Supported LBA Configurations for SCHED
Listed in the table below are the recommended standard configurations for LBA observations. All of these configurations are available in NRAO SCHED from SCHED v9.2 (March 2010) onwards. If the desired configuration is not present please contact the VLBI observers for help.
Standard LBA setups use up to 8x16 MHz channels. Dual polarization recording is recommended, in which case up to 4x16 MHz channels are available in each polarization (512 Mbps recording rate). A special mode using up to 4x64 MHz channels is also available (allowing 1 Gbps recording). The table below indicates the availability of LBA telescopes in the main observing bands.
Configuration | Antenna (y/n indicates if the configuration is supported). |
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Name | Central Frequency (MHz) |
Polarisation | ATCA 6 x 22m |
Mopra 22m |
Parkes 64m |
Tid 70m (DSS43) |
Tid 34m (DSS34) |
Tid 34m (DSS35) |
Tid 34m (DSS36) |
Hobart 26m |
Ceduna 30m |
Hartebeesthoek 26m |
Warkworth |
Warkworth 12m |
AuScope 12m |
lba21cm*.setup | 1400 | dual or LCP | y | y | y (linear) | y (LCP only) | n | n | n | y (linear) | y (linear) | n | n |
y |
n |
lba18cm*.setup | 1650 | dual or LCP | y | y | y (linear) | y (LCP only) | n | n | n | y (linear) | y (linear) | y | n | n | n |
lba13cm*.setup | 2268 | dual or RCP | y | y | y (linear) | y | y (single pol only) | n | y (single pol only) | y | y | y | n | y | y (linear) |
lba6cm*.setup | 4816 | dual or RCP | y | y | y | n | n | n | n | y | y | y | n | n | y (linear) |
lba5cm*.setup | 6500 | dual or RCP | y | y | y | n | n | n | n | y | y | y | y | n | y (linear) |
lba3cm*.setup | 8425 | dual or RCP | y | y | y | y | y (single pol only) | y | y | y | y | y | y | y | y (linear) |
lba1cm*.setup | 22200 | dual or LCP | y | y | y | y | n | n | n | y | y | y | n | n | n |
Ka band (custom) | ~32000 | Dual | y | y | n | n | y | y | y | n | n | n | n | n | n |
"Single pol only" indicates that either RCP or LCP may be selected, but not both at the same time.
"linear" indicates the feeds are dual pol linear. These can be converted to a circular basis post-correlation if a bright calibrator is observed.