论文标题
使用长波长阵列搜索宇宙黎明
Using the Long Wavelength Array to Search for Cosmic Dawn
论文作者
论文摘要
从第一颗恒星的形成（称为宇宙黎明或第一光）中寻找氢的光谱特征是世界各地的持续努力。该签名应作为21厘米过渡的温度相对于宇宙微波背景的温度降低，并被认为位于100 MHz以下的位置。该实验发表了潜在的检测，以检测全局EOR信号（边缘）的合作，其剖面构成了大约78 MHz的意外深度和宽度（Bowmanet。Al2018; arxiv：arxiv：1810.05912）。如果得到验证，则该检测将对$λ$ CDM宇宙学内的当前结构形成范式产生深远的影响。我们提出了一种尝试检测边缘合作与位于美国新墨西哥州塞维利塔国家野生动物保护区（LWA-SV）的长波长阵列站报告的光谱签名。 LWA-SV与其他仪器不同，因为它是256个元件天线阵列，并提供了光束成形功能，应有助于校准和检测。我们报告了LWA-SV的第一个限制，并着眼于提高这些限制的未来计划。
The search for the spectral signature of hydrogen from the formation of the first stars, known as Cosmic Dawn or First Light, is an ongoing effort around the world. The signature should present itself as a decrease in the temperature of the 21-cm transition relative to that of the Cosmic Microwave Background and is believed to reside somewhere below 100 MHz. A potential detection was published by the Experiment to Detect the Global EoR Signal (EDGES) collaboration with a profile centered around 78 MHz of both unexpected depth and width (Bowman et. al 2018; arXiv:1810.05912). If validated, this detection will have profound impacts on the current paradigm of structure formation within $Λ$CDM cosmology. We present an attempt to detect the spectral signature reported by the EDGES collaboration with the Long Wavelength Array station located on the Sevilleta National Wildlife Refuge in New Mexico, USA (LWA-SV). LWA-SV differs from other instruments in that it is a 256 element antenna array and offers beamforming capabilities that should help with calibration and detection. We report first limits from LWA-SV and look toward future plans to improve these limits.
