论文标题
宇宙黎明的第一个类星体的诞生
Inception of a first quasar at cosmic dawn
论文作者
论文摘要
宇宙黎明最早的类星体由大量积聚到十亿个太阳能的超级质量黑洞。通过直接崩溃机制形成的大量黑洞种子被认为是最有前途的候选人，但是在宇宙早期，它们如何与宿主星系一起生长和进化仍然未知。我们在这里提出了宇宙辐射流体动力学模拟的结果10^9〜m _ {\ odot} $从$ z = 26 $下降到$ z = 16 $。我们的结果表明，MBH接近X射线的能量沉积抑制了Pop III星形的形成约12 Myr，同时这些X射线催化$ \ rm H_2 $形成，从而导致流行III星团形成500 $ \ rm m _ rm m_ _ {\ odot} $ in Close viciential的500 $ \ rm \ rm m _ {\ odot} $。我们发现，流行III的恒星形成模式由于块状积聚而在Pop II中是偶发性和爆发性，这是连续的。 $ z \ sim 16 $的主机星系的恒星质量为$ \ rm 2 \ times 10^7〜m _ {\ odot} $，带有星形形成率（sfr）的$ \ rm \ rm \ sim 0.1-1 〜m _ {\ odot}/yr $。总共，MBH增生$ \ rm 1.5 \ times 10^6〜m _ {\ odot} $在120 Myr期间，平均增生率为$ \ rm \ rm \ sim 0.01〜m _ {\ odot}/yr $，与Eddingdon的平均分数为50 \％。
Earliest quasars at the cosmic dawn are powered by mass accretion onto supermassive black holes of a billion solar masses. Massive black hole seeds forming through the direct collapse mechanism are considered the most promising candidates but how do they grow and co-evolve with their host galaxies at early cosmic times remains unknown. We here present results from a cosmological radiation hydrodynamical simulation including self-consistent modeling of both Pop III and Pop II star formation, their radiative and supernova feedback in the host galaxy along with X-ray feedback from an accreting massive black hole (MBH) of $\rm 10^5 ~M_{\odot}$ in a halo of $\rm 2 \times 10^9~M_{\odot}$ from $z=26$ down to $z=16$. Our results show that energy deposition from X-rays in the proximity of MBH suppresses Pop III star formation for about 12 Myr while at the same time these X-rays catalyze $\rm H_2$ formation which leads to the formation of a Pop III star cluster of 500 $\rm M_{\odot}$ in the close vicinity of the MBH. We find that mode of star formation for Pop III is episodic and bursty due to the clumpy accretion while for Pop II it is continuous. The stellar mass of the host galaxy at $z \sim 16$ is $\rm 2 \times 10^7~M_{\odot}$ with a star formation rate (SFR) of $\rm \sim 0.1-1~M_{\odot}/yr$. In total, the MBH accretes $\rm 1.5 \times 10^6~M_{\odot}$ during 120 Myr with the mean accretion rate of $\rm \sim 0.01~M_{\odot}/yr$ corresponding to an average Eddington fraction of 50\%.
