ПРИНЦИПИ ПІДГОТОВКИ СПІВРОБІТНИКІВ НАЦІОНАЛЬНОЇ ПОЛІЦІЇ З ДОМЕДИЧНОЇ ДОПОМОГИ

Based on the experience of organizing and conducting trainings for the National Police in the field of premedical care, the program “First on the spot” sets out the key principles of such training, which underlie long-term knowledge and practical skills aimed at rescuing a person in urgent need. The basic principle of training for the premedical aid of National Police staff is its standardization in various educational institutions and educational departments. The rules of such standardization include: the availability of a unified material and technical base, the corresponding training facilities, prepared according to the standard program of instructors for provision of medical assistance, the availability of uniform teaching materials. The second principle is the system approach. It consists in a clear understanding of the role of the police in the system of succession assistance to victims and patients, taking into account the existing system of emergency medical care, both in individual and in mass cases, which is achieved through joint training with rescuers and physicians. The third principle is the introduction of a continuity of education system for the police system for medical assistance. The implementation of these principles is the key to long-term knowledge and practical skills aimed at rescuing people in urgent situations, because global statistics indicate that the police are coming to the scene quickly. The training of the National Police in the field of premedical assistance is an important element of their training. The introduction of the principles of standardizing the training of police officers on medical assistance, the systematic approach and the continuity of education is a key to successful completion of their tasks as well as to save lives in urgent situations.На основі досвіду організації і проведення навчання співробітників Національної поліції з домедичної допомоги за програмою «Перший на місці події» сформульовано ключові принципи такої підготовки, які лежать в основі довготривалих знань і практичних навичок, спрямованих на порятунок людини у невідкладному стані. Основним принципом підготовки з домедичної допомоги співробітників Національної поліції є її стандартизованість у різних навчальних закладах і навчальних відділеннях. До правил такої стандартизації належать: наявність уніфікованої матеріально-технічної бази, відповідних навчальних приміщень, підготовлених за стандартною програмою інструкторів з надання домедичної допомоги, наявність єдиних навчально-методичних матеріалів. Другим принципом є системний підхід. Він полягає в чіткому усвідомленні ролі поліцейських у системі спадкоємного надання допомоги постраждалим і хворим з урахуванням існуючої системи екстреної медичної допомоги як в одиничних, так і в масових випадках, що досягається шляхом спільних з рятувальниками і медиками тренувань. Третім принципом є запровадження для поліцейських системи безперервності освіти з домедичної допомоги. Впровадження зазначених принципів є запорукою довготривалих знань і практичних навичок, спрямованих на порятунок людини у невідкладному стані, адже світова статистика вказує, що найшвидше на місце події прибувають саме поліцейські. Навчання співробітників Національної поліції з домедичної допомоги є важливим елементом їх службової підготовки. Запровадження принципів стандартизації підготовки поліцейських з домедичної допомоги, системного підходу та безперервності освіти є запорукою успішного виконання ними як поставлених завдань, так і рятування життя особам у невідкладному стані

Large-Scale Gravitational Instability and Star Formation in the Large Magellanic Cloud

Large-scale star formation in disk galaxies is hypothesized to be driven by global gravitational instability. The observed gas surface density is commonly used to compute the strength of gravitational instability, but according to this criterion star formation often appears to occur in gravitationally stable regions. One possible reason is that the stellar contribution to the instability has been neglected. We have examined the gravitational instability of the Large Magellanic Cloud (LMC) considering the gas alone, and considering the combination of collisional gas and collisionless stars. We compare the gravitationally unstable regions with the on-going star formation revealed by Spitzer observations of young stellar objects. Although only 62% of the massive young stellar object candidates are in regions where the gas alone is unstable, some 85% lie in regions unstable due to the combination of gas and stars. The combined stability analysis better describes where star formation occurs. In agreement with other observations and numerical models, a small fraction of the star formation occurs in regions with gravitational stability parameter Q > 1. We further measure the dependence of the star formation timescale on the strength of gravitational instability, and quantitatively compare it to the exponential dependence expected from numerical simulations.Comment: Accepted for publication in ApJ, 10 pages, 5 figure

Molecular Gas in the Low Metallicity, Star Forming Dwarf IC 10

We present a complete survey of CO 1->0 emission in the Local Group dwarf irregular IC 10. The survey, conducted with the BIMA interferometer, covers the stellar disk and a large fraction of the extended HI envelope with the sensitivity and resolution necessary to detect individual giant molecular clouds (GMCs) at the distance of IC 10 (950 kpc). We find 16 clouds with a total CO luminosity of 1 x 10^6 K km s^-1 pc^2, equivalent to 4 x 10^6 Msun of molecular gas using the Galactic CO-to-H2 conversion factor. Observations with the ARO 12m find that BIMA may resolve out as much as 50% of the CO emission, and we estimate the total CO luminosity as 2.2 x 10^6 K km s^-1 pc^2. We measure the properties of 14 GMCs from high resolution OVRO data. These clouds are very similar to Galactic GMCs in their sizes, line widths, luminosities, and CO-to-H2 conversion factors despite the low metallicity of IC 10 (Z ~ 1/5 Zsun). Comparing the BIMA survey to the atomic gas and stellar content of IC 10 we find that most of the CO emission is coincident with high surface density HI. IC 10 displays a much higher star formation rate per unit molecular (H2) or total (HI+H2) gas than most galaxies. This could be a real difference or may be an evolutionary effect - the star formation rate may have been higher in the recent past.Comment: 21 pages, 14 figures, Accepted to Ap

