The 3D skeleton of the SDSS

Simple item page
dc.creatorSousbie, Thierry
dc.creatorPichon, Christophe
dc.creatorCourtois, Hélène
dc.creatorColombi, Stéphane
dc.creatorNovikov, Dmitri
dc.date2006-02-28
dc.date.accessioned2026-07-07T07:00:55Z
dc.date.available2026-07-07T07:00:55Z
dc.descriptionThe length of the three-dimensional filaments observed in the fourth public data-release of the SDSS is measured using the {\em local skeleton} method. It consists in defining the set of points where the gradient of the smoothed density field is extremal along its isocontours, with some additional constraints on local curvature to probe actual ridges in the galaxy distribution. A good fit to the mean filament length per unit volume, $\cal{L}$, in the SDSS survey is found to be ${\cal{L}}=(52500\pm6500) (L/{\rm Mpc})^{-1.75\pm0.06}\rm{Mpc}/(100 \rm{Mpc})^{3}$ for $8.2 \leq L \leq 16.4$ Mpc, where $L$ is the smoothing length in Mpc. This result, which deviates only slightly, as expected, from the trivial behavior ${\cal{L}} \propto L^{-2}$, is in excellent agreement with a $Λ$CDM cosmology, as long as the matter density parameter remains in the range $0.25 < Ω_{\rm matter} < 0.4$ at one sigma confidence level, considering the universe is flat. These measurements, which are in fact dominated by linear dynamics, are not significantly sensitive to observational biases such as redshift distortion, edge effects, incompleteness, and biasing between the galaxy distribution and the dark matter distribution. Hence it is argued that the local skeleton is a rather promising and discriminating tool for the analysis of filamentary structures in three-dimensional galaxy surveys.
dc.description5 pages, 3 figures, 1 table. submitted to Apj Letters
dc.identifierhttps://arxiv.org/abs/astro-ph/0602628
dc.identifierhttp://arxiv.org/abs/astro-ph/0602628
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/108124
dc.subjectAstrophysics
dc.titleThe 3D skeleton of the SDSS
dc.typetext

Files

Collections

arXiv