Christian Knigge Department of Physics & Astronomy University of Southampton Christian Knigge University of Southampton Southampton Nick Higginbottom James Matthews Sam Mangham STScI Knox Long QUB Stuart Sim UNLV Daniel Proga Quasar Unification Via Disk Winds: From Phenomenology To Physics

Christian Knigge Department of Physics & Astronomy University of Southampton Outline Quasar Unification – The Disk Wind Paradigm Testing the Paradigm: The Quasar Radiative Transfer and Ionization Project – Goals – Tools – Results – Plans Summary

Christian Knigge Department of Physics & Astronomy University of Southampton AGN/QSO Unification Evidence for Outflows: Broad Absorption Lines Reichard et al. (2003) ≈15% of QSOs show broad, blue-shifted UV absorption features (Weymann+91; Hewett+03; Reichard+03; Knigge+08;Allen+11…)

Christian Knigge Department of Physics & Astronomy University of Southampton AGN/QSO Unification Other Evidence for Outflows Mini-BALs and blueshifted NALs X-ray UFOs Hamann+97 Chartas+02 Mehdipour+10 X-ray warm absorbers

Christian Knigge Department of Physics & Astronomy University of Southampton AGN/QSO Unification Could the outflow also produce broad emission lines? QSO BAL QSO BALs UV emitting disk BELs Murray, Chiang+95,97,98

Christian Knigge Department of Physics & Astronomy University of Southampton AGN/QSO Unification The Disk Wind Paradigm Elvis 2000

Christian Knigge Department of Physics & Astronomy University of Southampton AGN/QSO Unification The Disk Wind Paradigm Knigge+15

Christian Knigge Department of Physics & Astronomy University of Southampton The Quasar Radiative Transfer and Ionization Project Test the viability of disk-wind-based AGN/QSO unification Determine the significance of disk winds for feedback Overall Project Goals

Christian Knigge Department of Physics & Astronomy University of Southampton PYTHON: A 3-D Monte Carlo ionization and radiative transfer code ( (Long & Knigge 2002; Higginbottom+13+14; Matthews+15) –Designed specifically for simulations of astrophysical outflows –Arbitrary geometry and velocity fields Built-in kinematic models (e.g. bi-conical rotating disk wind) Read in external dynamical models (e.g. from hydro codes) –Arbitrary type and number of radiation sources, including Optically thick accretion disk (BB or stellar atmosphere) X-ray emitting corona (PL) –Solves for temperature and ionization state through the outflow Thermal equilibrium (radiative and adiabatic processes) Ionization equilibrium (radiative and collisional processes) –Predicts emergent spectra and line profiles QUARTZ Tools

Christian Knigge Department of Physics & Astronomy University of Southampton QUARTZ PYTHON: Monte Carlo Ionization and Radiative Transfer

Christian Knigge Department of Physics & Astronomy University of Southampton Can disk wind models reproduce UV broad absorption lines? (Higginbottom+13) What are the implied mass-loss rates and energetics? ( Higginbottom+13) What is the wind driving mechanism? (Higginbottom+14) Can disk wind models match reverberation mapping data? (Mangham+15) Can the same disk winds –O–Operate in the presence of strong X-rays? (Matthews+15) –P–Produce broad UV/optical emission lines? (Matthews+15) QUARTZ Results and Plans See James Matthews’ Talk!

Christian Knigge Department of Physics & Astronomy University of Southampton QUARTZ Project I: A Simple Benchmark Model for BALQSOs Higginbottom+13

Christian Knigge Department of Physics & Astronomy University of Southampton QUARTZ Project I: A Simple Benchmark Model for BALQSOs Higginbottom+13 + Benchmark model produces realistic UV broad absorption lines –R–Requires – sufficient to produce feedback -- But BALs only exist for weak L X – Otherwise outflow becomes over-ionized -- No strong broad emission lines See James Matthews’ talk for a possible solution for both issues! Cool & Dense Slow Outflow Fast Rotation Hot & Dilute Fast Outflow Slow Rotation

