A new galaxy supercluster?

Panko, Elena; Флин, П.

doi:10.1080/10556790601134789

Cited by 13 publications

(24 citation statements)

References 6 publications

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“…The PF Catalog of galaxy structures (hereafter PFCat; Panko & Flin 2006) is the observational basis for the present study. The catalog was created using data from the Muenster Red Sky Survey (hereafter MRSS; Ungruhe et al 2003), which is a large-scale galaxy catalog covering an area of about 5000 deg 2 in the southern hemisphere, complete to a magnitude limit of r F = 18.3 mag.…”

Section: The Catalog Of Galaxy Structuresmentioning

confidence: 99%

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The Evolution of Low-Redshift Galaxy Structures

Biernacka

Флин

Panko

2009

ApJ

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Ellipticities for 6188 low-redshift (z < 0.18) poor and rich galaxy structures have been examined along with their evolution using an optical observational base that is statistically complete. The shape of each structure projected on the celestial sphere was determined using the covariance ellipse method. Analysis of the data indicates that structure ellipticity changes with redshift, being smaller for nearby objects and greater for those located further away. Such a change is also described better by quadratic or exponential relations than by a simple linear scheme. It is concluded that between redshifts of z = 0.18 and z = 0 we observe the dynamical evolution of galaxy clusters. Such a change in ellipticity with redshift is expected in ΛCDM models.

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Section: The Catalog Of Galaxy Structuresmentioning

confidence: 99%

“…The two-dimensional Voronoi tessellation technique (Ramella et al 1999(Ramella et al , 2001Panko & Flin 2006) was applied to the galaxy catalog to search for overdense regions. The resulting PFCat includes 6188 such structures, with at least 10 galaxies in each structure field.…”

Section: The Catalog Of Galaxy Structuresmentioning

confidence: 99%

The Evolution of Low-Redshift Galaxy Structures

Biernacka

Флин

Panko

2009

ApJ

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“…The catalogue of 6188 galaxy clusters (hereafter PF, Panko & Flin (2006)) served as observational basis of our studies. It is prepared applying Voronoy tessellation technique (Ramella et al 1999(Ramella et al , 2001 to Muenster Red Sky Survey (MRSS, Ungruhe et al (2003)).…”

Section: Observational Datamentioning

confidence: 99%

The Binggeli effect

Biernacka¹,

Panko²,

Godlowski³

et al. 2014

Proc. IAU

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“…The 2D Voronoi tessellation technique (Ramella et al 2001;Panko & Flin 2006) was applied to the galaxy catalog to search for overdense regions. As a result, PF includes 6188 such structures, with at least 10 galaxies in each structure field.…”

Section: Observational Datamentioning

confidence: 99%

“…We analysed some properties of galaxies structures based on the PF catalog of galaxy structures (Panko & Flin 2006) and the Tully NBG catalog (Tully 1988). At first, we analyzed the orientation of galaxies in the 247 optically selected rich Abell clusters, having at least 100 members.…”

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Some Properties of Galaxy Structures

et al. 2011

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Abstract. We analysed some properties of galaxies structures based on the PF catalog of galaxy structures (Panko & Flin 2006) and the Tully NBG catalog (Tully 1988). At first, we analyzed the orientation of galaxies in the 247 optically selected rich Abell clusters, having at least 100 members. The distribution of the position angles of galaxies as well as of two angles describing spatial orientation of the galaxy planes were tested for isotropy, applying three statistical tests. We found the relation between the anisotropy and the cluster richness. The relation between the galaxy alignment and the Bautz-Morgan morphological type of the parent cluster is not present. A statistically marginal relation between the velocity dispersion and cluster richness is observed. We also analyzed ellipticities for 6188 low redshift (z < 0.18) poor and rich galaxy structures which have been examined along with their evolution. Finally, we analyzed the Binggeli effect and found that the orientation of galaxy groups in the Local Supercluster (LSC), is strongly correlated with the distribution of neighbouring groups in the scale up to about 20 Mpc. Analysis of galaxy structures from the PF catalog shows quite different situation -the efect is observed only for more elongated structures (e ≤ 0.3). The effect is present in a distance range of about 60 h −1 Mpc.

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A new galaxy supercluster?

Cited by 13 publications

References 6 publications

The Evolution of Low-Redshift Galaxy Structures

The Evolution of Low-Redshift Galaxy Structures

The Binggeli effect

Some Properties of Galaxy Structures

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