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Metsähovi observatory, Finland. Small log-per attached to the rim of a 37 GHz parabolic dish tracking the sun.
Observations 170 MHz - 870 MHz in linear, horizontal polarization.
File-ID = MRO
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Ondrejov observatory, Czech
Republic. Original "Würzburg Riese" (German Radar dish of World War II)
7m dish with linear polarized feed covering 150 MHz - 870 MHz
File-ID = OSRA
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Bleien observatory Switzerland.
7m parabolic dish tracking the sun. Feed: log-per 100 MHz - 4 GHz,
currently observing 170 MHz - 870 MHz in two polarizations LHCP and
RHCP.
File-ID = BLEN7M
File-ID = BLENSW
File-ID = PHOENIX2
File-ID = PHOENIX3
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Station Humain of Royal Observatory of Belgium.
Log-per feed CLP-5130 attached to the rim of an old parabolic dish. The
dish is tracking the sun. Linear polarization 45 MHz - 870 MHz
File-ID = ROB
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Birr castle, Ireland. Antenna
operated by TCD. Antenna is tracking the sun in linear horizontal
polarization. Observations in two bands, 45 MHz - 870 MHz and 20 MHz -
90 MHz
File-ID = BIR
File-ID = BIRO
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Anchorage, Alaska. Log-per hoizontally polarized, tracking the sun only in azimuth. Observing range 45 MHz - 870 MHz
File-ID = ALASKA
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KASI
Daejeon, South Korea. Large log-per hoizontal polarization tracking the
sun in azimuth and elevation. Observations 45 MHz - 870 MHz.
File-ID = KASI
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RCAG
Khurel Togoot near Ulaan Baatar, Mongolia. Log-per horizontally
polarized in fixed sky position (sun-rise). Observations 175 MHz
- 450 MHz.
File-ID = RCAG
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ISTP
Badary near Irkutsk, Russian Federation. Log-per mounted on the upper
rim of a dish. Polarization rotates while the sun is tracked during the
day. Observations 45 MHz - 450 MHz
File-ID = SSRT
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Station
'Orbita' near Almaty, Kazakhstan. The log-per made of titanium is
mounted at the lower rim of the 12m dish. Observations 45 MHz - 870 MHz
in linear horizontal polarization.
File-ID = ALMATY
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IIA in Gauribidanur near Bangalore, India. Linear polarized log-per pointing to zenith.Observations 45 MHz - 410 MHz.
File-ID = GAURI
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TIFR, Ooty Tamil Nadu, India.
Linear polarized log-per pointing to zenith.Observations 45 MHz - 450 MHz.
File-ID = OOTY
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UoM, Poste de Flacq Mauritius. Linear polarized log-per pointing to zenith. Observations 45 MHz - 870 MHz
File-ID = MRT
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UNAM Mexico. Linear horizontally polarized log-per observing 170 MHz - 450 MHz.
No sun-tracker, fixed in sky-position.
File-ID = UNAM
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Hans Michlmayr Perth, Australia. Linear log-per horizontally polarized tracking the sun. Observations 45 MHz - 870 MHz.
File-ID = PERTH
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CINESPA Costa rica. Unknown feed on parabolic dish in fixed sky position. Status unknown
File-ID = CINESPA
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INPE Cachoeira Paulista, Brazil. Two orthogonal linear polarized log-per in fixed sky-position.
Status currently unknown.
File-ID = INPE
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SWMC Space Weather Monitoring Center Helwan University,
Egypt
Logarithmic-
periodic
antenna 6m x 6m
File-ID = SWMC |
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Radio Astronomy Laboratory of CrAO, RT-22
Katsively, Yalta
Crimea, Ukraine
File-ID = KRIM
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University of Pune, Institute for electronic science.
File-ID=PUNE
longitude=73.9°
latitude=18.5°
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SCO
Slovak Central Observatory Hurbanovo, Slovakia
latitude=47.5°N
longitude=18.0°E
Antenna:
CLP-5130 Create
File-ID=
HURBANOVO
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Trieste Astronomical Observatory
via G.B. Tiepolo 11
I 34131 Trieste
Location: Basovizza (Trieste), Italy
Latitude: 45° 38´ 37´´ N
Longitude: 13° 52´ 34´´ E
Altitude: 400 m
Telescope: Single steerable paraboloid
Diameter: 10 m
Area: 70 m2
Height: 16.4 m
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University of Nairobi, Kenya
File-ID=KENYA
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Callisto project
in Malaysia is hosted by Malaysian National Space Agency (ANGKASA)
and there are three (3) universities that collaborate in this project: (1) University
of Malaya, (2) University Kebangsaan Malaysia and (3) Universiti Teknologi
MARA.
File-ID=MALAYSIA
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| Ahmedabad, India in preparation, spectrometer delivered
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Sri Lanka in preparation, spectrometer delivered
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La Réunion in planning
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Idle status: Melbourne, Hawaii, Mannheim
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Possible candiates: Ethiopia, Scotland, Ecuador, Peru, Turkey, Spain, Nigeria
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IDL map
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Cumulative coverage of all
Callisto spectrometer locations (left), assuming all instruments are working
and all antennas are tracking the sun. In fact both is not the case.
Therfore it makes sense to have some redundancy. We still have small gaps (white areas left) in winter season between 16 UT
and 20 UT and also around 1 UT again in winter-season (related to
northern side of the world).
Triangles: data o.k.
Stars: no data yet
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