Reference stars compiled catalogue around extragalactic radio sources. Reduction techniques and the first results

Some differential reference stars catalogues around extragalactic radio sources obtained from photographic and CCD-observations at different observatories are considered. Compiled catalogue of star positions in fields of 30 ×30 is intended for reduction of ERS optical observations using the telescopes equipped with CCD-cameras. Photographic observations of the fields around 74 ERS were made at the Pulkovo Observatory, around 115 ERS – at the AO KNU, around 188 ERS – at the AIRA in Bucharest. The 208 fields around ERS at NAO using the telescope equipped with a CCD-camera were obtained. The first results of the creation of uniform compiled catalogue are given. Astrometric positions for stars brighter than 16 magnitude in more than 20 fields around ERS are presented. A comparison of our results with those of other authors is made

Optical counterpart positions of extragalactic radio sources and connecting optical and radio reference frames

We discuss the results of an investigation of astrometric positions of extragalactic radio sources from a list for the International Celestial Reference Frame. About 300 fields around extragalactic radio sources were observed during the years 2000-2003. The observations were performed mainly using two telescopes equipped with CCD cameras at TUG, Turkey (Russian-Turkish Telescope - RTT150) and at YAO (1 m telescope), (Kunming, China). The mean accuracies of the measured positions are 38 mas in right ascension and 35 mas in declination. A comparison between the measured optical positions determined using the UCAC2 catalog and the radio positions from the current ICRF shows that the overall optical-minus- radio offsets are -4 and +15 mas for right ascension and declination, respectively. The formal internal errors of these mean offsets are 4 mas. The results of optical positions with respect to the reference catalogue 2MASS are also given. A search for a relation between optical and radio reference frames indicates that the orientation angles are near zero within their accuracy of about 5 mas. The link accuracy becomes 3 mas when our observations are combined with other studies. © ESO, 2010

Results of joint project on linking optical-radio reference frames

Results of international co-operation between observatories from China, Russia, Turkey, and Ukraine on refinement of linking optical and radio reference frames are discussed. About 300 fields around extragalactic radio sources in the selected fields of extragalactic radio sources from −40 to +70 degrees in declination were observed with CCD ground-based telescopes. The catalogue of optical positions of more than 200 ERS with average accuracy 30 mas in ICRF by using of secondary reference stars from the UCAC2 and USNO-B1.0 catalogues was obtained as a result of this cooperation. The intermediate internal estimation of link between optical and radio reference frames was shown the angle values near zero within an accuracy of about 6 mas by using of secondary reference stars from UCAC2. A comparison of presented results with those of other investigations was made

Results of observations of asteroids at the Russian–Turkish RTT-150 telescope from 2004–2013

© 2015, Allerton Press, Inc. We report the results of analysis of the data volume containing 13834 topocentric positions of 231 asteroids obtained from observations at the Russian–Turkish RTT-150 telescope (TÜBITAK (Scientific and Technological Research Council of Turkey), Turkey) in 2004–2013. The positions of asteroids were calculated with the differential reduction method in the ICRS system with the use of the reference catalogs of the UCAC series. The observational program covered the main-belt asteroids closely encountering the other asteroids and the near-Earth asteroids (NEA). For the main belt asteroids, the mean-square error of one position was 84 and 68 mas in right ascension and declination, respectively, while it was 160 and 120 mas, respectively, for NEAs. The obtained volume of the asteroid positions widens the arc of groundbased observations of these bodies, which is important for evaluating their orbital elements with a higher accuracy. Moreover, observations of the main-belt asteroids in the periods of close encounters yield valuable material to solve the problem on accurate estimation of the masses of asteroids with a dynamic method. It has been shown that the supplementing of the input dataset with the here-reported observational volume decreases the error in the estimates of the perturbing asteroid mass and the orbital parameters of perturbed bodies

The astrometric Gaia-FUN-SSO observation campaign of 99 942 Apophis

Astrometric observations performed by the Gaia Follow-Up Network for Solar System Objects (Gaia-FUN-SSO) play a key role in ensuring that moving objects first detected by ESA's Gaia mission remain recoverable after their discovery. An observation campaign on the potentially hazardous asteroid (99 942) Apophis was conducted during the asteroid's latest period of visibility, from 12/21/2012 to 5/2/2013, to test the coordination and evaluate the overall performance of the Gaia-FUN-SSO . The 2732 high quality astrometric observations acquired during the Gaia-FUN-SSO campaign were reduced with the Platform for Reduction of Astronomical Images Automatically (PRAIA), using the USNO CCD Astrograph Catalogue 4 (UCAC4) as a reference. The astrometric reduction process and the precision of the newly obtained measurements are discussed. We compare the residuals of astrometric observations that we obtained using this reduction process to data sets that were individually reduced by observers and accepted by the Minor Planet Center. We obtained 2103 previously unpublished astrometric positions and provide these to the scientific community. Using these data we show that our reduction of this astrometric campaign with a reliable stellar catalog substantially improves the quality of the astrometric results. We present evidence that the new data will help to reduce the orbit uncertainty of Apophis during its close approach in 2029. We show that uncertainties due to geolocations of observing stations, as well as rounding of astrometric data can introduce an unnecessary degradation in the quality of the resulting astrometric positions. Finally, we discuss the impact of our campaign reduction on the recovery process of newly discovered asteroids.Comment: Accepted for publication in A&

