Analysis of electronic documents protection in the EDM system

Настоящая статья посвящена анализу защищенности электронных документов в информационных системах электронного документооборота. Рассматриваются основные специфичные процессы обработки информации содержащейся в электронном документе. Произведен анализ угроз информационной безопасности электронных документов и установлена взаимосвязь между основными видами угроз в системах ЭДО. Дана оценка защищенности современных систем ЭДО.This article is devoted to the analysis of electronic documents protection in electronic document management information systems. The basic processing specific information, contained in the electronic document. The analysis of threats to information security of electronic documents and the interrelation between the main types of threats in the EDF system. The estimation of the security of modern EDF system

МОДЕЛЬНАЯ САМООЦЕНКА ПРЕМИРУЕМОГО КАЧЕСТВА

The authors study capacity and comprehensive character of self-assessment principles in international and Russian models of awarding bonuses for the quality performance. They underline the diversity of approaches in different economic sectors, conformity with the levels of organization development of the companies, the difference of self-assessment models with the ISO 9000 standards, which consider only the processes aimed directly at creating qualitative final product. The bonus system is considered as a tool to increase economic effectiveness and higher performance of the staff of transport holding-type companies.Авторами рассматриваются потенциал и универсальность  использования принципов самооценки в моделях международных и национальных  премий за качество. Многообразие подходов в различных отраслях, соответствие  уровням организационного  развития компаний, отличие  моделей самооценки от более распространенных стандартов  серии ISO 9000, где учитываются  только процессы, непосредственно  направленные на создание качественного конечного продукта. Премиальная система как способ повышения экономической эффективности и результативности трудовой деятельности в условиях транспортного холдинга.

Starlight-polarization-based tomography of the magnetized ISM: Pasiphae's line-of-sight inversion method

We present the first Bayesian method for tomographic decomposition of the plane-of-sky orientation of the magnetic field with the use of stellar polarimetry and distance. This standalone tomographic inversion method presents an important step forward in reconstructing the magnetized interstellar medium (ISM) in 3D within dusty regions. We develop a model in which the polarization signal from the magnetized and dusty ISM is described by thin layers at various distances. Our modeling makes it possible to infer the mean polarization (amplitude and orientation) induced by individual dusty clouds and to account for the turbulence-induced scatter in a generic way. We present a likelihood function that explicitly accounts for uncertainties in polarization and parallax. We develop a framework for reconstructing the magnetized ISM through the maximization of the log-likelihood using a nested sampling method. We test our Bayesian inversion method on mock data taking into account realistic uncertainties from $Gaia$ and as expected for the optical polarization survey PASIPHAE according to the currently planned observing strategy. We demonstrate that our method is effective in recovering the cloud properties as soon as the polarization induced by a cloud to its background stars is higher than $\sim 0.1\%$, for the adopted survey exposure time and level of systematic uncertainty. Our method makes it possible to recover not only the mean polarization properties but also to characterize the intrinsic scatter, thus opening ways to characterize ISM turbulence and the magnetic field strength. Finally, we apply our method to an existing dataset of starlight polarization with known line-of-sight decomposition, demonstrating agreement with previous results and an improved quantification of uncertainties in cloud properties.Comment: 28 pages, including 2 appendices, submitted to A&

Bright-Moon Sky as a Wide-Field Linear Polarimetric Flat Source for Calibration

Next-generation wide-field optical polarimeters like the Wide-Area Linear Optical Polarimeters (WALOPs) have a field of view (FoV) of tens of arcminutes. For efficient and accurate calibration of these instruments, wide-field polarimetric flat sources will be essential. Currently, no established wide-field polarimetric standard or flat sources exist. This paper tests the feasibility of using the polarized sky patches of the size of around ten-by-ten arcminutes, at a distance of up to 20 degrees from the Moon, on bright-Moon nights as a wide-field linear polarimetric flat source. We observed 19 patches of the sky adjacent to the bright-Moon with the RoboPol instrument in the SDSS-r broadband filter. These were observed on five nights within two days of the full-Moon across two RoboPol observing seasons. We find that for 18 of the 19 patches, the uniformity in the measured normalized Stokes parameters $q$ and $u$ is within 0.2 %, with 12 patches exhibiting uniformity within 0.07 % or better for both $q$ and $u$ simultaneously, making them reliable and stable wide-field linear polarization flats. We demonstrate that the sky on bright-Moon nights is an excellent wide-field linear polarization flat source. Various combinations of the normalized Stokes parameters $q$ and $u$ can be obtained by choosing suitable locations of the sky patch with respect to the MoonComment: 8 pages including appendix, 6 figures and 3 tables. Submitted to Astronomy and Astrophysics for review. Comments are welcom

