The historical role of Islam in the public life of the Central Asian region of the CIS in the XX – XXI centuries

The article is devoted to the historical and contemporary aspects of Islam in Central Asia. It shows the confessional policy of the Russian Empire and the Soviet Union in Turkestan. The document proves that this policy was based on a combination of “hard” and “soft” management techniques and concludes that regional policies contributed to the transformation process in Central Asia. Furthermore, the article shows the role of Islam in regional modernization processes and the author identifies the key elements of the religious situation in the region, showing the main religious groups in the local Islamic communities. The paper notes the features of government policy in Central Asia in regard to Islam

Nonthermal Emission from a Supernova Remnant in a Molecular Cloud

In evolved supernova remnants (SNRs) interacting with molecular clouds, such as IC 443, W44, and 3C391, a highly inhomogeneous structure consisting of a forward shock of moderate Mach number, a cooling layer, a dense radiative shell and an interior region filled with hot tenuous plasma is expected. We present a kinetic model of nonthermal electron injection, acceleration and propagation in that environment and find that these SNRs are efficient electron accelerators and sources of hard X- and gamma-ray emission. The energy spectrum of the nonthermal electrons is shaped by the joint action of first and second order Fermi acceleration in a turbulent plasma with substantial Coulomb losses. Bremsstrahlung, synchrotron, and inverse Compton radiation of the nonthermal electrons produce multiwavelength photon spectra in quantitative agreement with the radio and the hard emission observed by ASCA and EGRET from IC 443. We distinguish interclump shock wave emission from molecular clump shock wave emission accounting for a complex structure of molecular cloud. Spatially resolved X- and gamma- ray spectra from the supernova remnants IC 443, W44, and 3C391 as might be observed with BeppoSAX, Chandra XRO, XMM, INTEGRAL and GLAST would distinguish the contribution of the energetic lepton component to the gamma-rays observed by EGRET.Comment: 14 pages, 4 figure, Astrophysical Journal, v.538, 2000 (in press

Star formation in M33: Spitzer photometry of discrete sources

Combining the relative vicinity of the Local Group spiral galaxy M33 with the Spitzer images, we investigate the properties of infrared (IR) emission sites and assess the reliability of the IR emission as a star formation tracer. The mid- and far-IR emission of M33 was obtained from IRAC and MIPS images from the Spitzer archive. We compared the photometric results for several samples of three known types of discrete sources (HII regions, supernovae remnants and planetary nebulae) with theoretical diagnostic diagrams, and derived the spectral energy distribution (from 3.6 to 24 micron) of each type of object. Moreover, we generated a catalogue of 24 micron sources and inferred their nature from the observed and theoretical colours of the known type sources. We estimated the star formation rate in M33 both globally and locally, from the IR emission and from the Halpha emission line. The colours of the typical IR emissions of HII regions, supernovae remnants and planetary nebulae are continuous among the different samples, with overlapping regions in the diagnostic diagrams. The comparison between the model results and the colours of HII regions indicates a dusty envelope at relatively high temperatures ~600 K, and moderate extinction Av < 10. The 24 micron sources IR colours follow the regions observationally defined by the three classes of known objects but the majority of them represent HII regions. The derived total IR luminosity function is in fact very similar to the HII luminosity function observed in the Milky Way and in other late type spirals. Even though our completeness limit is 5x10^37 ergs s-1, in low density regions we are able to detect sources five times fainter than this, corresponding to the faintest possible HII region. [abridged]Comment: 19 pages, 18 figures (low resolution), accepted for publication by A&A; corrected typo

The faint supernova remnant G 116.5+1.1 and the detection of a new candidate remnant

The extended supernova remnant G 116.5+1.1 was observed in the optical emission lines of Halpha+[N II], [S II] and [O III]; deep long-slit spectra were also obtained. The morphology of the remnant's observed emission is mainly diffuse and patchy in contrast to the known filamentary emission seen along the western limb. The bulk of the detected emission in the region appears unrelated to the remnant but there is one area of emission in the south-east which is characterized by a [S II]/Halpha ratio of ~0.5, implying a possible relation to G 116.5+1.1. If this is actually the case, it would imply a more extended remnant than previously realized. Emission in the [O III] 5007 A line image is not detected, excluding moderate or fast velocity shocks running into ionized interstellar clouds. Our current estimate of the distance to G 116.5+1.1 of ~3 kpc is in agreement with earlier estimates and implies a very extended remnant (69 pc x 45 pc). Observations further to the north-east of G 116.5+1.1 revealed a network of filamentary structures prominent in Halpha+[N II] and [S II] but failed to detect [O III] line emission. Long-slit spectra in a number of positions provide strong evidence that this newly detected emission arises from shock heated gas. Typical Halpha fluxes lie in the range of 9 to 17 x10^{-17} erg/s/cm^2/ arcsec^2, while low electron densities are implied by the intensities of the sulfur lines. Weak emission from the medium ionization line at 5007 A is detected in only one spectrum. Cool dust emission at 60 and 100 microns may be correlated with the optical emission in a limited number of positions. Surpisingly, radio emission is not detected in published surveys suggesting that the new candidate remnant may belong to the class of "radio quiet" supernova remnants.Comment: 10 pages, 5 figures, accepted for publication in A&

