We conduct a systematic study of galactic outflows in star-forming galaxies at z ~ 0–2 based on the absorption lines of optical spectra taken from SDSS DR7, DEEP2 DR4, and Keck (Erb et al.). We carefully make stacked spectra of homogeneous galaxy samples with similar stellar mass distributions at z ~ 0–2 and perform the multicomponent fitting of model absorption lines and stellar continua to the stacked spectra. We obtain the maximum (vmax) and central (vout) outflow velocities and estimate the mass loading factors (η), a ratio of the mass outflow rate to the star formation rate (SFR). Investigating the redshift evolution of the outflow velocities measured with the absorption lines whose depths and ionization energies are similar (Na I D and Mg I at z ~ 0–1; Mg II and C II at z ~ 1–2), we identify, for the first time, that the average value of vmax (vout) significantly increases by 0.05–0.3 dex from z ~ 0 to 2 at a given SFR. Moreover, we find that the value of η increases from z ~ 0 to 2 by η ∝ (1 + z)1.2±0.3 at a given halo circular velocity vcir, albeit with a potential systematics caused by model parameter choices. The redshift evolution of vmax (vout) and η is consistent with the galaxy-size evolution and the local velocity–SFR surface density relation and explained by high gas fractions in high-redshift massive galaxies, which is supported by recent radio observations. We obtain a scaling relation of ηvacir for α = -0.2 ± 1.1 in our z ~ 0 galaxies that agrees with the momentum-driven outflow model (α = -1) within the uncertainties.

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Published in The Astrophysical Journal, v. 850, no. 1, 51, p. 1-14.

© 2017. The American Astronomical Society. All rights reserved.

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Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England.

Due to the large number of funding sources, only the first few are listed in this section. For the complete list of funding sources, please download this article.

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