Comparison of the composition and metabolic potential of the reindeer’s rumen microbiome in the Yamal-Nenets and Nenets autonomous district of the Russian Arctic

The adaptive ability of reindeer to the harsh conditions of the Russian Arctic is not determined solely by the genome of the macroorganism and, of course, includes an extensive genetic and metabolic repertoire of the microbiome.The aim. To compare the taxonomic and predicted metabolic profiles of the rumen microbiome of adult reindeer living in the natural pastures of the Yamalo-Nenets and Nenets Autonomous districts of the Russian Federation.Materials and methods. Expeditions to the Yamal-Nenets and Nenets Autonomous districts of the Russian Arctic in 2017 were carried out to take samples of the rumen. The contents of the rumen were taken from clinically healthy reindeer individuals (at least 3 times repetition). To analyze the animal scar microbiota and determine metabolic profiles, 16S rRNA NGS sequencing was performed on a MiSeq device (Illumina, USA). Bioinformatic data analysis was performed using QIIME2 software ver. 2020.8. The noise sequences were filtered by DADA2. Silva 138 reference database was used for taxonomy analysis. Reconstruction and prediction of the functional content of the metagenome was carried out using the software complex PICRUSt2 (v. 2.3.0).Results. During NGS sequencing, a total of 223 768 sequences of the 16S rRNA gene of the reindeer scarring microbiome were studied. Significant (p ≤ 0.05) differences between the groups in 10 bacterial phyla and superphyla were revealed: Actinobacteriota, Spirochaetes, Chloroflexi, Verrucomicrobia, Bdellovibrionota, Synergistetes, Fusobacteriota, Myxococcota, Cyanobacteria, Campilobacterota. The results of the reconstruction and prediction of the functional content of the metagenome using the PICRUSt2 bioinformatic analysis made it possible to identify 328 potential metabolic pathways. Differences between the groups were revealed in 16 predicted metabolic pathways, among which the pathways of chlorophyllide and amino acid biosynthesis dominated

Gene expression in farm poultry under the influence of T-2 toxin and the use of biological preparations

Background. Feed-borne T-2 toxin may inhibit innate immune system function in birds.The aim. To evaluate the effect of T-2 toxin, artificially introduced with feed, on the expression level of a number of immunity-related genes in the tissues of the broiler digestive system.Materials and methods. The experiments were carried out in the vivarium of the FSC “VNITIP” RAS broilers of the Smena 8 cross from 33 to 47-day old. Experimental contamination of feed T-2 toxin was performed. The birds were divided into 4 groups of 5 animals each: I – control, receiving a diet without the introduction of T-2 toxin, II experimental – receiving a diet with the addition of T-2 toxin, III experimental – receiving a diet with the addition of T-2 toxin and the sorbent Zaslon2+, IV experimental – receiving a diet with the addition of T-2 toxin, the same sorbent Zaslon2+and Axtra Pro enzyme. The level of mRNA expression was analyzed by quantitative reverse transcription PCR.Results. The data obtained indicated the impact of T-2 toxin contamination of broiler feed on the modulation of the level of expression of genes associated with the functioning of the immune system in the cecum and pancreas. Exposure to T-2 toxin (group II) led to an increase in the expression of the pro-inflammatory gene IL-6 in the tissues of the caecum by 10.8 times and IL-8 in the pancreas by 3.89 times (p ≤ 0.05) compared with control group I. The effect of the sorbent, as well as the complex, including the sorbent and the enzyme, on the expression of broiler genes was positive. The sorbent without the enzyme showed greater efficiency than with the additional introduction of the enzyme

MASTER Optical Polarization Variability Detection in the Microquasar V404 Cyg/GS 2023+33

