The Structure of the Universe Beyond 100 Mpc

Alex Szalay宇宙的结构超过100 Mpc PI正在解决与星系的大规模分布有关的几个主要问题。对宇宙大尺度结构的研究是当今天体物理学中最动态发展的领域之一。各种宇宙学提供了涨落谱（平滑偏差）的估计。PI的这项工作有助于区分和限制各种宇宙论。特别是，PI正在测量非常大（100Mpc）尺度上星系分布的波动谱，与宇宙微波背景（CMB）波动的测量重叠。这项工作将在非常大的尺度上澄清功率谱的性质，将功率谱的小尺度和大尺度归一化锁在一起。分析技术可能在理解100毫微米以上尺度上波动的性质方面取得重大新进展。最不为人所知的，同时也是最有趣的起伏光谱部分是在100 - 300 Mpc之间的尺度上，接近相等和重组时的视界尺度，在那里我们有最有理由相信可能有什么东西留下了可探测的印记，就像CMB波动中的多普勒峰一样。＊＊＊

AST 98-02980 Alex Szalay The structure of the universe beyond 100 Mpc The PI is addressing several major questions related to the large scale distribution of galaxies. The study of large scale structure of the Universe is one of the most dynamically evolving areas of astrophysics today. Various cosmologies provide estimates of the fluctuation spectrum (deviation from smoothness). This work by the PI helps to distinguish and constrain various cosmologies. In particular, the PI is measuring the fluctuation spectrum of the galaxy distribution on very large ( 100Mpc) scales, overlapping with measurements of the cosmic microwave background (CMB) fluctuations. This work will clarify the nature of the power spectrum on very large scales, lock the small and large scale normalization of the power spectrum together. The analysis techniques may result in major new developments in understanding the nature of the fluctuations on scales over 100 Mpc. The least know, and at the same time the most interesting part of the fluctuation spectrum is on scales between 100 - 300 Mpc, close to the horizon scale at equality and recombination, where we have the most reasons to believe that something may have left a detectable imprint, like the Doppler peaks in the CMB fluctuations. ***