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Published June 20, 2020 | Accepted Version + Published
Journal Article Open

Effects of Stellar Feedback on Stellar and Gas Kinematics of Star-forming Galaxies at 0.6 < z < 1.0

Abstract

Recent zoom-in cosmological simulations have shown that stellar feedback can flatten the inner density profile of the dark matter halo in low-mass galaxies. A correlation between the stellar/gas velocity dispersion (σ_(star), σ_(gas)) and the specific star formation rate (sSFR) is predicted as an observational test of the role of stellar feedback in re-shaping the dark matter density profile. In this work we test the validity of this prediction by studying a sample of star-forming galaxies at 0.6 < z < 1.0 from the LEGA-C survey, which provides high signal-to-noise measurements of stellar and gas kinematics. We find that a weak but significant correlation between σ_(star) (and σ_(gas)) and sSFR indeed exists for galaxies in the lowest mass bin (M_* ~ 10¹⁰ M_⊙). This correlation, albeit with a ~35% scatter, holds for different tracers of star formation, and becomes stronger with redshift. This result generally agrees with the picture that at higher redshifts star formation rate was generally higher, and galaxies at M_* ≾ 10¹⁰ M_⊙ have not yet settled into a disk. As a consequence, they have shallower gravitational potentials more easily perturbed by stellar feedback. The observed correlation between σ_(star) (and σ_(gas)) and sSFR supports the scenario predicted by cosmological simulations, in which feedback-driven outflows cause fluctuations in the gravitation potential that flatten the density profiles of low-mass galaxies.

Additional Information

© 2020. The American Astronomical Society. Received 2019 December 26; revised 2020 May 28; accepted 2020 May 29; published 2020 June 16. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 194-A.2005 (The LEGA-C Public Spectroscopy Survey). D.P. acknowledges support from the NASA MUREP Institutional Opportunity (MIRO) through the grant NNX15AP99A. A.W. received support from NASA, through ATP grant 80NSSC18K1097 and HST grants GO-14734 and AR-15057 from STScI, the Heising-Simons Foundation, and a Hellman Fellowship.

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Published - Pelliccia_2020_ApJL_896_L26.pdf

Accepted Version - 2001.00590.pdf

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August 22, 2023
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