Data Access
This dataset contains solar dynamic spectrogram FITS files of the CALLISTO spectrometer data from the e-Callisto network of stations. The FITS file is composed of four parts: the ASCII-format header, the binary spectrum and two BIN tables. One table is for the time axis and the other for the frequency axis. FITSvfiles contain the keyword BUNIT in the primary header. If the BUNIT = 'SFU', then data are calibrated. If the BUNIT = 'digits', then data are raw data without any calibration. The naming convention for each file is of the form: STATION_YYYYMMDD_HHMMSS_CODE.fit.gz where STATION is a variable length station name and following the Date (YYYYMMDD) and UT time (HHMMSS) CODE is a two digit number that is an individual description of the front-end of the system. From the website http://e-callisto.org - The CALLISTO spectrometer is a programmable heterodyne receiver built in the framework of IHY2007 and ISWI by former Radio and Plasma Physics Group (PI Christian Monstein) at ETH Zurich, Switzerland. The main applications are observation of solar radio bursts and rfi-monitoring for astronomical science, education and outreach. The instrument natively operates between 45 and 870 MHz using a modern, commercially available broadband cable-TV tuner CD1316 having a frequency resolution of 62.5 KHz. The data obtained from CALLISTO are FIT-files with up to 400 frequencies per sweep. The data are transferred via a RS-232 cable to a computer and saved locally. Time resolution is 0.25 sec at 200 channels per spectrum (800 pixels per second). The integration time is 1 msec and the radiometric bandwidth is about 300 KHz. The overall dynamic range is larger than 50 dB. For convenient data handling several IDL- and Python-routines were written. Many CALLISTO instruments have already been deployed, including: 5 spectrometers in India (2 in Ooty, 1 in Gauribidanur, 1 in Pune, 1 in Ahmedabad), one in Badary near Irkutsk, Russian Federation, two in South Korea, three in Australia (Perth, Melbourne and Heathcote), two in Hawaii, two in Mexico, one in Costa Rica, two in Brazil, three in Mauritius, four in Ireland, one in Czech Republic, two in Mongolia, four in Germany, two in Alaska, two in Kazakhstan, one in Cairo, one in Nairobi, one in Sri Lanka, three in Trieste, one in Hurbanovo/Slovakia, two in Belgium, two in Finland, 8 in Switzerland, one in Sardinia, two in Spain, 5 in Malaysia, two in Indonesia, one in Scotland/UK one in Roztoky/Slovakia, one in Peru, one in Rwanda, one in Pakistan, one in Denmark, one in Japan and one in South Africa. Through the IHY/UNBSSI and ISWI instrument deployment program, CALLISTO is able to continuously observe the solar radio spectrum for 24h per day through all the year. All Callisto spectrometers together form the e-Callisto network. Callisto in addition is dedicated to do radio-monitoring within its frequency range with 13,200 channels per spectrum. The frequency range can be expanded to any range by switching-in a heterodyne up- or a down-converter. Instrument deployment including education and training of observers was financially supported by SNF, SSAA, NASA, Institute for Astronomy and North-South Center of ETH Zurich and a few private sponsors.
Version:2.3.0
This dataset contains solar dynamic spectrogram FITS files of the CALLISTO spectrometer data from the e-Callisto network of stations. The FITS file is composed of four parts: the ASCII-format header, the binary spectrum and two BIN tables. One table is for the time axis and the other for the frequency axis. FITSvfiles contain the keyword BUNIT in the primary header. If the BUNIT = 'SFU', then data are calibrated. If the BUNIT = 'digits', then data are raw data without any calibration. The naming convention for each file is of the form: STATION_YYYYMMDD_HHMMSS_CODE.fit.gz where STATION is a variable length station name and following the Date (YYYYMMDD) and UT time (HHMMSS) CODE is a two digit number that is an individual description of the front-end of the system. From the website http://e-callisto.org - The CALLISTO spectrometer is a programmable heterodyne receiver built in the framework of IHY2007 and ISWI by former Radio and Plasma Physics Group (PI Christian Monstein) at ETH Zurich, Switzerland. The main applications are observation of solar radio bursts and rfi-monitoring for astronomical science, education and outreach. The instrument natively operates between 45 and 870 MHz using a modern, commercially available broadband cable-TV tuner CD1316 having a frequency resolution of 62.5 KHz. The data obtained from CALLISTO are FIT-files with up to 400 frequencies per sweep. The data are transferred via a RS-232 cable to a computer and saved locally. Time resolution is 0.25 sec at 200 channels per spectrum (800 pixels per second). The integration time is 1 msec and the radiometric bandwidth is about 300 KHz. The overall dynamic range is larger than 50 dB. For convenient data handling several IDL- and Python-routines were written. Many CALLISTO instruments have already been deployed, including: 5 spectrometers in India (2 in Ooty, 1 in Gauribidanur, 1 in Pune, 1 in Ahmedabad), one in Badary near Irkutsk, Russian Federation, two in South Korea, three in Australia (Perth, Melbourne and Heathcote), two in Hawaii, two in Mexico, one in Costa Rica, two in Brazil, three in Mauritius, four in Ireland, one in Czech Republic, two in Mongolia, four in Germany, two in Alaska, two in Kazakhstan, one in Cairo, one in Nairobi, one in Sri Lanka, three in Trieste, one in Hurbanovo/Slovakia, two in Belgium, two in Finland, 8 in Switzerland, one in Sardinia, two in Spain, 5 in Malaysia, two in Indonesia, one in Scotland/UK one in Roztoky/Slovakia, one in Peru, one in Rwanda, one in Pakistan, one in Denmark, one in Japan and one in South Africa. Through the IHY/UNBSSI and ISWI instrument deployment program, CALLISTO is able to continuously observe the solar radio spectrum for 24h per day through all the year. All Callisto spectrometers together form the e-Callisto network. Callisto in addition is dedicated to do radio-monitoring within its frequency range with 13,200 channels per spectrum. The frequency range can be expanded to any range by switching-in a heterodyne up- or a down-converter. Instrument deployment including education and training of observers was financially supported by SNF, SSAA, NASA, Institute for Astronomy and North-South Center of ETH Zurich and a few private sponsors.
| Role | Person | |
|---|---|---|
| 1. | PrincipalInvestigator | spase://SMWG/Person/Christian.Monstein |
Access to a directory tree (ordered by year/month/day) of PNG format plots for the Callisto network. Within the same directory are the corresponding FITS data files.
Access to a directory tree (ordered by year/month/day) of FITS data files.