Receivers
The essential feature in radio astronomy receiver is the need for very sensitive detection of weak signals. At the same time the receiver need to be very stable to enable sufficiently long integration time of the weak signal. In VLBI receivers an important feature is the phase stability because the technique relies on the phase coherence of the several signal acquisitions. Better sensitivity can be achieved by using modern technology components such as HEMT based low noise amplifiers, cryogenic cooling, and computer aided simulation and design.
Status
Currently Metsähovi Radio Observatory operates the following receivers. The block diagram and more information is available on some receivers.
The essential feature in radio astronomy receiver is the need for very sensitive detection of weak signals. At the same time the receiver need to be very stable to enable sufficiently long integration time of the weak signal. In VLBI receivers an important feature is the phase stability because the technique relies on the phase coherence of the several signal acquisitions. Better sensitivity can be achieved by using modern technology components such as HEMT based low noise amplifiers, cryogenic cooling, and computer aided simulation and design.
Status
Currently Metsähovi Radio Observatory operates the following receivers. The block diagram and more information is available on some receivers.
| Receiver | Signal freq. [GHz] | IF freq. [GHz] |
Polarization | Trec [K] | Status |
| 22 GHz Continuum | 21.0-22.0/22.4-23.4 | 0.2-1.2 | Linear | 270 |  |
| 22 GHz VLBI | 21.980-22.480 | 0.5-1.0 | LCP/RCP | 60 | |
| 37 GHz Continuum/Solar | 35.3-36.3/37.3-38.3 | 0.5-1.5 | Linear | 280 | |
| Geo-VLBI |
8.15-8.65 2.21-2.35 |
0.5-0.98 0.68-0.82 |
RCP | 100 | |
| 43 GHz VLBI | 40-45 | 8.5-11.5/0.5-1.0 | LCP/RCP | 100 |  |
|
80-115 GHz Spectral Line |
80-115 | 1.0-1.6 | Linear | 150 | |
| 150 GHz VLBI | 129-175 | 3.7-4.2/0.5-1.0 | LCP/RCP | TBD |  |
| 84-98 GHz VLBI | 84-98 | TBD | LCP/RCP | TBD | |
| MCA | 4-15 | ? | ? | ? |