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information_for_astronomers:user_guide:eb-hsa [2014/08/26 09:08]
ubach
information_for_astronomers:user_guide:eb-hsa [2019/12/13 13:29]
ubach
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   - Proposals should be submitted using the NRAO web-based proposal submission tool at the advertised NRAO proposal deadlines. (Select VLBA and EB in the HSA section for VLBA+EB only observations)   - Proposals should be submitted using the NRAO web-based proposal submission tool at the advertised NRAO proposal deadlines. (Select VLBA and EB in the HSA section for VLBA+EB only observations)
   - Use the Walker/NRAO SCHED program for making the observing schedule, available from anonymous ftp at: ftp.aoc.nrao.edu ​ Directory: pub/sched\\ The SCHED manual can be read at: [[http://​www.aoc.nrao.edu/​~cwalker/​sched/​sched.html]]\\ A special section on the RDBE at: [[http://​www.aoc.nrao.edu/​~cwalker/​sched/​RDBE_system.html]]   - Use the Walker/NRAO SCHED program for making the observing schedule, available from anonymous ftp at: ftp.aoc.nrao.edu ​ Directory: pub/sched\\ The SCHED manual can be read at: [[http://​www.aoc.nrao.edu/​~cwalker/​sched/​sched.html]]\\ A special section on the RDBE at: [[http://​www.aoc.nrao.edu/​~cwalker/​sched/​RDBE_system.html]]
-  - All Effelsberg recordings will be made using the RDBE terminal and a MK5 disk recorder, as at the VLBA itself. Effelsberg has SCHED station name '​EB_RDBE'​.\\ For further details regarding the RDBE, consult: [[https://​science.nrao.edu/​facilities/​vlba/​docs/​manuals/​oss/​sig-path/rdbe]]+  - All Effelsberg recordings will be made using the RDBE terminal and a MK5 disk recorder, as at the VLBA itself. Effelsberg has SCHED station name '​EB_RDBE'​.\\ For further details regarding the RDBE, consult: [[https://​science.nrao.edu/​facilities/​vlba/​docs/​manuals/​oss/​sig-proc/rdbe]]
   - Deposit the schedule for EB_RDBE on the ASPEN file-server in Socorro, as for the VLBA schedule; the deadline is 2 weeks before the observation. The Effelsberg schedule will be retrieved from ASPEN by Effelsberg staff.   - Deposit the schedule for EB_RDBE on the ASPEN file-server in Socorro, as for the VLBA schedule; the deadline is 2 weeks before the observation. The Effelsberg schedule will be retrieved from ASPEN by Effelsberg staff.
     * The Effelsberg Observing Friend, Uwe Bach (ubach<​at>​mpifr-bonn.mpg.de) must be notified if any emergency changes are made to the schedule after that time.     * The Effelsberg Observing Friend, Uwe Bach (ubach<​at>​mpifr-bonn.mpg.de) must be notified if any emergency changes are made to the schedule after that time.
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   - 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 ยท Last modified: 2022/07/20 10:28 by ubach