Classical bulges, supermassive blackholes and AGN feedback: Extension to low-mass galaxies

Abstract

The empirical model of Lu et al. 2014a for the relation between star formation rate and halo mass growth is adopted to predict the classical bulge mass ($M_{\mathrm{cb}}$) - total stellar mass ($M_{\star }$) relation for central galaxies. The assumption that the supermassive black hole (SMBH) mass ($M_{\mathrm{BH}}$) is directly proportional to the classical bulge mass, with the proportionality given by that for massive galaxies, predicts a $M_{\mathrm{BH}}$ - $M_{\star }$ relation that matches well the observed relation for different types of galaxies. In particular, the model reproduces the strong transition at $M_{\star }=10^{10.5}$ - $10^{11}{M}_{\odot }$, below which $M_{\mathrm{BH}}$ drops rapidly with decreasing $M_{\star }$. Our model predicts a new sequence at $M_{\star }<10^{10.5}{M}_{\odot }$, where $M_{\mathrm{BH}}\propto M_{\star }$ but the amplitude is a factor of $\sim 50$ lower than the amplitude of the sequence at $M_{\star }>10^{11}{M}_{\odot }$. If all SMBH grow through similar quasar modes with a feedback efficiency of a few percent, the energy produced in low-mass galaxies at redshift $z\gtrsim 2$ can heat the circum-galactic medium up to a specific entropy level that is required to prevent excessive star formation in low-mass dark matter halos.

arXiv comment5 pages, 3 figures, submitted to Astrophysical Journal

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