Millimeter waves are part of radio waves having
frequency 30-300 GHz and wavelength 10-1 mm. The importance of
these waves has increased during recent years and new applications
have been developed in telecommunications, measurement technology,
medical electronics, industrial sensors, remote sensing, and radio
astronomy. The essential feature in these applications is need for
very sensitive detection of weak signals. This means that the
sensitivity of the receiver is the most important parameter of the
receiver. Better sensitivity can be achieved by using modern
technology components and design such as HEMTs, low noise
amplifiers, cryogenic cooling, and computer aided design.
At radio laboratory of Helsinki University of Technology (HUT)
the study of sensitive receivers and microwave components started
in the decade of 1960. The study has included e.g. parametric
amplifiers, Josephson junctions, Schottky mixers, FET and HEMT
low noise amplifiers, frequency multipliers, Gunn oscillators,
and phase locked local oscillators. A special feature in
improving the sensitivity of receiving systems has been cooling
of the active components by using cryogenic system with liquid
nitrogen or helium.
Figure 1: 2 mm receiver installed to the antenna of
Metsähovi Radio Observatory.
At Metsähovi Radio Observatory this study has continued.
Receiver system design, millimetre wave components, low frequency
parts, reliability, and electromagnetic interference problems
have been studied in order to build better and better receivers
for Metsähovi.
During last few years the construction of the following
receiving systems has been completed:
- VLBA-terminal for very long baseline interferometry including
formatter, baseband converters and read/write electronics,
- two channel 22 GHz helium cooled receiver for line
VLBI-measurements,
- Read/Write electronics for Mark IV upgrading: one unit for
Metsähovi, 5 units for different EVN stations in Europe, 7
units for JPL to be used in DSN stations, one unit for
Ny-Ålesund, Norway
- 37 GHz polarization receiver for solar research
- 43 GHz dual channel, cooled receiver for mm-VLBI
- 147 GHz cryogenic SIS receiver as a loan from IRAM, Spain,
for 2 mm VLBI observations
- 3 and 2 mm VLBI SIS receiver designed at Institute of Applied
Physics, Russian Academy of Sciences, Nizhny Novgorod, Russia
- 8.4 GHz and 2.28 GHz Geo-VLBI receiver
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Receivers at Metsähovi
Receiver |
Signal Freq. [GHz] |
IF freq. [GHz] |
Polarization |
Trec |
22 GHz Continuum |
21.0-22.0 / 22.4-23.4 |
0.2-1.2 |
Linear |
300 K |
22 GHz VLBI |
21.982-22.482 |
0.5-1.0 |
LCP / RCP |
60 K |
37 GHz Continuum/Solar |
35.3-36.3 / 37.3-38.3 |
0.5-1.5 |
Linear |
280 K |
37 GHz Solar |
37.0 |
0.25-1.0 |
4 Stokes |
420 K |
43 GHz VLBI |
40.0-45.0 |
8.5-11.5 / 0.5-1.0 |
LCP / RCP |
65 K |
80-115 GHz Spectral Line |
80-115 |
1.0-1.6 |
Linear |
150 K |
147 GHz VLBI |
147 |
3.7-4.2 / 0.5-1.0 |
LCP / RCP |
145 K |
3 and 2 mm VLBI |
84-115, 129-175 |
3.7-4.2 / 0.5-1.0 |
LCP / RCP |
100 K, 150 K |
Geo-VLBI |
8.15-8.65, 2.21-2.35 |
0.5-0.98, 0.68-0.82 |
RCP |
94 K,
102 K |
Receiver |
Receiver construction |
22 GHz Continuum |
Dual horn, Dicke-switched receiver at room temperature,
free running Gunn-oscillator as local oscillator, accurate
temperature control of microwave and IF-components, very
reliable and stable receiver |
22 GHz VLBI |
Cryogenic single sideband receiver, phase locked FET DRO
with frequency doubler as local oscillator (LO) |
37 GHz Continuum/Solar |
Dual horn, Dicke-switched receiver with a HEMT
preamplifier at room temperature , remote controllable
waveguide switch for selection between continuum or solar
observations, high dynamic range (log IF-amplifier) |
37 GHz Solar |
A mixer/ IF-preamplifier receiver with waveguide
ortho-mode transducer (OMT) and a correlation unit |
43 GHz VLBI |
Cooled dual channel receiver with HEMT preamplifiers and
a WR-22 polarizer ; two spectrally pure YIG- oscillators as
LO´s , digital phase locking with good long term phase
stability |
80-115 GHz Spectral Line |
Cryogenic beam-lead Schottky diode mixer receiver ,
widely tunable Gunn-oscillator as LO, analog phase locking
with high harmonic number (17-22) |
147 GHz VLBI |
A 2 mm SIS Receiver as a loan from Instituto de
RadioAstronomia Milimetrica (IRAM), Spain. Waveguide SIS
mixer with tuning backshort and corrugated feed horn in a 3
K cryostat. InP Gunn oscillator followed by a Schottky
diode frequency doubler as a LO. Phase locking with 16th
harmonic of a Rohde Schwarz synthesizer giving reference
frequency of 4.7125 GHz. The original IF band at 3.7-4.2
GHz is transferred with a second down converter to the
standard VLBI band of 0.5-1.0 GHz. Quasi-optical feed
system in front of the horn consists of 3 plane mirrors and
2 elliptical mirrors together with rotating chopper
beam-switch. This receiver has been disassembled and all
parts sent back to IRAM. |
3 and 2 mm VLBI |
A new cryogenic SIS receiver designed at IAP, Russia. SIS
mixer mounts inside the dewar are cooled down to 4.5 K with
a helium closed cycle refrigerator. Two mixers for 3 mm
allow the possibility for simultaneous circular
dual-polarization measurements. The local oscillator source
for the 3 mm band is an InP Gunn-oscillator and for 2 mm a
wideband tunable BWO is exploited. For phase locking the
Rohde & Schwarz synthesizer is used with a harmonic mixer
to create the PLL IF signal at 275 MHz. This mixing product
is divided by 11 and compared with the 5 MHz frequency
standard (multiplied by 5) for PLL feedback. Cryogenic HEMT
IF amplifiers with center frequency at 4 GHz and bandwidth
of 1 GHz followed by amplifiers at room temperature are
used for continuum output. With the second LO at 3.2 GHz
this IF band is transferred to the standard VLBI band of
0.5 - 1.0 GHz. |
Geo-VLBI |
Geodetic Observatory has ordered a new receiver from the
TTI Norte, Santander, Spain which is used at Metsähovi
for geodetic VLBI observations. The receiver operates at
two different bands i.e. 8150-8650 MHz and 2210-2350 MHz.
The receiver front end consists of cryogenic LNA's and a
bulky feed system and polarizers at room temperature. This
receiver needs a large subreflector (with diameter of 1.7
m) which is placed in the front of the original one,
therefore simultaneous observations with mm-receivers are
not possible. |
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