The Dark Matter Density in the Solar Neighborhood reconsidered

Both the gas flaring and the dip in the rotation curve, which was recently reconfirmed with precise measurements using the VERA VLBI array in Japan, suggest doughnut-like substructure in the dark matter (DM) halo. A global fit to all available data shows that the data are indeed best described by an NFW DM profile complemented by two doughnut-like DM substructures with radii of 4.2 and 12.4 kpc, which coincide with the local dust ring and the Monocerus ring of stars, respectively. Both regions have been suggested as regions with tidal streams from "shredded" satellites. If real, the radial extensions of these nearby ringlike structures enhance the local dark matter density by a factor of four to about 1.3$\pm0.3$ GeV/cm$^3$. It is shown that i) this higher DM density is perfectly consistent with the local gravitational potential determining the surface density and the local matter density (Oort limit), ii) previous determinations of the surface density were biased by the assumption of a smoothly varying DM halo and iii) the s-shaped gas flaring is explained. Such a possible enhancement of the local DM density is of great interest for direct DM searches and would change the directional dependence for indirect DM searches.Comment: 14 pages, 4 figures, extended version, accepted for publication in JCA

The Photometric and Kinematic Structure of Face-On Disk Galaxies. I. Sample Definition, H-alpha Integral Field Spectroscopy, and HI Line-Widths

We present a survey of the photometric and kinematic properties of 39 nearby, nearly face-on disk galaxies. Our approach exploits echelle-resolution integral-field spectroscopy of the H-alpha regions, obtained with DensePak on the WIYN 3.5m telescope Bench Spectrograph. This data is complemented by HI line-profiles observed with the Nancay radio telescope for 25 of these sample galaxies. Twelve additional line-widths are available for sample galaxies from the literature. In this paper, we introduce the goals of this survey, define the sample selection algorithm, and amass the integral field spectroscopic data and HI line-widths. We establish spatially-integrated H-alpha line-widths for the sample. We test the veracity of these spatially-integrated line profiles by convolving narrow-band imaging data with velocity field information for one of the sample galaxies, PGC 38268, and also by comparing to HI line profiles. We find HI and H-alpha line profiles to be similar in width but different in shape, indicating we are observing different spatial distributions of ionized and neutral gas in largely axisymmetric systems with flat outer rotation-curves. We also find vertical velocity dispersions of the ionized disk gas within several disk scale-lengths have a median value of 18 km/s and an 80% range of 12-26 km/s. This is only a factor of ~2 larger than what is observed for neutral atomic and molecular gas. With standard assumptions for intrinsic and thermal broadening for H-alpha, this translates into a factor of three range in turbulent velocities, between 8 and 25 km/s.Comment: 29 pages, 20 figures; accepted for publication in ApJ Supplement Serie

UV emission and Star Formation in Stephan's Quintet

we present the first GALEX UV images of the well known interacting group of galaxies, Stephan's Quintet (SQ). We detect widespread UV emission throughout the group. However, there is no consistent coincidence between UV structure and emission in the optical, H\alpha, or HI. Excluding the foreground galaxy NGC7320 (Sd), most of the UV emission is found in regions associated with the two spiral members of the group, NGC7319 and NGC7318b, and the intragroup medium starburst SQ-A. The extinction corrected UV data are analyzed to investigate the overall star formation activity in SQ. It is found that the total star formation rate (SFR) of SQ is 6.69+-0.65 M_\sun/yr. Among this, 1.34+-0.16 M_sun/yr is due to SQ-A. This is in excellent agreement with that derived from extinction corrected H\alpha luminosity of SQ-A. The SFR in regions related to NGC 7319 is 1.98+-0.58 M_\sun/yr, most of which(68%) is contributed by the disk. The contribution from the 'young tail' is only 15%. In the UV, the 'young tail' is more extended (~100 kpc) and shows a loop-like structure, including the optical tail, the extragalactic HII regions recently discovered in H\alpha, and other UV emission regions discovered for the first time. The UV and optical colors of the 'old tail' are consistent with a single stellar population of age t ~10^{8.5+-0.4} yrs. The UV emission associated with NGC 7318b is found in a very large (~80 kpc) disk, with a net SFR of 3.37+-0.25 M_sun/yr. Several large UV emission regions are 30 -- 40 kpc away from the nucleus of NGC7318b. Although both NGC7319 and NGC7318b show peculiar UV morphology, their SFR is consistent with that of normal Sbc galaxies, indicating that the strength of star formation activity is not enhenced by interactions.Comment: This paper will be published as part of the Galaxy Evolution Explorer(GALEX) Astrophysical Journal Letters Special Issue. Links to the full set of papers will be available at http:/www.galex.caltech.edu/PUBLICATIONS/ after November 22, 200

