We present the conceptual framework of the Astronomical Hub (AstroHub), a unified platform combining various optical instruments at a single observatory. Its major approach lies in arranging conditions for research groups to install telescopes and equipment and participate in joint projects. AstroHub is planned to integrate Virtual Observatory (VO) tools, FAIR data principles, and a telescope network to create a powerful and attractive ecosystem for both robust near-Earth object (NEO) monitoring and diverse deep space research. We provide an overview of the AstroHub development directions in the case study of the Assy-Turgen Observatory.

Spectral and photometric observations are a unique tool for studying the Resident Space Objects (RSO). Spectral observations are of particular value. They are precious sources of information in identifying and classifying RSO by their spectral features and studying the variation of these features caused by the influence of space weathering. The paper we present shows the results of the geostationary satellite (GEO) reflection spectra analysis. We use spectral observations to analyze reflective spectra and relevant parameters to develop the methodology of satellite identification. Spectral observations were obtained on the spectrograph mounted on a 1.5-meter telescope AZT-20 of the Assy-Turgen Observatory. Photometric characteristics derived from spectral observations show signs of dependence on the platform of a satellite and its service life in orbit. Comparison of observed and model reflective spectra indicates the possibility of identifying the satellite shape and its composite materials. The results of the work will be of interest for the study of space weathering on materials, will allow us to better understand the situation in GEO orbits, and refine the methods for near-miss events prediction, taking into account the geometry of objects and the properties of their surfaces.

Optical broad-band spectral shape measurements of gamma-ray bursts (GRBs) are typically made starting an hour or more after the trigger event. With our automated, rapid-response system, the Burst Simultaneous Three-channel Imager (BSTI) on the Nazarbayev University Transient Telescope at Assy-Turgen Astrophysical Observatory (NUTTelA-TAO), we began measurements of GRB200925B 129 s after the Swift BAT trigger. The temporal decay log slopes in the g', r', and i' bands in the time interval 129 s to 1029 s are -0.43 \pm 0.31, -0.43 \pm 0.15, and -0.72 \pm 0.14, respectively. During the decay phase, a shift in color from red to blue, a change in log slope of \{beta} from -2.73 to -1.52 was measured. The evolution in the optical spectral slope is consistent with a decrease in extinction caused by dust destruction.

ABSTRACT Instruments, such as the ROTSE, TORTORA, Pi of the Sky, MASTER-net, and others have recorded single-band optical flux measurements of gamma-ray bursts starting as early as ∼ 10 s after gamma-ray trigger. The earliest measurements of optical spectral shape have been made only much later, typically on hour time-scales, never starting less than a minute after trigger, until now. Beginning only 58 s after theSwift BAT triggered on GRB201015A, we observed a sharp rise in optical flux to a peak, followed by a power law temporal decay, ∝ t−0.81 ± 0.03. Flux was measured simultaneously in three optical bands, g′, r′, and i′, using our Burst Simultaneous Three-channel Imager on the Nazarbayev University Transient Telescope at Assy-Turgen Astrophysical Observatory telescope. Our data during the decay show strong colour evolution from red to blue, with a change in the optical log slope of +0.72 ± 0.14; during this time the X-ray log slope remained constant. We did not find evidence for a two-component jet structure or a transition from reverse to forward shock or a prompt emission component that would explain this change in slope. We find that the majority of the optical spectral slope evolution is consistent with a monotonic decay of extinction, evidence of dust destruction. Assuming a constant source spectral slope and an Small Magellanic Cloud-like extinction curve, we derive a change in the local extinction $A_\mathrm{v}^\mathrm{local}$ from ∼0.8 mag to 0.3 mag in ∼2500 s. This work shows that significant information about the early emission phase is being missed without such early observations with simultaneous multiband instruments.

Представлены результаты анализа многоволновых наблюдений длинного космического гамма-всплеска GRB 200829A. Красное смещение всплеска \(z\approx 1.29\pm 0.04\) определено фотометрическим методом на стадии послесвечения. В гамма-диапазоне событие является одним из самых ярких (в изотропном эквиваленте) \(E_{\textrm{iso}}\gtrsim 10^{54}\) эрг. Многоцветная кривая блеска послесвечения GRB 200829A характеризуется хроматизмом и наличием плато, плавно переходящего в степенное падение потока, которое можно также интерпретировать как квазисинхронную неоднородность (вспышку). Мы предполагаем, что наличие хроматической неоднородности в послесвечении не противоречит теории структурированного джета.

Results of spectral studies of fifteen Seyfert galaxies at red wavelengths based on long-term observations are presented. In this range there are lines of hydrogen Hα, [NII], [OI], and [SII]. Data on the absolute emission fluxes in the emission lines and in the continuum at the wavelength of λ = 6400 Å are presented. In order to objectively compare the examined galaxies with one another, the values of their luminosities were calculated in absolute units with the distances to these objects taken into account.

