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Structure in the Three-dimensional Galaxy Distribution. I. Methods and Example Results
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy.
2011 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, ISSN 0004-637X, Vol. 727, no 1, 48Article in journal (Refereed) Published
Abstract [en]

Three methods for detecting and characterizing structure in point data, such as that generated by redshift surveys, are described: classification using self-organizing maps, segmentation using Bayesian blocks, and density estimation using adaptive kernels. The first two methods are new, and allow detection and characterization of structures of arbitrary shape and at a wide range of spatial scales. These methods should elucidate not only clusters, but also the more distributed, wide-ranging filaments and sheets, and further allow the possibility of detecting and characterizing an even broader class of shapes. The methods are demonstrated and compared in application to three data sets: a carefully selected volume-limited sample from the Sloan Digital Sky Survey redshift data, a similarly selected sample from the Millennium Simulation, and a set of points independently drawn from a uniform probability distribution\mdasha so-called Poisson distribution. We demonstrate a few of the many ways in which these methods elucidate large-scale structure in the distribution of galaxies in the nearby universe.

Place, publisher, year, edition, pages
2011. Vol. 727, no 1, 48
Keyword [en]
cosmology: observations, galaxies: clusters: general, large-scale structure of universe, methods: data analysis
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:uu:diva-169801DOI: 10.1088/0004-637X/727/1/48ISI: 000285992000048OAI: oai:DiVA.org:uu-169801DiVA: diva2:507977
Available from: 2012-03-07 Created: 2012-03-06 Last updated: 2015-08-13Bibliographically approved

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Way, Michael J.
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