Abstract
Observational results suggest the co-evolution relationship between the supermassive black holes (SMBHs) and their host galaxies. However, the definitive conclusion of the correlation between the star formation rate (SFR) and central black hole accretion rate (BHAR) remains unclear. In this paper, the correlation between the BHAR and SFR is investigated in terms of cosmological simulation IllustrisTNG100-1. In simulation, BHs are divided into 2 types (quasar state and kinetic state) based on their accretion speed and the feedback mechanisms between the two are different. The strong positive correlation between BHAR and SFR for quasar state BHs and low-mass kinetic state BHs is revealed. However, for high mass kinetic-state BHs, the SFR manifestation a BHAR and BH mass-independent randomly distribution. According to the analysis, this phenomenon is attributed to the environmentally insensitive, self-regulate accretion rate for high mass BHs at late time. The properties of these BHs are described, which offers a guideline for high mass AGNs observation and theorical investigations on their accretion and feedback.
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