getting it all together: paradigms for agns

Hagaifest, Tel Aviv, 22 February 2006

Getting it all together:Getting it all together:Paradigms for AGNsParadigms for AGNs

Martin ElvisHarvard-Smithsonian Center for Astrophysics


AGN as a panacea?o overcooling problem/LF shapeo galaxy red sequence & bimodalityo decline of bright QSO’s

o MBH- relation

o QSO and galaxy ‘downsizing’o cluster cooling flow problem/entropy floor

R. Somerville: OIR lunch talk, 3/29/05


Two Paradigms for AGNs: 1. Obscuring Donut Tori 2. Accretion Disk Winds

Paradigms give context to observationsOnly useful when they make predictions

Bagel


Winds and Tori affect FeedbackQuickTime™ and a

TIFF (LZW) decompressorare needed to see this picture.

Murray, Chiang, Grossman & Voit 1995

• Winds:1. Location: mass, KE, mv, Z rates

2. Geometry: fc, vescape, escape route20%

• Torus: blocks 80% feedback to ISM


1. Bagel Tori:A Revisionist Approach


Modifying the Paradigm :I. A Disk Scale Torus


NGC1365: Rapid Compton-thick/-thin transitions• NH~1024cm-2 in 3 weeks • NH~1023cm-2 in 6 hours

0.1 1 10E (keV)

Compton thick

Constant extended component

Compton thin

XM

M c

t cm

-2 s

-1

NGC 1365

t (ksec)20 40 600

Har

dnes

s R

atio

Risaliti et al. 2005 ApJ 623, L93


Rapid NH Variability Small Obscurer Size

• 3 cases: • NGC1365, Risaliti et al. 2005

• NGC4388, Elvis et al. 2004

• NGC4151, Puccetti et al. 2006

• Hard for dusty absorber on parsec-scale

• Assume Keplerian motion of obscuring matter

R < 104102 t4

2 Rs

(t4 in 4-hours, in cm-3)

• BELR scale

NG

C41

51, N

GC

4388

, NG

C13

65

BELR

density

radi

us/r

g

Mol. Torus


Is the Inner Torus the Disk Wind?

• Eases torus physics:• Wind is steady state, but not static

• No problem supporting obscuring structure

• Large covering factor easy to create

• oversupply of BEL clouds? • Hydromagnetic wind?

• Low dust-to-gas ratio natural• If disk from ISM, not disrupted

stars

• Aids Feedback:• Radiation still blocked

• Matter escapesHost ISM can be affected

Kartje, Königl & Elitzur, 1999 ApJ 513, 180


Modifying the Paradigm :II. Host Galaxy Scale Torus


Standard Torus: 2 more Issues

• Disk - torus co-aligned• Equatorial wind can’t escape• Can’t see accretion disk edge-on

• Difficult for BEL polarization PA rotation - all type 1 AGNs are ~pole-on

• Viewing angle Netzer et al.1985, ApJ 292, 143 can’t be used to explain

‘continuum energy deficit’ and ‘ionizing photon deficit’ Binette et al. 1993

PASP 105, 1150

Netzer 1987 MNRAS 225, 55

Typical em. Line cloud

UV from disk

isotropicX-ray

Typical observer


Obscurer is Aligned with Host Disk

Kirhakos & Steiner 1990, AJ 99 1722

The missing edge-on type 1 AGNs

Host galaxy Axial ratio

Show up as IRAS AGNs

Host galaxy Axial ratio

Strong continuum polarization

PA(polarization) - PA(host disk)

Thompson & Martin 1988 ApJ 330, 121

Lawrence & Elvis 1982 ApJ,


Accretion Disk misaligned with Host diskUlvestad & Wilson 1984 ApJ 285, 439

PA host - kpc radio


Misaligned Obscurer & Accretion Disk

• Unobscured lines of sight sample all disk inclinations

• Netzer deficit can be solved

• AGN continuum reaches host ISM = torus

• Host ISM may be blown away,

but not instantly, else no obscuration will be seen

Host Galaxy Disk


2. Testing the Accretion Disk Wind

ParadigmMass loss rate in wind unknown to 106:

NELR - accretion disk


A measured WA radius in NGC4051


Time Evolving Photoionization measures RNicastro et al. (1999)Response is not instantaneous:

‘Ionization time’ and ‘Recombination time’measure ne independent of Ux and so measures R

Step function change

Gradual WA response


Warm Absorber Warm Absorber VariabilityVariability gives physics gives physics

Fully characterized plasma:• Density ne: recombination/ionization time lag to cont. changes

• Radial Distance, r: ne, ionization parameter (nph /ne), Lcont

• WA thickness, r: NH, ne

• WA temperature, T: amplitude of response to cont. changes.

