ABSTRACT Supermassive black hole feedback is thought to be responsible for the lack of star formation, or quiescence, in a significant fraction of galaxies. We explore how observable correlations between the specific star formation rate (sSFR), stellar mass (Mstar), and black hole mass (MBH) are sensitive to the physics of black hole feedback in a galaxy formation model. We use the IllustrisTNG simulation suite, specifically the TNG100 simulation and 10 model variations that alter the parameters of the black hole model. Focusing on central galaxies at z = 0 with Mstar > 1010 M⊙, we find that the sSFR of galaxies in IllustrisTNG decreases once the energy from black hole kinetic winds at low accretion rates becomes larg...
We describe a physical model of the outflows produced as a result of gas accretion on to a black hol...
We investigate the co-evolution of the black hole accretion rate ( BHAR) and the star formation rat...
We incorporate a model for black hole growth during galaxy mergers into the semi-analytical galaxy f...
Supermassive black hole feedback is thought to be responsible for the lack of star formation, or qui...
Evidence from across the electromagnetic spectrum supports the theory that black hole (BH) feedback ...
Observations have revealed the significant growth of a population of 'quiescent' galaxies with reduc...
We present a relationship between the black hole mass, stellar mass, and star formation rate of a di...
International audienceWe describe a physical model of the outflows produced as a result of gas accre...
International audienceWe describe a physical model of the outflows produced as a result of gas accre...
We study the population of supermassive black holes (SMBHs) and their effects on massive central gal...
We study the population of supermassive black holes (SMBHs) and their effects on massive central gal...
We study the population of supermassive black holes (SMBHs) and their effects on massive central gal...
none11siThis article has been accepted for publication in MNRAS ©: 2018 The Author(s) Published by O...
We describe a physical model of the outflows produced as a result of gas accretion on to a black hol...
We describe a physical model of the outflows produced as a result of gas accretion on to a black hol...
We describe a physical model of the outflows produced as a result of gas accretion on to a black hol...
We investigate the co-evolution of the black hole accretion rate ( BHAR) and the star formation rat...
We incorporate a model for black hole growth during galaxy mergers into the semi-analytical galaxy f...
Supermassive black hole feedback is thought to be responsible for the lack of star formation, or qui...
Evidence from across the electromagnetic spectrum supports the theory that black hole (BH) feedback ...
Observations have revealed the significant growth of a population of 'quiescent' galaxies with reduc...
We present a relationship between the black hole mass, stellar mass, and star formation rate of a di...
International audienceWe describe a physical model of the outflows produced as a result of gas accre...
International audienceWe describe a physical model of the outflows produced as a result of gas accre...
We study the population of supermassive black holes (SMBHs) and their effects on massive central gal...
We study the population of supermassive black holes (SMBHs) and their effects on massive central gal...
We study the population of supermassive black holes (SMBHs) and their effects on massive central gal...
none11siThis article has been accepted for publication in MNRAS ©: 2018 The Author(s) Published by O...
We describe a physical model of the outflows produced as a result of gas accretion on to a black hol...
We describe a physical model of the outflows produced as a result of gas accretion on to a black hol...
We describe a physical model of the outflows produced as a result of gas accretion on to a black hol...
We investigate the co-evolution of the black hole accretion rate ( BHAR) and the star formation rat...
We incorporate a model for black hole growth during galaxy mergers into the semi-analytical galaxy f...