The Ursa Major supercluster of galaxies: I. The luminosity function

Копылов, А. И.; Kopylova, F. G.

doi:10.1134/1.1351557

Cited by 14 publications

(27 citation statements)

References 25 publications

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“…For comparison, the galaxy number overdensity for the richer Corona Borealis supercluster is 7 (Small et al 1998). The simulation performed in this paper and the Hubble diagram constructed previously (Kopylova and Kopylov 1998) show that the core of the system may be at the stage of gravitational collapse.…”

Section: Introductionmentioning

confidence: 99%

Peculiar motions in the region of the Ursa Major supercluster of galaxies

Kopylova

Копылов

2007

Astron. Lett.

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Abstract. We have investigated the peculiar motions of clusters of galaxies in the Ursa Major (UMa) supercluster and its neighborhood. Based on SDSS (Sloan Digital Sky Survey) data, we have compiled a sample of early-type galaxies and used their fundamental plane to determine the cluster distances and peculiar velocities. The samples of early-type galaxies in the central regions (within R 200 ) of 12 UMa clusters of galaxies, in three main subsystems of the superclusterthe filamentary structures connecting the clusters, and in nine clusters from the nearest UMa neighborhood have similar parameters. The fairly high overdensity (3 by the galaxy number and 15 by the cluster number) suggests that the supercluster as a whole is gravitationally bound, while no significant peculiar motions have been found: the peculiar velocities do not exceed the measurement errors by more than a factor of 1.5-2. The mean random peculiar velocities of clusters and the systematic deviations from the overall Hubble expansion in the supercluster are consistent with theoretical estimates. For the possible approach of the three UMa subsystems to be confirmed, the measurement accuracy must be increased by a factor of 2-3.

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Section: Introductionmentioning

confidence: 99%

Peculiar motions in the region of the Ursa Major supercluster of galaxies

Kopylova

Копылов

2007

Astron. Lett.

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“…In what follows, we compare our findings with the most relevant studies performed on the CBr in order to compare the GPM efficiency with respect to alternative methodologies (Bahcall and Soneira 1984 (BS);Postman et al 1988 (PGH); Cappi and Maurogordato 1992 (C/M); Small et al 1997Small et al (S97), 1998Kopylova and Kopylov 1998 …”

Section: Comparison With Other Studiesmentioning

confidence: 99%

Does the Corona Borealis Supercluster form a giant binary-like system?

Pillastrini¹

2016

Astrophys Space Sci

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The distribution of local gravitational potentials generated by a complete volume-limited sample of galaxy groups and clusters filling the Corona Borealis region has been derived to search for new gravitational hints in the context of clustering analysis unrevealed by alternative methodologies. Mapping such a distribution as a function of spatial positions, the deepest potential wells in the sample trace unambiguously the locations of the densest galaxy cluster clumps providing the physical keys to bring out gravitational features connected to the formation, composition and evolution of the major clustered structures filling that region. As expected, the three deepest potential wells found at Equatorial coordinates: (~ 230°, ~ 28°, z ~ 0.075), (~ 240°, ~ 27°, z ~ 0.09) and, (227°, 5.8°, z ~ 0.0788) correspond to massive superclusters of galaxy groups and clusters identified as the Corona Borealis, A2142 and Virgo-Serpent, respectively. However, the deepest isopotential contours around the Corona Borealis and A2142 superclusters seem to suggest a gravitational feature similar to a giant binary-like system connected by a filamentary structure. To a first approximation, it seems unlikely that this hypothesized system could be gravitationally bound.

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“…The X‐ray centre has coordinates α 2000 = 15 h 44 m 56 s , δ 2000 =+36° 06′ 04″. A2124 is dominated by a single cD galaxy (α 2000 = 15 h 44 m 59 s , δ 2000 =+36° 06′ 34″), with a velocity of v = 19810 km s −1 and R magnitude of 12.49 (Kopylova & Kopylov 1998). Blakeslee & Metzger (1999) identified an arc‐like object at z = 0.573 located 27 arcsec along the major axis from the centre of this cD galaxy.…”

Section: The Cluster A2124mentioning

confidence: 99%

BeppoSAXtemperature maps of galaxy clusters in the Corona Borealis supercluster: A2061, A2067 and A2124

Marini

Bardelli

Zucca

et al. 2004

Monthly Notices of the Royal Astronomical Society

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In this paper we present the analysis of BeppoSAX observations of the cluster pairs A2061–A2067 and A2122–A2124, located in the Corona Borealis supercluster, which have been selected as candidate merging clusters. The aim of this work is to study the physics of the intracluster medium and to look for the possible presence of merging signatures. We derived the global temperatures and abundances and the temperature profiles and maps for these clusters. We do not find any significant evidence of interaction between the clusters forming the pairs, but we detect a candidate shock inside A2061. On the basis of the X‐ray and optical properties of this cluster we propose a scenario in which a group is falling inside A2061. This interaction is in the phase in which the cores have not yet met and in which the formation of a shock is expected.

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The Ursa Major supercluster of galaxies: I. The luminosity function

Cited by 14 publications

References 25 publications

Peculiar motions in the region of the Ursa Major supercluster of galaxies

Peculiar motions in the region of the Ursa Major supercluster of galaxies

Does the Corona Borealis Supercluster form a giant binary-like system?

BeppoSAXtemperature maps of galaxy clusters in the Corona Borealis supercluster: A2061, A2067 and A2124

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