Feedback: in the form of outflow

AGN driven outflow

M82 Blue: Chandra Red: Spitzer Cyan: Optical

Star formation driven outflow

Two categories of the gas in a SF/SB galaxy wind Ambient interstellar medium Energetic fluid created by thermalization of the SB’s stellar eject or AGN The hydrodynamical interaction between these two generates the multiphase starburst-driven galactic wind.

Observations of multiphase wind (cold, warm, hot gas & dust) X-ray Morphology and kinematics of interstellar emission lines (e.g. Ha…) Outflow kinematics in the interstellar absorption lines (e.g. MgII, NaD)

From X-ray: Hot Gas Escapes from Dwarf Starbursts Martin 1999, Heckman et al 2000, Martin 2004 Rotation Speed  Tremonti et al V c = 130 km/s

From optical absorption lines --NaD(5890,5896A) Low- ionization potential 5.1eV (Martin et al. 2005, 2006) V = -96 km/s V = -435 km/s

Circular velocityStar formation rate Outflow velocity isothermal escape speed From optical absorption lines (Rupke et al. 2005a,b,c) Murray et al. 2004, Martin 2005

Stack spectrum and stellar continuum Mg I He I Na I

Two-component fit of ISM Na D Line center shift: outflow velocity Voff Line strength (EW): covering factor Cf Line width b Line ratio τ 0

Two-component fit of ISM Na D Line center shift: outflow velocity Voff Line strength (EW): covering factor Cf Line width b Line ratio τ 0

Inclination effect face on edge on

Isolate the main driver of the observed correlation: Disk-like components

Isolate the main driver of the observed correlation: outflow components

Outflow velocity vs. SFR V off ~ SFR 0.3

Martin et al Spectra from LRIS on Keck I Using multi-components to fit each absorption line

Through the fitting in last slides, they find that components with different velocity have different covering factor  outflow is accelerating