On 2015 June 15, the Swift space observatory discovered that the Galactic black hole candidate V404 Cyg was undergoing another active X-ray phase, after 25 years of inactivity. The 12 telescopes of the MASTER Global Robotic Net located at six sites across four continents were the first ground-based observatories to start optical monitoring of the microquasar after its gamma-ray wake up at 18h 34m 09s U.T. on 2015 June 15. In this paper, we report, for the first time, the discovery of variable optical linear polarization, changing by 4%-6% over a timescale of ∼1 hr, on two different epochs. We can conclude that the additional variable polarization arises from the relativistic jet generated by the black hole in V404 Cyg. The polarization variability correlates with optical brightness changes, increasing when the flux decreases.Fil: Lipunov, V.. M.V.Lomonosov Moscow State University. Physics Department; RusiaFil: Gorbovskoy, E.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Krushinskiy, V.. Kourovka Astronomical Observatory, Ural Federal University; RusiaFil: Vlasenko, D.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Tiurina, N.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Balanutsa, P.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Kuznetsov, A.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Budnev, N.. Applied Physics Institute. Irkutsk State University; RusiaFil: Gress, O.. Applied Physics Institute, Irkutsk State University; RusiaFil: Tlatov, A.. Kislovodsk Solar Station of the Main (Pulkovo) Observatory RAS; RusiaFil: Rebolo Lopez, L.. Instituto de Astrofsica de Canarias; EspañaFil: Serra-Ricart, M.. Instituto de Astrofsica de Canarias; EspañaFil: Buckley, D. A. H.. South African Astronomical Observatory; SudáfricaFil: Israelyan, G.. Instituto de Astrofsica de Canarias; EspañaFil: Lodieu, N.. Instituto de Astrofisica de Canarias; EspañaFil: Ivanov, K.. Applied Physics Institute. Irkutsk State University; RusiaFil: Yazev, S.. Applied Physics Institute, Irkutsk State University; RusiaFil: Sergienko, Y.. Blagoveschensk State Pedagogical University; RusiaFil: Gabovich, A.. Blagoveschensk State Pedagogical University; RusiaFil: Yurkov, V.. Blagoveschensk State Pedagogical University; RusiaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Saffe, Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Podesta, R.. Observatorio "Felix Aguiklar". Universidad Nacional de San Juan; ArgentinaFil: Lopez, C.. Observatorio "Felix Aguilar". Universidad nacional de San juan; Argentin

Three-stage Collapse of the Long Gamma-Ray Burst from GRB 160625B Prompt Multiwavelength Observations

This article presents the early results of synchronous multiwavelength observations of one of the brightest gamma-ray bursts (GRBs) GRB 160625B with the detailed continuous fast optical photometry of its optical counterpart obtained by MASTER and with hard X-ray and gamma-ray emission, obtained by the Lomonosov and Konus-Wind spacecraft. The detailed photometry led us to detect the quasi-periodical emission components in the intrinsic optical emission. As a result of our analysis of synchronous multiwavelength observations, we propose a three-stage collapse scenario for this long and bright GRB. We suggest that quasiperiodic fluctuations may be associated with forced precession of a self-gravitating rapidly rotating superdense body (spinar), whose evolution is determined by a powerful magnetic field. The spinar’s mass allows it to collapse into a black hole at the end of evolution

