On determining the shape of matter distributions

Details On determining the shape of matter distributions On determining the shape of matter distributions

2011-07-27

arxiv.org/abs/1107.5582v1

Astrophysical Journal Supplement, Volume 197, Issue 2, Article ID 30, 2011

Astronomy and Astrophysics

Astrophysics

Instrumentation and Methods for Astrophysics

8 pages, 6 figures, submitted to ApJS

Scientific paper

10.1088/0067-0049/197/2/30

A basic property of objects, like galaxies and halos that form in cosmological structure formation simulations, is their shape. Here, we critically investigate shape determination methods that are commonly used in the literature. It is found that using an enclosed integration volume and weight factors r^{-2} and r_{ell}^{-2} (elliptical radius) for the contribution of each particle or volume element in the shape tensor leads to biased axis ratios and smoothing of details when calculating the local shape as a function of distance from the center. To determine the local shape of matter distributions as a function of distance for well resolved objects (typically more than O(10^4) particles), we advocate a method that (1) uses an ellipsoidal shell (homoeoid) as an integration volume without any weight factors in the shape tensor and (2) removes subhalos.

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