The first supermassive black holes: indications from models for future observations. Issue 2 (26th February 2019)

• Record Type: Journal Article
• Authors: Amarantidis, Stergios; Afonso, José; Messias, Hugo; Henriques, Bruno; Griffin, Andrew; Lacey, Cedric; Lagos, Claudia del P; Gonzalez-Perez, Violeta; Dubois, Yohan; Volonteri, Marta; Matute, Israel; Pappalardo, Ciro; Qin, Yuxiang; Chary, Ranga-Ram; Norris, Ray P
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 485:Issue 2(2019)
• Page Start: 2694
• Page End: 2709
• Publication Date: 2019-02-26
• Subjects: galaxies: high-redshift -- quasars: general -- radio continuum: galaxies -- X-rays: galaxies; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz551
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We present an exploration of the expected detection of the earliest active galactic nuclei (AGNs) in the Universe from state-of-art galaxy formation and evolution semi-analytic models and hydrodynamical simulations. We estimate the number and radiative characteristics of supermassive black holes (SMBHs) at z ≥ 6, a redshift range that will be intensively explored by the next generation of telescopes, in particular in the radio through the Square Kilometre Array (SKA) and at high energies with ESA's Athena X-ray Observatory. We find that Athena will be able to observe over 5000 AGN deg −2 at the Epoch of Re-ionization (EoR), 6 ≤ z ≤ 10. Similarly, for the same redshift range the models/simulations suggest that SKA will detect at least 400 AGN deg −2 . Additionally, we stress the importance of the volume of the simulation box as well as the initial physical conditions of the models/simulations on their effect on the luminosity functions (LFs) and the creation of the most massive SMBHs that we currently observe at the EoR. Furthermore, following the evolution of the accretion mode of the SMBHs in each model/simulation, we show that, while the quasar dominates over the radio mode at the EoR, detection at radio wavelengths still reaches significant numbers even at the highest redshifts. Finally, we present the effect that the radiative efficiency has on the LFs by comparing results produced with a constant value for the radiative efficiency and more complex calculations based on the spin of each SMBH.