1. In this toy scenario, metal enriched clouds entrained in galactic winds gives rise to absorption lines in quasar spectra, as illustrated in the above panels as are expected for COS and HIRES/UVES spectra… Background quasar configuration… (these are simulated spectra from our  CDM simulations, see Sec 2 below for details) Using Galaxy Winds to Constrain Galaxy Evolution Christopher Churchill 1, Anatoly Klypin 1, Daniel Ceverino 2, Glenn Kacprzak 3, Jessica Evans 1, & Elizabeth Klimek 1 (1) New Mexico State University, (2) Hebrew University of Jerusalem, (3) Swinburne University 1. INTRODUCTION, MOTIVATION, AND SIMULATIONS 2. BACKGROUND QSO METHOD: EXAMINING GALACTIC WINDS 3. EVOLUTION OF WINDS 4. STACKING - “DOWN THE BARREL” 5. STACKING - IMPACT PARAMETER BINS, V 90, & SFR 5. A WORK IN PROGRESS The spectra of bright z=2-3 star bursting galaxies exhibit many “interstellar” lines in absorption and these lines indicate outflow on the order of 1000 km/s. The signal to noise of the individual spectra are low, so it is necessary to stack the spectra in the rest-frame of each galaxy in order to obtain a higher signal-to-noise composite spectrum. The continuum source is the nuclear region of the galaxy, thus the term “down the barrel”. (RIGHT) The panel on right shows a composite spectrum of Steidel and collaborators (unpublished) for which the mean galaxy properties are given. Also shown are expanded views of absorption for three bright lensed galaxies. (LEFT) The profiles we obtain from our simulations using the “down the barrel” technique. Our simulation galaxies show similar profiles (though we do not reproduce the slow recovery of flux in the blue wing). Our ultimate goal is to obtain quantitative comparison- but there are few published observations at this time. (RIGHT) The observed distribution of velocities in absorption (blue) and the distribution of Lyman  emission peaks (red) from starburst galaxies (Steidel, 1997, private comm). The absorption velocities are of the mean optical depth centroids. (FAR RIGHT) The distribution of absorption velocities from the down the barrel spectra from our simulations for CIV, OVI, and Lyman  (in absorption). The mean outflow velocity of OVI is 115 km/s, which compares to the mean observed velocity of 165 km/s. (note the axes are in opposite directions). (observations) (simulations) (observations vs. simulations) (LEFT) The schematic illustration of the experiment of stacking the background galaxies in various impact parameter bins. In the side view, the observer is to the left. (ABOVE LEFT) Observational results for three impact parameter bins, D=0 (red), 8-40, (blue) and 40-80 (magenta) kpc (Stiedel, private com). (ABOVE RIGHT) Simulation result for comparison. Note the trend for lower optical depth with increasing impact parameter is duplicated. (FAR LEFT) V 90 from many galaxies in our simulations vs star formation rate. We find V 90 ~ SFR 0.5. The blue, green and red points are the results of Weiner etal, which fairly well match our simulations. The absorption profiles for MgII are shown for the three galaxies. Analysis of mock quasar spectra of metal absorption lines in the proximity of formed galaxies in cosmological simulations is a promising technique for understanding the role of galaxies in IGM physics, or IGM physics in the role of galaxy formation. We are undertaking a wholesale approach to use  CDM simulations to interpret absorption line data from redshift 1-3 starbursting galaxies (Lyman Break Galaxies, etc). We compare to DEEP galaxies (Weiner et al. 2009) and the collective work of Steidel et al. (2009, private comm) on z=2-3 galaxies. The simulations are performed using the Eulerian Gasdynamics + Nbody Adaptive Refinement Tree (Kravstov 1999) code with resolutions of 20-50 pc. Here, we motivate and present our work in progress to compare the absorption line properties obtained from the gas in the simulations to the observed absorption properties. Direct line of sight “Down the Barrel” configuration… In this toy scenario, Lyman  emission is powered by correlated supernovae (star bursting phase). Lyman  emission is redshifted out of the rest-frame of the wind on the observer side and is seen in emission, whereas the metal lines are seen blue shifted in absorption. grid of LOS Geometric distribution of infalling and outflowing gas (determined from abs spectra) Z=3.5Z=1.0Z=3.5 Z=1.0 Using the absorption profiles from the simulations selected by OVI (red), CIV (blue) and Lyman  absorption (green), we plot the cell radial velocity relative to the simulated galaxy for z=3.5 and z=1.0. The simulations winds peter out and become infall by z=1.0. (We believe this is due to undesired overcooling.) JUST THE FACTS… ABSORPTIONABSORPTION SIMULATIONSSIMULATIONS [kpc] [cm -3 ] D = position on LOS Z/Z sun = gas metallicity n H = hydrogen number density V = cell volume f H = HI ionization fraction T = gas temperature = cell velocity consider a random gas cell in the simulations Line of Sight Cell Properties Simulated Spectra sky view line of sight (LOS) (observer) background galaxies; spectra are co-added in various impact parameter bins target galaxy red = side A blue = side B observed simulations simulated spectra observed simulations REFERENCES: Ceverino, D., & Klypin, A. 2009, ApJ, 695, 292 Ferland, G., et al., 1998, PASP, 110, 761 Haardt, F., & Madau, P. 1996, ApJ, 461, 20 Kravstov, A., Klypin, A., & Khokhlov, A. 1997, ApJS, 111, 73 Kravstov, A. 1999, PhD, New Mexico State University Kravstov, A. 2003, ApJ,L, 590, L1 Kravstov, A., Gneden, O., & Klypin, A. 2004, ApJ, 609, 482 Miller, G., & Scalo, J. 1979, ApJS, 41, 513 Steidel, C. 2009, private communication Weiner, B., et al. 2009, ApJ, 692, 197 Woosley, S., & Weaver, T. 1995, ApJS, 101, 181 (courtesy C. Steidel) Steidel et al. (private comm) Ceverino & Klypin (2009)