论文标题
宇宙的电源可能仍在早期开始并结束很晚：与CMB各向异性和21厘米全球信号面对面
Cosmic Reionization May Still Have Started Early and Ended Late: Confronting Early Onset with CMB Anisotropy and 21 cm Global Signals
论文作者
论文摘要
三个光晕质量组释放的星光的相对数量的相对量形成了全球电离历史：原子冷却晕圈（ACHS），病毒温度> 10^4 K，即（1）即使在恢复后（hmachs，> 〜10^9 msun）或（2）抑制（lmassive）的（lmassive sopression sar sartressions），即使在重新离子（hmachs> 〜10^9 ms）中形成恒星，并在恒星中进行抑制（ H2-Cooling Minihalos（MHS），带有TVIR <10^4 K，其星形形成主要受H2隔离的Lyman-Werner（LW）背景抑制。我们先前的工作表明，包括MHS引起了两阶段的电源 - 由MHS驱动，然后迅速上升到X〜0.1，随后迅速上升到X〜1，由ACHS驱动 - 在CMB极化各向异性中具有签名，预计将被Planck Satellite检测到。在此预测的激励下，我们对全局校准半分析进行了与Planck CMB数据和边缘全局21cm吸收功能进行比较，用于以下模型：（1）ACHS，无反馈； （2）ACH，自我调节； （3）ACH和MHS，自我调节。模型（3）与普朗克电子模式极化数据非常吻合，即使是高还原电离的大量尾巴，超出了普朗克协作（2018）提出的极限。没有模型复制边缘特征。对于型号（3），| DTB | <〜60 mk的边缘槽，一个数量级的较浅，吸收始于较高的Z，但在频谱上是毫无特色的。 MHS中人口III星人的早期发作与当前的限制兼容，但前提是折现边缘解释，或者我们不包含其包含帐户的其他过程。
The global history of reionization was shaped by the relative amounts of starlight released by three halo mass groups: atomic-cooling halos (ACHs) with virial temperatures Tvir > 10^4 K, either (1) massive enough to form stars even after reionization (HMACHs, >~ 10^9 Msun) or (2) less-massive (LMACHs), subject to star formation suppression when overtaken by reionization, and (3) H2-cooling minihalos (MHs) with Tvir < 10^4 K, whose star formation is predominantly suppressed by the H2-dissociating Lyman-Werner (LW) background. Our previous work showed that including MHs caused two-stage reionization - early rise to x ~ 0.1, driven by MHs, followed by a rapid rise, late, to x ~ 1, driven by ACHs - with a signature in CMB polarization anisotropy predicted to be detectable by the Planck satellite. Motivated by this prediction, we model global reionization semi-analytically for comparison with Planck CMB data and the EDGES global 21cm absorption feature, for models with: (1) ACHs, no feedback; (2) ACHs, self-regulated; and (3) ACHs and MHs, self-regulated. Model (3) agrees well with Planck E-mode polarization data, even with a substantial tail of high-redshift ionization, beyond the limit proposed by the Planck Collaboration (2018). No model reproduces the EDGES feature. For model (3), |dTb| <~ 60 mK across the EDGES trough, an order of magnitude too shallow, and absorption starts at higher z but is spectrally featureless. Early onset reionization by Population III stars in MHs is compatible with current constraints, but only if the EDGES interpretation is discounted or else other processes we did not include account for it.
