Related Results and Activities in Western Pacific VLBI Network

Astronomy and Astrophysics – Astronomy

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Antennas, Low Noise, Receivers, Frequency Ranges, Very Long Base Interferometry, Extragalactic Radio Sources, Sensitivity, Radio Observation, Radio Astronomy, Pulsars, Parabolic Reflectors, Panels, Millimeter Waves, Masers, Continuums, Astronomy

Scientific paper

CRL's 34 m antenna at Kashima which is equiped with low noise receivers which operate from 1.5 GHz to 43 GHz covers most of the radio astronomical bands in this frequency range. The antenna has extremely accurate surface panels and is highly efficient even on the millimeter wavelength. Many kinds of single dish observations and radio astronomical VLBI observations have been performed. Domestic VLBI experiments between the Kashima 34 m Nobeyama 45 m antennas are called KNIFE and are highly sensitive on the short centimeter and millimeter wavelengths. VLBI experiments between the Usuda 64 m and the Kashima 34 m antenna called UKAI and are highly sensitive on the 2 GHz and 8 GHz bands. This paper reviews published work on radio astronomy by using data obtained from the 34 m antenna at Kashima. The results of observations of astronomical masers, extragalactic radio continuum sources, pulsars, and interplanetary scintillation (IPS ) observation are presented.

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