Cosmoglobe DR1. III. First full-sky model of polarized synchrotron emission from all WMAP and Planck LFI data

We present the first model of full-sky polarized synchrotron emission that is derived from all WMAP and Planck LFI frequency maps. The basis of this analysis is the set of end-to-end reprocessed Cosmoglobe Data Release 1 sky maps presented in a companion paper, which have significantly lower instrumental systematics than the legacy products from each experiment. We find that the resulting polarized synchrotron amplitude map has an average noise rms of $3.2\,\mathrm{\mu K}$ at 30 GHz and $2^{\circ}$ FWHM, which is 30% lower than the recently released BeyondPlanck model that included only LFI+WMAP Ka-V data, and 29% lower than the WMAP K-band map alone. The mean $B$-to-$E$ power spectrum ratio is $0.40\pm0.02$, with amplitudes consistent with those measured previously by Planck and QUIJOTE. Assuming a power law model for the synchrotron spectral energy distribution, and using the $T$--$T$ plot method, we find a full-sky inverse noise-variance weighted mean of $\beta_{\mathrm{s}}=-3.07\pm0.07$ between Cosmoglobe DR1 K-band and 30 GHz, in good agreement with previous estimates. In summary, the novel Cosmoglobe DR1 synchrotron model is both more sensitive and systematically cleaner than similar previous models, and it has a more complete error description that is defined by a set of Monte Carlo posterior samples. We believe that these products are preferable over previous Planck and WMAP products for all synchrotron-related scientific applications, including simulation, forecasting and component separation.Comment: 15 pages, 15 figures, submitted to A&

Cosmoglobe: Towards end-to-end CMB cosmological parameter estimation without likelihood approximations

We implement support for a cosmological parameter estimation algorithm as proposed by Racine et al. (2016) in Commander, and quantify its computational efficiency and cost. For a semi-realistic simulation similar to Planck LFI 70 GHz, we find that the computational cost of producing one single sample is about 60 CPU-hours and that the typical Markov chain correlation length is $\sim$100 samples. The net effective cost per independent sample is $\sim$6 000 CPU-hours, in comparison with all low-level processing costs of 812 CPU-hours for Planck LFI and WMAP in Cosmoglobe Data Release 1. Thus, although technically possible to run already in its current state, future work should aim to reduce the effective cost per independent sample by at least one order of magnitude to avoid excessive runtimes, for instance through multi-grid preconditioners and/or derivative-based Markov chain sampling schemes. This work demonstrates the computational feasibility of true Bayesian cosmological parameter estimation with end-to-end error propagation for high-precision CMB experiments without likelihood approximations, but it also highlights the need for additional optimizations before it is ready for full production-level analysis.Comment: 10 pages, 8 figures. Submitted to A&

Cosmoglobe DR1 results. I. Improved Wilkinson Microwave Anisotropy Probe maps through Bayesian end-to-end analysis

We present Cosmoglobe Data Release 1, which implements the first joint analysis of WMAP and Planck LFI time-ordered data, processed within a single Bayesian end-to-end framework. This framework builds directly on a similar analysis of the LFI measurements by the BeyondPlanck collaboration, and approaches the CMB analysis challenge through Gibbs sampling of a global posterior distribution, simultaneously accounting for calibration, mapmaking, and component separation. The computational cost of producing one complete WMAP+LFI Gibbs sample is 812 CPU-hr, of which 603 CPU-hrs are spent on WMAP low-level processing; this demonstrates that end-to-end Bayesian analysis of the WMAP data is computationally feasible. We find that our WMAP posterior mean temperature sky maps and CMB temperature power spectrum are largely consistent with the official WMAP9 results. Perhaps the most notable difference is that our CMB dipole amplitude is $3366.2 \pm 1.4\ \mathrm{\mu K}$, which is $11\ \mathrm{\mu K}$higher than the WMAP9 estimate and$2.5\ {\sigma}$ higher than BeyondPlanck; however, it is in perfect agreement with the HFI-dominated Planck PR4 result. In contrast, our WMAP polarization maps differ more notably from the WMAP9 results, and in general exhibit significantly lower large-scale residuals. We attribute this to a better constrained gain and transmission imbalance model. It is particularly noteworthy that the W-band polarization sky map, which was excluded from the official WMAP cosmological analysis, for the first time appears visually consistent with the V-band sky map. Similarly, the long standing discrepancy between the WMAP K-band and LFI 30 GHz maps is finally resolved, and the difference between the two maps appears consistent with instrumental noise at high Galactic latitudes. All maps and the associated code are made publicly available through the Cosmoglobe web page.Comment: 65 pages, 61 figures. Data available at cosmoglobe.uio.no. Submitted to A&

