# Imprints of the super-Eddington accretion on the quasar clustering

## TL;DR

This study explores how super-Eddington accretion influences quasar clustering, revealing that radiative efficiency impacts the relationship between quasar luminosity and host halo mass, with implications for understanding black hole growth.

## Contribution

Introduces a semi-analytic model incorporating radiative efficiency effects of super-Eddington accretion on quasar clustering, linking accretion physics to large-scale structure observations.

## Key findings

- Quasar host halo mass depends on luminosity when limited by Eddington luminosity.
- Quasar bias aligns with observations for bright quasars under Eddington limit.
- Radiative efficiency affects the luminosity-halo mass relation.

## Abstract

Super-Eddington mass accretion has been suggested as an efficient mechanism to grow supermassive black holes (SMBHs). We investigate the imprint left by the radiative efficiency of the super-Eddington accretion process on the clustering of quasars using a new semi-analytic model of galaxy and quasar formation based on large-volume cosmological $N$-body simulations. Our model includes a simple model for the radiative efficiency of a quasar, which imitates the effect of photon trapping for a high mass accretion rate. We find that the model of radiative efficiency affects the relation between the quasar luminosity and the quasar host halo mass. The quasar host halo mass has only weak dependence on quasar luminosity when there is no upper limit for quasar luminosity. On the other hand, it has significant dependence on quasar luminosity when the quasar luminosity is limited by its Eddington luminosity. In the latter case, the quasar bias also depends on the quasar luminosity, and the quasar bias of bright quasars is in agreement with observations. Our results suggest that the quasar clustering studies can provide a constraint on the accretion disc model.