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40m RT basic technical information
Observing modes
Spectral observations. These observations are available under several standard modes: position switching, frequency switching, Wobbler Switching, and On-The-Fly (OTF) position-switch mapping (IMPORTANT: see below). Position Switch observations can be programmed ad-hoc using several phases. The spectral backends are Fast Fourier Spectrometers (FFTs) with 100 MHz, 500 MHz, 1.5 GHz and 2.5 GHz bandwidths with 6 kHz, 30 kHz, 180 kHz and 38 kHz resolution respectively.
Important Notes:
- Wobbler Switching is offered in shared-risk mode, with offset throws ranging from ±160 to ±400 arcsec, and wobbling frequencies ranging from 0.0625 and 0.25 Hz.
- On-the-fly spectral mapping in the Q and W bands is available with the full bandwidth of 18.5 GHz.
- W band (72 - 90 GHz) observations are available for a limited number of hours in the semester (night time only, from 2 hours after sunset to sunrise, due to thermal distortion in the telescope structure), with a bandwidth of 18.5 GHz.
- The tri-band (K/Q/W) dual polarization VLBI mode with DBBC3 backends is currently NOT being offered. Only DBBC2, single-band VLBI observations are offered for the time being.
- Keep in mind that there is usually a strong demand for objects in the region between 2:00 and 9:00 LST. Depending on the proposal ranking, Requesting sources in this LST range could therefore find it harder for observations to be carried out
Available observing frequencies:
- C band: 4.9 - 5.4 GHz & 6.1 - 6.6 GHz (currently Single-Dish Director Discretionary Time or VLBI only)
- X Band: 8.1 - 8.9 GHz (currently Single-Dish Director Discretionary Time or VLBI only)
- K Band: 21 - 25 GHz (currently VLBI only)
- Q Band: 31.3 - 50.6 GHz (for technical details see Tercero et al, 2021)
- W Band: 72 - 90 GHz (for technical details see Tercero et al, 2021)
Instantaneous bandwidth, spectral resolution, angular resolution, aperture efficiency, main beam efficiency and Jy/K conversion
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