Glimmering in the Dark: Modeling the Low-mass End of the M ∙-σ Relation and of 
the Quasar Luminosity Function

Pacucci, Fabio; Loeb, Abraham; Mezcua, Mar; Martín-Navarro, Ignacio

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Journal Article

Glimmering in the Dark: Modeling the Low-mass End of the M _∙-σ Relation and of the Quasar Luminosity Function

MPS-Authors

Pacucci, Fabio
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Loeb, Abraham
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mezcua, Mar
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Martín-Navarro, Ignacio
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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https://ui.adsabs.harvard.edu/abs/2018ApJ...864L...6P
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Citation

Pacucci, F., Loeb, A., Mezcua, M., & Martín-Navarro, I. (2018). Glimmering in the Dark: Modeling the Low-mass End of the M _∙-σ Relation and of the Quasar Luminosity Function. The Astrophysical Journal, 864.

Cite as: https://hdl.handle.net/21.11116/0000-0005-CBDC-F

Abstract

The {M}_\bullet{--}σ relation establishes a connection between central black holes (BHs) and their host spheroids. Supported by observations at {M}_\bullet≳ {10}⁵ {M}_☉, there is limited data on its validity at lower masses. Employing a semi-analytical model to simulate the combined evolution of BHs and their host galaxies, we predict the observational consequences of assuming a bimodality in the accretion efficiency of BHs, with low-mass BHs ({M}_\bullet≲ {10}⁵ {M}_☉) accreting inefficiently. We predict a departure from the {M}_\bullet{--}σ relation at a transitional BH mass ̃ {10}⁵ {M}_☉, with lower-mass BHs unable to reach the mass dictated by the relation and becoming disconnected from the evolution of the host galaxy. This prediction is an alternative to previous works suggesting a flattening of the relation at ̃ {10}⁵{--}{10}⁶ {M}_☉. Furthermore, we predict a deficit of BHs shining at bolometric luminosities ̃ {10}⁴² {erg} {{{s}}}^-1. Joined with a detection bias, this could partly explain the scarce number of intermediate-mass BHs detected. Conversely, we predict an increase in source density at lower bolometric luminosities, < {10}⁴² {erg} {{{s}}}^-1. Because our predictions assume a bimodal population of high-redshift BH seeds, future observations of fainter BHs will be fundamental for constraining the nature of these seeds.