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

Tempel, Elmo; Tamm, A.; Gramann, Mirt; Tuvikene, T.; Liivamägi, L. J.; Suhhonenko, I.; Kipper, Rain; Einasto, M.; Saar, E.

doi:10.1051/0004-6361/201423585

Cited by 219 publications

(494 citation statements)

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“…We selected data about superclusters and their galaxy and group content from the supercluster and group catalogues by Liivamägi et al (2012) and Tempel et al (2012Tempel et al ( , 2014. These catalogues are based on the MAIN sample of the eighth and tenth data release of the SDSS (Aihara et al 2011;Ahn et al 2014) with apparent Galactic extinction-corrected r magnitudes r ≤ 17.77 and redshifts 0.009 ≤ z ≤ 0.200.…”

Section: Datamentioning

confidence: 99%

Sloan Great Wall as a complex of superclusters with collapsing cores

Einasto

Lietzen

Gramann

et al. 2016

A&A

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Context. The formation and evolution of the cosmic web is governed by the gravitational attraction of dark matter and antigravity of dark energy (cosmological constant). In the cosmic web, galaxy superclusters or their high-density cores are the largest objects that may collapse at present or during the future evolution. Aims. We study the dynamical state and possible future evolution of galaxy superclusters from the Sloan Great Wall (SGW), the richest galaxy system in the nearby Universe. Methods. We calculated supercluster masses using dynamical masses of galaxy groups and stellar masses of galaxies. We employed normal mixture modelling to study the structure of rich SGW superclusters and search for components (cores) in superclusters. We analysed the radial mass distribution in the high-density cores of superclusters centred approximately at rich clusters and used the spherical collapse model to study their dynamical state. Results. The lower limit of the total mass of the SGW is approximately M = 2.5 × 10 16 h −1 M . Different mass estimators of superclusters agree well, the main uncertainties in masses of superclusters come from missing groups and clusters. We detected three high-density cores in the richest SGW supercluster (SCl 027) and two in the second richest supercluster (SCl 019). They have masses of 1.2−5.9 × 10 15 h −1 M and sizes of up to ≈60 h −1 Mpc. The high-density cores of superclusters are very elongated, flattened perpendicularly to the line of sight. The comparison of the radial mass distribution in the high-density cores with the predictions of spherical collapse model suggests that their central regions with radii smaller than 8 h −1 Mpc and masses of up to M = 2 × 10 15 h −1 M may be collapsing. Conclusions. The rich SGW superclusters with their high-density cores represent dynamically evolving environments for studies of the properties of galaxies and galaxy systems.

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Section: Datamentioning

confidence: 99%

Sloan Great Wall as a complex of superclusters with collapsing cores

Einasto

Lietzen

Gramann

et al. 2016

A&A

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“…in Chernin & Teerikorpi 2014). We have also marked the location (SDSS groups) around which the galaxy groups (with less than 50 members) extracted from the SDSS-DR10 survey are concentrated (masses from the virial theorem; Tempel et al 2014). …”

Section: Example Systems Of Galaxiesmentioning

confidence: 99%

A graph of dark energy significance on different spatial and mass scales

Teerikorpi

Heinämäki

Nurmi

et al. 2015

A&A

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Context. The current cosmological paradigm sees the formation and evolution of the cosmic large-scale structure as governed by the gravitational attraction of dark matter (DM) and the repulsion of dark energy (DE). Aims. We characterize the relative importance of uniform and constant dark energy, as given by the Λ term in the standard ΛCDM cosmology, in galaxy systems of different scales from groups to superclusters.Methods. An instructive "Λ significance graph" is introduced where the matter-DE density ratio ρ M /ρ Λ for different galaxy systems is plotted against the radius R. This presents gravitation-and DE-dominated regions and directly shows the zero velocity radius, the zero-gravity radius, and the Einstein-Straus radius for any fixed value of mass. Results. Example galaxy groups and clusters from the local universe illustrate the use of the Λ significance graph. These are generally located deep in the gravity-dominated region ρ M /ρ Λ > 2, and are virialized. Extended clusters and the main bodies of superclusters can reach down near the borderline between gravity-dominated and DE-dominated regions ρ M /ρ Λ = 2. The scale-mass relation from the standard two-point correlation function intersects this balance line near the correlation length. Conclusions. The log ρ M /ρ Λ vs. log R diagram is a useful and versatile way to characterize the dynamical state of systems of galaxies within the Λ-dominated expanding universe.

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“…We use the galaxy and group samples as compiled in Tempel et al (2014b) that cover the main contiguous area of the survey. The flux-limited catalogue extends to 574 h −1 Mpc and includes 588193 galaxies and 82458 groups.…”

Section: Galaxy Samplementioning

confidence: 99%

“…The flux-limited catalogue extends to 574 h −1 Mpc and includes 588193 galaxies and 82458 groups. In Tempel et al (2014b) the finger-of-god effect is suppressed using the detected galaxy groups.…”

Section: Galaxy Samplementioning

confidence: 99%

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Detecting multi-scale filaments in galaxy distribution

Tempel

2014

Proc. IAU

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Abstract. The main feature of the spatial large-scale galaxy distribution is its intricate network of galaxy filaments. This network is spanned by the galaxy locations that can be interpreted as a three-dimensional point distribution. The global properties of the point process can be measured by different statistical methods, which, however, do not describe directly the structure elements. The morphology of the large-scale structure, on the other hand, is an important property of the galaxy distribution. Here, we apply an object point process with interactions (the Bisous model) to trace and extract the filamentary network in the presently largest galaxy redshift survey, the Sloan Digital Sky Survey (SDSS data release 10). We search for multi-scale filaments in the galaxy distribution that have a radius of about 0.5, 1.0, 2.0, and 4.0 h −1 Mpc. We extract the spines of the filamentary network and divide the detected network into single filaments.

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

Cited by 219 publications

References 100 publications

Sloan Great Wall as a complex of superclusters with collapsing cores

Sloan Great Wall as a complex of superclusters with collapsing cores

A graph of dark energy significance on different spatial and mass scales

Detecting multi-scale filaments in galaxy distribution

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