Galactic and Extragalactic Samples of Supernova Remnants: How They Are Identified and What They Tell Us

Supernova remnants (SNRs) arise from the interaction between the ejecta of a supernova (SN) explosion and the surrounding circumstellar and interstellar medium. Some SNRs, mostly nearby SNRs, can be studied in great detail. However, to understand SNRs as a whole, large samples of SNRs must be assembled and studied. Here, we describe the radio, optical, and X-ray techniques which have been used to identify and characterize almost 300 Galactic SNRs and more than 1200 extragalactic SNRs. We then discuss which types of SNRs are being found and which are not. We examine the degree to which the luminosity functions, surface-brightness distributions and multi-wavelength comparisons of the samples can be interpreted to determine the class properties of SNRs and describe efforts to establish the type of SN explosion associated with a SNR. We conclude that in order to better understand the class properties of SNRs, it is more important to study (and obtain additional data on) the SNRs in galaxies with extant samples at multiple wavelength bands than it is to obtain samples of SNRs in other galaxiesComment: Final 2016 draft of a chapter in "Handbook of Supernovae" edited by Athem W. Alsabti and Paul Murdin. Final version available at https://doi.org/10.1007/978-3-319-20794-0_90-

Yersinia enterocolitica palearctica serobiotype O:3/4 - a successful group of emerging zoonotic pathogens

<p>Abstract</p> <p>Background</p> <p>High-pathogenic <it>Y. enterocolitica </it>ssp. <it>enterocolitica </it>caused several human outbreaks in Northern America. In contrast, low pathogenic <it>Y. enterocolitica </it>ssp. <it>palearctica </it>serobiotype O:3/4 is responsible for sporadic cases worldwide with asymptomatic pigs being the main source of infection. Genomes of three <it>Y. enterocolitica </it>ssp. <it>palearctica </it>serobiotype O:3/4 human isolates (including the completely sequenced Y11 German DSMZ type strain) were compared to the high-pathogenic <it>Y. enterocolitica </it>ssp. <it>enterocolitica </it>8081 O:8/1B to address the peculiarities of the O:3/4 group.</p> <p>Results</p> <p>Most high-pathogenicity-associated determinants of <it>Y. enterocolitica </it>ssp. <it>enterocolitica </it>(like the High-Pathogenicity Island, <it>yts1 </it>type 2 and <it>ysa </it>type 3 secretion systems) are absent in <it>Y. enterocolitica </it>ssp. <it>palearctica </it>serobiotype O:3/4 genomes. On the other hand they possess alternative putative virulence and fitness factors, such as a different <it>ysp </it>type 3 secretion system, an RtxA-like and insecticidal toxins, and a N-acetyl-galactosamine (GalNAc) PTS system (<it>aga</it>-operon). Horizontal acquisition of two prophages and a tRNA-Asn-associated GIYep-01 genomic island might also influence the <it>Y. enterocolitica </it>ssp. <it>palearctica </it>serobiotype O:3/4 pathoadaptation. We demonstrated recombination activity of the PhiYep-3 prophage and the GIYep-01 island and the ability of the <it>aga</it>-operon to support the growth of the <it>Y. enterocolitica </it>ssp. <it>enterocolitica </it>O:8/1B on GalNAc.</p> <p>Conclusions</p> <p><it>Y. enterocolitica </it>ssp. <it>palearctica </it>serobiotype O:3/4 experienced a shift to an alternative patchwork of virulence and fitness determinants that might play a significant role in its host pathoadaptation and successful worldwide dissemination.</p