• Pressure, P: ne, T

• Mass outflow rate, mdot: ne, velocity v

See: Mathur, Elvis & Wilkes 1995 ApJ 452, 230.

Nicastro, Fiore, Perola & Elvis 1999, ApJ 512, 184


NGC4051: Rapid Variability in XMM

~30 ksec

High State HS

Low State LS

XMM-Newton Reflection Grating Spectrometer (RGS) HS and LS spectra…


4X flux increasein ~30 ksec

NGC4051 RGS: strong WA spectral changes

WA is DENSE and COMPACT


4X flux increase

RGS Data EPIC Data

Comparing RGS & EPIC spectral changes

First noted by Ogle et al. 2004

Fe L shell UTA


Krongold et al., 2005, ApJ, submitted

NGC 4051: Two Warm Absorber Components in Photoionization Equilibrium

log Ux(t), measured

log Ux(t), predicted

from photoionization

equilibrium

High Ionization phase

Low Ionization phase

XMM EPIC Light Curve


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

daysHard to get with partial covering:

X-ray source is small


Measurement of HIP ne and hence R

• At extremes (high and low) HIP is out of photoionization equilibrium teq

i,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)R(HIP) = (1.3- 2.6)x 10 = (1.3- 2.6)x 101515 cm cm = (0.5-1.0) light = (0.5-1.0) light

daysdays


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

either the LIP is embedded in the HIP - pressure balance • or the LIP is a boundary layer of the HIP


Scale Map of an AGN: outer

• 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 H broad emission line region (BELR) • R(H) = 5.9 light-days (Peterson et al. 2000)

light-dayslight-days 5510101515

HIP

~HeII ~HeII

BELRBELR

HH BELBELRR

Dusty molecular

torusLIP

Dust sublimation radius


Scale Map of an AGN: inner

• RHIP ~ 0.5-1 light-day ~2200 - 4400 Rg • Mbh=1.9+/-0.78 x 106 Msol (Peterson et al. 2004) *face-on?

Disk winds arise on accretion disk scale• Consistent with high-ionization BEL size

• R(HeII) ~< 2 light days. HeII blueshift ~400km/s = wind signature?

• Thin: R = 10% - 20% R

rrgg 10010000

20020000

30030000

40040000

50050000

HIPgravitationagravitationally unstablelly unstableHeII BEL

NGC4151 D+Ea CIII] abs.


WA radial velocity < escape velocity!

Arav, Korista & de Kool 2002, ApJ 566, 699

Arav, Korista, de Kool, Junkkarinen & Begelman 1999 ApJ 516, 27

CIV doublet 2:1 ratio

Departures from 2:1 ratio give covering factor

Strong UV Evidence for Transverse winds


AGN Cosmological Feedback• Location determines mass loss rate

Mdotout = 0.8 mp NH vr R f()

= 2-5% mdot(acc)• lower than 10% normally assumed

• Total WA mass deposited in Intergalactic Medium:• If: lifetime =108yr Mtot(out)=(0.4-2)x104 Msol in NGC4051

• Mdot(out) M(BH) for constant Rg

• Quasar MBH = 108-109 Msol

Mtot(quasar) = 106-107 Msol • comparable with ULIRGs

Krongold et al. 2006 ApJ, submitted


Confirms Major Features of Elvis ‘funnel wind’Elvis 2000 ApJ 545, 63; 2003 astro-ph/0311436

Conical geometry

Pressure balance

Becoming a secure basis for physical wind models: will allow extrapolation

Thin

Wind


Funnel Disk Wind Model Predictions

X-ray ‘Warm Absorbers’

0. WA AGN is non-spherical

1. Same gas as UV NALs

2. Outflows

3. Narrow lines

4. Ionization consistent with NALs

5. Few (2-3) phases of (T, P)

6. Pressure balance between phases

Broad Emission Line Region (BELR)

7. Rotating, large scale height

Broad Absorption Line Region (BALR)

8. Scattering in normal quasars -

BELs, continuum, Fe-K

9. Rotating

UV Narrow Absorption Lines (NALs)

10. Common in high L quasars too

11. v ~ 1/2 vdetach (BAL)

12. Close to continuum source

Elvis 2000 ApJ 545, 63; 2003 astro-ph/0311436


Caveats to Mass Loss Rates• Only one object

• ‘Narrow Line Seyfert 1’• Unusually distant BELR ~10xRg(normal) higher Mdotout

• Unusally weak wind? (= eigenvector 1?)

