Anatomy of luminosity functions: the 2dFGRS example

Tempel, Elmo; Einasto, J.; Einasto, M.; Saar, E.; Tago, E.

doi:10.1051/0004-6361:200810274

Cited by 65 publications

(75 citation statements)

References 124 publications

(191 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The faint-end of the LF of the most dense environments is slightly different, but the number of galaxies in this region is also small and the dip of the LF may be caused purely by selection effects in the SDSS, as mentioned above. The bright-end of the LF of the least dense environments is also slightly different from that in other environments, because generally, very bright galaxies are absent from the low density environments (Tempel et al 2009). …”

Section: Luminosity Functions In Different Environmentsmentioning

confidence: 88%

“…In Tempel et al (2009) A&A 529, A53 (2011) we have found that the global environment has an important role in determining galaxy properties. Some studies have been dedicated only to special regions: e.g., Mercurio et al (2006) investigate the Shapley supercluster.…”

Section: Introductionmentioning

confidence: 92%

“…A similar double-power law was also used by Vale & Ostriker (2004) to fit the mass-luminosity relation in their subhalo model and by Cooray & Milosavljević (2005) to fit the LF of central galaxies. Since several papers have shown that the Schechter function is not a best fit for the LF (Blanton et al 2005;Mercurio et al 2006;Yang et al 2008;Tempel et al 2009), especially at the bright end, we shall use the double-power law for analytical approximation. Parameters for the LF approximations are given in Table 3.…”

Section: Determining Environmental Densitiesmentioning

confidence: 99%

See 2 more Smart Citations

Galaxy morphology, luminosity, and environment in the SDSS DR7

Tempel

Saar

Liivamägi

et al. 2011

A&A

Self Cite

102

138

View full text Add to dashboard Cite

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.

show abstract

Section: Luminosity Functions In Different Environmentsmentioning

confidence: 88%

Section: Introductionmentioning

confidence: 92%

Section: Determining Environmental Densitiesmentioning

confidence: 99%

See 1 more Smart Citation

Galaxy morphology, luminosity, and environment in the SDSS DR7

Tempel

Saar

Liivamägi

et al. 2011

A&A

Self Cite

102

138

View full text Add to dashboard Cite

show abstract

“…In each region some galaxies are single. They may be the brightest galaxies of faint groups in which other member galaxies are too faint to be observed within SDSS survey magnitude limits (Tempel et al 2009). We estimated the masses of these faint groups using the number of single galaxies in a region, and median masses of groups with less then five member galaxies.…”

Section: Masses and Mass-to-light Ratiosmentioning

confidence: 99%

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

Einasto

Gramann

Saar

et al. 2015

A&A

View full text Add to dashboard Cite

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.

show abstract

“…For example, rich superclusters contain high-density cores that may contain merging X-ray clusters and may be collapsing (Small et al 1998;Bardelli et al 2000;Einasto et al 2001;Rose et al 2002;Einasto et al 2007cEinasto et al , 2008. A supercluster environment with a wide range of densities affects the properties of galaxies, groups, and clusters located there (Einasto et al 2003b;Plionis 2004;Wolf et al 2005;Haines et al 2006;Einasto et al 2007d;Porter et al 2008;Tempel et al 2009;Fleenor & Johnston-Hollitt 2010;Tempel et al 2011;Einasto et al 2011b). Einasto et al (2011b) showed that the dynamical evolution of one of the richest superclusters in the Sloan Great Wall (SCL 111, SCl 024 in L10 catalogue) is almost finished, while the richest member of the Wall, SCl 126 (SCl 061) is still dynamically active.…”

Section: Discussionmentioning

confidence: 99%

Principal Component Analysis

Næs

Brockhoff

Tomić

2010

Statistics for Sensory and Consumer Science

View full text Add to dashboard Cite

Context. The study of superclusters of galaxies helps us to understand the formation, evolution, and present-day properties of the large-scale structure of the Universe. Aims. We use data about superclusters drawn from the SDSS DR7 to analyse possible selection effects in the supercluster catalogue, to study the physical and morphological properties of superclusters, to find their possible subsets, and to determine scaling relations for our superclusters. Methods. We apply principal component analysis and Spearman's correlation test to study the properties of superclusters. Results. We have found that the parameters of superclusters do not correlate with their distance. The correlations between the physical and morphological properties of superclusters are strong. Superclusters can be divided into two populations according to their total luminosity: high-luminosity ones with L g > 400 10 10 h −2 L ⊙ , and low-luminosity systems. High-luminosity superclusters form two sets, which are more elongated systems with the shape parameter K 1 /K 2 < 0.5 and less elongated ones with K 1 /K 2 > 0.5. The first two principal components account for more than 90% of the variance in the supercluster parameters. We use principal component analysis to derive scaling relations for superclusters, in which we combine the physical and morphological parameters of superclusters. Conclusions. The first two principal components define the fundamental plane, which characterises the physical and morphological properties of superclusters. Structure formation simulations for different cosmologies, and more data about the local and high redshift superclusters are needed to understand the evolution and the properties of superclusters better.

show abstract

Anatomy of luminosity functions: the 2dFGRS example

Cited by 65 publications

References 124 publications

Galaxy morphology, luminosity, and environment in the SDSS DR7

Galaxy morphology, luminosity, and environment in the SDSS DR7

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

Principal Component Analysis

Contact Info

Product

Resources

About