The Metallicity-Luminosity Relation, Effective Yields, and Metal Loss in Spiral and Irregular Galaxies

I present results on the correlation between galaxy mass, luminosity, and metallicity for a sample of spiral and irregular galaxies having well-measured abundance profiles, distances, and rotation speeds. Additional data for low surface brightness galaxies from the literature are also included for comparison. These data are combined to study the metallicity-luminosity and metallicity-rotation speed correlations for spiral and irregular galaxies. The metallicity luminosity correlation shows its familiar form for these galaxies, a roughly uniform change in the average present-day O/H abundance of about a factor 100 over 11 magnitudes in B luminosity. However, the O/H - V(rot) relation shows a change in slope at a rotation speed of about 125 km/sec. At faster V(rot), there appears to be no relation between average metallicity and rotation speed. At lower V(rot), the metallicity correlates with rotation speed. This change in behavior could be the result of increasing loss of metals from the smaller galaxies in supernova-driven winds. This idea is tested by looking at the variation in effective yield, derived from observed abundances and gas fractions assuming closed box chemical evolution. The effective yields derived for spiral and irregular galaxies increase by a factor of 10-20 from V(rot) approximately 5 km/sec to V(rot) approximately 300 km/sec, asympotically increasing to approximately constant y(eff) for V(rot) > 150 km/sec. The trend suggests that galaxies with V(rot) < 100-150 km/sec may lose a large fraction of their SN ejecta, while galaxies above this value tend to retain metals.Comment: 40 pages total, including 7 encapsulated postscript figures. Accepted for publication in 20 Dec 2002 Ap

Star Formation Thresholds in Galactic Disks

We report the first results of a detailed study of the star formation law in a sample of 32 nearby spiral galaxies with well-measured rotation curves, HI and H$_2$ (as traced by CO) surface density profiles, and new \Ha CCD photometry. Our results strongly support the view that the formation of gravitationally bound interstellar clouds regulates the onset of widespread star formation -- at least in the outer regions of galactic disks.Comment: Will appear in July 1 ApJ. Abbreviated abstract. Postscript version available at http://www.astro.caltech.edu/~clm

СТАН МІНЕРАЛІЗАЦІЇ КІСТКОВОЇ ТКАНИНИ У ДІТЕЙ З ХРОНІЧНИМ ГАСТРОДУОДЕНІТОМ

The analysis of biochemical indeces of mineral metabolism and the results of densitometry in children with chronic gastroduodenitis (the duration of disease — 1-5 years) have revealed the signs of osteologic pathology associated with mineral metabolism disturbances, depending on alkaline phosphatase aectivity. The findings of our investigation prove the necessity of seeking the ways to correct osteologic changes.Проведено анализ биохимических показателей минерального обмена веществ й результатов денситометрии у детей с хроническим гастродуоденитом при сроке заболевания 1-5 лет. Результати исследований показали наличие признаков остеопороза й остеосклероза на фоне нарушенного минерального обмена в зависимости от активности щелочной фосфатази, что указывает на необходимость поиска коррекции выявленных изменений.Проведено аналіз біохімічних показників мінерального обміну речовин та результатів денситометрії у дітей з хронічним гастродуоденітом при терміні захворювання 1-5 років. Результати досліджень показали наявність ознак остеопорозу та остеосклерозу на тлі порушеного мінерального обміну в залежності від активності лужної фосфатази, що вказує на необхідність пошуку корекції виявлених змін

The Updated Zwicky Catalog (UZC)

The Zwicky Catalog of galaxies (ZC), with m_Zw<=15.5mag, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing: (1) coordinates with <~2 arcsec errors for all of the Nuzc catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7,257 galaxies in the CfA2 redshift survey not previously published; for another 5,625 CfA redshifts we list the remeasured or uniformly re-reduced value. Among our new measurements, Nmul are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interactions among galaxies. All of the new redshifts correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. About 1,000 of our new measurements were motivated either by inadequate signal-to-noise in the original spectrum or by an ambiguous identification of the galaxy associated with a ZCAT redshift. The redshift catalog we include here is ~96% complete to m_Zw<=15.5, and ~98% complete (12,925 galaxies out of a total of 13,150) for the RA(1950) ranges [20h--4h] and [8h--17h] and DEC(1950) range [-2.5d--50d]. (abridged)Comment: 34 pp, 7 figs, PASP 1999, 111, 43