Dust in Historical Galactic Type Ia Supernova Remnants with Herschel

The origin of interstellar dust in galaxies is poorly understood, particularly the relative contributions from supernovae and the cool stellar winds of low-intermediate mass stars. Here, we present Herschel PACS and SPIRE photometry at 70-500um of the historical young supernova remnants: Kepler and Tycho; both thought to be the remnants of Type Ia explosion events. We detect a warm dust component in Kepler's remnant with T = 82K and mass 0.0031Msun; this is spatially coincident with thermal X-ray emission optical knots and filaments, consistent with the warm dust originating in the circumstellar material swept up by the primary blast wave of the remnant. Similarly for Tycho's remnant, we detect warm dust at 90K with mass 0.0086Msun. Comparing the spatial distribution of the warm dust with X-rays from the ejecta and swept-up medium, and Ha emission arising from the post-shock edge, we show that the warm dust is swept up interstellar material. We find no evidence of a cool (25-50 K) component of dust with mass >0.07Msun as observed in core-collapse remnants of massive stars. Neither the warm or cold dust components detected here are spatially coincident with supernova ejecta material. We compare the lack of observed supernova dust with a theoretical model of dust formation in Type Ia remnants which predicts dust masses of 0.088(0.017)Msun for ejecta expanding into surrounding densities of 1(5)cm-3. The model predicts that silicon- and carbon-rich dust grains will encounter the interior edge of the observed dust emission at 400 years confirming that the majority of the warm dust originates from swept up circumstellar or interstellar grains (for Kepler and Tycho respectively). The lack of cold dust grains in the ejecta suggests that Type Ia remnants do not produce substantial quantities of iron-rich dust grains and has important consequences for the 'missing' iron mass observed in ejecta.Comment: 17 pages, 14 figures, accepted for publication in MNRAS, final version including corrected typos and reference

Dust in Supernovae and Supernova Remnants I : Formation Scenarios

Supernovae are considered as prime sources of dust in space. Observations of local supernovae over the past couple of decades have detected the presence of dust in supernova ejecta. The reddening of the high redshift quasars also indicate the presence of large masses of dust in early galaxies. Considering the top heavy IMF in the early galaxies, supernovae are assumed to be the major contributor to these large amounts of dust. However, the composition and morphology of dust grains formed in a supernova ejecta is yet to be understood with clarity. Moreover, the dust masses inferred from observations in mid-infrared and submillimeter wavelength regimes differ by two orders of magnitude or more. Therefore, the mechanism responsible for the synthesis of molecules and dust in such environments plays a crucial role in studying the evolution of cosmic dust in galaxies. This review summarises our current knowledge of dust formation in supernova ejecta and tries to quantify the role of supernovae as dust producers in a galaxy.Peer reviewe

RAPD-PCR typing of Yersinia enterocolitica (Enterobacteriaceae) O:3 serotype strains isolated from pigs and humans

Sixteen strains of Yersinia enterocolitica serotype O:3, isolated from apparently healthy pigs collected in Rio de Janeiro, and four human strains of serotypes O:4, O:5, O:6 and O:13 were analyzed by RAPD-PCR. The strains were grouped into five genotypic profiles according to the amplification patterns obtained with three random primers. Fifteen of the 16 pig strains had identical amplification patterns, which was named genotypic profile 1. The one different profile was named genotypic profile 2. Genotypic profile 1 was also exhibited by the O:6 human serotype strain. The O:4 and O:13 human serotype strains showed similar amplification profiles with two primers. However, the third primer induced a distinct profile in each strain. Therefore, these two strains were placed into genotypic profile 3 and 4, respectively. Each primer produced a completely different amplification profile in the O:5 human serotype strain; therefore, it was named genotypic profile 5. The presence or absence of plasmids in the strains studied did not affect the amplification results. These results show that genetic variations can exist within a serotype, and strains of different serotypes can exhibit the same amplification profile when compared using other primers.<br>Foram utilizados três "primers" aleatórios para caracterizar pela técnica RAPD-PCR 16 cepas de Yersinia enterocolitica do sorotipo O:3, isoladas de suínos sadios do Rio de Janeiro. Pelos resultados dos padrões de amplificação, as 16 cepas dos suínos e as 4 cepas humanas usadas como referência (sorotipos O:4, O:5, O:6 e O:13) foram agrupadas em 5 perfis genotípicos. Quinze cepas de suínos apresentaram um padrão de amplificação idêntico (perfil genotípico 1) e somente uma apresentou um perfil de amplificação diferente (perfil genotípico 2). O mesmo padrão de amplificação do perfil genotípico 1 foi também observado em uma cepa humana do sorotipo O:6. As cepas humanas dos sorotipos O:4 e O:13 exibiram perfis de amplificação semelhantes com 2 "primers", porém com o terceiro "primer" cada uma apresentou um perfil próprio. Essas duas cepas foram enquadradas, cada uma, em um tipo de perfil (perfis genotípicos 3 e 4, respectivamente). A cepa humana do sorotipo O:5 apresentou um perfil de amplificação com cada "primer" completamente diferente dos observados nas outras cepas (perfil genotípico 5). A presença ou ausência de plasmídios nas cepas estudadas não interferiu nos resultados das amplificações. Esses resultados mostram que dentro de um mesmo sorotipo podem existir modificações genéticas e que cepas de sorotipos diferentes apresentam o mesmo perfil de amplificação com alguns "primers", comprovando que o RAPD-PCR é uma ferramenta eficaz para reagrupamento de cepas e poderá ser útil em estudos epidemiológicos para rastreamento de uma cepa e assim acompanhar a disseminação de Y. enterocolitica