In this research, we investigated the observed spectra of the hot peculiar star HD25354 with an effective temperature Teff = 12,800 K, identified the lines of radioactive chemical elements, including the elements with short decay time, and estimated the abundances of these elements. We tried to confirm or reject the existence of promethium lines and lines of other radioactive elements which were detected in previous investigations of this star and explain the physical mechanisms which are responsible for the synthesis of these elements in the stellar atmosphere. We used two high-dispersion spectra of HD25354 observed with the 2 m telescope of Terskol observatory with resolving power near R = 60,000, and a signal to noise ratio near 200. The spectrum of the star from the archive of the 1.93 m telescope of Haute-Provence observatory was also used. The observations were compared with synthetic spectra and the abundance of promethium was found using the best four lines of this element in the observed spectra: logN(Pm) = 5.84 ± 0.16 in the scale logN(H) = 12. It is comparable to the abundances of stable lanthanides in the atmosphere of this star. The abundance of thorium derived from two lines of double-ionized thorium is logN(Th) = 3.59 ± 0.15. The upper limits for technetium, radium, actinium, uranium, and americium abundances are found to be equal to 4.0, 3.0, 1.25, 3.5, and 4.0, respectively. Maybe the existence of promethium lines and lines of other unstable chemical elements in the spectra of HD25354, as well as the other stars of our Galaxy, Magellanic Clouds, and Fornax dwarf galaxy, can be explained by contamination of its atmosphere by the products of kilonova outburst and by symmetric decay of chemical elements with long decay times located at the island of stability (atomic numbers Z = 110–128) of transfermium elements. Maybe the decay of superheavy elements of the island of stability can be one of the reasons for the enhanced abundances of rare earth lanthanides in different types of stars.

Over the past decades, the achievements in astronomical instrumentation have given rise to a number of novel advanced studies related to the analysis of large arrays of observational data. One of the most famous of these studies is a study of transient events in the near and far space and a search for exoplanets. The main requirements for such kinds of projects are a simultaneous coverage of the largest possible field of view with the highest possible detection limits and temporal resolution. In this study, we present a similar project aimed at creating an extensive, continuously updated survey of transient events and exoplanets. To date, the core of the project incorporates several 0.07–2.5 m optical telescopes and the 6-m BTA telescope of the Special Astrophysical Observatory of RAS (Russia), a number of other Russian observatories and the Bonhyunsan observatory of the Korea Astronomy and Space Science Institute (South Korea). Our attention is mainly focused on the description of two groups of small, wide-angle optical telescopes for primary detection. All the telescopes are originally designed for the goals of the project and may be of interest to the scientific community. A description is also given for a new, high-precision optical spectrograph for the Doppler studies of transient and exoplanet events detected within the project. We present here the philosophy, expectations and first results obtained during the first year of running the project.

The high-resolution fiber echelle Cassegrain spectrograph for the 2-m telescope at the Shamakhy Astrophysical Observatory (ShaFES) is described. The optical circuit and the schematic of the suspended part of the spectrograph are presented. The spectrograph operates in two modes with a spectral resolution of 27 500 and 55 000 in the 370–850 nm wavelength range. The results of its testing are analyzed. The results and the procedure of test observations are detailed, and the spectrograph itself and ShaFES observational data are compared with similar instruments and the corresponding experimental data. The spectrograph provides an opportunity to measure spectra of 8m and 10m stars with a signal-to-noise ratio of S/N = 150–200 at λ = 580 nm with a 1-h exposure and resolution of R = 55 000 and 27 500, respectively.

Abstract—We report the results of laboratory tests of the first version of the high-resolution fiber-fed spectrograph designed for the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS). During laboratory tests a spectral resolution of about 70 000 was achieved. The peak efficiency of the entire optical path of the spectrograph (without light losses at the CCD, primary mirror of the 6-m telescope, and in the atmosphere) at 620 nm and with the equivalent slit widths of the 1″.5 and 0″.75 are equal to 8% and 4%, respectively. The resolving power R = 70 000 and 100 000 can be reached with the sky aperture 0″.75 and 0″.4 respectively. In the current version of the spectrograph these regimes of operation are implemented by mechanic aperturing of the slit. A dedicated projecting camera has been developed and is currently manufactured to operate with a collimated 200-mm diameter beam, which will make it possible to increase the spectral resolution up to 100 000. A two-beam image slicer will be used to maintain the luminous efficiency of the instrument at least at the 6% level.

