CLEAR: The Gas-phase Metallicity Gradients of Star-forming Galaxies at 0.6 < z < 2.6
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CLEAR : The Gas-phase Metallicity Gradients of Star-forming Galaxies at 0.6 < z < 2.6. / Simons, Raymond C.; Papovich, Casey; Momcheva, Ivelina; Trump, Jonathan R.; Brammer, Gabriel; Estrada-Carpenter, Vicente; Backhaus, Bren E.; Cleri, Nikko J.; Finkelstein, Steven L.; Giavalisco, Mauro; Ji, Zhiyuan; Jung, Intae; Matharu, Jasleen; Weiner, Benjamin.
I: Astrophysical Journal, Bind 923, Nr. 2, 203, 22.12.2021.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - CLEAR
T2 - The Gas-phase Metallicity Gradients of Star-forming Galaxies at 0.6 < z < 2.6
AU - Simons, Raymond C.
AU - Papovich, Casey
AU - Momcheva, Ivelina
AU - Trump, Jonathan R.
AU - Brammer, Gabriel
AU - Estrada-Carpenter, Vicente
AU - Backhaus, Bren E.
AU - Cleri, Nikko J.
AU - Finkelstein, Steven L.
AU - Giavalisco, Mauro
AU - Ji, Zhiyuan
AU - Jung, Intae
AU - Matharu, Jasleen
AU - Weiner, Benjamin
PY - 2021/12/22
Y1 - 2021/12/22
N2 - We report on the gas-phase metallicity gradients of a sample of 238 star-forming galaxies at 0.6 < z < 2.6, measured through deep near-infrared Hubble Space Telescope slitless spectroscopy. The observations include 12 orbit depth Hubble/WFC3 G102 grism spectra taken as a part of the CANDELS Ly alpha Emission at Reionization (CLEAR) survey, and archival WFC3 G102+G141 grism spectra overlapping the CLEAR footprint. The majority of galaxies in this sample are consistent with having a zero or slightly positive metallicity gradient (dZ/dR >= 0, i.e., increasing with radius) across the full mass range probed (8.5 < log M (*)/M (circle dot) < 10.5). We measure the intrinsic population scatter of the metallicity gradients, and show that it increases with decreasing stellar mass-consistent with previous reports in the literature, but confirmed here with a much larger sample. To understand the physical mechanisms governing this scatter, we search for correlations between the observed gradient and various stellar population properties at fixed mass. However, we find no evidence for a correlation with the galaxy properties we consider-including star formation rates, sizes, star formation rate surface densities, and star formation rates per gravitational potential energy. We use the observed weakness of these correlations to provide material constraints for predicted intrinsic correlations from theoretical models.
AB - We report on the gas-phase metallicity gradients of a sample of 238 star-forming galaxies at 0.6 < z < 2.6, measured through deep near-infrared Hubble Space Telescope slitless spectroscopy. The observations include 12 orbit depth Hubble/WFC3 G102 grism spectra taken as a part of the CANDELS Ly alpha Emission at Reionization (CLEAR) survey, and archival WFC3 G102+G141 grism spectra overlapping the CLEAR footprint. The majority of galaxies in this sample are consistent with having a zero or slightly positive metallicity gradient (dZ/dR >= 0, i.e., increasing with radius) across the full mass range probed (8.5 < log M (*)/M (circle dot) < 10.5). We measure the intrinsic population scatter of the metallicity gradients, and show that it increases with decreasing stellar mass-consistent with previous reports in the literature, but confirmed here with a much larger sample. To understand the physical mechanisms governing this scatter, we search for correlations between the observed gradient and various stellar population properties at fixed mass. However, we find no evidence for a correlation with the galaxy properties we consider-including star formation rates, sizes, star formation rate surface densities, and star formation rates per gravitational potential energy. We use the observed weakness of these correlations to provide material constraints for predicted intrinsic correlations from theoretical models.
KW - ABUNDANCE GRADIENTS
KW - CHEMICAL EVOLUTION
KW - ANGULAR-MOMENTUM
KW - MASS
KW - STELLAR
KW - ACCRETION
KW - DYNAMICS
KW - HIZELS
KW - MODELS
KW - ORIGIN
U2 - 10.3847/1538-4357/ac28f4
DO - 10.3847/1538-4357/ac28f4
M3 - Journal article
VL - 923
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 203
ER -
ID: 299751684