 HIP gravitationally unstable HeII BEL rg 1000 2000 3000 5000 4000 Warm Absorber (wind) Location: inner • RHIP ~ 0.5-1 light-day ~2200 - 4400 Rg • Mbh=1.9+/-0.78 x 106 Msol (Peterson et al. 2004)  Disk winds arise on accretion disk scale • Consistent with high-ionization BEL size • R(HeII) ~< 2 light days. HeII blueshift ~400km/s = wind signature? • Close to gravitational instability radius • R(grav. unstable) = 1330 rg x (k/kes)2/3 (Goodman 2003)

  18. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 NGC4051 Wind Location: Summary • Disk wind • dense • consistent with pressure balance • associated with high ionization BELR • is gravitational instability implicated? • Rules Out: • NELR, Torus and Continuous Flow • Can now move on to assess Mass/KE outflow rates - needs geometry

  19. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 2. Wind Geometry

  20. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Murray, Chiang, Grossman & Voit 1995 Wind Geometry Equatorial winds would impact Torus no escape, no effect on host, IGM some fireworks: few 1000 km/s impacting mol. cloud: large, ongoing SNR shocks • Winds not equatorial: • large scale height/covering factor50% AGNs have Winds • Or torus and accretion disk not aligned

  21. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 UV Evidence for Transverse winds Arav, Korista & de Kool 2002, ApJ 566, 699 Arav, Korista, de Kool, Junkkarinen & Begelman 1999 ApJ 516, 27 Departures from 2:1 ratio give covering factor CIV doublet 2:1 ratio

  22. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 NGC4051 Warm absorber is radially thin • From the independent measure of NH(HIP)3.2x1021cm-2 R = 1.23 NH/ne R(LIP) < 9x1012 cm R(HIP) = (1.9-7.2)x1014 cm • (R/R)HIP = 0.1-0.2; (R/R)LIP < 10-3 • From the estimates of ne and (neR2): (R/R) = 1.23 NH ne-1/2 (neR2)-1/2  (R/R)LIP = 1 % (R/R)HIP  eitherthe LIP is embedded in the HIP (pressure balance) • orthe LIP is a boundary layer of the HIP

  23. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 dr=vdt R() R() r  q Cylindrical/Conical Geometry • NGC4051 Wind is Thin: spherical shells are implausible needs impulsive ejection; inconsistent with 50% of AGN having WA • would become a continuous flow - testable by re-observing in 2006 • Next simplest symmetry: cylindrical (or bi-conical)Elvis 2000

  24. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Conical geometry Confirms Major Features of Elvis ‘funnel wind’ Elvis 2000 ApJ 545, 63; 2003 astro-ph/0311436 Pressure balance Becoming a secure basis for physical wind models: will allow extrapolation

  25. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Conical/Polar Winds Avoid Torus can escape to affect host, IGM

  26. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 2. Wind Mass, KE rates

  27. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 NH >10 times lower with new models PHASE (Krongold et al., 2003) NGC 3783 Bound-free edges only full PHASE model Black line: includes bound-bound lines Mass Outflow Rates vs Mass Accretion Rate Mdotout = 0.8pmpNH vr R f(q,j) • MdotHIP = (4.3 - 9.2) x 10-5 Msol yr-1 • MdotLIP < 6 x 10-5 Msol๏yr-1 = 0.02 Mdotacc • Mdotout = 2% - 5% Mdotacc • KEWIND = 2.5 X 1037 erg s-1 • SMALL Mdotoutinsensitive to q, j unless j>75o, q<10o

  28. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 AGN wind mass deposited to IGM • If lifetime =108yr  Mtot(out)=(0.4-2)x104Msol • Mdotout scales with BH mass if at same Rg MBH(NGC4051) = 2 x 106 Msol  for MBH = 108-109Msol  Mtot(quasar) = 106-107 Msol KEtot(wind) = 1055 erg small, but comparable with ULIRGs

  29. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Caveats • Only one object • ‘Narrow Line Seyfert 1’ • Unusually distant BELR ~10xRg(normal)  higher Mdotout • Unusally weak wind?(= eigenvector 1?) • Low Mbh1.9 x 106 Msollow Mdotout? • Mdotout Scales with BH mass if at constant Rg • Mdotout = 0.8 p mp NH vrR f(j,q) = A Mbh • ‘Very High Ionization’ (Fe-K) absorber?  Larger Mdot • Steady state winds not the whole story?

