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The geometry of the filamentary environment of galaxy clusters
Cosmology and Nongalactic Astrophysics · Submitted 3 Nov 2010
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Scatter in mock cluster mass measurements, for several observables, is often correlated with the observational direction relative to these local sheets, most often for richness and weak lensing, somewhat less for Compton decrement, and least often for velocity dispersions.
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The abstract, sentence by sentence
We construct a filament catalogue using an extension of the halo based filament finder of Zhang et al.(2009), in a 250 Mpc/h side N-body simulation, and study the properties of filaments ending upon or surrounding galaxy clusters (within 10 Mpc/h). In this region, the majority of filamentary mass, halo mass, and galaxy richness centered upon the cluster tends to lie in sheets, which are not always coincident. Fixing a sheet width of 3 Mpc/h for definiteness, we find the sheet orientations and (connected) filamentary mass, halo mass and richness fractions relative to the surrounding sphere. Filaments usually have one or more endpoints outside the sheet determined by filament or halo mass or richness, with at least one having a large probability to be aligned with the perpendicular of the plane. Scatter in mock cluster mass measurements, for several observables, is often correlated with the observational direction relative to these local sheets, most often for richness and weak lensing, somewhat less for Compton decrement, and least often for velocity dispersions. The long axis of the cluster also tends to lie in the sheet andits orientiation relative to line of sight also correlates with mass scatter.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We construct a filament catalogue using an extension of the halo based filament finder of Zhang et al.(2009), in a 250 Mpc/h side N-body simulation, and study the properties of filaments ending upon or surrounding galaxy clusters (within 10 Mpc/h). | method 0.67 | 0.94 | 0.05 | asserted 0.98 |
| s1 | In this region, the majority of filamentary mass, halo mass, and galaxy richness centered upon the cluster tends to lie in sheets, which are not always coincident. | result 1.00 | 0.88 | 0.35 | asserted 0.98 |
| s2 | Fixing a sheet width of 3 Mpc/h for definiteness, we find the sheet orientations and (connected) filamentary mass, halo mass and richness fractions relative to the surrounding sphere. | method 0.96 | 0.94 | 0.06 | asserted 0.96 |
| s3 | Filaments usually have one or more endpoints outside the sheet determined by filament or halo mass or richness, with at least one having a large probability to be aligned with the perpendicular of the plane. | result 1.00 | 0.91 | 0.20 | asserted 0.80 |
| s4 | Scatter in mock cluster mass measurements, for several observables, is often correlated with the observational direction relative to these local sheets, most often for richness and weak lensing, somewhat less for Compton decrement, and least often for velocity dispersions. | result 1.00 | 0.88 | 0.18 | asserted 0.84 |
| s5 | The long axis of the cluster also tends to lie in the sheet andits orientiation relative to line of sight also correlates with mass scatter. | result 1.00 | 0.90 | 0.16 | asserted 0.83 |
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Original abstract
We construct a filament catalogue using an extension of the halo based filament finder of Zhang et al.(2009), in a 250 Mpc/h side N-body simulation, and study the properties of filaments ending upon or surrounding galaxy clusters (within 10 Mpc/h). In this region, the majority of filamentary mass, halo mass, and galaxy richness centered upon the cluster tends to lie in sheets, which are not always coincident. Fixing a sheet width of 3 Mpc/h for definiteness, we find the sheet orientations and (connected) filamentary mass, halo mass and richness fractions relative to the surrounding sphere. Filaments usually have one or more endpoints outside the sheet determined by filament or halo mass or richness, with at least one having a large probability to be aligned with the perpendicular of the plane. Scatter in mock cluster mass measurements, for several observables, is often correlated with the observational direction relative to these local sheets, most often for richness and weak lensing, somewhat less for Compton decrement, and least often for velocity dispersions. The long axis of the cluster also tends to lie in the sheet andits orientiation relative to line of sight also correlates with mass scatter.
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How the literature uses it
2 arXiv papers cite this in 2 sentences
What it cites · 12 sentences without a confident label
Compares with 2 papers
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We find more massive halos have more filaments ending upon them, shown in Fig. [ref], bottom, just as found by [ref] with their different finders.
Multiscale Phenomenology of the Cosmic Web · Statistics of filaments around clusters · 0.92
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The work most similar to ours in focus, studying clusters as filament endpoints, is in [ref] , some related results are also found and compared in [ref] (see also [ref] , who found a cluster as an intersection of filaments in observational data).
The persistent cosmic web and its filamentary structure II: Illustrations · Filament finder · 0.84
Cites as background 26 papers
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The environments of clusters have been studied within several contexts and using several methods, e.g. galaxy and dark matter density around clusters [ref] , filamentary growth (e.g. [ref] ) around clusters, filamentary counts [ref] , in particular the geometry and properties of superclusters, e.g., [ref] , and the cluster alignment studies such as mentioned above.
Multiscale Phenomenology of the Cosmic Web · Introduction · 0.98
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The environments of clusters have been studied within several contexts and using several methods, e.g. galaxy and dark matter density around clusters [ref] , filamentary growth (e.g. [ref] ) around clusters, filamentary counts [ref] , in particular the geometry and properties of superclusters, e.g., [ref] , and the cluster alignment studies such as mentioned above.
Clusters and the Cosmic Web · Introduction · 0.98
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The environments of clusters have been studied within several contexts and using several methods, e.g. galaxy and dark matter density around clusters [ref] , filamentary growth (e.g. [ref] ) around clusters, filamentary counts [ref] , in particular the geometry and properties of superclusters, e.g., [ref] , and the cluster alignment studies such as mentioned above.
Morphological Properties of Superclusters of Galaxies · Introduction · 0.98
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