第一批氢原子恒星在红移20处的特征
The signature of the first stars in atomic hydrogen at redshift 20
摘要：
暗物质和重子物质在早期宇宙中以不同的速度运动，这强烈抑制了某些区域的恒星形成。据估计，这在与恒星相关的21厘米谱线上留下了约2 mK的大尺度波动信号，红移为20，尽管这一估计忽略了由于X射线和抑制的主要增强而导致的气体加热的关键贡献。巨大的速度差减少了晕的丰度，并要求第一批恒星形成大约100万太阳质量的晕，大大超过先前的预期。在这里，我们报告了第一批恒星在z=20（宇宙年龄~ 1.8亿年）的分布模拟，将所有这些成分在一个400 Mpc的盒子。我们发现，这些恒星的21厘米签名是一个增强的（10 mK）的波动信号在100 Mpc的规模，其特征在于一个平坦的功率谱与突出的重子声学振荡。使用Murchison宽场阵列或低频阵列等仪器，但设计为在50-100 MHz范围内工作，可以在1000小时的积分时间内实现看到该信号所需的灵敏度。
英文摘要：
Dark and baryonic matter moved at different velocities in the early Universe, which strongly suppressed star formation in some regions. This was estimated to imprint a large-scale fluctuation signal of about 2 mK in the 21-cm spectral line of atomic hydrogen associated with stars at a redshift of 20, although this estimate ignored the critical contribution of gas heating due to X-rays and major enhancements of the suppression. A large velocity difference reduces the abundance of halos and requires the first stars to form in halos of about a million solar masses, substantially greater than previously expected. Here we report a simulation of the distribution of the first stars at z=20 (cosmic age of ~180 Myr), incorporating all these ingredients within a 400 Mpc box. We find that the 21-cm signature of these stars is an enhanced (10 mK) fluctuation signal on the 100-Mpc scale, characterized by a flat power spectrum with prominent baryon acoustic oscillations. The required sensitivity to see this signal is achievable with an integration time of a thousand hours with an instrument like the Murchison Wide-field Array or the Low Frequency Array but designed to operate in the range of 50-100 MHz.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