Christian Knigge Department of Physics & Astronomy University of Southampton Can disk wind models reproduce UV broad absorption lines? (Higginbottom+13) What are the implied mass-loss rates and energetics? ( Higginbottom+13) What is the wind driving mechanism? (Higginbottom+14) Can disk wind models match reverberation mapping data? (Mangham+15) Can the same disk winds –O–Operate in the presence of strong X-rays? (Matthews+15) –P–Produce broad UV/optical emission lines? (Matthews+15) QUARTZ Results and Plans

Christian Knigge Department of Physics & Astronomy University of Southampton QUARTZ Project II: A full ionization and radiative transfer calculation for a hydrodynamic line-driven disk wind model Proga+08

Christian Knigge Department of Physics & Astronomy University of Southampton QUARTZ Project II: A full ionization and radiative transfer calculation for a hydrodynamic line-driven disk wind model + Hydrodynamic modelling predicts a strong line-driven disk wind + Strong broad absorption lines -- Treatment of ionization and radiative transfer is highly approximate  This really matters for line-driven winds! Proga+04

Christian Knigge Department of Physics & Astronomy University of Southampton Higginbottom+14 Proga+04 Sim+11 QUARTZ Project II: A full ionization and radiative transfer calculation for a hydrodynamic line-driven disk wind model The ionization state of the outflow is much higher than assumed in the hydro model –cf Sim+11 No significant broad absorption or emission lines are produced Line-driving cannot operate in this outflow This does not mean that line-driven disk winds cannot exist! BUT: Need self-consistent radiation- hydrodynamics to reliably model line-driven disk winds! (Higginbottom et al, in prep) Higginbottom+14

Christian Knigge Department of Physics & Astronomy University of Southampton Can disk wind models reproduce UV broad absorption lines? (Higginbottom+13) What are the implied mass-loss rates and energetics? ( Higginbottom+13) What is the wind driving mechanism? (Higginbottom+14) Can disk wind models match reverberation mapping data? (Mangham+15) Can the same disk winds –O–Operate in the presence of strong X-rays? (Matthews+15) –P–Produce broad UV/optical emission lines? (Matthews+15) QUARTZ Results and Plans

Christian Knigge Department of Physics & Astronomy University of Southampton QUARTZ Project III: Disk Wind Reverberation Mapping RM has so far mostly been used to obtain SMBH masses from line-to-continuum lags But total line lags are only “zeroth-order” RM “Full” RM can provide BLR structure and kinematics, but requires –Time resolution –Velocity resolution  echo images (aka velocity-delay maps) (aka 2-D transfer functions) Observations are now happening! (e.g. Bentz+10; Pancoast+12+14; de Rosa+15) Need theoretically predicted echo images for lines formed in disk wind models! Welsh & Horne 1991 Mangham+15 Bentz+06 Continuum Light Curve Emission Line Light Curve

Christian Knigge Department of Physics & Astronomy University of Southampton QUARTZ Project III: Disk Wind Reverberation Mapping C IV velocity-delay map for the H13 benchmark model (Mangham+15) Accounts self-consistently for: Ionization/emissivity structure Radiative transfer effects

Christian Knigge Department of Physics & Astronomy University of Southampton Accretion disk winds matter – they can –produce/affect almost all observational AGN/QSO signatures –provide a natural and physical AGN/QSO unification mechanism –inject energy/momentum into the host galaxy ( feedback) QUARTZ collaboration –test the viability AGN/QSO unification via disk winds –Determine the importance of disk winds for feedback –A simple disk wind model can reproduce BALQSOs (Higginbottom+13) –Ionization + RT calculations show that hydro models of line-driven winds are not self-consistent (Higginbottom+14) –Broad emission lines and X-rays (Matthews+15) –Disk-wind reverberation mapping (Mangham+15) –Full hydro+ionization+RT modelling of line-driven winds (Higginbottom+16) Summary { { { Goals Results Plans