Groups of galaxies in the SDSS Data Release 7

Tago, E.; Saar, E.; Tempel, Elmo; Einasto, J.; Einasto, M.; Nurmi, P.; Heinämäki, P.

doi:10.1051/0004-6361/200913687

Cited by 101 publications

(162 citation statements)

References 64 publications

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“…We have updated and improved our previous galaxy group catalogues, which are constructed on the basis of the FoF method, following a similar procedure as used in previous papers (Tago et al 2008(Tago et al , 2010Tempel et al 2012). The group-finding method was applied to flux-and volume-limited samples drawn from the SDSS main contiguous area, covering 7221 square degrees in the sky.…”

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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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%

“…Below, we briefly outline the method and report on the improvements made with respect to Tago et al (2008Tago et al ( , 2010.…”

Section: Flux-limited Galaxy Groups/clustersmentioning

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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“…The main galaxy sample of the SDSS includes galaxies brighter than the limiting r-band Petrosian magnitude 17.77. Our galaxy sample is described in detail in Tago et al (2010); in total, this sample includes 583 362 galaxies.…”

Section: Galaxy Samplementioning

confidence: 99%

“…Using local environmental densities, we get similar results: for ellipticals (that are dominantly red), the faint-end slope is changing with density, and for spirals (that are dominantly blue), the faint-end slope is practically constant. We shall discuss the group environment in more details in a forthcoming study, using the group catalogue from Tago et al (2010).…”

Section: Comparison With Earlier Workmentioning

confidence: 99%

Galaxy morphology, luminosity, and environment in the SDSS DR7

Tempel

Saar

Liivamägi

et al. 2011

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138

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Aims. We study the influence of the environment on the evolution of galaxies by investigating the luminosity function (LF) of galaxies of different morphological types and colours at different environmental density levels. Methods. We construct the LFs separately for galaxies of different morphology (spiral and elliptical) and of different colours (red and blue) using data from the Sloan Digital Sky Survey (SDSS), correcting the luminosities for the intrinsic absorption. We use the global luminosity density field to define different environments, and analyse the environmental dependence of galaxy morphology and colour. The smoothed bootstrap method is used to calculate confidence regions of the derived luminosity functions. Results. We find a strong environmental dependency for the LF of elliptical galaxies. The LF of spiral galaxies is almost environment independent, suggesting that spiral galaxy formation mechanisms are similar in different environments. Absorption by the intrinsic dust influences the bright-end of the LF of spiral galaxies. After attenuation correction, the brightest spiral galaxies are still about 0.5 mag less luminous than the brightest elliptical galaxies, except in the least dense environment, where spiral galaxies dominate the LF at every luminosity. Despite the extent of the SDSS survey, the influence of single rich superclusters is present in the galactic LF of the densest environment.

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“…The main sample of galaxies is complete to 565 h −1 Mpc distance. To suppress the cluster finger-of-god redshift distortions, we used groups of galaxies based on the LRGs that were extracted using the method described in Tago et al (2010). The method of constructing the luminosity-density fields based on these data samples is discussed in Sect.…”

Section: Density Field Datamentioning

confidence: 99%

Large-scale environments ofz < 0.4 active galaxies

Lietzen¹,

Heinämäki²,

Nurmi³

et al. 2011

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Context. Properties of galaxies depend on their large-scale environment. As the influence of active galactic nuclei (AGN) in galaxy evolution is becoming more evident, their large-scale environments may help us understand the evolutionary processes leading to activity. The effect of activity can be seen particularly by showing whether different types of active galaxies are formed by similar mechanisms. Aims. Our aim is to study the supercluster-scale environments of active galaxies up to redshift 0.4. Our data include quasars, BL Lac objects, Seyfert, and radio galaxies. Methods. We used a three-dimensional, low-resolution luminosity-density field constructed of a sample of luminous red galaxies in the seventh data release of the Sloan Digital Sky Survey. We calculated the average density of this field in a volume of a 3 h −1 Mpc sphere around each AGN for estimating the environmental density levels of different types of AGN. This analysis gives us the distribution of AGN in the global environment of superclusters, filaments, and voids. Results. Our results show that, while radio-quiet quasars and Seyfert galaxies are mostly located in low-density regions, radio galaxies have higher environmental densities. BL Lac objects usually have low-density environments, but some of them are also in very high-density regions. Conclusions. Our results give support to the theory of galaxy evolution where galaxies are affected by two modes of AGN feedback: quasar mode that turns a blue star-forming galaxy into a red and dead one, and radio mode that regulates the growth of massive elliptical galaxies. We conclude that quasars are in lower density environments than radio galaxies, most likely because the galaxies in rich environments have evolved to a state suitable for radio-loud activity earlier. Galaxies in poor environment have evolved more slowly, and are still going through the earlier quasar-mode feedback in galaxy evolution.

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Groups of galaxies in the SDSS Data Release 7

Cited by 101 publications

References 64 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

Galaxy morphology, luminosity, and environment in the SDSS DR7

Large-scale environments ofz < 0.4 active galaxies

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