TY - JOUR
T1 - CLEAR
T2 - The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
AU - Matharu, Jasleen
AU - Papovich, Casey
AU - Simons, Raymond C.
AU - Momcheva, Ivelina
AU - Brammer, Gabriel
AU - Ji, Zhiyuan
AU - Backhaus, Bren E.
AU - Cleri, Nikko J.
AU - Estrada-Carpenter, Vicente
AU - Finkelstein, Steven L.
AU - Finlator, Kristian
AU - Giavalisco, Mauro
AU - Jung, Intae
AU - Muzzin, Adam
AU - Nelson, Erica J.
AU - Pillepich, Annalisa
AU - Trump, Jonathan R.
AU - Weiner, Benjamin
N1 - Funding Information:
J.M. thanks the anonymous referee for a thorough review of the manuscript. J.M. thanks Matteo Fossati, Erica J. Nelson, and Annalisa Pillepich for providing the KMOS, 3D-HST, and TNG50 measurements, respectively, which made the comparisons to Wilman et al. (), Nelson et al. (), and Pillepich et al. () possible. J.M. also thanks Robert Kennicutt for helpful discussions regarding the results in this paper. This work is based on data obtained from the Hubble Space Telescope through program No. GO-14227. Support for program No. GO-14227 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work is supported in part by the National Science Foundation through grant AST 1614668. V.E.C. acknowledges support from the NASA Headquarters under the Future Investigators in NASA Earth and Space Science and Technology (FINESST) award 19-ASTRO19-0122. This work was supported in part by NASA contract NNG16PJ33C, the Studying Cosmic Dawn with WFIRST Science Investigation Team. J.M., C.P., and V.E.C. are also grateful for the support from the George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University. Support for program AR-16151 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. 3D
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/9/1
Y1 - 2022/9/1
N2 - Using spatially resolved Hα emission line maps of star-forming galaxies, we study the spatial distribution of star formation over a wide range in redshift (0.5 ≲ z ≲ 1.7). Our z ∼ 0.5 measurements come from deep Hubble Space Telescope (HST) Wide Field Camera 3 G102 grism spectroscopy obtained as part of the CANDELS Lyα Emission at Reionization Experiment. For star-forming galaxies with log(M */M ⊙) ≥ 8.96, the mean Hα effective radius is 1.2 ± 0.1 times larger than that of the stellar continuum, implying inside-out growth via star formation. This measurement agrees within 1σ with those measured at z ∼ 1 and z ∼ 1.7 from the 3D-HST and KMOS3D surveys, respectively, implying no redshift evolution. However, we observe redshift evolution in the stellar mass surface density within 1 kpc (Σ1kpc). Star-forming galaxies at z ∼ 0.5 with a stellar mass of log(M */M ⊙) = 9.5 have a ratio of Σ1kpc in Hα relative to their stellar continuum that is lower by (19 ± 2)% compared to z ∼ 1 galaxies. Σ1kpc,Hα /Σ1kpc,Cont decreases toward higher stellar masses. The majority of the redshift evolution in Σ1kpc,Hα /Σ1kpc,Cont versus stellar mass stems from the fact that log(Σ1kpc,Hα ) declines twice as much as log(Σ1kpc,Cont) from z ∼ 1 to 0.5 (at a fixed stellar mass of log(M */M ⊙) = 9.5). By comparing our results to the TNG50 cosmological magneto-hydrodynamical simulation, we rule out dust as the driver of this evolution. Our results are consistent with inside-out quenching following in the wake of inside-out growth, the former of which drives the significant drop in Σ1kpc,Hα from z ∼ 1 to z ∼ 0.5.
AB - Using spatially resolved Hα emission line maps of star-forming galaxies, we study the spatial distribution of star formation over a wide range in redshift (0.5 ≲ z ≲ 1.7). Our z ∼ 0.5 measurements come from deep Hubble Space Telescope (HST) Wide Field Camera 3 G102 grism spectroscopy obtained as part of the CANDELS Lyα Emission at Reionization Experiment. For star-forming galaxies with log(M */M ⊙) ≥ 8.96, the mean Hα effective radius is 1.2 ± 0.1 times larger than that of the stellar continuum, implying inside-out growth via star formation. This measurement agrees within 1σ with those measured at z ∼ 1 and z ∼ 1.7 from the 3D-HST and KMOS3D surveys, respectively, implying no redshift evolution. However, we observe redshift evolution in the stellar mass surface density within 1 kpc (Σ1kpc). Star-forming galaxies at z ∼ 0.5 with a stellar mass of log(M */M ⊙) = 9.5 have a ratio of Σ1kpc in Hα relative to their stellar continuum that is lower by (19 ± 2)% compared to z ∼ 1 galaxies. Σ1kpc,Hα /Σ1kpc,Cont decreases toward higher stellar masses. The majority of the redshift evolution in Σ1kpc,Hα /Σ1kpc,Cont versus stellar mass stems from the fact that log(Σ1kpc,Hα ) declines twice as much as log(Σ1kpc,Cont) from z ∼ 1 to 0.5 (at a fixed stellar mass of log(M */M ⊙) = 9.5). By comparing our results to the TNG50 cosmological magneto-hydrodynamical simulation, we rule out dust as the driver of this evolution. Our results are consistent with inside-out quenching following in the wake of inside-out growth, the former of which drives the significant drop in Σ1kpc,Hα from z ∼ 1 to z ∼ 0.5.
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U2 - 10.3847/1538-4357/ac8471
DO - 10.3847/1538-4357/ac8471
M3 - Article
AN - SCOPUS:85138858506
SN - 0004-637X
VL - 937
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 16
ER -