Carbon lines at limitedly low frequencies

Detection of several absorption recombination radio lines of carbon at 26 MHz in Cas A direction resulted in an attempt to select similar situations (a gas cloud projection on the intense source of the nonthermal radio emission) that are promising for detecting lines of such a kind. Recommendations are given for observations to be made

Linking of the BENSON graph-plotter with the Elektronika-1001 computer

A device, developed by the Institute of Space Research of the Academy of Sciences of the USSR, for linking the Elektronika-100I computer with the BENSON graph-plotter is described. Programs are compiled which provide display of graphic and alphanumeric information. Instructions for their utilization are given

Vlbi research in the ”Radioastron” project: structure of the H2O maser in NGC 2071 IRS 1

В рамках научной программы интерферометра «Радиоастрон» обработаны данные наблюдений мазера Н2О на частоте 22.2280 ГГц в туманности NGC 2071. В наблюдениях принимали участие космический радиотелескоп (КРТ — 10 м) и три радиотелескопа наземной сети: РТ — 32 м (Медичина, Италия), РТ — 32 м (Торунь, Польша) и РТ — 64 м (Калязин, РФ). Получена карта распределения мазерных пятен, где присутствуют 13 пространственных компонентов в интервале VLSR = (4.7—20.5) км/с. Зафиксирован компонент (VLSR = 14.3 км/с), для которого на наземно-космических базах наблюдается корреляция. На основании анализа зависимости функции видности от величины проекций баз предложена двухкомпонентная модель пространственной структуры этого компонента с размерами протяженной и компактной составляющей 4 и 0.06 мс, т. е. 1.56 и 0.023 a. e. соответственно.Within the Radioastron interferometer scientific program, observational data of the H2O maser at a frequency of 22.2280 GHz in the NGC 2071 nebula were processed. A space radio telescope (SRT — 10 m) and three radio telescopes of the ground network: RT — 32 m (Medicina, Italy), RT — 32 m (Torun, Poland) and RT —64 m (Kalyazin, RF) took part in the observations. A map of the maser spot distribution has been obtained, where there are 13 spatial components with VLSR in the range 4.7 — 20.5 km/s. Correlation is observed on ground-space baselines for the component on VLSR = 14.3 km/s. Based on the visibility function dependence analysis from the baseline projection values, there was proposed a twocomponent model of this component spatial structure with the dimensions of the extended and compact constituent of 4 and 0.06 msec, i.e. 1.56 and 0.023 au, respectively

Recent updates on the Maser Monitoring Organisation

The Maser Monitoring Organisation (M2O) is a research community of telescope operators, astronomy researchers and maser theoreticians pursuing a joint goal of reaching a deeper understanding of maser emission and exploring its variety of uses as tracers of astrophysical events. These proceedings detail the origin, motivations and current status of the M2O, as was introduced at the 2021 EVN symposium