Robyn Levine JILA, University of Colorado Fermilab with Nick Gnedin AGN Outflows in a Cosmological Context: An Empirical Approach

Cosmological Simulation dark matter distribution A Description of Outflows AGN distribution -luminosity function -density bias -fraction of AGN with outflows Spherical Outflow Model

2dF GOODS Luminosity Function L B B-band luminosity of AGN (in units L ,B )  f faint-end slope (constant in z  1.58)  b bright-end slope (z-dependent) Schirber & Bullock 2002

density profile + AGN Sample Simulation Box

Radio-loud Quasars Collimated jets of relativistic plasma Spreads into overpressured cocoon BAL AGNs Clouds ejected at v ≤ 1% c ~10% covering fraction? Radio loud jets 10% of AGN BAL outflows 50% of low-L AGN Crenshaw et al % of high-L AGN Hewett & Foltz 2003

AGN Outflows Spherical symmetry Similar treatment for BAL outflows and RLQ  AGN << t Hubble 2 expansion phases –Sedov-Taylor phase (energy conserved) –Pressure Equilibrium phase

AGN + outflows Sample Simulation Box

Ly  forest constraints on F(z) Outflows create voids in the Ly  forest Low-z –Use baryon fraction for forest,  Ly   (Penton, Stocke, & Shull 2004)  99.6% free for voids in simple model –  Ly  combined with N H -1+  m relation of Davé et al. (1999)  70-97% free for voids High-z –Studies of gaps in Ly  forest predict voids occupy < 20% for 1.7 < z < 3.8 (Duncan et al. 1989)

Kinetic Fraction  k = L k / L bol Ly-  forest at z=0 Ly-  forest at z=2-3

AGN Bias AGN trace high density regions: AGN more biased at higher redshift larger bias  smaller filling fraction

Weak Lensing Arithmetic Weak Lensing = Gravity Gravity = Total Matter (x 8  G/c 4 ) Total Matter = Dark Matter + AGN have enough energy to move all the gas in the universe over cosmological distances… Baryons

Can Outflows affect P(k)?

Two Competing Effects… Clustering of AGNs increases power AGNs move gas from small to large scales P(k)

That’s A Mess! If outflows affect > 10% of the volume: >1% reduction in large-scale power AGN are highly clustered: transfer of small-scale power to large scales, f B f AGN b AGN 2 ~ 1% We do not know even the sign of the effect!

Summary  Even with small mechanical efficiencies, AGN outflows fill the IGM by z~2  AGN outflows potentially affect the matter power spectrum  redistribute baryons (from small to large scales)  decreases power  bias in AGN distribution  increases power