Методика измерений массовой доли соевого ингибитора трипсина: особенности разработки и аттестации

   Modern industrialization increases the requirements for the accuracy of identifying allergens, especially those that have a negative impact – soy trypsin inhibitor (STI). Correct determination of the presence of STI in food products containing soybeans is key for product safety control and labeling. The authors set a goal to develop and certify a method for measuring the mass fraction of STI using an enzyme-linked immunosorbent assay – a technique that may increase the specificity of the method and avoid false-negative results.   The object of research was a method for analyzing food allergens – an enzyme-linked immunosorbent assay carried out with a set of reagents produced by XEMA LLC. In the process of developing the measurement method, the main methodological factors influencing the accuracy of the measurement results were optimized: sample weight, time of its extraction, time and speed of sample centrifugation, ratio of supernatant liquid to ELISA buffer, incubation temperature, interaction time of the allergen-antibody complex with the coloring agent, the wavelength for measuring absorbance, and the maximum time for measuring absorbance after introduction of the stop reagent.   The developed method was tested during an interlaboratory experiment with the participation of 5 laboratories. Metrological characteristics were established in accordance with RMG 61–2010. The proposed method was certified in accordance with the requirements of GOST R8.563-2009, No. 102–FZ. The method has a wide range of quantitative determination of the mass fraction of STI from 0.5 to 25.0 μg/kg (ppb) with a detection limit of 0.1 μg/kg (ppb) and a relative error of 40 %. Based on the results of the research, the Federal Information Fund for Ensuring the Uniformity of Measurements (FIF) registered a certified method for identifying and quantifying the content of non-infectious food allergens of plant protein origin in samples of all types of food products and objects related to the requirements for food products, swabs taken from working surfaces during production control using reagent kits for an enzyme-linked immunosorbent assay produced by XEMA LLC No. FR.1.31.2022.43884. The method is intended for use in testing laboratories involved in monitoring the quality and safety of manufactured products; it can be used to confirm product compliance with the mandatory requirements established in the Technical Regulations of the Customs Union TR CU022/2012.   Современная индустриализация повышает требования к точности определения аллергенов, особенно в отношении оказывающих негативное воздействие, среди них – соевый ингибитор трипсина (СИТ). Корректное определение наличия СИТ в пищевых продуктах, содержащих соевые бобы, является ключевым для контроля безопасности и маркировки продукции. Сложилась общепринятая практика определять аллергены сои количественно с помощью аналитических методов анализа. Авторы данной статьи поставили цель разработать и аттестовать методику измерений массовой доли СИТ методом иммуноферментного анализа – методику, способную повысить специфичность метода и избежать ложноотрицательных результатов ее применения.   Объектом исследования стал метод анализа пищевых аллергенов – иммуноферментный анализ, реализованный набором реагентов производства ООО «ХЕМА».   В процессе разработки методики измерений оптимизированы основные методические факторы, влияющие на точность результатов измерений: масса пробы, время ее экстракции, время и скорость центрифугирования пробы, соотношение надосадочной жидкости и ИФА-буфера, температура инкубации, время взаимодействия комплекса антитело-аллерген с окрашивающим агентом, длина волны для измерения оптической плотности и максимальное время для измерения оптической плотности после введения стоп-реагента. Разработанная методика апробирована в ходе межлабораторного эксперимента с участием 5 лабораторий. Метрологические характеристики установлены в соответствии с РМГ 61–2010. Предлагаемый метод был аттестован в соответствии с требованиями ГОСТ Р 8.563-2009, № 102–ФЗ. Метод имеет широкий диапазон количественного определения массовой доли СИТ от 0,5 до 25,0 мкг/кг (ppb) с пределом обнаружения 0,1 мкг/кг (ppb) и относительной погрешностью 40 %. По результатам проведенного исследования в Федеральном информационном фонде по обеспечению единства измерений (ФИФ) зарегистрирована аттестованная методика идентификации и количественного определения содержания неинфекционных пищевых аллергенов белкового растительного происхождения в пробах всех видов пищевых продуктов и объектов, связанных с требованиями к пищевой продукции, смывов, отбираемых с рабочих поверхностей при проведении производственного контроля, с помощью наборов реагентов для иммуноферментного анализа производства ООО «ХЕМА» № ФР.1.31.2022.43884. Методика предназначена для применения в испытательных лабораториях, занимающихся контролем качества и безопасности выпускаемой продукции, может быть использована для подтверждения соответствия продукции обязательным требованиям, установленным в Техническом регламенте Таможенного союза ТР ТС 022/2012

