66 research outputs found
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 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 , 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 and
is within 0.2 %, with 12 patches exhibiting uniformity within 0.07 % or
better for both and 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 and 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
at 30 GHz and 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 -to- power
spectrum ratio is , 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 -- plot method,
we find a full-sky inverse noise-variance weighted mean of
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
100 samples. The net effective cost per independent sample is 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 , which is $11\
\mathrm{\mu K}2.5\ {\sigma}$ 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 , 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
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