The specific star formation rate function at different mass scales and quenching: a comparison between cosmological models and SDSS
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The specific star formation rate function at different mass scales and quenching : a comparison between cosmological models and SDSS. / Katsianis, Antonios; Xu, Haojie; Yang, Xiaohu; Luo, Yu; Cui, Weiguang; Dave, Romeel; Lagos, Claudia Del P.; Zheng, Xianzhong; Zhao, Ping.
I: Monthly Notices of the Royal Astronomical Society, Bind 500, Nr. 2, 01.2021, s. 2036-2048.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - The specific star formation rate function at different mass scales and quenching
T2 - a comparison between cosmological models and SDSS
AU - Katsianis, Antonios
AU - Xu, Haojie
AU - Yang, Xiaohu
AU - Luo, Yu
AU - Cui, Weiguang
AU - Dave, Romeel
AU - Lagos, Claudia Del P.
AU - Zheng, Xianzhong
AU - Zhao, Ping
PY - 2021/1
Y1 - 2021/1
N2 - We present the eddington bias corrected specific star formation rate function (sSFRF) at different stellar mass scales from a subsample of the Sloan Digital Sky Survey Data Release DR7 (SDSS), which is considered complete both in terms of stellar mass (M-*) and star formation rate (SFR). The above enable us to study qualitatively and quantitatively quenching, the distribution of passive/star-forming galaxies and perform comparisons with the predictions from state-of-the-art cosmological models, within the same M-* and SFR limits. We find that at the low-mass end (M-* = 10(9.5)-10(10)M(circle dot)) the sSFRF is mostly dominated by star-forming objects. However, moving to the two more massive bins (M-* = 10(10)-10(10.5) M-circle dot and M* = 10(10.5)-10(11)M(circle dot)) a bimodality with two peaks emerges. One peak represents the star-forming population, while the other describes a rising passive population. The bi-modal form of the sSFRFs is not reproduced by a range of cosmological simulations (e.g. Illustris, EAGLE, Mufasa, and IllustrisTNG) which instead generate mostly the star-forming population, while a bi-modality emerges in others (e.g. L-Galaxies, Shark, and Simba). Our findings reflect the need for the employed quenching schemes in state-of-the-artmodels to be reconsidered, involving prescriptions that allow 'quenched galaxies' to retain a small level of SF activity (sSFR = 10(-11) 10(-12) yr(-1)) and generate an adequate passive population/bi-modality even at intermediate masses (M-* = 10(10)-10(10.5)M(circle dot)).
AB - We present the eddington bias corrected specific star formation rate function (sSFRF) at different stellar mass scales from a subsample of the Sloan Digital Sky Survey Data Release DR7 (SDSS), which is considered complete both in terms of stellar mass (M-*) and star formation rate (SFR). The above enable us to study qualitatively and quantitatively quenching, the distribution of passive/star-forming galaxies and perform comparisons with the predictions from state-of-the-art cosmological models, within the same M-* and SFR limits. We find that at the low-mass end (M-* = 10(9.5)-10(10)M(circle dot)) the sSFRF is mostly dominated by star-forming objects. However, moving to the two more massive bins (M-* = 10(10)-10(10.5) M-circle dot and M* = 10(10.5)-10(11)M(circle dot)) a bimodality with two peaks emerges. One peak represents the star-forming population, while the other describes a rising passive population. The bi-modal form of the sSFRFs is not reproduced by a range of cosmological simulations (e.g. Illustris, EAGLE, Mufasa, and IllustrisTNG) which instead generate mostly the star-forming population, while a bi-modality emerges in others (e.g. L-Galaxies, Shark, and Simba). Our findings reflect the need for the employed quenching schemes in state-of-the-artmodels to be reconsidered, involving prescriptions that allow 'quenched galaxies' to retain a small level of SF activity (sSFR = 10(-11) 10(-12) yr(-1)) and generate an adequate passive population/bi-modality even at intermediate masses (M-* = 10(10)-10(10.5)M(circle dot)).
KW - methods: numerical
KW - galaxies: evolution
KW - galaxies: formation
KW - galaxies: star formation
KW - cosmology: theory
KW - ACTIVE GALACTIC NUCLEI
KW - SIMULATING GALAXY FORMATION
KW - BLACK-HOLE GROWTH
KW - STELLAR MASS
KW - RED SEQUENCE
KW - SEMIANALYTIC MODELS
KW - COLOR DISTRIBUTIONS
KW - ILLUSTRIS PROJECT
KW - EAGLE SIMULATIONS
KW - EVOLUTION
U2 - 10.1093/mnras/staa3236
DO - 10.1093/mnras/staa3236
M3 - Journal article
VL - 500
SP - 2036
EP - 2048
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 2
ER -
ID: 299502733