• Low Mbh 1.9 x 106 Msol low Mdotout? • Mdotout Scales with BH mass if at constant Rg

– Mdotout = 0.8 mp NH vr R f() = A Mbh

• ‘Very High Ionization’ (Fe-K) absorber? Larger Mdot • Partial covering? Nahum

• Steady state winds not the whole story?• Cen A ring


Quasar Physics: The Big QuestionsQuasar Physics: The Big Questions1. massive black hole Proposed: Lynden-Bell 1969Demonstrated in AGN: Wandel & PetersonQuestions: Origin, co-evolution,

spin, Penrose process; GR tests

2. accretion disk ?Proposed: Lynden-Bell 1969, Pringle & Rees 1972,

Shakura & Sunyaev 1972Demonstrated?: Shields78, Malkan82, Eracleous?Questions: proof. Viscosity=(MRI?), ang.mom,RIAF

3. relativistic jet Proposed: Rees 1967 [PhD], Blandford & Rees 1974Demonstrated: Cohen et al. (VLBI)Questions: acceleration mechanism

(Penrose/Blandford-Znajek?)

4. Disk wind atmosphereBELR, WA,BALs, NELR

Proposed: many times (from Mushotzky et al.1972 on)

Demonstrated: Krongold et al. 2006 - NGC4051

Questions: acceleration mechanism; M/Medd, eigenvector 1, impact on environment

5. Obscuring torusProposed: Lawrence & Elvis 1982Demonstrated: Antonucci & Miller

1985 Questions: Bagel, Disk and/or host


AGN Winds & Tori: Paradigm Shifts

Accretion Disk Winds • RULES OUT: NELR, torus, continuous

• R = few 1000 Rs = HiBEL region?

•Thin: R/R = 10%-20%

• Pressure balance

• Conical flows/funnel-shaped

• BAL-like NH down cone Elvis 2000

• Feedback: Mass, KE, Z flux are smal

•lstill a lot of extrapolation involved

• AGN Winds are not a panacea

Bagel Tori: Need 2 types of torus

Large (kpc), host oriented

Torus is host ISM

Random alignments allow radiation to impact host ISM

Small (104 Rg) disk orientedWind can affect host ISM,but not radiation

AGN structure details matter

to cosmology…

and can be solved


Imaging QuasarsImaging Quasars

Low z BELR sizes are ~0.1 mas

Resolvable with planned ground interferometers

VLT-I, Ohana

Ideal telescopes:

•Image the wind in space and velocity

•5 km-10 km IR 2m interferometer at ‘Dome C’ in Antartica

•0.5-1km UV space interferometer

= NASA ‘Stellar Imager’

Quasar community should hi-jack SI!

Sizes are implicit in:

Peterson et al. 1999 ApJL 520, 659.

Kaspi et al. 2001 ApJ 533, 631

What we really want is to look at quasar atmospheres

SOLVE QUASAR ATMOSPHERES

No more fancy indirect deductions!

Elvis & Karovska, 2002 ApJ


Thermal Pressure Driven

As in Supernovae(but continuous)

Vmax ~ Vsound ~ 100km/s

Isotropic pressure

~100% filling factor

Krolik & Kriss 1995; Balsara & Krolik 1993; Begelman, deKool & Sikora 1991 CR acceleration

Magnetic ‘slingshot’

As in T Tauri stars

Vmax ~ c

Flows along field lines

Uses scary B fields

Blandford & Payne 1982; Emmering, Blandford & Shlosman 1992; Königl & Kartje 1994; Bottorf et al. 1997; Everett, Königl, Kartje 2001; Proga 2000; Proga 2003

