Spatially resolved star formation and inside-out quenching in the TNG50 simulation and 3D-HST observations
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Spatially resolved star formation and inside-out quenching in the TNG50 simulation and 3D-HST observations. / Nelson, Erica J.; Tacchella, Sandro; Diemer, Benedikt; Leja, Joel; Hernquist, Lars; Whitaker, Katherine E.; Weinberger, Rainer; Pillepich, Annalisa; Nelson, Dylan; Terrazas, Bryan A.; Nevin, Rebecca; Brammer, Gabriel B.; Burkhart, Blakesley; Cochrane, Rachel K.; van Dokkum, Pieter; Johnson, Benjamin D.; Marinacci, Federico; Mowla, Lamiya; Pakmor, Rudiger; Skelton, Rosalind E.; Speagle, Joshua; Springel, Volker; Torrey, Paul; Vogelsberger, Mark; Wuyts, Stijn.
In: Monthly Notices of the Royal Astronomical Society, Vol. 508, No. 1, 11.2021, p. 219-235.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - Spatially resolved star formation and inside-out quenching in the TNG50 simulation and 3D-HST observations
AU - Nelson, Erica J.
AU - Tacchella, Sandro
AU - Diemer, Benedikt
AU - Leja, Joel
AU - Hernquist, Lars
AU - Whitaker, Katherine E.
AU - Weinberger, Rainer
AU - Pillepich, Annalisa
AU - Nelson, Dylan
AU - Terrazas, Bryan A.
AU - Nevin, Rebecca
AU - Brammer, Gabriel B.
AU - Burkhart, Blakesley
AU - Cochrane, Rachel K.
AU - van Dokkum, Pieter
AU - Johnson, Benjamin D.
AU - Marinacci, Federico
AU - Mowla, Lamiya
AU - Pakmor, Rudiger
AU - Skelton, Rosalind E.
AU - Speagle, Joshua
AU - Springel, Volker
AU - Torrey, Paul
AU - Vogelsberger, Mark
AU - Wuyts, Stijn
PY - 2021/11
Y1 - 2021/11
N2 - We compare the star-forming main sequence (SFMS) of galaxies - both integrated and resolved on 1kpc scales - between the high-resolution TNG50 simulation of IllustrisTNG and observations from the 3D-HST slitless spectroscopic survey at z similar to 1. Contrasting integrated star formation rates (SFRs), we find that the slope and normalization of the star-forming main sequence in TNG50 are quantitatively consistent with values derived by fitting observations from 3D-HST with the Prospector Bayesian inference framework. The previous offsets of 0.2-1 dex between observed and simulated main-sequence normalizations are resolved when using the updated masses and SFRs from Prospector. The scatter is generically smaller in TNG50 than in 3D-HST for more massive galaxies with M-*> 10(10)M(circle dot), by similar to 10-40 per cent, after accounting for observational uncertainties. When comparing resolved star formation, we also find good agreement between TNG50 and 3D-HST: average specific star formation rate (sSFR) radial profiles of galaxies at all masses and radii below, on, and above the SFMS are similar in both normalization and shape. Most noteworthy, massive galaxies with M-*> 10(10.5)M(circle dot), which have fallen below the SFMS due to ongoing quenching, exhibit a clear central SFR suppression, in both TNG50 and 3D-HST. In contrast, the original Illustris simulation and a variant TNG run without black hole kinetic wind feedback, do not reproduce the central SFR profile suppression seen in data. In TNG, inside-out quenching is due to the supermassive black hole (SMBH) feedback model operating at low accretion rates.
AB - We compare the star-forming main sequence (SFMS) of galaxies - both integrated and resolved on 1kpc scales - between the high-resolution TNG50 simulation of IllustrisTNG and observations from the 3D-HST slitless spectroscopic survey at z similar to 1. Contrasting integrated star formation rates (SFRs), we find that the slope and normalization of the star-forming main sequence in TNG50 are quantitatively consistent with values derived by fitting observations from 3D-HST with the Prospector Bayesian inference framework. The previous offsets of 0.2-1 dex between observed and simulated main-sequence normalizations are resolved when using the updated masses and SFRs from Prospector. The scatter is generically smaller in TNG50 than in 3D-HST for more massive galaxies with M-*> 10(10)M(circle dot), by similar to 10-40 per cent, after accounting for observational uncertainties. When comparing resolved star formation, we also find good agreement between TNG50 and 3D-HST: average specific star formation rate (sSFR) radial profiles of galaxies at all masses and radii below, on, and above the SFMS are similar in both normalization and shape. Most noteworthy, massive galaxies with M-*> 10(10.5)M(circle dot), which have fallen below the SFMS due to ongoing quenching, exhibit a clear central SFR suppression, in both TNG50 and 3D-HST. In contrast, the original Illustris simulation and a variant TNG run without black hole kinetic wind feedback, do not reproduce the central SFR profile suppression seen in data. In TNG, inside-out quenching is due to the supermassive black hole (SMBH) feedback model operating at low accretion rates.
KW - galaxies: evolution
KW - galaxies: formation
KW - galaxies: high-redshift
KW - galaxies: star formation
KW - galaxies: structure
KW - SIMILAR-TO 1
KW - STELLAR POPULATION SYNTHESIS
KW - LENS-AMPLIFIED SURVEY
KW - EARLY-TYPE GALAXIES
KW - H-ALPHA MAPS
KW - MAIN-SEQUENCE
KW - BLACK-HOLES
KW - ILLUSTRISTNG SIMULATIONS
KW - FORMATION HISTORIES
KW - COSMOLOGICAL SIMULATIONS
U2 - 10.1093/mnras/stab2131
DO - 10.1093/mnras/stab2131
M3 - Journal article
VL - 508
SP - 219
EP - 235
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 1
ER -
ID: 281600761