Galaxy groups in the 2dFGRS: the group-finding algorithm and the 2PIGG catalogue

Eke, V. R.; Baugh, Carlton M.; Cole, Shaun; Frenk, Carlos S.; Norberg, Peder; Peacock, J. A.; Baldry, I. K.; Bland-Hawthorn, Joss; Bridges, Terry; Cannon, R. D.; Colless, Matthew; Collins, Chris; Couch, Warrick J.; Dalton, Gavin; Propris, Roberto De; Driver, Simon P.; Efstathiou, G.; Ellis, Richard S.; Glazebrook, Karl; Jackson, C. A.; Lahav, O.; Lewis, Ian; Lumsden, S. L.; Maddox, Steve; Madgwick, Darren; Peterson, Bruce A.; Sutherland, William J.; Taylor, Keith

doi:10.1111/j.1365-2966.2004.07408.x

Cited by 344 publications

(466 citation statements)

References 46 publications

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“…The value b com is given in units of the mean pairwise separation of galaxies in the survey. Eke et al (2004) is redshift dependent (because of the constant LL in physical units) and is slightly lower (up to 0.12) than that used by Eke et al (2004) and Berlind et al (2006). The ratio of the radial-totransversal LLs in our catalogues is slightly lower than in Eke et al (2004) and higher than in Berlind et al (2006).…”

Section: Construction Of Volume-limited Groups/clustersmentioning

confidence: 84%

“…One may argue whether it might be better to use an ellipsoidal LL distribution. Tests have shown, however, that the cylindrical kernel reproduces recovered galaxy groups better (Eke et al 2004).…”

Section: Flux-limited Galaxy Groups/clustersmentioning

confidence: 99%

“…Eke et al (2004) is redshift dependent (because of the constant LL in physical units) and is slightly lower (up to 0.12) than that used by Eke et al (2004) and Berlind et al (2006). The ratio of the radial-totransversal LLs in our catalogues is slightly lower than in Eke et al (2004) and higher than in Berlind et al (2006). Compared with our previous volume-limited catalogues based on SDSS DR7 (Tago et al 2010), the LL values used in this paper are higher by up to 50%, depending on the volume-limited sample and distance.…”

Section: Construction Of Volume-limited Groups/clustersmentioning

confidence: 99%

“…In several papers (e.g. Eke et al 2004;Berlind et al 2006;Yang et al 2007;Robotham et al 2011) the mock catalogues were used to find the "best" values for FoF parameters. However, no universally good value exists.…”

Section: Flux-limited Galaxy Groups/clustersmentioning

confidence: 99%

“…Today, many extensive FoF group and cluster catalogues are available, varying in the sample data and details of the group-finder algorithm (e.g. Tucker et al 2000;Eke et al 2004;Tago et al 2006Tago et al , 2008.…”

Section: Introductionmentioning

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

222

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: Construction Of Volume-limited Groups/clustersmentioning

confidence: 84%

Section: Flux-limited Galaxy Groups/clustersmentioning

confidence: 99%

Section: Construction Of Volume-limited Groups/clustersmentioning

confidence: 99%

Section: Flux-limited Galaxy Groups/clustersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

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

Tempel

Tamm

Gramann

et al. 2014

A&A

222

488

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Clusters and groups of galaxies in the 2dF galaxy redshift survey: A new catalogue

Tago¹,

Einasto²,

Saar³

et al. 2006

Astron. Nachr.

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We create a new catalogue of groups and clusters, applying the friends-of-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N -body simulations and compare properties of these haloes and the 2dF groups. We show that at large distances from the observer luminous and intrinsically greater groups dominate, but in these groups only very bright members are seen, which form compact cores of the groups. These two effects almost cancel each other, so that the mean sizes and densities of groups do not change considerably with distance. Our final sample contains 10750 groups in the Northern part, and 14465 groups in the Southern part of the 2dF survey with membership N gal ≥ 2. We estimate the total luminosities of our groups, correcting for group members fainter than the observational limit of the survey. The cluster catalogue is available at our web-site

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The environmental dependence of the stellar mass of active galactic nucleus host galaxies and dependence of the clustering properties of active galactic nucleus host galaxies on the stellar mass

Deng

Wen

2021

Astron Nachr

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We used two volume-limited active galactic nucleus (AGN) host galaxy samples constructed by Deng & Wen (2020, RMxAA, 56, 87), and explored the environmental dependence of the stellar mass of AGN host galaxies. In the luminous volume-limited AGN host galaxy sample, the stellar mass of AGN host galaxies apparently depends on local environments: high mass AGN host galaxies exist preferentially in the dense regions of the universe, while low mass AGN host galaxies are located preferentially in low density regions. But in the faint volume-limited AGN host galaxy sample, this dependence is fairly weak. We also examined the dependence of the clustering properties of AGN host galaxies on the stellar mass by cluster analysis, and found that in the luminous volume-limited AGN host galaxy sample, low mass AGN host galaxies preferentially form isolated galaxies, close pairs, and small groups, while high mass AGN host galaxies preferentially inhabit the dense groups and clusters. A substantial dependence of the clustering properties of AGN host galaxies on the stellar mass is also observed in the faint volume-limited AGN host galaxy sample, which is inconsistent with the environmental dependence of the stellar mass of AGN host galaxies in the faint volume-limited AGN host galaxy sample. This is likely due to the galaxy number of the faint volume-limited AGN host galaxy sample being too small to ensure an ideal statistical analysis.

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Galaxy groups in the 2dFGRS: the group-finding algorithm and the 2PIGG catalogue

Cited by 344 publications

References 46 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

Clusters and groups of galaxies in the 2dF galaxy redshift survey: A new catalogue

The environmental dependence of the stellar mass of active galactic nucleus host galaxies and dependence of the clustering properties of active galactic nucleus host galaxies on the stellar mass

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