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Highlights • The Corona Borealis/A2142 as a supercluster binary-like system has been revised. • Tidal analysis confirms a balanced gravitational interaction between them. • A peculiar velocity sample supports a flow of the A2142 region towards the CB. • The peculiar velocity sample may be biased by selection effect due to remoteness. • Even if the interaction between them is evident, the true dynamics remain unclear. Abstract The recent hypothesis of a giant supercluster binary-like structure formed by the Corona Borealis and its close companion Abell 2142 (supercluster) belongs to a little known area of investigation as the dynamics of gravitationally interacting galaxy supercluster pairs. From the observational point of view this structure approximates the configuration of a binary-like system in linear orbit interconnected by a huge filamentary structure which, if confirmed, it would be the first case to date observed at z ≥ 0.07. Given the importance to disentangle this issue, a follow-up analysis has been performed on the region constrained by the common envelop of the two superclusters in order to search for new hints to confirm their mutual gravitational interaction. Observational signatures of that interaction have been found mapping the inner peculiar motions where the observed negative peculiar velocities measured within the A2142 (supercluster) region suggest a general matter flow toward the Corona Borealis supercluster. Besides, analyzing the effects on both superclusters due to the mutual impact of the external tidal forces, turns out that their inner dynamics remain unperturbed up to the turnaround radii. Outside, where the binding forces are overlapped by the tidal ones, the outskirts of both superclusters should be unstable and subject to fragmentation. Such a scenario indicates that both superclusters interact with comparable and reciprocal tidal perturbations leaving the whole system in a substantial dynamical equilibrium. The origin of such a dynamical dichotomy would be explained either by a much more massive Corona Borealis supercluster than that estimated in the present work or by a selection effect biasing the small sample of peculiar velocities due to the remoteness of the system worsened by the large uncertainty on their measurements. [ABSTRACT FROM AUTHOR]

We present results of the study of peculiar motions of 57 clusters and groups of galaxies in the regions of the Corona Borealis (CrB), Bootes (Boo), Z5029/A1424, A1190, A1750/A1809 superclusters of galaxies and the galaxy clusters located beyond massive structures (0.05 < z < 0.10). Using the SDSS (Data Release 8) data, a sample of early-type galaxies was compiled in the systems under study, their fundamental planes were built, and relative distances and peculiar velocities were determined. Within the galaxy superclusters, significant peculiar motions along the line of sight are observed with rms deviations of 652 ± 50 kms-in CrB, 757 ± 70 kms-in Boo. In the most massive A2065 cluster in the CrB supercluster, no peculiar velocity was found. Peculiar motions of the other galaxy clusters can be caused by their gravitational interaction both with A2065 and with the A2142 supercluster. It has been found that there are two superclusters projected onto each other in the region of the Bootes supercluster with a radial velocity difference of about 4000 kms. In the Z 5029/A1424 supercluster near the rich Z5029 cluster, the most considerable peculiar motions with a rms deviations of 1366 ± 170 kms are observed. The rms deviations of peculiar velocities of 20 clusters that do not belong to large-scale structures is equal to 0 ± 20 kms. The whole sample of the clusters under study has the mean peculiar velocity equal to 83 ± 130 kms relative to the cosmic microwave background. [ABSTRACT FROM AUTHOR]

The first high-precision BVRI light curves of the eclipsing binary AS CrB were presented and were analyzed by the 2015 version of the W-D code. It is found that AS CrB is an extreme mass-ratio, deep contact binary with a fill-out factor of f = 59.6 ± 2.5 % and a mass ratio of q = 0.172 ± 0.008 . Based on the photometric solution and the Dartmouth isochrones model, the masses, radii, and luminosities of the components are estimated as follows: M 1 = 1.25 ± 0.15 M ⊙ , M 2 = 0.21 ± 0.06 M ⊙ , R 1 = 1.40 ± 0.07 R ⊙ , R 2 = 0.67 ± 0.04 R ⊙ , L 1 = 3.2 ± 0.2 L ⊙ , and L 2 = 0.72 ± 0.04 L ⊙ , with an estimated distance 459 ± 42 pc. These uncertainties mainly come from the errors of the color used to estimate the temperature of the primary star. By investigating all of the available times of light minima, it is found that the Observed-Calculated [ ( O − C ) ] curve shows a long-term period increase, with a rate of d P / d t = + ( 3.46 ± 0.01 ) × 10 − 7 day/year. As an extreme mass-ratio contact binary, AS CrB may merge into a single star, such as an FK Com-type star or a blue straggler, because of the orbital instability. [ABSTRACT FROM AUTHOR]

Table 1 in the paper should be: Position of galaxy systems in the sky and their dynamic properties [ABSTRACT FROM AUTHOR]

Offers a look at the gamma ray bursts (GRB) 000301C in the constellation Corona Borealis. How microlensing caused the brightening of the GRB000301C.