Перегляд за Автор "Biernacka, Monika"

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  • Ескіз
    Документ
    The Evolution of Low-Redshift Galaxy Structures
    (2009) Biernacka, Monika; Flin, Piotr; Panko, Olena O.; Панько, Олена Олексіївна; Панько, Елена Алексеевна
    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.
  • Ескіз
    Документ
    The Investigation of the Luminosity Function for Sample 6168 Galaxy Clusters
    (2018) Godlowski, Wlodzimierz; Popiela, Joanna; Biernacka, Monika; Bajan, Katarzyna; Panko, Olena O.; Pajowska, Paulina; Flin, Piotr; Панько, Олена Олексіївна; Панько, Елена Алексеевна
    The issue of construction of the luminosity function is an important problem for analysis of large scale structure statistics and interpretation of astronomical object counts In the present paper we discuss the the issure of the construction of the luminosity function for galaxy clusters. The problem is solved based on counting brightness of galaxies belonging to 6168 galaxy clusters selected from Panko & Flin (2006) Catalogue. We show that the galaxy clusters are characterized by the luminosity function signi cantly di erent than that obtained for both: individual optical galaxies and radiogalaxies. We discuss the signi cance of this result for the theories of the structure formation.
  • Ескіз
    Документ
    The Properties of Nearby Galaxy Structures
    (2009) Biernacka, Monika; Flin, Piotr; Juszczyk, T.; Panko, Olena O.; Панько, Олена Олексіївна; Панько, Елена Алексеевна
    We constructed the statistically uniform catalogue of 6188 galaxy structures, having at least 10 members in the structure field. These structures were extracted through the application of the Voronoi tessellation to Muenster Red Sky Survey which is a catalogue of galaxies based on scans of 217 ESO plates in the region covering about 5000 square degrees. We found that the shape of structures projected on the celestial sphere is different for rich and poor structures, which can reflect condition during their formation. Recent (for z < 0.18) weak dynamical evolution of galaxy clusters is observed. The distributions of position angles of ten brightest galaxies in structure are isotropic. The position angle of the brightest cluster member tend to be align with the parent cluster major axis only in the case of BM type I clusters, this is clusters containing cD galaxy.
  • Ескіз
    Документ
    The Shape of Galaxy Structures
    (The Astrophysical Journal, 2009) Panko, Olena O.; Juszczyk, Teresa; Biernacka, Monika; Flin, Piotr; Панько, Олена Олексіївна; Панько, Елена Алексеевна
    An analysis is presented for a statistically complete sample of 547 galaxy structures with z 0.16, each containing at least 10 objects. The sample was divided according to structure richness, representing 10 richness classes, with the distribution of ellipticities differing among individual classes. Mean ellipticity varies from 0.34 to 0.18, less well populated structures being more elongated that richer ones. Statistics indicate that structures with at least 50 members originate from the same population. The mean redshift of a structure class is a function of richness, with less well populated classes exhibiting greater mean redshifts than richer galaxy clusters. Further analysis reveals a dependence of the ellipticity-redshift correlation on structure richness. Among rich galaxy clusters there is an anticorrelation between the parameters, the strongest correlation occurring for the most poorly populated galaxy classes.