Abstract We present the results of the analysis of spectral observations taken a few minutes before, at the time, and in the first minutes after the impact of the DART probe on the asteroid Dimorphos. Our analysis showed signs of Na i, Li i, and K i alkali metal emissions appearing at the time of the impact and for several minutes after it.

One of the main tasks of the situational awareness system in near-Earth space is to determine the type and class of observed objects by analyzing its reflection spectra. This paper proposes a methodology and interpretation of the spectral observational data of geostationary orbit satellites obtained at the Tian Shan Astronomical Observatory (Kazakhstan) from June-December 2021. 8 geostationary objects, the type and design features of which are known were selected as observation targets. The selected satellites are stable (no fast rotation of these objects was detected) and have large reflecting surface areas. An analysis of the obtained reflection spectra shows the dependence on the phase angle of the object. The studies carried out are especially relevant for objects in high orbits, where the only currently available methods of detection and study are ground-based optical photometry and spectroscopy using meter-class telescopes.

На базе многолетних наблюдений представлены результаты спектральных исследований пятнадцати сейфертовских галактик в красной области длин волн. В данном диапазоне расположены линии водорода Hα, [NII], [OI] и [SII]. Представлены данные об абсолютных потоках излучения в эмиссионных линиях и в непрерывном спектре на длине волны λ= 6400Å . Для того, чтобы объективно сравнивать исследуемые галактики друг с другом, получены значения их светимостей в абсолютных единицах, рассчитанные с учетом расстояний до этих объектов. The results of spectral studies of fifteen Seyfert galaxies in the red wavelength region based on the long-term observations, are presented. Some emission lines Hα , [NII], [OI] и [SII] are located in this wavelength range. Data on the absolute fluxes of radiation in emission lines and in continuum at the wavelength of λ= 6400Å are presented. In order to objectively compare the studied galaxies with each other, the values of their luminosities in absolute units were calculated, taking into account the distances to these objects.

Галактики с активными ядрами, и в частности сейфертовские галактики демонстрируют спектральную и фотометрическую переменность на временных интервалах от нескольких часов до нескольких лет. Источниками переменности могут быть газово-пылевые облака в окрестностях черной дыры, и отдельные звезды, периодически проходящие через аккреционный диск. Возможной причиной переменности может быть двойственная природа центральной черной дыры. В Астрофизическом институте им. Фесенкова спектральные наблюдения сейфертовских галактик проводятся на протяжении 50 лет. Для наблюдений используются телескоп АЗТ-8 и 1- метровые рефлекторы, расположенные на высокогорной Обсерватории ТШАО. В данной статье приводятся результаты спектральных и фотометрических исследований галактики NGC 5548. Анализ ее кривой блеска свидетельствует о том, что имеют место практически постоянные колебания значений B V R величин в пределах ~ 0m.3. Кроме того, прослеживается тенденция плавного изменения среднего уровня блеска, в частности, в сторону его повышения. Фрагменты спектрограмм, полученных в разные годы, содержат эмиссионные линии Hα и [NII] и дают возможность оценить изменения уровня континуума, формы профилей и потоков излучения в широкой компоненте водородной линии. Так, наблюдалось значительное увеличение ширины эмиссионных крыльев линии Hα. Кроме того, в 2004 г на коротковолновом крыле Hα появилась дополнительная эмиссионная деталь, которая просуществовала до 2018г. Лучевая скорость эмиссии менялась со временем, вызывая ее видимое смещение вдоль профиля основной линии. Подобные дополнительные эмиссии с переменными лучевыми скоростями могут создаваться эмиссионными объектами, движущимися в поле тяготения центрального тела.

Several powerful outbursts have been observed during many years of observations of the symbiotic object MWC 560. The last active stage began in the autumn of 2018 and continues to the present. Observations of this event began at the Fesenkov Astrophysical Institute at the beginning of 2019. In our previous article we published the results obtained in early 2019. A light curve of the object and emission line profiles are presented; it is noted that a broad absorption band formed in a high velocity collimated jet vanishes. In this article we present the results of further spectral and photometric observations of MWC 560. It is to be noted that in 2021 the brightness of this object is sustained at a high level exceeding that obtained during the previous outbursts. In addition, at the end of 2020 a tendency toward a gradual weakening of the radiative fluxes in the emission lines was remarked. The profiles of all the lines have absorption components shifted to the “blue” by 52±5 km/s. It may be assumed that during this outburst there was partial (or complete) destruction of the accretion disk, so that the source of the high velocity collimated jet vanished. The gradual reduction in the radiative fluxes in the emission lines may be caused by a drop in the power of ionizing radiation.

