The 25 m diameter polar mounted decimetre-wave telescope was built in 1963. It is used mainly for astronomical VLBI observations of, e.g., star forming regions, radio stars, and active galactic nuclei, but occasionally as a single dish for, e.g., observations of interstellar molecules.
Position
Latitude: 57° 23' 35.0456" N
Longitude: 11° 55' 03.9685" E
Elevation: 18.01 meters
Receivers
The telescope is equipped with the following receivers:
| 0.8 - 1.2 GHz |
100 K |
HEMT amplifier |
Dual |
| 1.2 - 1.8 GHz |
30 K |
HEMT amplifier |
Dual |
| 4.5 - 6.7 GHz |
50 K |
HEMT amplifier |
Dual |
| 6.0 - 6.7 GHz |
80 K |
HEMT mixer |
Dual |
The telescope control system Bifrost is used for both the 25 m telescope and the 20 m telescope.
The BIFROST User's Handbook explains how to use it: Bifrost_Users_Handbook_12jun2020.pdf
VLBI back-end
The VLBI back-end consists of digital base band converters (DBBC). Data is recorded on the Flexbuff system or transported directly to the correlator through the internet (e-VLBI). We have two parallell VLBI systems and can observe with the 20 m and 25 m telescope in VLBI-mode simultaneously.
Spectral line back-end
The back-end for spectral line observations is a 8192 channel FFT based spectrometer with the following characteristics:
| HRF |
50, 25, 10 MHz |
6.103, 3.058, 1.221 kHz |