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 |
| 4.5-5.3 GHz |
80 K |
FET amplifier |
Dual |
| 6.0-6.7 GHz |
80 K |
HEMT mixer |
Dual |
The computer control system (Pegasus) for the 25 m antenna uses the same operating system as the 20 m telescope. Thus, essentially the same program controls both telescopes.
VLBI back-end
The VLBI back-end consists of digital base band converters (DBBC). Data is recorded on the Mark 5 system or transported directly to the correlator through the internet (e-VLBI). We have 2 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 hybrid digital autocorrelation spectrometer with the following characteristics:
| ACS |
0.05, ..., 6.4, 12.8 MHz |
0.03, ..., 4, 8 kHz |