We present the results of an experimental study of an advanced moderate-resolution spectrograph based on a cascade of narrow-band holographic gratings. The main goal of the project is to achieve a moderately high spectral resolution with R up to 5000 simultaneously in the 4300–6800 Å visible spectral range on a single standard CCD, together with an increased throughput. The experimental study consisted of (1) resolution and image quality tests performed using the solar spectrum, and (2) a total throughput test performed for a number of wavelengths using a calibrated lab monochromator. The measured spectral resolving power reaches values over R > 4000 while the experimental throughput is as high as 55%, which agrees well with the modeling results. Comparing the obtained characteristics of the spectrograph under consideration with the best existing spectrographs, we conclude that the used concept can be considered as a very competitive and cheap alternative to the existing spectrographs of the given class. We propose several astrophysical applications for the instrument and discuss the prospect of creating its full-scale version.

In this paper we describe the echelle spectrograph of the 2 meter telescope of the Rozhen National Astronomical Observatory. The spectrograph is a cross-dispersed, bench-mounted, fiber-fed instrument giving a resolution from $\sim$30000 to $\sim$45000. The spectral range obtained in one single image is from 3900 to 9000 {\AA}. We describe the parameters of the fiber injection and the guiding unit, of the spectrograph itself, and of the detector. The identified orders and the resulting resolving power are presented. The opportunity to increase of the resolution by using a narrower slit is discussed and the corresponding loss of flux is calculated. The expected signal-to-noise ratio for a set of stars of different magnitudes was derived. Some of the first results obtained with ESpeRo are shortly described.

AbstractSelected results of 1994-2004 optical photometric and high-resolution spectral observations including those obtained in the frame of a coordinated CIS countries campaign “Optical Monitoring of Unique Astrophysical Objects” and their comparison with ASM/RXTE X-ray data are briefly reviewed.

A time series of high-resolution spectra was observed in the optical wavelength region for the bright proto-planetary nebula IRAS 22272+5435 (HD 235858), along with a simultaneous monitoring of its radial velocity and BV R-C magnitudes. The object is known to vary in light, color, and velocity owing to pulsation with a period of 132 days. The light and color variations are accompanied by significant changes in spectral features, most of which are identified as lines of carbon-bearing molecules. According to the observations, the C-2 Swan system and CN Red system lines are stronger near the light minimum. A photospheric spectrum of the central star was calculated using new self-consistent atmospheric models. The observed intensity variations in the C2 Swan system and CN Red system lines were found to be much larger than expected if due solely to the temperature variation in the atmosphere of the pulsating star. In addition, the molecular lines are blueshifted relative to the photospheric velocity. The site of formation of the strong molecular features appears to be a cool outflow triggered by the pulsation. The variability in atomic lines seems to be mostly due variations of the effective temperature during the pulsation cycle. The profiles of strong atomic lines are split, and some of them are variable in a timescale of a week or so, probably because of shock waves in the outer atmosphere.

Using spectra of the star AE Aur (HD 34078), covering the period 1997-2015, we suggest that two strong molecular features of CH and CH+ underwent detectable changes of intensity. In the last five years both CH and CH+ declined sharply and systematically, with the CH/CH+ ratio steadily growing. No variations in the radial velocities of the observed interstellar features was detected during the covered period.

В статье приведены данные по влиянию гуминовой кормовой добавки «ПИТЭР ПИТ» на здоровье и продуктивные качества ремонтного молодняка крупного рогатого скота. Отмечено, что она не оказывает отрицательного влияния на самочувствие животных и их клинические показатели, стимулирует кроветворную функцию и окислительные процессы в организме. Применение гуминовой кормовой добавки способствует повышению аппетита у телят, обеспечивая увеличение среднесуточного прироста более чем на 12 %, снижению затрат энергетических кормовых единиц и переваримого протеина на 1 кг прироста живой массы соответственно на 7,7 и 5 %. Также в статье рассмотрены результаты применения витаминно-минеральной кормовой добавки «Витасоль» в рационах высокопродуктивных коров. Приведены данные ее положительного влияния на гематологический статус, корректировку минерального обмена и молочную продуктивность животных.

