40m RT basic technical information
Spectral observations. These observations are available under several standard modes: position switching, frequency switching and On-The-Fly (OTF) position-switch mapping (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.
Continuum observations. These observations are restricted to total power pointing drifts or focus drifts. Position switch using a wobbler or a beam switch are not available. Currently there are several backends offering a bandwidth of 2.5 GHz, 1.5 GHz, 500 MHz or 100 MHz depending on the observed frequency.
- 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
- 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.
- On-the-fly spectral mapping in the Q and W bands is available with the full bandwidth of 18.5 GHz.
- The tri-band (K/Q/W) dual polarization VLBI mode with DBBC3 backends is currently under testing. These observations are considered to be in shared risk mode for the time being.
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 Single-Dish Director Discretionary Time or VLBI only)
- Q Band: 31.3 - 50.6 GHz
- W Band: 72 - 90 GHz
Instantaneous bandwidth, spectral resolution, angular resolution, aperture efficiency, main beam efficiency and Jy/K conversion