期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 500, 期 2, 页码 2036-2048出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa3236
关键词
methods: numerical; galaxies: evolution; galaxies: formation; galaxies: star formation; cosmology: theory
资金
- Tsung-Dao Lee Institute Fellowship
- Shanghai Jiao Tong University
- National Science Foundation of China [11773076, 12073078, 11833005, 11890692, 11621303]
- Shanghai Natural Science Foundation [15ZR1446700]
- Key Laboratory for Particle Physics, Astrophysics and Cosmology, Ministry of Education
- European Research Council [670193]
- ARC Centre of Excellencefor All Sky Astrophysics in 3 Dimensions (ASTRO 3D) [CE170100013]
- Danish National Research Foundation
- National Key Research and Development Program of China [2017YFA0402703]
- Chinese Academy of Sciences (CAS) through a China-Chile Joint Research Fund (CCJRF) [1809]
- STFC [ST/R000972/1] Funding Source: UKRI
The study presents the corrected specific star formation rate function (sSFRF) at different stellar mass scales and explores the distribution of passive/star-forming galaxies, finding a bimodality in sSFRF that is not replicated in some cosmological simulations. The findings reflect the necessity to reconsider the quenching schemes in state-of-the-art models, suggesting the need for prescriptions that allow quenched galaxies to exhibit some level of star formation activity.
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)).
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