The first supermassive black holes: indications from models for future observations
The first supermassive black holes: indications from models for future observations
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DOI：
10.1093/mnras/stz551
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发表时间：
2019-02
影响因子：
4.8
通讯作者：
S. Amarantidis;J. Afonso;H. Messias;B. Henriques;Andrew J Griffin;C. Lacey;C. Lagos;V. Gonzalez-Perez-V
中科院分区：
文献类型：
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作者：
S. Amarantidis;J. Afonso;H. Messias;B. Henriques;Andrew J Griffin;C. Lacey;C. Lagos;V. Gonzalez-Perez-V
我们提出了一个探索的最早的活动星系核（AGN）在宇宙中的最先进的星系形成和演化的半解析模型和流体动力学模拟的预期检测。我们估计超大质量黑洞（SMBHs）的数量和辐射特性为$z\geq 6$，这是下一代望远镜将深入探索的红移范围，特别是通过平方公里阵列（SKA）和欧空局雅典娜X射线天文台的高能量无线电。我们发现，雅典娜将能够观察到超过5000 AGN/$\rm deg^2$在再电离时代（EoR），$6\leq z \leq 10$。类似地，对于相同的红移范围，模型/模拟表明SKA将至少探测到400 AGN/$\rm deg^2$。此外，我们强调的重要性，体积的模拟箱，以及初始物理条件的模型/模拟对它们的影响的光度函数（LF）和创建的最大规模的SMBH，我们目前观察到的EoR。此外，在每个模型/模拟中的SMBHs的吸积模式的演变之后，我们表明，虽然类星体在EoR的无线电模式中占主导地位，但即使在最高的红移下，在无线电波长处的检测仍然达到显著的数字。最后，我们提出的效果，辐射效率上的LF通过比较产生的结果与恒定值的辐射效率和更复杂的计算的基础上的自旋的每个SMBH。
We present an exploration of the expected detection of the earliest Active Galactic Nuclei (AGN) in the Universe from state-of-art galaxy formation and evolution semi-analytic models and hydro-dynamical simulations. We estimate the number and radiative characteristics of Super Massive Black Holes (SMBHs) at $z\geq 6$, 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/$\rm deg^2$ at the Epoch of Re-ionization (EoR), $6\leq z \leq 10$. Similarly, for the same redshift range the models/simulations suggest that SKA will detect at least 400 AGN/$\rm deg^2$. 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.