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The energetics of starburst-driven outflows at z ∼ 1 from KMOS.

Swinbank, A.M. and Harrison, C.M. and Tiley, A.L. and Johnson, H.L. and Smail, I. and Stott, J.P. and Best, P.N. and Bower, R.G. and Bureau, M. and Bunker, A. and Cirasuolo, M. and Jarvis, M. and Magdis, G.E. and Sharples, R.M. and Sobral, D. (2019) 'The energetics of starburst-driven outflows at z ∼ 1 from KMOS.', Monthly notices of the Royal Astronomical Society., 487 (1). pp. 381-393.

Abstract

We present an analysis of the gas outflow energetics from KMOS observations of 529 main-sequence star-forming galaxies at z 1 using broad, underlying Hα and forbid- den lines of [Nii] and [Sii]. Based on the stacked spectra for a sample with median star- formation rates and stellar masses of SFR=7M⊙ / yr and M⋆ =(1.0±0.1)×1010M⊙ respectively, we derive a typical mass outflow rate of ˙Mwind =1–4M⊙ yr−1 and a mass loading of ˙Mwind / SFR=0.2–0.4. By comparing the kinetic energy in the wind with the energy released by supernovae, we estimate a coupling efficiency between the star formation and wind energetics of ǫ 0.03. The mass loading of the wind does not show a strong trend with star-formation rate over the range 2–20M⊙ yr−1, although we identify a trend with stellar mass such that dM/ dt / SFR/M0.26±0.07 ⋆ . Finally, the line width of the broad Hα increases with disk circular velocity with a sub-linear scal- ing relation FWHMbroad /v0.21±0.05. As a result of this behavior, in the lowest mass galaxies (M⋆ < ∼ 1010M⊙), a significant fraction of the outflowing gas should have suf- ficient velocity to escape the gravitational potential of the halo whilst in the highest mass galaxies (M⋆ > ∼ 1010M⊙) most of the gas will be retained, flowing back on to the galaxy disk at later times.

Item Type:Article
Full text:(AM) Accepted Manuscript
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Status:Peer-reviewed
Publisher Web site:https://doi.org/10.1093/mnras/stz1275
Publisher statement:© 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
Date accepted:02 May 2019
Date deposited:17 May 2019
Date of first online publication:09 May 2019
Date first made open access:No date available

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