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Quasar Outflows Doron Chelouche (IAS and TAU) Quasar Outflows: The X-ray perspective Doron Chelouche Institute for Advanced Study, Princeton NJ •Introduction Outline (currently at: Tel-Aviv University, Israel) •Model •NGC 3783 •Conclusions Quasar Outflows Doron Chelouche (IAS and TAU) Phenomenology: BAL flows NAL flows •blueshifted absorption lines •common in type-I quasars Introduction •velocity range: 102-105 km s-1 Relevant to: Kaspi et al. 2002 •Accretion-ejection processes •Quasar structure (unification) •Galaxy and cluster formation Proga et al. 2000 Elvis M. Determining the flow properties is essential for investigating these issues Quasar Outflows Aim: Doron Chelouche (IAS and TAU) to determine the flow properties Mean: by comparing model predictions to observations Kaspi et al. 2002 Model predictions method photoionization dynamics Spectral features (line, continuum) Flow properties (v, M) Flow properties are poorly constrained Quasar Outflows Doron Chelouche (IAS and TAU) Solution: Combine detailed photoionization and dynamical calculations heating (T ) cooling (T ) 0 i i i photoionizations Xi (T ) recombinations X i (T ) 0X ,i dv 1 dP arad g ... dr dr (r , v,...) Model v Next step: Comparing to observations Quasar Outflows Doron Chelouche (IAS and TAU) •>100 absorption lines •Continuum absorption •Continuum variability Kaspi et al. 2002 Pure photoionization models NGC 3783 George et al. 98 Krongold et al. 03 Netzer et al. 03 ????? Rest wavelength (A) What is the physics characterizing the multiphase flow? Quasar Outflows Doron Chelouche (IAS and TAU) The dynamical viewpoint NGC 3783 Arav 1996 de Kool et al. 2002 Calculating… mixed phases reminiscent of a turbulent medium ; [ min , max ] Ionization potential Kaspi et al. 2002 Quasar Outflows Doron Chelouche (IAS and TAU) Summary of X-ray results for NGC3783 NGC 3783 •The flow is energy driven (radiative acceleration is negligible) •The flow is launched beyond the accretion disk association?) (torus •The mass loss rate is similar to/smaller than the mass accretion rate (much smaller than previous estimates) Crenshaw et al. 1999 •The flow density structure is reminiscent of a turbulent ISM (triggered by the central star cluster?) Reeves et al. 2003 Quasar Outflows Doron Chelouche (IAS and TAU) •Studying quasar outflows is important for understanding accretion phenomena, quasar structure, and galaxy/cluster formation conclusions Thank you! •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)