3 Ways to Accelerate Quasar Winds

Radiation Line Driven

As in O-stars

Vmax ~ 2x VKepler ~ 10000km/s

Radial pressure (at large R)

Force is highly ionization dependent

Mushotzky, Solomon & Strittmatter 1972 BALs; Wolfe 1974 BELR; deKool & Begelman 1995; Murray, Chiang, Grossman & Voit, 1995 BALs; Murray & Chiang 1995 Warm Absorbers; Chiang & Murray 1996 BELR; Proga , Stone & Drew 1999 CVs; Proga 2000; Proga 2003 BELR; Chelouche & Netzer


AGN as Dust FactoriesAGN as Dust FactoriesElvis, Marengo & Karovska, 2002 ApJ, 567, L107

• BEL gas expands in an outflowing wind from high densities

• Cools to <1000 K while still at high pressure

• BEL adiabats track through dust formation zone of AGB stars

• Applies to Carbon-rich and Oxygen-rich grains

• BELR wind must make dust• Central continuum less important than for

AGB star dust

• NGC1068 11.7m dust emission follows ENELR Galliano et al. 2003

• Is this BELR created dust?

• What are the signatures of BEL-origin vs ISM-origin dust?

Cooling BEL clouds

Oxygen rich dustCooling BEL clouds

Carbon rich dust

NGC1068 11.7m. Tomono 2001


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 1055 ergs

~100 Etot(wind) in NGC4051

Mgas ~ 106 Msol Includes swept up ISM

v~600 km/s; t(outburst) 107 yrsImpulsive injection? Merger ~ 107 yrOnly visible in Cen A (D=3 Mpc)

20 ks Chandra HRC (blue)

HI Contours


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

R()

rR()

dr=vdt


BAL = end-on NAL?2

0

1

0

0 )()(

−−

⎟⎟⎠

⎞⎜⎜⎝

⎛⎟⎟⎠

⎞⎜⎜⎝

⎛=

RR

vRv

nRn HH

dr=vdt

R()

rR()

NH(obs)

NH(cone)

Mass Conservation

2/11

0

2

00

111)(

⎪⎭

⎪⎬⎫

⎪⎩

⎪⎨⎧

⎥⎥⎦

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⎢⎢⎣

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⎞⎜⎜⎝

⎛+=

−

∞

RR

vv

vRv Eq. of Motion

2-2422

0

00

cm1010~

1

N −

⎟⎟⎠

⎞⎜⎜⎝

⎛+

=∞

∞

vvRnH

H

HIP LIP


Standard Torus: Standard Issues

• How is donut supported? • Covering fraction >50%,

yet cold (dusty)

• Cloud-cloud collisions should flatten structure

• Thick clumpy accretion needs Mtorus>MEdd see SgrA*

Vollmer, Beckert & Duschl 2004 A&A 413, 949


Mass Outflow Rates

MdotHIP =

(4.3 - 9.2) x 10-5 M s o l yr-1

MdotLIP < 6 x 10-5 Msol๏yr-1 = 0.02 Mdotacc

Mdotout = 2% - 5% Mdotacc

Mdotout insensitive to unless >75o, <10o

Mdotout = 0.8 mp NH vr R f()

PHASE (Krongold et al., 2003)

NGC 3783Bound-free edges only

full PHASE model

Black line: includes bound-bound lines

NH >10 times smaller with new models

• If lifetime =108yr Mtot(out)=(0.4-2)x104 Msol

• Mdotout scales with BH mass if at same Rg

MBH(NGC4051) = 2 x 106 Msol

for MBH = 108-109 Msol

Mtot(quasar) = 106-107 Msol

KEtot(wind) = 1055 erg

small, but comparable with ULIRGs


AGN & Cosmological Feedback• AGN: Zero to hero in cosmology

• Invoked in many areas:• Co-evolution of SMBHs & their hosts

• Prevention of star formation in mergers

• Creation of the upper mass limit for galaxies

• Inhibition of vooling flows

• Enrichment of the IGM

• Creation of dust at high z

R. Somerville: CfA lunch talk, March 2005

Data

Bimodal galaxy colors

Simulation

getting it all together: paradigms for agns

Documents

accretion disk edge

accretion disk windsparadigms

torus host ism

disk scale torusngc1365

density ne

wind unknown

hydromagnetic wind

gas ratio naturalif