Abstract
We present the galactic stellar age -- velocity dispersion relation obtained from a semi-analytic model of galaxy formation. We divide galaxies into two populations: galaxies which have over-massive/under-massive black holes (BHs) against the best-fitting BH mass -- velocity dispersion relation. We find that \textcolor{red}{galaxies with larger velocity dispersion have older stellar ages. We also find that} galaxies with over-massive BHs have older stellar ages. These results are consistent with observational results obtained from Martin-Navarro et al. (2016). \textcolor{red}{We tested the model with weak AGN feedback and find that galaxies with larger velocity dispersion have a younger stellar age.}
Highlights
There is a lot of work aimed at understanding star formation histories by comparing theoretical models with observational results
We neglect the mass which might be in the dusty torus surrounding a super massive black holes (SMBHs) since it is uncertain that how the dusty tori form and grow with their host galaxies
The bright end slope of K-band luminosity function of galaxies at z ∼ 0 is sensitive to the strength of the radio-mode AGN feedback
Summary
There is a lot of work aimed at understanding star formation histories by comparing theoretical models with observational results. Recent theoretical work has revealed that in order to explain observational properties of galaxies, some feedback effects are important, which suppress star formation activities by heating or ejecting cold gas (e.g., Springel et al, 2005; Okamoto et al, 2010; Vogelsberger et al, 2014). It is necessary to compare theoretical models with “statistical” observational properties of galaxies in order to investigate the existence of AGN feedback because individual AGN has different stages of AGN and star formation activities. Martín-Navarro et al (2016) present evidence of existing AGN feedback by re-analyzing observational data They divide galaxy sample obtained from van den Bosch (2016) between “over-/under- massive black hole galaxies” following the MBH − σ relation.
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