AGN Outflows: Observations Doron Chelouche (IAS)

The Physics of AGN Flows as Revealed by Observations

Doron Chelouche*

Institute for Advanced Study, Princeton

Out

line

*Chandra Fellow

•Observations

•Modeling

•Testing

•Results

•Questions

Crenshaw et al. 1999

Korista et al. (1993)

BALQSOs: 15-25% of QSOs 0% of Seyferts

Velocities of order 104 km/sWide troughsSuggestive of radiation pressureacceleration

NALQSOs: ~30% of quasars ~50% of Seyferts

Velocities of order 103 km/sNarrow troughs

Das et al. 2005

[OIII]

Hα

AGN

Veilleux et al.2001

Velocities of order 103km/sObserved in nearby objects

AGN Outflows: Observations Doron Chelouche (IAS)

obse

rvat

ions

Observations

AGN Outflows: Observations Doron Chelouche (IAS)

The X-ray Revolution

•Many lines & edges•Large range of gas temperatures •Direct view of the ionizing continuum•Source variability

obse

rvat

ions

Mass loss rate•Implications for AGN fueling•Understand how much (enriched) gas is injected into the host and IGM

M

Launching radius•Relation to other quasar components (Accretion disk? BLR? Torus? NLR?)

r

Because it’s there…

AGN Outflows: Observations Doron Chelouche (IAS)

KLKinetic luminosity

•Do quasars emit more than just photons?•What are the effects on the host and on the IGM – quasar feedback.

mot

ivat

ion

Why do we care?

How to estimate the flow parameters?

AGN Outflows: Observations Doron Chelouche (IAS)

Crenshaw et al. 1999

1) Fit a (Gaussian) absorption line

2) Estimate the column density, NH

3) Measure the velocity, v

4)

5) .

6) .

13221 km/s101cm101

1.0

yrM

v

pc

rNCM HIg

HI

BUT…

410~

f

f MM

Dessart & Owocki 2005

mod

elin

g

2vMLK

?r

Do photoionization models help?

AGN Outflows: Observations Doron Chelouche (IAS)

NOT MUCH…

Since the relevant physics is not included

2rLTT

Kaspi et al. (2002)

),/( 2HNnrLphysicsphysics

mod

elin

g

AGN Outflows: Observations Doron Chelouche (IAS)

)const (e.g.,Geometry

on conservatiEnergy

2

vr

constE

gaaaadr

dvv

ii

CRradmagneticgas

Photoionization & dynamical modelingm

odel

ing

AGN Outflows: Observations Doron Chelouche (IAS)

Do we really need that level of sophistication?(the case of stellar winds)

•Asymmetric UV emission lines

•Symmetric X-ray lines

Owocki et al.

KK LL

MM

1.0

0.1

mod

elin

g

thermalmomentum vs. thermal

One simple test…

AGN Outflows: Observations Doron Chelouche (IAS)

v

r

Radiativly driven

Thermally driven

Kaspi et al. (2002)pcr 1.0~ pcr 1~

test

ing

AGN Outflows: Observations Doron Chelouche (IAS)

Netzer et al. (2003)

pcr 1

gFrad /

T

1

30xsolar

(for the low ionizationcomponent)

thermal

test

ing

test

ing

AGN Outflows: Observations Doron Chelouche (IAS)

v

T

Optically thin flows

Optically thick flows

collimated

v

effT

Thermally driven

Another simple test…

Temperature dependent velocity!

AGN Outflows: Observations Doron Chelouche (IAS)

Ionization potential

Kaspi et al. 2002

Suggests flow components are co-spatialtest

ing

NGC5548

NGC7469

NGC4151

NGC3783

resu

ltsAGN Outflows: Observations Doron Chelouche (IAS)

A proposed model: Multiphase thermal wind

NGC 5548 MCG-6-30-15 NGC 3783

•Photo-heating, radiative cooling, adiabatic cooling (NLTE)

•Spherical geometry

•Absorption and emission spectrum (escape probability)

•Radiation pressure force

AGN Outflows: Observations Doron Chelouche (IAS)

resu

lts

NLRlaunchBLR

BolometricK

accretionoutflow

RrR

LL

MM

310

AGN Outflows: Observations Doron Chelouche (IAS)

Das et al. 2005

Everett & Murray 2006

NLRlaunchBLR

BolometricK

outflow

RrR

LL

yrMM

2

1

10~

1~

Adiabatic cooling problem?

resu

lts

AGN Outflows: Observations Doron Chelouche (IAS)

ques

tions

•What is the source of the outflow? Torus? Stars?•Have we accounted for all heating processes?•Is thermal instability necessary to observe outflows?•Where is the dust?•What is the source for quasar feedback?•What happens in high-L quasars?•What happens in LINERs?•Is high-T gas prerequisite for “high” velocity outflows?•What is the relation to UV flows?