  30. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 20 ks Chandra HRC (blue) HI Contours Centaurus A (NGC5128) ‘Smoke Ring’M. Karovska et al 2002 Smoke Ring: R ~ 8 kpc; kT~0.6 keV LX~ 4 x 1038 erg/s Eth ~1.2 x 1055ergs ~100 Etot(wind) in NGC4051 Mgas ~ 106 Msol Includes swept up ISM • v~600 km/s; • t(outburst) 107 yrs • Impulsive injection? Merger ~ 107 yr • Only visible in Cen A (D=3 Mpc)

  31. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Tori

  32. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 3. A Larger Torus:Host Galaxy Scale

  33. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Obscuring Torus: What and Where? • Canonical donut? • Dynamic structure? • Tied to host? • Wind? • Aligned with disk? • Aligned with host? • Aligned with neither? Answers affect feedback

  34. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Urry C.M. & Padovani P. 1985 PASP, 107, 803. [706 ADS citations] Tori in AGNs • Clearly there is a flattened obscuring region in most AGNs • >20 year old result • Keel 1980, Lawrence & Elvis 1982, deZotti & Gaskell 1985, Antonucci & Miller 1985…. • Axisymmetry requires a torus • Butis this toroid the `donut’ shaped parsec-scale object usually invoked? Polarized broad emission lines in the Type 2 (narrow line) AGN NGC1068

  35. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 AGN Obscuring Torus What does a torus explain? • Hidden Broad Line Regions • Ionization cones • Ratio of type2/type1 AGNs ~ 4:1 Hidden Broad Emission Line Antonucci & Miller 1985 ApJ 297, 621 Tadhunter & Tsvetanov 1989 Nature 341, 422

  36. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 The Standard Torus • Molecular Torus posited by Krolik & Begelman (1988 ApJ 392, 702): • Large scale height: h/r~0.7 • r~1pc [set by dust sublimation radius] • NH~1024cm-2 ~ Compton thick

  37. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 UV from disk Typical em. Line cloud isotropicX-ray Typical observer Netzer 1987 MNRAS 225, 55 Torus Issues • How is donut supported? • Covering fraction >50%, yet cold (dusty) • Cloud-cloud collisions should flatten structure • Thick clumpy accretion needs Mtorus>MEddsee SgrA*Vollmer, Beckert & Duschl 2004 A&A 413, 949 • Can’t see accretion disk edge-on • Difficult for BEL polarization PA rotation - all type 1 AGNs are ~pole-on • Limb darkening can’t be used to explain ‘continuum energy deficit’ Netzer et al. 1985, ApJ 292, 143and ‘ionizing photon deficit’Binette et al. 1993 PASP 105, 1150

  38. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Torus believed to Align with Accretion Disk Ulvestad & Wilson 1984 ApJ 285, 439 DPA host - kpc radio • Radio Jets misaligned with host disk • Polarization aligned with radio jets Antonucci 1983 Nature 303, 158 • So obscurer not aligned with host disk

  39. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 NGC1068 Kinematics ‘ionization cones’ AGN CO warped disk Hollow ‘ionization cones’ Torus Invented for NGC1068 Yet not needed in NGC 1068 itself: • IRAM CO mapping suggests a warped disk on ~70pc scale Schinnerer et al. 2000 ApJ 533, 850 • NGC 1068 has hollow `ionization’cones Crenshaw & Kraemer 2000 ApJ 532, L101 I.e. Matter bounded - a true outflow cone • Not ISM illuminated by collimated continuum • Still leaves type1:type2 ratio

