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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?