The astrometric Gaia-FUN-SSO observation campaign of 99942 Apophis

© 2015 ESO. Aims. Astrometric observations performed by the Gaia Follow-Up Network for Solar System Objects (Gaia-FUN-SSO) play a key role in ensuring that moving objects first detected by ESA's Gaia mission remain recoverable after their discovery. An observation campaign on the potentially hazardous asteroid (99 942) Apophis was conducted during the asteroid's latest period of visibility, from 12/21/2012 to 5/2/2013, to test the coordination and evaluate the overall performance of the Gaia-FUN-SSO. Methods. The 2732 high quality astrometric observations acquired during the Gaia-FUN-SSO campaign were reduced with the Platform for Reduction of Astronomical Images Automatically (PRAIA), using the USNO CCD Astrograph Catalogue 4 (UCAC4) as a reference. The astrometric reduction process and the precision of the newly obtained measurements are discussed. We compare the residuals of astrometric observations that we obtained using this reduction process to data sets that were individually reduced by observers and accepted by the Minor Planet Center. Results. We obtained 2103 previously unpublished astrometric positions and provide these to the scientific community. Using these data we show that our reduction of this astrometric campaign with a reliable stellar catalog substantially improves the quality of the astrometric results. We present evidence that the new data will help to reduce the orbit uncertainty of Apophis during its close approach in 2029. We show that uncertainties due to geolocations of observing stations, as well as rounding of astrometric data can introduce an unnecessary degradation in the quality of the resulting astrometric positions. Finally, we discuss the impact of our campaign reduction on the recovery process of newly discovered asteroids

ANALYSIS OF ASTEROID’S OBSERVATIONS IN OPEN PHOTOMETRIC DATABASES

Today there are several open photometric databases containing important information for the study of the physical properties of asteroids. These databases are based on the results of various measurements of the different sets of objects. The study of statistical correlations between the various databases could significantly expand the list of asteroids with known physical parameters. We present the results of the comparative analysis of the determination of the albedo, diameters and absolute magnitudes of asteroids of five open sources (AKARI, IRAS, NEOWISE, HORIZONS and Pan-STARRS1). The infrared survey WISE (relatively to asteroids is NEOWISE project) and photometric survey Pan-STARRS1 are the widest databases of the absolute magnitudes and the albedo of asteroids providing information about 139356 and 248457 objects respectively. These surveys contain 73301 common asteroids. The obtained statistical relationships between the databases based on a common set of asteroids are presented.  

MODERN CCD OBSERVATIONS OF SELECTED MINOR PLANETS FOR THE CONNECTION OF DYNAMIC AND KINEMATIC COORDINATE SYSTEMS

One of the methods of determining the orientation parameters of the dynamic and kinematic coordinate systems is to use of long-term series of ground-based observations of selected asteroids. For achievement of the best accuracy of the link parameters the high precision and uniformly covering the asteroids orbit observations are necessary. The analysis of the available observations of selected asteroids was made with usage MPC database. The value of the true anomaly at the moment of observation was selected as parameter of orbit covering. It is shown that there are orbital segments without precise observations. This was taken into account when forming the observational list for the telescope KT-50 (Mobitel complex). 1596 positions of 50 asteroid have been obtained during 2014- 2016. The comparison of the calculated positions with ephemeris obtained by on-line service HORIZONS was made. The RMS errors of the differences (O-C) were about 0.1 arcsec for both coordinates. The comparison of the obtained results with observations of the some ground based observatories and Hipparcos satellite shows high accuracy and uniformity of Nikolaev asteroid observations.

THE RESULTS OF OBSERVATIONS OF MUTUAL PHENOMENA OF THE GALILEAN SATELLITES OF JUPITER IN 2009 AND 2015 IN NIKOLAEV ASTRONOMICAL OBSERVATORY

The Earth and Jupiter once in 6 years have simultaneous passage of the ecliptic plane due to their orbital movement around the Sun. This makes it possible to observe the mutual occultations and eclipses in the Galilean satellites of Jupiter. We took part in the observational campaigns of the mutual phenomena in 2009 and 2014-15. The observations were made with a B/W CCD camera WAT-902H at the telescope MCT (D = 0.115 m, F = 2.0 m) of the Nikolaev Astronomical Observatory. The light curves of mutual phenomena in the satellites of Jupiter were obtained as a result of processing photometric observations. The exact moments of maximum phases and the amplitudes of the light variation have been determined from the analysis of the light curves. The data sets for the light curves have been sent in the IMCCE (Institute de Mecanique et de calcul des ephemerides, France) that coordinates the PHEMU campaigns