Бас редактор: МҰТАНОВ Ғалымқайыр Мұтанұлы, техника ғылымдарының докторы, профессор, ҚР ҰҒА академигі, ҚР БҒМ ҒК «Ақпараттық және есептеу технологиялары институты» бас директорының м.а.(Алматы, Қазақстан) Н=5 Редакция алқасы: ҚАЛИМОЛДАЕВ Мақсат Нұрәділұлы (бас редактордың орынбасары), физика-математика ғылымдарының докторы, профессор, ҚР ҰҒА академигі, ҚР БҒМ ҒК «Ақпараттық және есептеу технологиялары институты» бас директорының кеңесшісі, зертхана меңгерушісі (Алматы, Қазақстан) Н=7 БАЙГУНЧЕКОВ Жұмаділ Жаңабайұлы (бас редактордың орынбасары), техника ғылымдарының докторы, профессор, ҚР ҰҒА академигі, Кибернетика және ақпараттық технологиялар институты, Сатпаев университетінің Қолданбалы механика және инженерлік графика кафедрасы, (Алматы, Қазақстан) Н=3 ВОЙЧИК Вальдемар, техника ғылымдарының докторы (физика), Люблин технологиялық университетінің профессоры (Люблин, Польша) H=23 БОШКАЕВ Қуантай Авғазыұлы, Ph.D. Теориялық және ядролық физика кафедрасының доценті, әл-Фараби атындағы Қазақ ұлттық университеті (Алматы

The objects IRAS 06053+1837 and IRAS 22023+5249, are considered as planetary nebula candidates. They have far infrared colors, which are typical to planetary nebulae. Their rather cool stars are surronded by envelopes, in which some low-excitation emission lines are formed. BV photometry of the object IRAS 22023+5249, carried out in 2017-2020, resulted the scatter of B and V values within 0(m).25 and 0(m).10 respectively. Moreover a tendency of the gradual increasing of brightness is revealed. Absolute fluxes and equivalent widths of the H beta, H alpha, [NII], 6548, 6583A and HeI, 6678A emission lines in the spectrum of IRAS 22023+5249 are determined. The strengthening of the emission lines is confirmed. Most likely increasing of an effective temperrature of the star is responsible for observable variations. As a whole spectral and photometric characteristics of the object IRAS 22023+5249 correspond to its status as a low-excitation planetary nebula. For the object IRAS 06053+1837observable data are obtained in 2014-2019. Much larger the scatter of B V R values is observed: 0(m).50, 0(m).15 and 0(m).30 respectively. The only HI emission lines are presented in its spectrum. Asymmetrical profiles of lines have broad wings on the short wavelength side. The evolutionary status of the object is not defined; its characteristics, are more similar to those of the young AeBe Herbig stars.

Seyfert galaxies are much closer than the rest intergalactic objects and therefore the study of them is the most suitable and it gives an information about the physical processes occurring in objects of this type. Spectra of the Seyfert 1 galaxies (Sy1) are represented by a set of forbidden and permitted emission lines. The latter ones consist of a narrow and a broad (up to 10000 km/s) components. The ionization source is an accretion disk. the energy of which is generated due to the accretion of the surrounding matter onto a central supermassive black hole. The region of formation of the broad hydrogen lines (BLR) consists of dense clouds of gas fibers and jets located near the gravitational center and rotating around it at high velocities. The sizes of BLR are about a few tenths of a parsec. The region of formation of narrow forbidden lines and narrow components of hydrogen lines (NLR) is more extended and farther from the center NLR has a lower density of gas. The extension of NLR in the galaxies is determined by the time delay (reverberation). As it turned out, they are from several light days to several light weeks and depend on the luminosity of the active nucleus of the Seyfert galaxy.This paper presents the results of photometric and spectral observations of Seyfert galaxies NGC4151 and NGC 7469. Observations were carried out with the 70-cm telescope AZT-8. Eastern and Western 1-meter telescopes of the Tien Shan Astronomical Observatory of the Fesenkov Astrophysical Institute. The estimations of brightness of NGC4151 (in the B V filters) and NGC7469 (in B V R filters) were obtained from 2013 to 2019. Based on the observational data. the light curves of the studied objects were made. Spectra of the galaxies were obtained in the absolute units. Variations of the level of continuum at two wavelengths lambda=5100 angstrom and 6300 angstrom were studied.

