宇宙大尺度结构列表

这是迄今为止发现的宇宙大尺度结构列表。所使用的测量单位是光年(光在真空中，一儒略年中传播的距离，约为9.46万亿公里)。 这个列表包括超星系团、大尺度纖維狀結構和超大類星體群(LQG)。这些结构是根据它们的最长维度列出的。 这个列表只是指物质与已定界限的耦合，而不是一般意义上的物质耦合(例如，充满整个宇宙的宇宙微波背景辐射)。本清单中的所有结构都是根据它们的主要限制是否已经确定而定义的。 有一些理由让我们对这份清单保持谨慎： 隐带，或者说银河系所占据的天空的一部分，阻挡了来自几个结构的光线，使得它们的极限不能精确地识别出来。 有些结构太远了，即使用最强大的望远镜也看不到。 有些结构没有定义的限制或端点。所有的结构都被认为是宇宙网络的一部分，这是一个决定性的观点。大多数结构被附近的星系重叠，这就产生了一个如何仔细定义结构极限的问题[需要解释]。 解释观测数据需要对引力透镜效应、红移等进行假设。 宇宙空洞是星系纤维状结构和其他大尺度结构之间的巨大空间。技术上来说，它们不是结构。它们是包含极少或根本没有星系的巨大空间。理论上它们是由宇宙形成初期的量子涨落引起的。 下面是迄今为止发现的最大空洞的列表。每个空洞都根据其最长的尺度进行排名。 Horvath, Istvan; Bagoly, Zsolt; Hakkila, Jon; Tóth, L. Viktor. Anomalies in the GRB spatial distribution. Proceedings of Science. 2014: 78. Bibcode:2014styd.confE..78H. arXiv:1507.05528 . doi:10.22323/1.233.0078 .  Horvath, Istvan; Hakkila, Jon; Bagoly, Zsolt. Possible structure in the GRB sky distribution at redshift two. Astronomy & Astrophysics. 2014, 561: id.L12. Bibcode:2014A&A...561L..12H. 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S2CID 119095484. arXiv:1901.08681 . doi:10.3847/1538-4357/ab0ebf .  Haslbauer, Moritz; Banik, Indranil; Kroupa, Pavel. The KBC void and Hubble tension contradict $\Lambda$CDM on a Gpc scale $-$ Milgromian dynamics as a possible solution. Monthly Notices of the Royal Astronomical Society. October 23, 2020, 499 (2): 2845–2883. Bibcode:2020MNRAS.499.2845H. arXiv:2009.11292 . doi:10.1093/mnras/staa2348 .  Bahcall, N. A.; Soneira, R. M. (1982) "An approximately 300 MPC void of rich clusters of galaxies" (PDF) Astrophysical Journal, Part 1, vol. 262, Nov. 15, 1982, p. 419-423. Bibcode：1982ApJ...262..419B doi:10.1086/160436 Einasto, Jaan; Einasto, Maret; Gramann, Mirt (1989) "Structure and formation of superclusters. IX - Self-similarity of voids" (PDF) Royal Astronomical Society, Monthly Notices (ISSN 0035-8711), vol. 238, May 1, 1989, p. 155-177. Bibcode：1989MNRAS.238..155E S.A. Pustilnik (SAO), D. Engels (Hamburg), A.Y. Kniazev (ESO, SAO), A.G. Pramskij, A.V. Ugryumov (SAO), H.-J. Hagen (Hamburg) (2005) [ "HS 2134+0400 - new very metal-poor galaxy, a representative of void population?"] arXiv:astro-ph/0508255v1 Bibcode：2006AstL...32..228P doi:10.1134/S1063773706040025 红移，被称为“z”，是天体物理学中的一个基本概念，用来测量类星体等天体由于远离地球而发出的光谱线移动。较高的红移值直接对应于较远的宇宙距离。