ОПЫТ ЛЕЧЕНИЯ СВИЩА КУЛЬТИ ПРАВОГО ГЛАВНОГО БРОНХА С ПРИМЕНЕНИЕМ СОСУДИСТОГО ОККЛЮДЕРА

Goal: to close the fistula of right main bronchus stump with the use of the vascular occluder of ASD. The clinical case is described. Materials and methods. The fistula of right main bronchus, developed after final pulmonectomy on the right performed due to emergency indications caused fibrous cavernous tuberculosis, complicated by pulmonary hemorrhage, was closed by ASD occluder with 8 mm diameter, relevant to the diameter of bronchopleural fistula. Empyema space was first of all sanitated through thoracostoma, the volume of right hemithorax was reduced due preceding seven-costal posterosuperior thoracoplasty. The intervention was done under local anesthesia with double monitoring from tracheal lumen by bronchoscope and from thoracostoma space. The intervention lasted for 20 minutes. Results. Air discharge stopped immediately after the installation of the occluder. The patient demonstrated significant improvement of respiration and voicing even without pleural space plugging. In the follow-up period in 12 months the occluder was covered by epithelium fully stopping the air inflow from bronchus into pleural space. Management of bronchial fistula with ASD occluder is a fast, safe and effective intervention.Цель работы: закрытие свища культи правого главного бронха при помощи сосудистого окклюдера ASD. Приведен клинический пример.Методы и материалы. Закрытие свища правого главного бронха, возникшего после выполнения по неотложным показаниям заключительной пульмонэктомии справа по поводу фиброзно-кавернозного туберкулеза, осложненного легочным кровотечением, осуществлялось АSD-окклюдером диаметром 8 мм, что соответствовало диаметру бронхоплеврального свища. Полость эмпиемы была прежде санирована через торакостому, объем правого гемиторакса уменьшен за счет предшествовавшего выполнения семиреберной задневерхней торакопластики. Процедура выполнена под местной анестезией под двойным контролем - из просвета трахеи посредством бронхоскопа и из полости торакостомы. Продолжительность процедуры составила 20 мин.Результаты. Сброс воздуха прекратился сразу же после установки окклюдера. Пациент отметил существенное улучшение дыхания и появление голоса даже без тампонирования плевральной полости. В последующем периоде наблюдения через 12 мес. отмечается покрытие устройства слоем эпителия с полным прекращением поступления воздуха из бронхов в плевральную полость. Лечение бронхиального свища с применением ASD-окклюдера является быстровыполнимой, безопасной и эффективной процедурой

BeyondPlanck X. Planck LFI frequency maps with sample-based error propagation

We present Planck LFI frequency sky maps derived within the BeyondPlanck framework. This framework draws samples from a global posterior distribution that includes instrumental, astrophysical and cosmological parameters, and the main product is an entire ensemble of frequency sky map samples. This ensemble allows for computationally convenient end-to-end propagation of low-level instrumental uncertainties into higher-level science products. We show that the two dominant sources of LFI instrumental systematic uncertainties are correlated noise and gain fluctuations, and the products presented here support - for the first time - full Bayesian error propagation for these effects at full angular resolution. We compare our posterior mean maps with traditional frequency maps delivered by the Planck collaboration, and find generally good agreement. The most important quality improvement is due to significantly lower calibration uncertainties in the new processing, as we find a fractional absolute calibration uncertainty at 70 GHz of $\delta g_{0}/g_{0} =5 \cdot 10^{-5}$, which is nominally 40 times smaller than that reported by Planck 2018. However, the original Planck 2018 estimate has a non-trivial statistical interpretation, and this further illustrates the advantage of the new framework in terms of producing self-consistent and well-defined error estimates of all involved quantities without the need of ad hoc uncertainty contributions. We describe how low-resolution data products, including dense pixel-pixel covariance matrices, may be produced directly from the posterior samples without the need for computationally expensive analytic calculations or simulations. We conclude that posterior-based frequency map sampling provides unique capabilities in terms of low-level systematics modelling and error propagation, and may play an important role for future CMB B-mode experiments. (Abridged.)Comment: 32 pages, 23 figures, data available from https://www.cosmoglobe.uio.no