IV. Related Results of Recent Activities in CRL

IV-4. Radio Astronomy with the Kashima 34m Antenna

by Hiroshi TAKABA, Takahiro IWATA, Michito IMAE, Noriyuki KURIHARA, Noriyuki KAWAGUCHI, Yuji SUGIMOTO, Taizo YOSHINO, Fujinobu TAKA- HASHI, Hitoshi KIUCHI, Shin'ichi HAMA, Yukio TAKAHASHI, Yasuhiro KOYAMA, Yuko HANADO, Mamoru SEKIDO, Jun'ichi NAKAJIMA, Tetsuro KONDO, Jun AMAGAI, and Akihiro KANEKO

Abstract

CRL's 34 m antenna at Kashima which is equipped 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 and the 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 antennas were 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 34m antenna at Kashima. The results of observations of astronomical masers, extragalactic radio continuum sources, pulsars, and interplanetary scintillation (IPS) observations are presented.

For request of pre-prints, please send e-mail to the main author (takaba(AT)nict.go.jp). Last Update: Feb. 21, 1995