Detecting filamentary pattern in the cosmic web: a catalogue of filaments for the SDSS

Tempel, Elmo; Stoica, Radu; Martı́nez, Vicent J.; Liivamägi, L. J.; Castellan, Gwénaëlle; Saar, E.

doi:10.1093/mnras/stt2454

Cited by 253 publications

(427 citation statements)

References 103 publications

(133 reference statements)

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“…As a next step, we plan to use the new catalogue to map the large-scale galactic filaments (similarly to Tempel et al 2014) and to construct a catalogue of superclusters (similarly to Liivamägi et al 2012). …”

Section: Discussionmentioning

confidence: 99%

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Tempel

Tamm

Gramann

et al. 2014

A&A

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230

488

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We provide flux-and volume-limited galaxy group and cluster catalogues based on the spectroscopic sample of the galaxies of SDSS data release 10. We used a modified friends-of-friends method with a variable linking length in the transverse and radial directions to identify as many realistic groups as possible. The flux-limited catalogue incorporates galaxies down to m r = 17.77 mag. It includes 588 193 galaxies and 82 458 groups. The volume-limited catalogues are complete for absolute magnitudes down to M r,lim = −18.0, −18.5, −19.0, −19.5, −20.0, −20.5, and −21.0; the completeness is achieved within different spatial volumes. Our analysis shows that flux-and volume-limited group samples are well compatible, especially for the larger groups/clusters. Dynamical mass estimates based on radial velocity dispersions and group extent in the sky were added to the extracted groups.

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Section: Discussionmentioning

confidence: 99%

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Tempel

Tamm

Gramann

et al. 2014

A&A

Self Cite

230

488

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“…From this catalogue we extracted galaxy filaments which had at least one member galaxy from the A2142 supercluster with distance d ≤ 0.8 h −1 Mpc from the filament axis, as defined for filament members in Tempel et al (2014a). From this initial sample we included in our sample of A2142 filaments those with member galaxies with global density D8 ≥ 4.8.…”

Section: Galaxy Filamentsmentioning

confidence: 99%

Unusual A2142 supercluster with a collapsing core: distribution of light and mass

Einasto

Gramann

Saar

et al. 2015

A&A

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Context. Superclusters of galaxies can be used to test cosmological models of the formation and evolution of the largest structures in the cosmic web, and of galaxy and cluster evolution in superclusters. Aims. We study the distribution, masses, and dynamical properties of galaxy groups in the A2142 supercluster. Methods. We analyse the global luminosity density distribution in the supercluster and divide the supercluster into the high-density core and the low-density outskirts regions. We find galaxy groups and filaments in these regions, calculate their masses and mass-tolight ratios and analyse their dynamical state with 1D and 3D statistics. We use the spherical collapse model to study the dynamical state of the supercluster. Results. In the A2142 supercluster rich groups and clusters lie along an almost straight line forming the 50 h −1 Mpc long main body of the supercluster. The A2142 supercluster has a very high density core surrounded by lower-density outskirts. The total estimated mass of the supercluster is M est = 6.2 × 10 15 M . More than a half of groups with at least ten member galaxies in the supercluster lie in the high-density core of the supercluster, centred at the X-ray cluster A2142. Most of the groups in the core region are multimodal. In the outskirts of the supercluster, the number of groups is larger than in the core, and groups are poorer. The orientation of the axis of the cluster A2142 follows the orientations of its X-ray substructures and radio halo, and is aligned along the supercluster axis. The high-density core of the supercluster with the global density D8 ≥ 17 and perhaps with D8 ≥ 13 may have started to collapse. Conclusions. A2142 supercluster with collapsing core and straight body, is an unusual object among superclusters. In the course of the future evolution, the supercluster may split into several systems.

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“…The halos themselves have different morphologies; they can be in overdense or underdense environments, and they can inhabit different types of structures in the cosmic web. Halos in simulations, and galaxies in observations, are found in filaments, walls, and voids, and obviously there are many in clusters and superclusters [22,23,48,49]. In this section, we investigate the morphological dependence of the Vainshtein mechanism for dark matter halos.…”

Section: Dark Matter Halosmentioning

confidence: 99%

The Vainshtein mechanism in the cosmic web

Falck

Koyama

Zhao

et al. 2014

J. Cosmol. Astropart. Phys.

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We investigate the dependence of the Vainshtein screening mechanism on the cosmic web morphology of both dark matter particles and halos as determined by ORIGAMI. Unlike chameleon and symmetron screening, which come into effect in regions of high density, Vainshtein screening instead depends on the dimensionality of the system, and screened bodies can still feel external fields. ORIGAMI is well-suited to this problem because it defines morphologies according to the dimensionality of the collapsing structure and does not depend on a smoothing scale or density threshold parameter. We find that halo particles are screened while filament, wall, and void particles are unscreened, and this is independent of the particle density. However, after separating halos according to their large scale cosmic web environment, we find no difference in the screening properties of halos in filaments versus halos in clusters. We find that the fifth force enhancement of dark matter particles in halos is greatest well outside the virial radius. We confirm the theoretical expectation that even if the internal field is suppressed by the Vainshtein mechanism, the object still feels the fifth force generated by the external fields, by measuring peculiar velocities and velocity dispersions of halos. Finally, we investigate the morphology and gravity model dependence of halo spins, concentrations, and shapes.

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Detecting filamentary pattern in the cosmic web: a catalogue of filaments for the SDSS

Cited by 253 publications

References 103 publications

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Unusual A2142 supercluster with a collapsing core: distribution of light and mass

The Vainshtein mechanism in the cosmic web

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