The Pushchino radio observatory operates three radio telescopes, as briefly described below:
RT-22 LPI Radio Telescope – is a parabolic reflector with its main dish of 22m in diameter. Accuracy of the main dish surface provides telescope’s effective operation up to mm wavelengths. The telescope’s receivers have the latest cooled low noise preamplifiers. The major scientific programs deal with star formation regions research by observations of atomic and molecular radio lines, and investigations of compact radio sources structures using interferometer technique with the resolution of hundredth and thousandth part of arcsecond.
Wide-Band Cross-type Radio Telescope DKR-1000 – is a meridian instrument consisting of two arms: East-West and North-South. Each arm represents a parabolic cylinder with the width of 40m and is 1km long. Wide-band feeds allowing to observe in the range from 2.5 up to 10 meter band are situated along the focal line of both arms. The DKR-1000 radio telescope provides unique possibilities for pulsar investigations, observations of spectral radio lines corresponding to transitions between levels with principal quantum numbers near 750(!), and studies of the radio sources flux density variations.
BSA LPI Radio Telescope – is a phased array comprising 16384 dipoles and covering an area of 18 acres. Its operating wavelength is 3m, and the telescope is world’s most sensitive instrument in the range. BSA LPI is an indispensable one for the whole series dynamic processes in the near-Sun and interplanetary plasma, studies of pulsar radio emission, and analysis of the compact radio sources structure in the meter range of wavelengths.
|geographic longitude:||37°37′ 53″|
|geographic latitude:||54°49′ 20″|
|altitude above sea level:||200 m|
|diameter telescope:||22 m|
|cross antenna radio telescope:||1000 meter length; collecting area: 2×8000 m2|
|BCA transit array:||collecting area: 25000 x sin(el) m2 with el = elevation in (o)|
|small transit array:||1344 dipoles|
Available observing mode: single dish, Very Long Baseline Interferometry (VLBI).
Frequencies used currently:
|Frequency band||Observing mode|
|37.0 – 45.00 MHz||single dish|
|57.0 – 65 MHz||single dish|
|109 – 113 MHz||single dish|
|400 – 440 MHz||single dish|
|8.39 – 8.41 GHz||single dish, VLBI|
|14.96 – 15.04 GHz||single dish, VLBI|
|18 – 26 GHz||single dish, VLBI|
|34 – 38 GHz||single dish, VLBI|
Pulsar physics; Pulsar astrometry and Pulsar time scale; Solar super corona, interplanetary plasma, solar wind (solar-terrestrial connections); Physics of interstellar plasma (via observations of pulsars and spectral radio lines); Extragalactic radio sources; Searching of the transient radio sources and the bursts-like events (radio counterpart of gamma-ray bursts, detection of SHE cosmic rays, etc.); RADIOASTRON project