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KURVS: the outer rotation curve shapes and dark matter fractions of z ∼1.5 star-forming galaxies

Lookup NU author(s): Dr Chris HarrisonORCiD

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This work is licensed under a Creative Commons Attribution 4.0 International License (CC BY 4.0).


Abstract

© 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. We present first results from the KMOS Ultra-deep Rotation Velocity Survey (KURVS), aimed at studying the outer rotation curves shape and dark matter content of 22 star-forming galaxies at z ∼1.5. These galaxies represent 'typical' star-forming discs at z ∼1.5, being located within the star-forming main sequence and stellar mass-size relation with stellar masses 9.5 ≤ log(M*/M⊙) ≤ 11.5. We use the spatially resolved H α emission to extract individual rotation curves out to 4 times the effective radius, on average, or ∼10-15 kpc. Most rotation curves are flat or rising between three and six disc scale radii. Only three objects with dispersion-dominated dynamics (vrot/σ0 ∼0.2) have declining outer rotation curves at more than 5σ significance. After accounting for seeing and pressure support, the nine rotation-dominated discs with vrot/σ0 ≥ 1.5 have average dark matter fractions of at the effective radius, similar to local discs. Together with previous observations of star-forming galaxies at cosmic noon, our measurements suggest a trend of declining dark matter fraction with increasing stellar mass and stellar mass surface density at the effective radius. Measurements of simulated EAGLE galaxies are in quantitative agreement with observations up to log, and overpredict the dark matter fraction of galaxies with higher mass surface densities by a factor of ∼3. We conclude that the dynamics of typical rotationally-supported discs at z ∼1.5 is dominated by dark matter from effective radius scales, in broad agreement with cosmological models. The tension with observations at high stellar mass surface density suggests that the prescriptions for baryonic processes occurring in the most massive galaxies (such as bulge growth and quenching) need to be reassessed.


Publication metadata

Author(s): Puglisi A, Dudzeviciute U, Swinbank M, Gillman S, Tiley AL, Bower RG, Cirasuolo M, Cortese L, Glazebrook K, Harrison C, Ibar E, Molina J, Obreschkow D, Oman KA, Schaller M, Shankar F, Sharples RM

Publication type: Article

Publication status: Published

Journal: Monthly Notices of the Royal Astronomical Society

Year: 2023

Volume: 524

Issue: 2

Pages: 2814-2835

Print publication date: 01/09/2023

Online publication date: 08/07/2023

Acceptance date: 20/06/2023

Date deposited: 15/08/2024

ISSN (print): 0035-8711

ISSN (electronic): 1365-2966

Publisher: Oxford University Press

URL: https://doi.org/10.1093/mnras/stad1966

DOI: 10.1093/mnras/stad1966

Data Access Statement: The data used in this paper are available through the ESO archive.


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Funding

Funder referenceFunder name
STFC ST/P000541/1
STFC ST/T000244/1
United Kingdom Research and Innovation grant (code: MR/V022830/1)

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