paper

Empirical Constraints of Super-Galactic Winds at z >= 0.5

arXiv:1205.4037 · doi:10.1111/j.1365-2966.2012.21327.x

Abstract

(Abridged) Under the hypothesis that MgII absorbers found near the minor axis of a galaxy originate in the cool phase of winds, we carry out a study to constrain the properties of large-scale outflows at redshift z >= 0.5 based on the observed relative motions of individual absorbing clouds with respect to the positions and orientations of the galaxies. We identify in the literature four highly inclined disk galaxies located within 50 kpc and with the minor axis oriented within 45 degrees of a background QSO sightline. Deep HST images of the galaxies are available for accurate morphologies of the galaxies. Echelle spectra of the QSO members are also available in public archives for resolving the velocity field of individual absorption clumps. Three galaxies in our sample are located at rho=8-34 kpc and exhibit strong associated MgII absorption feature with Wr(2796) >= 0.8 Å. One galaxy, located at an impact parameters rho=48 kpc, does not show an associated MgII absorber to a 3-sigma limit of Wr(2796)=0.01Å. Combining known inclination and orientation angles of the star-forming disks, and resolved absorption profiles of the associated absorbers at rho < 35 kpc, we explore the parameter space for the opening angle theta_0 and the velocity field of large-scale galactic outflows as a function of z-height, v(z). We find that the absorption profiles of the MgII doublets and FeII series are compatible with the gas being either accelerated or decelerated, depending on theta_0, though accelerated outflows are valid only for a narrow range of theta_0. Under an acceleration scenario, we compare the derived with predictions from Murray et al. (2011) and find that if the gas is being accelerateted by the radiation and ram pressure forces from super star clusters, then the efficiency of thermal energy input from a supernova explosion is epsilon <= 0.01.

13 pages, 10 figures. Accepted for publication in MNRAS

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