Radial velocity measurements, BVRC photometry, and high-resolution spectroscopy in the wavelength region from blue to near-infrared are employed in order to clarify the evolutionary status of the carbon-enhanced metal-poor star HD 112869 with a unique ratio of carbon isotopes in the atmosphere. An LTE abundance analysis was carried out using the method of spectral synthesis and new self-consistent 1D atmospheric models. The radial velocity monitoring confirmed semiregular variations with a peak-to-peak amplitude of about 10 km s(-1) and a dominating period of about 115 days. The light, color, and radial velocity variations are typical of the evolved pulsating stars. The atmosphere of HD 112869 appears to be less metal-poor than reported before, [Fe/H] = -2.3 +/- 0.2 dex. Carbon-to-oxygen and carbon isotope ratios are found to be extremely high, C/O similar or equal to 12.6 and C-12/C-13 greater than or similar to 1500, respectively. The s-process elements yttrium and barium are not enhanced, but neodymium appears to be overabundant. The magnesium abundance seems to be lower than the average found for CEMP stars, [Mg/Fe] < +0.4 dex. HD 112869 could be a single low-mass halo star in the stage of asymptotic giant branch evolution.

The rotation curve of the Galaxy is generally thought to be flat. However, using radial velocities from interstellar molecular clouds, as is common in rotation curve determination, seems to be incorrect and may lead to wrongly inferring that the rotation curve is flat indeed. Tests based on photometric and spectral observations of bright stars may also be misleading. The rotation tracers (OB stars) are affected by motions around local gravity centers and by pulsation effects seen in such early-type objects. To get rid of the latter involves extensive observing work. We introduce a method of studying the kinematics of the thin disk of our Galaxy outside the solar orbit in a way that avoids these problems. We propose a test based on observations of interstellar Ca II H and K lines that determines both radial velocities and distances. We implemented the test using stellar spectra of thin disk stars at Galactic longitudes of 135 degrees and 180 degrees. Using this method, we constructed the rotation curve of the thin disk of the Galaxy. The test leads to the obvious conclusion that the rotation curve of the thin gaseous galactic disk, represented by the Ca II lines, is Keplerian outside the solar orbit rather than flat.

We propose a project of a high-resolution (R = 100 000) fiber-fed spectrograph for comprehensive studies of stellar atmospheres, exoplanet searches, asteroseismological studies, studies of stellar magnetism, active nuclei of bright galaxies, interstellar medium, etc. We present the optical scheme of the instrument. The operating wavelength region spans from 4000 to 7500 A. We also present the optical scheme of the pre-fiber optic unit of the spectrograph. The unit supports four main modes of spectroscopic observations: the mode of traditional spectroscopy with the spectrum of the studied object taken along with the background spectrum in the immediate vicinity of the object; the mode of the simultaneous recording of the spectrum of the object and that of the wavelength standard; the mode of high-precision spectroscopy with an iodine cell, and the mode of spectropolarimetric observations with the measurement of all the Stokes parameters.

We propose a project of a high-resolution (R = 100 000) fiber-fed spectrograph for comprehensive studies of stellar atmospheres, exoplanet searches, asteroseismological studies, studies of stellar magnetism, active nuclei of bright galaxies, interstellar medium, etc. We present the optical scheme of the instrument. The operating wavelength region spans from 4000 to 7500 Å. We also present the optical scheme of the pre-fiber optic unit of the spectrograph. The unit supports four main modes of spectroscopic observations: the mode of traditional spectroscopy with the spectrum of the studied object taken along with the background spectrum in the immediate vicinity of the object; the mode of the simultaneous recording of the spectrum of the object and that of the wavelength standard; the mode of high-precision spectroscopy with an iodine cell, and the mode of spectropolarimetric observations with the measurement of all the Stokes parameters.

The article presents analysis of different dosage feed additive vitasalt infl uence on hematologic indexes, digestive processes of highly productive black and white cattle. They have mentioned that in a case of increasing they it as alt dosa geat farm diet of the experimental animals they noticed the increase of morphologic and bio-chemical characteristics of blood. These characteristics have approached the physiologic norm for milking cows. The data we have got has au then tic in crease. The study of digestion in rumen of ruminants has let determine metabolic changes in protein metabolism. During the farm experiment we have determined that in a case of increasing feed additive dosage there is increase of total, protein and non-protein nitrogen in rumen. Wehavenoticedrumenliquidр Нincreaseandthe approach of this index to physiologic norm of milking cows. Thus, feed additive vitasalt usage in diet has led to normalization of metabolic processes in ruminants’ rumen and approaching the physiologic norms of hematologic indexes.