  40. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 DPA kpc - pc 0o 45o 90o Middelberg et al. 2004 Radio alignments are problematic • kpc radio Jets misaligned with VLBI pc-scale radio* Middelberg et al. 2004 • Too few objects to test alignment with host disk • What about polarization? • Coming up! *Some concerns about self-calibration technique (J. Gallimore, private communication)

  41. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 ESO0103-G35 NGC7314 NGC5506 NGC2992 NGC526A Is the Torus Instead Aligned with the Host Galaxy Disk? • Obscured AGN hosts preferentially edge-on? • E.g. “Piccinotti Sample” • 32 AGNs Hard X-ray Selected (2-10keV) • 5 `Narrow Emission Line Galaxies’ • Large NH • Red optical spectra • Seyfert 1.8, 1.9 • Ha/Hb(broad)>5

  42. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 deZotti & Gaskell 1985 A&A 147, 1 reddened log(Ha/Hb) Face-on Host galaxy Axial ratio Obscuration Aligned with Host Disk Lawrence & Elvis 1982 ApJ 256, 410 log(Hb/LX) Hb absorbed log(L3.5mm/LX) Edge-on Edge-on Face-on Host galaxy Axial ratio

  43. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Show up as IRAS AGNs Host galaxy Axial ratio Obscurer is Aligned with Host Disk Kirhakos & Steiner 1990, AJ 99 1722 Thompson & Martin 1988 ApJ 330, 121 PA(polarization) - PA(host disk) Host galaxy Axial ratio The missing edge-on type 1 AGNs Strong continuum polarization

  44. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Host Galaxy Aligned Obscurer • dominated by galaxy potential • too large to be outer limit of BELR, disk? • large scale height from warps? • Solves problems: • unobscured lines of sight sample all disk inclinations (for random disk/host orientation) • photon, energy deficits may be solved • AGN continuum reaches host galaxy ISM (= torus) • Host ISM may be blown away • but not instantly else no obscuration will be seen

  45. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 4. A Smaller Torus:Disk Wind Scale

  46. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 DNH /NH NH (1022) Another Possibility: A Compact Torus • Virtually all obscured AGN have variable NHRisaliti, Elvis & Nicastro, 2002 • 5 < Nclouds < 10 • 2 timescales: ~< 6 months, ~5 years • Inner and Outer obscuring tori? Structure Function 3 examples…

  47. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 NGC4151: ~1day NH variations Puccetti et al. 2005 DNH ~ 2-3 x1022cm-2 in ~ 2 days BeppoSAX 1996 July 150ksec A C B D NH 1022cm-2 1 2 5

  48. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 RXTE PCA: NGC 4388 5 months 4 hours NGC4388: 4 hour NH variations Elvis et al. 2004 ApJ 615, L25 RXTE 1 day outburst; NH 1/10 normal DNH ~ 1022cm-2 in 4 hours Expected ~ 1/year for ~1 day if due to Poisson clouds moving at BELR velocities

  49. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 NGC 1365 Compton thin Constant extended component XMM ct cm-2 s-1 Compton thick 0.1 1 keV 10 Hardness Ratio 0 20 40 60 t (ksec) NGC1365: Rapid Compton-thick/-thin transitions • Normally Compton-thick: e.g. Chandra 2002 Dec • Compton-thin 3 weeks later- XMM • Compton-thick 3 weeks later still- XMM • DNH~1024cm-2 • Evidence for DNH~1023cm-2 in 6 hours

  50. AGN and Galaxy Evolution, Castel Gandolfo, 3-6 October 2005 Mol. Torus radius/rg NGC4151, NGC4388, NGC1365 BELR density Rapid Variability - Small Size • Short timescale hard to reconcile with parsec-scale absorber: even dense clouds move too slowly • Assume Keplerian motion of obscuring matter R < 104 r102 t42 Rs (t4 in 4-hours, r in cm-3)

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