This is a study of spectral and photometric observations of the binary system with an X-ray component V725 Tauri=A0535+262. It consists of a giant star HDE 245770 of spectral class O9.7 and the pulsar A0535+26 with a pulsation period of ~103 s. Active stages of this object, accompanied by “giant” X-ray outbursts, have been observed repeatedly. The last events occurred during 2009-2011. Our studies in 2017-2020 yielded the following data: over the last three years the B and V band brightness of the object has remained at a high level and began to decrease at the end of 2019. Here, beginning in 2016 a gradual increase in the radiative fluxes in the Hβ and Hα emission lines has been observed. At present the equivalent widths of these lines exceed the values recorded during the time of the gigan X-ray outburst of 2011. Previous studies have shown that a similar combination of the characteristics of this object, specifically an increase in emission line fluxes as the brightness decreases. is detected just before the onset of an active stage.

RAS20462 + 3416 belongs to low-mass post-AGB stars with a dense compact envelope, which was formed in the process of the mass loss by the star at the end of the pulsating AGB phase. The spectrum of the object consists of the HI, [NII], [SII] emission lines and of HeI, which is mainly observed in absorbtion. The temperature of the central star corresponds to the value Teff = 19500 +/- 500., the electron density is 10(4) cm(-3). Several episodes of gas ejection from the atmosphere of the central star were recorded. So, in 1993 - 1994, PCygni profiles appeared in the UV and optical spectral lines. The stellar wind velocity was similar to 800 - 990 km/s. The photometric variability of the object was noted by many authors. In particular, quasi- periodic oscillations of brightness in the optical range with an amplitude of 0. (m)1 - 0. (m)2 and a period of similar to 4 days were detected. Rapid fluctuations in brightness can be caused by stellar pulsations and continuing mass loss. In this paper, we present new spectral and photometric data obtained mainly in 2015- 2018. Irregular brightness variations were detected in B, V, and R filters with an amplitude of similar to 0(m). 4. The results of spectral observations indicate a gradual increase in emission line fluxes. Thus, absolute fluxes in H beta, H alpha, [NII] lines increased by about 30 - 40%. In terms of its physical parameters and the nature of the spectrum, the object is similar to a young planetary nebula of low excitation. However, the irregular variability of brightness and fluxes in emission lines, as well as the observed episodes of the matter ejection, indicate that the shell formation has not finishhed. Most likely this object can be considered as a protoplanetary nebula.

The description of an optical complex at the Assy-Turgen Observatory (Kazakhstan) is given. This complex is suited for astrometric and photometric observations of active and passive objects (small-size space debris included) in geostationary orbits. It may be used to reveal, identify, and track potentially hazardous objects (asteroids and comets). The results of test observations are presented.

We present our observations of electromagnetic transients associated with GW170817/GRB 170817A using optical telescopes of Chilescope observatory and Big Scanning Antenna (BSA) of Pushchino Radio Astronomy Observatory at 110 MHz. The Chilescope observatory detected an optical transient of ∼19 m on the third day in the outskirts of the galaxy NGC 4993; we continued observations following its rapid decrease. We put an upper limit of 1.5 × 10 4 Jy on any radio source with a duration of 10–60 s, which may be associated with GW170817/GRB 170817A. The prompt gamma-ray emission consists of two distinctive components—a hard short pulse delayed by ∼2 s with respect to the LIGO signal and softer thermal pulse with T ∼ 10 keV lasting for another ∼2 s. The appearance of a thermal component at the end of the burst is unusual for short GRBs. Both the hard and the soft components do not satisfy the Amati relation, making GRB 170817A distinctively different from other short GRBs. Based on gamma-ray and optical observations, we develop a model for the prompt high-energy emission associated with GRB 170817A. The merger of two neutron stars creates an accretion torus of ∼10 −2 M ⊙ , which supplies the black hole with magnetic flux and confines the Blandford–Znajek-powered jet. We associate the hard prompt spike with the quasispherical breakout of the jet from the disk wind. As the jet plows through the wind with subrelativistic velocity, it creates a radiation-dominated shock that heats the wind material to tens of kiloelectron volts, producing the soft thermal component.

The symbiotic object EG And consists of a giant star (M4III) and a white dwarf. Numerous studies of this object show that its light curve has two minima. There are different hypotheses regarding the source of the secondary minimum, but the problem has not yet been solved. In this paper we present data from photometric and spectral observations of EG And during 2009-2018: B, V, and R magnitudes in the Johnson system and fluxes in the Hβ and Hα emission lines. An analysis of these data showed that the emission fluxes correlate with the orbital phase. The highest fluxes are observed near the secondary minimum. At the same time, emission fluxes are still observed in the primary minimum but attenuated by roughly a factor of 7-10. This indicates that the size of the ionized zone exceeds that of the giant star. On the whole, the light curve for 2009-2018 is consistent with previous photometric data. Rapid (over a few minutes) fluctuations in the brightness of this object are detected in the V and R bands with amplitudes of ~0m.15 and 0m.35, respectively.