First gravitational-wave burst GW150914: MASTER optical follow-up observations

The Advanced LIGO observatory recently reported the first direct detection of the gravitational waves (GWs) predicted by Einstein & Sitzungsber. We report on the first optical observations of the GW source GW150914 error region with the Global MASTER Robotic Net. Between the optical telescopes of electromagnetic support, the covered area is dominated by MASTER with an unfiltered magnitude up to 19.9 mag (5σ). We detected several optical transients, which proved to be unconnected with the GW event. The main input to investigate the final error box of GW150914 was made by the MASTER-SAAO robotic telescope, which covered 70 per cent of the final GW error box and 90 per cent of the common localization area of the LIGO and Fermi events. Our result is consistent with the conclusion (Abbott et al. 2016a) that GWs from GW150914 were produced in a binary black hole merger. At the same time, we cannot exclude that MASTER OT J040938.68-541316.9 exploded on 2015 September 14.Fil: Lipunov, V. M.. Lomonosov Moscow State University; RusiaFil: Kornilov, V.. Lomonosov Moscow State University; RusiaFil: Gorbovskoy, E.. Lomonosov Moscow State University; RusiaFil: Buckley, D. A. H.. South African Astronomical Observatory; SudáfricaFil: Tiurina, N.. Lomonosov Moscow State University; RusiaFil: Balanutsa, P.. Lomonosov Moscow State University; RusiaFil: Kuznetsov, A.. Lomonosov Moscow State University; RusiaFil: Greiner, J.. Max-Planck-Institut für extraterrestrische Physik; AlemaniaFil: Vladimirov, V.. Lomonosov Moscow State University; RusiaFil: Vlasenko, D.. Lomonosov Moscow State University; RusiaFil: Chazov, V.. Lomonosov Moscow State University; RusiaFil: Kuvshinov, D.. Lomonosov Moscow State University; RusiaFil: Gabovich, A.. Blagoveschensk State Pedagogical University; RusiaFil: Potter, S. B.. South African Astronomical Observatory; SudáfricaFil: Kniazev, A.. South African Astronomical Observatory; SudáfricaFil: Crawford, S.. South African Astronomical Observatory;Fil: Rebolo Lopez, R.. Instituto de Astrofacuteisica de Canarias Vía Láctea; EspañaFil: Serra Ricart, M.. Instituto de Astrofacuteisica de Canarias Vía Láctea; EspañaFil: Israelian, G.. Instituto de Astrofacuteisica de Canarias Vía Láctea; EspañaFil: Lodieu, N.. Instituto de Astrofacuteisica de Canarias Vía Láctea; EspañaFil: Gress, O.. Irkutsk State University; RusiaFil: Budnev, N.. Irkutsk State University; RusiaFil: Ivanov, K.. Irkutsk State University; RusiaFil: Poleschuk, V.. Irkutsk State University; RusiaFil: Yazev, S.. Irkutsk State University; RusiaFil: Tlatov, A.. Russian Academy of Sciences. Pulkovo Astronomical Observatory; RusiaFil: Senik, V.. Russian Academy of Sciences. Pulkovo Astronomical Observatory; RusiaFil: Yurkov, V.. Blagoveschensk State Pedagogical University; RusiaFil: Dormidontov, D.. Russian Academy of Sciences. Pulkovo Astronomical Observatory; RusiaFil: Parkhomenko, A.. Russian Academy of Sciences. Pulkovo Astronomical Observatory; RusiaFil: Sergienko, Yu.. Blagoveschensk State Pedagogical University; RusiaFil: Podestá, Ricardo César. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: López, Carlos Eduardo. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Saffe, Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Podestá, Florencia. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Mallamaci, Claudio Carlos. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; Argentin

Probing into emission mechanisms of GRB 190530A using time-resolved spectra and polarization studies : Synchrotron Origin?

Multipulsed GRB 190530A, detected by the Gamma-ray Burst Monitor (GBM) and Large Area Telescope onboard Fermi, is the sixth most fluent GBM burst detected so far. This paper presents the timing, spectral, and polarimetric analysis of the prompt emission observed using AstroSat and Fermi to provide insight into the prompt emission radiation mechanisms. The time-integrated spectrum shows conclusive proof of two breaks due to peak energy and a second lower energy break. Time-integrated (55.43 ± 21.30 per cent) as well as time-resolved polarization measurements, made by the Cadmium Zinc Telluride Imager (CZTI) onboard AstroSat, show a hint of high degree of polarization. The presence of a hint of high degree of polarization and the values of low energy spectral index (αpt) do not run over the synchrotron limit for the first two pulses, supporting the synchrotron origin in an ordered magnetic field. However, during the third pulse, αpt exceeds the synchrotron line of death in few bins, and a thermal signature along with the synchrotron component in the time-resolved spectra is observed. Furthermore, we also report the earliest optical observations constraining afterglow polarization using the MASTER (P < 1.3 per cent) and the redshift measurement (z = 0.9386) obtained with the 10.4 m GTC (Gran Telescopio Canarias) telescopes. The broad-band afterglow can be described with a forward shock model for an ISM (interstellar medium)-like medium with a wide jet opening angle. We determine a circumburst density of n0 ∼ 7.41, kinetic energy EK ∼ 7.24 × 1054 erg, and radiated gamma-ray energy Eγ,iso ∼ 6.05 × 1054 erg