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Дата изменения: Mon Jun 4 20:13:00 2001 Дата индексирования: Tue Oct 2 05:57:07 2012 Кодировка: Поисковые слова: ngc 5128 |
Figure 2 shows the entire telescope system. Comparing the LMT to a conventional telescope, we see that they are similar with the exception of the mount. The top parts, consisting in a focusing system and a detector, are identical, but there is some cost saving in the upper end structure since it does not have to be tilted. The largest savings accrue due to the simple tripod mount.
While an LMT can only observe a zenith strip of constant declination,
its observing efficiency compared to that of a classical telescope is
very high (no slew, no field acquisition, no lost readout time). The
tracking will be done with the Time Delay Integration technique (TDI,
also known as the drift scan technique), and low-resolution
spectroscopy can be carried out with interference filters. A
semi-classical on-axis glass corrector capable of about
degree field will be used to remove the TDI
distortion. With a classical corrector, the TDI technique degrades the
images since the technique moves CCD pixels at a constant speed in a
straight line, while fixed-sky elements appear to move at different speeds
along slightly curved trajectories. This latitude-dependent
deformation is zero at the equator and increases with increasing
latitude.
A more detailed description of the ILMT project is available at:
http://vela.astro.ulg.ac.be/lmt/