Observational properties of a general relativistic instability supernova from a primordial supermassive star
Observational properties of a general relativistic instability supernova from a primordial supermassive star
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DOI：
10.1093/mnras/stab622
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发表时间：
2021-03
影响因子：
15
通讯作者：
T. Moriya;Ke-Jung Chen;K. Nakajima;N. Tominaga;S. Blinnikov
中科院分区：
文献类型：
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作者：
T. Moriya;Ke-Jung Chen;K. Nakajima;N. Tominaga;S. Blinnikov
我们提出了一个广义相对论不稳定性超新星（GRSN）从55,500 M的原始（人口III）的星星的预期观测性质。超过104 M <$m的超大质量恒星可能存在于早期宇宙中。它们通常被认为是通过广义相对论不稳定性坍缩成为种子黑洞，形成超大质量（109 M <$）黑洞，被观测为高红移类星体。然而，其中一些可能会爆炸为GRSNe，如果爆炸性的氦燃烧解除了由广义相对论不稳定性引发的坍缩后的超大质量恒星的束缚。我们进行了辐射流体动力学模拟的GRSN开始前不久的冲击爆发。我们发现GRSN的特征是在静止坐标系中有一个持续时间长（550 d）的发光（1.5 × 1044 erg s−1）平台相，光球温度约为5000 K。当它出现在高红移时，平台相持续数十年，并且它可能在未来的深近红外成像调查中被观察到。特别是银河再电离探测器（G-REX）和詹姆斯·韦伯太空望远镜（JWST）获得的29 AB等的近红外图像，使我们能够识别到1 × 15的GRSN。更深的图像使我们能够发现更高红移的GRSNe。它们的颜色非常红，可以通过颜色信息与其他持久源（如高红移星系）区分开来。我们的结论是，即使没有时间域信息，深近红外图像也能够限制宇宙中原始超大质量恒星的GRSNe的存在。
We present the expected observational properties of a general relativistic instability supernova (GRSN) from the 55,500 M⊙ primordial (Population III) star. Supermassive stars exceeding 104 M⊙ may exist in the early Universe. They are generally considered to collapse through the general relativistic instability to be seed black holes to form supermassive (∼ 109 M⊙) black holes observed as high-redshift quasars. Some of them, however, may explode as GRSNe if the explosive helium burning unbinds the supermassive stars following the collapse triggered by the general relativistic instability. We perform the radiation hydrodynamics simulation of the GRSN starting shortly before the shock breakout. We find that the GRSN is characterized by a long-lasting (550 d) luminous (1.5 × 1044 erg s−1) plateau phase with the photospheric temperature of around 5000 K in the rest frame. The plateau phase lasts for decades when it appears at high redshifts and it will likely be observed as a persistent source in the future deep near-infrared imaging surveys. Especially, the near-infrared images reaching 29 AB magnitude that can be obtained by Galaxy and Reionization EXplorer (G-REX) and James Webb Space Telescope (JWST) allow us to identify GRSNe up to I ≃ 15. Deeper images enable us to discover GRSNe at even higher redshifts. Having extremely red color, they can be distinguished from other persistent sources such as high-redshift galaxies by using color information. We conclude that the deep near-infrared images are able to constrain the existence of GRSNe from the primordial supermassive stars in the Universe even without the time domain information.