Differences

This shows you the differences between two versions of the page.

Link to this comparison view

information_for_astronomers:user_guide:eb-hsa [2014/08/26 09:08]
ubach
information_for_astronomers:user_guide:eb-hsa [2019/06/06 10:58] (current)
ubach
Line 12: Line 12:
   - Phase-cal tones are injected for all secondary focus receivers (and for the 3mm receiver). There is no phase-cal signal for the 18/21cm or other prime focus receivers.\\ Note, also, that the phase of the phase-cal signal is not recovered after switching receivers during receiver-agile observations.   - Phase-cal tones are injected for all secondary focus receivers (and for the 3mm receiver). There is no phase-cal signal for the 18/21cm or other prime focus receivers.\\ Note, also, that the phase of the phase-cal signal is not recovered after switching receivers during receiver-agile observations.
   - The Effelsberg drive speed is slower than for VLBA antennas - currently 25 deg/min in azimuth and 15 deg/min in elevation.\\ Note also that observations at low elevation are restricted by the surrounding hills (see the [[information_for_astronomers:user_guide:antenna|horizon diagram]]).   - The Effelsberg drive speed is slower than for VLBA antennas - currently 25 deg/min in azimuth and 15 deg/min in elevation.\\ Note also that observations at low elevation are restricted by the surrounding hills (see the [[information_for_astronomers:user_guide:antenna|horizon diagram]]).
-  -  As the Effelsberg antenna beamwidth is ca. 4 times smaller than those of VLBA antennas, periodic pointing checks are essential, especially during short wavelength observations.\\ Observers should leave frequent gaps in their VLBI schedules (~10 mins each) to allow the telescope operators to make these checks. They should be about every two hours at 4cmand more frequently at shorter wavelengths.+  -  As the Effelsberg antenna beamwidth is ca. 4 times smaller than those of VLBA antennas, periodic pointing checks are essential, especially during short wavelength observations.\\ Observers should leave frequent gaps in their VLBI schedules (~10 mins each) to allow the telescope operators to make these checks. At 6cm and 3.6cm a pointing every hours is sufficient, at shorter wavelength a gap every 2 hours is recommended.
   - Observers using NON-STANDARD frequency set-up files (i.e. not one supplied with the current version of SCHED) should contact the Effelsberg technical friend, Uwe Bach, well before the observations so that any special files can be made in good time.\\ Technical friend e-mail: ubach<at>mpifr-bonn.mpg.de   - Observers using NON-STANDARD frequency set-up files (i.e. not one supplied with the current version of SCHED) should contact the Effelsberg technical friend, Uwe Bach, well before the observations so that any special files can be made in good time.\\ Technical friend e-mail: ubach<at>mpifr-bonn.mpg.de
   - HSA observations will be correlated at the VLBA correlator in Socorro.    - HSA observations will be correlated at the VLBA correlator in Socorro. 
  
  
 
information_for_astronomers/user_guide/eb-hsa.txt · Last modified: 2019/06/06 10:58 by ubach     Back to top