Some Properties of Galaxy Structures
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 distri...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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De Gruyter
2011-06-01
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| Series: | Open Astronomy |
| Subjects: | |
| Online Access: | https://doi.org/10.1515/astro-2017-0289 |
| _version_ | 1818366459908194304 |
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| author | Flin Piotr Biernacka Monika Godłowski Włodzimierz Panko Elena Piwowarska Paulina |
| author_facet | Flin Piotr Biernacka Monika Godłowski Włodzimierz Panko Elena Piwowarska Paulina |
| author_sort | Flin Piotr |
| collection | DOAJ |
| description | 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. |
| first_indexed | 2024-12-13T22:36:30Z |
| format | Article |
| id | doaj.art-75cae3db700e433d89656e495e1c0c88 |
| institution | Directory Open Access Journal |
| issn | 2543-6376 |
| language | English |
| last_indexed | 2024-12-13T22:36:30Z |
| publishDate | 2011-06-01 |
| publisher | De Gruyter |
| record_format | Article |
| series | Open Astronomy |
| spelling | doaj.art-75cae3db700e433d89656e495e1c0c882022-12-21T23:28:57ZengDe GruyterOpen Astronomy2543-63762011-06-0120225125810.1515/astro-2017-0289astro-2017-0289Some Properties of Galaxy StructuresFlin Piotr0Biernacka Monika1Godłowski Włodzimierz2Panko Elena3Piwowarska Paulina4Institute of Physics, Jan Kochanowski University, Swietokrzyska 15, 25-406 Kielce, PolandInstitute of Physics, Jan Kochanowski University, Swietokrzyska 15, 25-406 Kielce, PolandInstitute of Physics, Opole University, Oleska 48, 45-041 Opole, PolandKalinenkov Astronomical Observatory, Nikolaev State University, Nikolskaya 24, Nikolaev, 54030, UkraineInstitute of Physics, Opole University, Oleska 48, 45-041 Opole, PolandWe 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.https://doi.org/10.1515/astro-2017-0289galaxiesclusters and groupsgalaxiesorientationevolution |
| spellingShingle | Flin Piotr Biernacka Monika Godłowski Włodzimierz Panko Elena Piwowarska Paulina Some Properties of Galaxy Structures Open Astronomy galaxies clusters and groups galaxies orientation evolution |
| title | Some Properties of Galaxy Structures |
| title_full | Some Properties of Galaxy Structures |
| title_fullStr | Some Properties of Galaxy Structures |
| title_full_unstemmed | Some Properties of Galaxy Structures |
| title_short | Some Properties of Galaxy Structures |
| title_sort | some properties of galaxy structures |
| topic | galaxies clusters and groups galaxies orientation evolution |
| url | https://doi.org/10.1515/astro-2017-0289 |
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