1. AGN Outflows: Observations Doron Chelouche (IAS) The Physics of AGN Flows as Revealed by Observations Doron Chelouche* Institute for Advanced Study, Princeton Outline *Chandra Fellow Observations Modeling Testing Results Questions

2. Crenshaw et al. 1999 Korista et al. (1993) BALQSOs: 15-25% of QSOs 0% of Seyferts Velocities of order 10 4 km/s Wide troughs Suggestive of radiation pressure acceleration NALQSOs: ~30% of quasars ~50% of Seyferts Velocities of order 10 3 km/s Narrow troughs Das et al. 2005 [OIII] HαHα AGN Veilleux et al.2001 Velocities of order 10 3 km/s Observed in nearby objects AGN Outflows: Observations Doron Chelouche (IAS) observations Observations

3. 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 observations

4. Mass loss rate Implications for AGN fueling Understand how much (enriched) gas is injected into the host and IGM Launching radius Relation to other quasar components (Accretion disk? BLR? Torus? NLR?) Because it’s there… AGN Outflows: Observations Doron Chelouche (IAS) Kinetic luminosity Do quasars emit more than just photons? What are the effects on the host and on the IGM – quasar feedback. motivation Why do we care?

5. 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, N H 3) Measure the velocity, v 4) 5). 6). BUT… Dessart & Owocki 2005 modeling Do photoionization models help?

6. AGN Outflows: Observations Doron Chelouche (IAS) NOT MUCH… Since the relevant physics is not included Kaspi et al. (2002) modeling

7. AGN Outflows: Observations Doron Chelouche (IAS) Photoionization & dynamical modeling modeling

8. 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. modeling

9. thermal momentum vs. thermal One simple test… AGN Outflows: Observations Doron Chelouche (IAS) Radiativly driven Thermally driven Kaspi et al. (2002) testing

10. AGN Outflows: Observations Doron Chelouche (IAS) Netzer et al. (2003) 30xsolar (for the low ionization component) thermal testing

11. AGN Outflows: Observations Doron Chelouche (IAS) Optically thin flows Optically thick flows collimated Thermally driven Another simple test… Temperature dependent velocity!

12. AGN Outflows: Observations Doron Chelouche (IAS) Ionization potential Kaspi et al. 2002 Suggests flow components are co-spatial testing NGC5548 NGC7469 NGC4151 NGC3783

13. results AGN 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

14. AGN Outflows: Observations Doron Chelouche (IAS) results

15. AGN Outflows: Observations Doron Chelouche (IAS) Das et al. 2005 Everett & Murray 2006 Adiabatic cooling problem? results

16. AGN Outflows: Observations Doron Chelouche (IAS) questions 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?