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The tenth list of objects from the BIG (Byurakan-IRAS Galaxies) sample, containing 104 galaxies identified with 60 point sources from the IRAS PSC catalog, is introduced. The identifications have been made in the region +69°≤δ≤+73° and 09h50m≤α≤15h20m with an area of 107 sq.deg. The identified objects include 13 Sy candidates, 5 compact star-formation galaxies, 11 interacting pairs (including 5 “merger” candidates) and 1 interacting triple system, 5 LSB galaxies, and 5 groups. 21 objects are also identified with radio sources. The optical coordinates, their deviations from the IR coordinates, V stellar magnitudes, morphological types, angular sizes of the central regions, and position angles have been determined. The identified galaxies are of Sa-Sc, SB, and Irr morphological types, the optical stellar magnitudes lie in the range 15m.0-21m.5, and the angular sizes of the central regions lie in the range 3″-32″. Finding charts from the DSS2 are included for these objects.

The results of a morphological classification of 580 galaxies with a UV excess, included in the lists in [M. A. Kazarian, Astrofizika,15, 5 (1979); ibid.,15, 193 (1979); M. A. Kazarian and É. S. Kazarian, ibid.,16, 17 (1980); ibid.,18, 512 (1982); ibid.,19, 213 (1983)], are presented. For this we have developed a set of symbols, using the types E, S, and Ir introduced by Hubble, as well as symbols introduced by other authors and us. This set enabled us to make the morphological classification. Direct photographs obtained on the 2.6-m and 6-m telescopes were used to classify 141 of the galaxies (over 24%), while Palomar Atlas charts were used for the remaining 439 galaxies. These galaxies were divided into two groups based on classification conditions, and data on each group are given in Tables 1 and 2, respectively. The results for each group, given in Table 3, show that with the transition from early types, such as C and E, to later types, such as S and Ir, the relative number of galaxies going into one group (Table 1), in which the classification was based on direct photographs, increases in comparison with the number going into the other group (Table 2).

We used modified holographic Ricci dark energy to find anisotropic LRS Bianchi type I cosmological model in five-dimensions based on Lyra geometry. The exact solutions of the Einstein field equations were obtained by using hybrid expansion law (HEL). We have investigated the interacting and noninteracting dark energy and dark matter. It is found that at late times the equation of state parameter (EOS) for non-interacting case behaves like a cosmological constant whereas it behaves like phantom dark energy for interacting model. Some cosmological parameters and stability of the models are discussed. The physical and geometric aspects of the models have been analysed. They are consistent with the recent observational results.

The spectral subtypes and luminosity classes are given for 15 comparatively faint M stars found on plates of the First Byurakan Spectroscopic Survey. Two of them are classified as M dwarfs. Most of the new M stars are probably Mirids.