Important scientific achievements


1) A new bright galaxy of the Local Group VV124 (UGC4879) is found. The last discovery of such a bright galaxy of the Local Group was made 40 years ago. Taking into account all the works of recent years on the search for nearby galaxies, it can be stated that the VV124 is the latest found bright galaxy belonging to the Local Group of galaxies.

Kopylov A.I., Tikhonov N.A., Fabrika S.N., Drozdovsky I.O., Valeev A.F., MNRAS Lett, V. 387, Issue 1, L45, 2008.

Tikhonov N.A., Fabrika S.N., Sholukhova O.N., Kopylov A.I., Astronomy Letters, V. 36, Issue 5, p. 309,  2010.


vv124

Fig. 1.  Galaxy  VV124 (BTA image
).


2) Within a few decades, there was a popular hypothesis about the possibility for primary young galaxies with low metalicity and the first wave of star formation in the history of these galaxies to be found in the relatively close neighborhood of our galaxy. As a sample of galaxies of this type the 1Zw18 galaxy has been always called for. Using the Hubble Space Telescope images, we carried out stellar photometry for 1Zw18 and for the first time we had found in this galaxy red giants with the age of several billion years, which immediately rejected the hypothesis that the galaxy was young.


Tikhonov N.A., Astronomy Letters, V.33, Iss.3, p.137, 2007.



3) Dynamical and photometrical (near-infrared, in K-band) characteristics of 183 groups and clusters of galaxies located in the regions of superclusters of galaxies Hercules, Leo, Ursa Major, Bootes, Corona Borealis and outside superclusters having radial velocities in the interval 0.012<z<0.09 (+ Virgo cluster) based on the archival data from the SDSS, 2MASX, NED catalogues are determined. The IR-luminosity of the systems of galaxies mainly corresponding to the luminosity of old stars from early-type galaxies allows to the first approximation to estimate their masses according to the correlation between dynamical mass and IR-luminosity. For systems of galaxies in the regions of the Hercules and  Leo superclusters the dwarf-to-giant ratio of galaxies in the r-band is evaluated, and it is found that this ratio increases with increasing X-ray luminosity at log LX > 43.5 erg/s.


Kopylova F.G., Kopylov A.I., Ast. Bull. 64, 1, 2009.
Kopylova F.G., Kopylov A.I., 2011, Astron. Lett., 37, 219, 2011.
Kopylova F.G., Astroph. Bull. 68, 253, 2013.
Kopylova F.G., Kopylov A.I., Astron. Lett., 39, 1, 2013.
Kopylova F.G., Kopylov A.I., Ast. Bull. 70, 123, 2015.


fig2

Fig. 3. K-luminosity of 183 galaxy groups and clusters depending on their dynamic mass M200 is shown. Blue squares show x-ray clusters of galaxies with the dispersion of radial velocities >400 km/s, red squares – groups with the dispersion of radial velocities <400 km/s, and cyan squares show systems without LX   measurements.








4) Using the data of catalogues of SDSS DR7-8 we investigated the peculiar motions of groups and clusters of galaxies in the regions of Ursa Major, Hercules, Leo and Bootes superclusters. For this purpose, we compiled a samples of ealy-type galaxies in them and determined the fundamental plane distances and peculiar velocities. For all superclusters of galaxies is Hubble's law between the radial velocity and distance obtained by the fundamental plane of early-type galaxies. Within their regions the following peculiar motion rms deviations along the line of sight are observed: 736±50 km/s in Hercules, 625±70 km/s in Leo, 370±50 km/s (rich clusters) in Bootes and 290±120 km/s in UMa.

Kopylova F.G., Kopylov A.I., Astron. L. 33, 211, 2007.
λΟΠΩΜΟΧΑ ζ.η., λΟΠΩΜΟΧ α.ι., οΤήΕΤ σαο ςαξ, 2012.
Kopylova F.G., Kopylov A.I., 2014, Astron. L. 40, 595, 2014.


fig3


Fig. 4. The map of distribution of galaxies and clusters in the region of Hercules and Leo superclusters with radial velocities in the range of cz = 8000–13000 km/s.









5) The study was performed of four complex (bimodal) Abell clusters with difference of radial velocities between the subclusters of about 3000 km/s, which may be due either to the gravitational interaction between very massive clusters at a collision on the line close to the line-of-sight or the projection along the line-of-sight of non-connected clusters. Using observational data from the 1-m telescope of SAO RAS and data of the SDSS catalogue we measured photometric relative distances (by the Kormendy relation and the fundamental plane) and revealed the structure of clusters A1035, A1569, A1775 and A1831. It is found that subclusters in these clusters are not bound gravitationally, and for them the Hubble law is obeyed.

Kopylov A.I., Kopylova F.G., Ast. Bull. 62, 311, 2007.
Kopylov A.I., Kopylova F.G., Ast. Bull. 64, 207, 2009.
Kopylov A.I., Kopylova F.G., Ast. Bull. 65, 205, 2010.
Kopylov A.I., Kopylova F.G., Ast. Bull. 67, 17, 2012.

fig4

Fig. 5. The Hubble diagram (velocity [zspec] – distance [zphot]) is shown for four bimodal clusters of galaxies (A-components to left, B-components to right), and for the cluster A1589, the nearest rich neighbour (12 Mpc) of the cluster A1569A.