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

Pelliccia, Debora and Mobasher, Bahram and Darvish, Behnam and Lemaux, Brian C. and Lubin, Lori M. and Hirtenstein, Jessie and Shen, Lu and Wu, Po-Feng and El-Badry, Kareem and Wetzel, Andrew and Jones, Tucker (2020) Effects of Stellar Feedback on Stellar and Gas Kinematics of Star-forming Galaxies at 0.6 < z < 1.0. Astrophysical Journal Letters, 896 (2). Art. No. L26. ISSN 2041-8213. https://resolver.caltech.edu/CaltechAUTHORS:20200622-104136805

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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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/2041-8213/ab9815DOIArticle
https://arxiv.org/abs/2001.00590arXivDiscussion Paper
ORCID:
AuthorORCID
Pelliccia, Debora0000-0002-3007-0013
Darvish, Behnam0000-0003-4919-9017
Lemaux, Brian C.0000-0002-1428-7036
Lubin, Lori M.0000-0003-4249-5315
Hirtenstein, Jessie0000-0002-5368-8262
Shen, Lu0000-0001-9495-7759
Wu, Po-Feng0000-0002-9665-0440
El-Badry, Kareem0000-0002-6871-1752
Wetzel, Andrew0000-0003-0603-8942
Jones, Tucker0000-0001-5860-3419
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.
Funders:
Funding AgencyGrant Number
NASANNX15AP99A
NASA80NSSC18K1097
NASA Hubble FellowshipGO-14734
NASA Hubble FellowshipAR-15057
Heising-Simons FoundationUNSPECIFIED
Hellman Family FoundationUNSPECIFIED
Subject Keywords:Galaxy evolution ; Galaxy kinematics ; Galaxy dynamics ; Galaxy dark matter halos ; Spectroscopy ; Photometry
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Galaxy evolution (594); Galaxy kinematics (602); Galaxy dynamics (591); Galaxy dark matter halos (1880); Spectroscopy (1558); Photometry (1234)
Record Number:CaltechAUTHORS:20200622-104136805
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200622-104136805
Official Citation:Debora Pelliccia et al 2020 ApJL 896 L26
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:103951
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:23 Jun 2020 19:36
Last Modified:23 Jun 2020 19:36

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