SDSS DR7 superclusters

Liivamägi, L. J.; Tempel, Elmo; Saar, E.

doi:10.1051/0004-6361/201016288

Cited by 139 publications

(320 citation statements)

References 44 publications

(79 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%

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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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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%

“…Details of the calculation of the density fields are given in Liivamägi et al (2012). For consistency reasons, a brief description is given below.…”

Section: Appendix A: the Cataloguesmentioning

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

222

488

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“…Connected volumes above a certain density threshold were defined as superclusters. The calculation of the luminosity density field, corrections for the faint galaxies missing from the catalogue, and determination of superclusters are described in detail in Liivamägi et al (2012).…”

Section: Datamentioning

confidence: 99%

“…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%

“…Einasto et al (2003Einasto et al ( , 2008 noted that in the core region of the richest supercluster in the SGW (SCl 126 in their study, SCl 027 in Liivamägi et al 2012, this notation is also used in our study) the concentration of galaxy clusters in a sphere with diameter smaller than 10 h −1 Mpc is very high. This region is a good candidate for a collapsing core of the supercluster.…”

Section: Introductionmentioning

confidence: 99%

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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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