TY - JOUR
T1 - The building up of observed stellar scaling relations of massive galaxies and the connection to black hole growth in the TNG50 silation
AU - Vaa, S.
AU - Huertas-Company, M.
AU - Pillepich, A.
AU - Nelson, D.
AU - Rodriguez-Gomez, V.
AU - Dekel, A.
AU - Faber, S. M.
AU - Iglesias-Navarro, P.
AU - Koo, D. C.
AU - Primack, J.
N1 - Publisher Copyright:
© 2022 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
PY - 2022/1/1
Y1 - 2022/1/1
N2 - We study how mock-observed stellar morphological and structural properties of massive galaxies are built up between $z$ = 0.5 and $z$ = 3 in the TNG50 cosmological silation. We generate mock images with the properties of the CANDELS survey and derive Sersic parameters and optical rest-frame morphologies as usually done in the observations. Overall, the silation reproduces the observed evolution of the abundances of different galaxy morphological types of star-foing and quiescent galaxies. The log M - log Re and log M - log 1 relations of the silated star-foing and quenched galaxies also match the observed slopes and zeropoints to within 1. In the silation, galaxies increase their observed central stellar mass density (1) and transfo in morphology from irregular/clumpy systems to noal Hubble-type systems in the star foation main sequence at a characteristic stellar mass of 1010.5 M which is reflected in an increase of the central stellar mass density (1). This morphological transfoation is connected to the activity of the central super massive black holes (SMBHs). At low stellar masses (109 < M/M < 1010) SMBHs grow rapidly, while at higher mass SMBHs switch into the kinetic feedback mode and grow more slowly. During this low-accretion phase, SMBH feedback leads to the quenching of star-foation, along with a siltaneous growth in 1, partly due to the fading of stellar populations. More compact massive galaxies grow their SMBHs faster than extended ones of the same mass and end up quenching earlier. In the TNG50 silation, SMBHs predominantly grow via gas accretion before galaxies quench, and 1 increases substantially after SMBH growth slows down. The silation predicts therefore that quiescent galaxies have higher 1 values than star-foing galaxies for the same SMBH mass, which disagrees with alternative models, and may potentially be in tension with some observations.
AB - We study how mock-observed stellar morphological and structural properties of massive galaxies are built up between $z$ = 0.5 and $z$ = 3 in the TNG50 cosmological silation. We generate mock images with the properties of the CANDELS survey and derive Sersic parameters and optical rest-frame morphologies as usually done in the observations. Overall, the silation reproduces the observed evolution of the abundances of different galaxy morphological types of star-foing and quiescent galaxies. The log M - log Re and log M - log 1 relations of the silated star-foing and quenched galaxies also match the observed slopes and zeropoints to within 1. In the silation, galaxies increase their observed central stellar mass density (1) and transfo in morphology from irregular/clumpy systems to noal Hubble-type systems in the star foation main sequence at a characteristic stellar mass of 1010.5 M which is reflected in an increase of the central stellar mass density (1). This morphological transfoation is connected to the activity of the central super massive black holes (SMBHs). At low stellar masses (109 < M/M < 1010) SMBHs grow rapidly, while at higher mass SMBHs switch into the kinetic feedback mode and grow more slowly. During this low-accretion phase, SMBH feedback leads to the quenching of star-foation, along with a siltaneous growth in 1, partly due to the fading of stellar populations. More compact massive galaxies grow their SMBHs faster than extended ones of the same mass and end up quenching earlier. In the TNG50 silation, SMBHs predominantly grow via gas accretion before galaxies quench, and 1 increases substantially after SMBH growth slows down. The silation predicts therefore that quiescent galaxies have higher 1 values than star-foing galaxies for the same SMBH mass, which disagrees with alternative models, and may potentially be in tension with some observations.
KW - evolution
KW - foation
KW - galaxies
KW - galaxies
KW - galaxies
KW - high-redshift
UR - http://www.scopus.com/inward/record.url?scp=85121264831&partnerID=8YFLogxK
U2 - 10.1093/mnras/stab3149
DO - 10.1093/mnras/stab3149
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AN - SCOPUS:85121264831
SN - 0035-8711
VL - 509
SP - 2654
EP - 2673
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -