High-redshift superwinds as the source of the strongest MgII absorbers: A feasibility analysis

We present High Resolution Echelle Spectrometer/Keck profiles of four extremely strong (W-r > 1.8 Angstrom) Mg II absorbers at 1 < z < 2. The profiles display a common kinematic structure, having a sharp drop in optical depth near the center of the profile and strong, black-bottomed absorption on either side. This symmetric-inverted structure, with a velocity spread of several hundred kilometers per second, is suggestive of superwinds arising in actively star-forming galaxies. Low-ionization absorption of similar strength has been observed in local star-forming galaxies. The Mg II absorbers with W-r > 1.8 Angstrom evolve away from z = 2 to the present. We propose that a substantial fraction of these very strong absorbers are due to superwinds and that their evolution is related to the redshift evolution of star-forming galaxies. Based on the observed redshift number density of W-r > 1.8 Angstrom Mg II absorbers at 1 < z < 2, we explore whether it is realistic that superwinds from starbursting galaxies could give rise to these absorbers. Finally, we do an analysis of the superwind connection to damped Ly alpha absorbers (DLAs). DLAs and superwinds evolve differently and usually have different kinematic structure, indicating that superwinds probably do not give rise to the majority of DLAs.