Out

line

Quasar Outflows Doron Chelouche (IAS and TAU)

•Introduction

•Model

•NGC 3783

•Conclusions

Quasar Outflows: The X-ray perspective

Doron Chelouche

Institute for Advanced Study, Princeton NJ

(currently at: Tel-Aviv University, Israel)

Proga et al. 2000

Intro

duct

ion

Quasar Outflows Doron Chelouche (IAS and TAU)

Phenomenology:

•blueshifted absorption lines

•common in type-I quasars

•velocity range: 102-105 km s-1

BAL flows

Relevant to:

•Accretion-ejection processes

•Quasar structure (unification)

•Galaxy and cluster formation

Kaspi et al. 2002

NAL flows

Elvis M.

Determining the flow properties is essential for investigating these issues

Mod

elQuasar Outflows Doron Chelouche (IAS and TAU)

Aim: to determine the flow properties

Mean: by comparing model predictions to observations

Kaspi et al. 2002

Flow properties are poorly constrained

predictionsmethod

Spectral features(line, continuum)

Flow properties(v, )

photoionization

dynamics

•

M

Mod

elSolution: Combine detailed photoionization and dynamical calculations

Quasar Outflows Doron Chelouche (IAS and TAU)

{ }

,...),(

...1

0)()(

0)()(

,

vrdrdPga

drdvv

TionsrecombinatTationsphotoioniz

TcoolingTheating

rad

iXXX

iii

ii

ρρρ

=

+−−=

=−

=−∑

Next step: Comparing to observations

Quasar Outflows Doron Chelouche (IAS and TAU)

NG

C 3

783

•>100 absorption lines

•Continuum absorption

•Continuum variability

Rest wavelength (A)

Pure photoionization models

George et al. 98

Krongold et al. 03

Netzer et al. 03

?????

What is the physics characterizing the multiphase flow?

Kaspi et al. 2002

Arav 1996

Quasar Outflows Doron Chelouche (IAS and TAU)

Ionization potential

Kaspi et al. 2002NG

C 3

783The dynamical viewpoint

de Kool et al. 2002

Calculating…mixed phases reminiscent

of a turbulent medium

],[ ; maxmin ρρξρ β∝

Reeves et al. 2003

Summary of X-ray results for NGC3783

•The flow is energy driven (radiative acceleration is negligible)

•The flow is launched beyond the accretion disk (torus association?)

•The mass loss rate is similar to/smaller than the mass accretion rate (much smaller than previous estimates)

•The flow density structure is reminiscent of a turbulent ISM (triggered by the central star cluster?)N

GC

378

3Quasar Outflows Doron Chelouche (IAS and TAU)

Crenshaw et al. 1999

conc

lusi

ons

Quasar Outflows Doron Chelouche (IAS and TAU)

•Studying quasar outflows is important for understanding accretion phenomena, quasar structure, and galaxy/cluster formation

•High resolution and S/N X-ray grating spectra provide a unique view of such flows

•Realistic spectral fits accounting for hundreds of line and continuum features are feasible

•Combined dynamical, photoionization, and spectral modeling can reveal the physical properties of the ouflowing gas

•Similar models can be used to study gas dynamics in other systems (e.g., X-ray binaries)Th

ank

you!