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首页> 外文期刊>The Astrophysical journal >THE NUMBER AND OBSERVABILITY OF POPULATION III SUPERNOVAE AT HIGH REDSHIFTS
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THE NUMBER AND OBSERVABILITY OF POPULATION III SUPERNOVAE AT HIGH REDSHIFTS

机译：高红移人口III超新星的数量和可观测性

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摘要

We consider the feasibility of detecting Population III pair-instability supernovae (PISNe) at very high redshifts with the James Webb Space Telescope (JWST). Four published estimates for the PISN rate show a rather wide dispersion, between 50 and 2200 deg~(-2) yr~(-1). Correcting problems with several of these, we conclude that even a fairly optimistic estimate is probably a further order of magnitude lower than this range, at a rate of the order of 4 deg~(-2) yr~(-1) at z ～ 15 and 0.2 deg~(-2) yr~(-1) at z ～ 25, both with substantial uncertainty. Although such supernovae (SNe) would be bright enough to be readily detectable with the JWST at any relevant redshift, the lower number densities derived here would likely require either a dedicated wide-angle search strategy or a serendipitous search. We expect that typically about 1 deg~2 (or 500 JWST NIRCam images) at 4.5 μm must be imaged to detect one PISN at z ～ 15 and about 35 deg~2 to detect one at z ～ 25. If some Population III star formation persists to lower redshifts at z ～ 5, then PISNe may also be detectable in wide-angle ground-based Z-band imaging surveys at Z_(AB) ～ 23, at a density of the order of 1 deg~(-2) of surveyed area. In the Appendix we consider the possible effects of intergalactic dust in obscuring high-redshift SNe or other high-redshift sources. We show that the obscuration at a given rest wavelength will peak at some maximum redshift and thereafter decline. While it may be a significant effect in observations of the very high redshift universe, it is unlikely, even under rather pessimistic assumptions, to completely obscure primordial objects.
机译：我们考虑使用詹姆斯·韦伯太空望远镜（JWST）在很高的红移下检测III号种群对不稳定的超新星（PISNe）的可行性。 PISN速率的四个已发布的估计值显示出相当大的离散，介于50和2200 deg-（-2）yr〜（-1）之间。纠正其中的一些问题，我们得出结论，即使相当乐观的估计也可能比该范围低一个数量级，在z〜时约为4度〜（-2）yr〜（-1）。 z〜25时分别为15和0.2 deg〜（-2）yr〜（-1），均具有较大的不确定性。尽管这样的超新星（SNe）足够亮，可以在任何相关的红移情况下用JWST轻易地检测到，但此处得出的较低数字密度可能会需要专用的广角搜索策略或偶然的搜索。我们预期通常必须在4.5μm处成像约1 deg〜2（或500 JWST NIRCam图像）才能在z〜15处检测到一个PISN，而在35 deg〜2时则必须在z〜25处检测到一个PISN。在z〜5持续到较低的红移，那么PISNe在Z_（AB）〜23的广角地面Z波段成像调查中也可能被检测到，密度约为1度〜（-2）。调查区域。在附录中，我们考虑了星际尘埃可能对高红移SNe或其他高红移源造成的影响。我们表明，在给定的静止波长下的遮盖力将在某个最大红移时达到峰值，然后下降。尽管这可能对非常高的红移宇宙的观测产生重大影响，但即使在相当悲观的假设下，也不太可能完全遮盖原始物体。

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