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lbaops:lbascheduling [2019/09/26 17:42]
cormac [ATCA Issues]
lbaops:lbascheduling [2020/02/11 14:32] (current)
cormac
Line 47: Line 47:
 Since April 2017 Hobart and Ceduna should normally be scheduled as HOB_DBBC and CDDBBC to use the DBBC, unless otherwise instructed. Since April 2017 Hobart and Ceduna should normally be scheduled as HOB_DBBC and CDDBBC to use the DBBC, unless otherwise instructed.
  
-Tid antennas should usually be scheduled to use the LBA DAS unless otherwise instructed. +Tid antennas should usually be scheduled to use the DVP unless otherwise instructed. 
  
 ===== DAS Setups ===== ===== DAS Setups =====
 Some LBA observatories use the ATNF DAS, which is a digital filter bank. The ATNF observatories (Parkes, ATCA, Mopra) each have  Some LBA observatories use the ATNF DAS, which is a digital filter bank. The ATNF observatories (Parkes, ATCA, Mopra) each have 
-2 DAS installed, while 1 is available at Hobart and Ceduna. The DAS have two independent "IFPs" which sample the +2 DAS installed, while 1 is available at Hobart and Ceduna (though they normally use the DBBC). The DAS have two independent "IFPs" which sample the 
 analogue signal and produce up to two digitised channels each, which are then recorded. The two IFPs are generally  analogue signal and produce up to two digitised channels each, which are then recorded. The two IFPs are generally 
 connected to the two polarisations of the receiver but can be set up to record two different frequencies of the same  connected to the two polarisations of the receiver but can be set up to record two different frequencies of the same 
Line 68: Line 68:
 Older versions of SCHED will not necessarily produce a correct .vex file for a current observation. Older versions of SCHED will not necessarily produce a correct .vex file for a current observation.
  
-SCHED is installed on linux machines at ATNF (hydra and draco) or+SCHED is installed on linux machines at ATNF (e.g. draco) or
 can be obtained from ftp://ftp.aoc.nrao.edu/pub/sched/ . can be obtained from ftp://ftp.aoc.nrao.edu/pub/sched/ .
 Example LBA .key files are distributed with the latest version of SCHED Example LBA .key files are distributed with the latest version of SCHED
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 ==== Frequency setup ==== ==== Frequency setup ====
 +Please prepare your schedule using one of the standard LBA setup files
 +distributed with SCHED ($SCHED/setups/lba*). The lba* setup files distributed
 +with SCHED should cover all standard continuum modes. If your schedule requires
 +a non-standard mode or frequency (e.g., for spectral line observations) then
 +please consult with ATNF staff before submitting your schedule.
 +
 The ATCA and Mopra  LO chain generally restricts the frequency selection to 1 MHz steps. For continuum experiments this The ATCA and Mopra  LO chain generally restricts the frequency selection to 1 MHz steps. For continuum experiments this
 should not cause any difficulty (particularly if you use the standard setups!). For spectral line experiments, letting  should not cause any difficulty (particularly if you use the standard setups!). For spectral line experiments, letting 
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 However, the mixed backends on the LBA, with their often mismatched filters, means that SCHED's automated Doppler setting often does not work for LBA experiments. Its use is deprecated, but if used its results should be carefully checked. However, the mixed backends on the LBA, with their often mismatched filters, means that SCHED's automated Doppler setting often does not work for LBA experiments. Its use is deprecated, but if used its results should be carefully checked.
 +
 +
 ==== Fringe Finders  ====  ==== Fringe Finders  ==== 
  
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 Note that you must reset the intent to some other value (e.g. OBSERVE_TARGET) on the following scan or the previous intent will be inherited by all ensuing scans! Note that you must reset the intent to some other value (e.g. OBSERVE_TARGET) on the following scan or the previous intent will be inherited by all ensuing scans!
  
 +
 +==== Amplitude Calibration ====
 +
 +Tsys measurements from LBA telescopes are frequently missing or subject to significant errors, especially at frequencies where RFI is an issue. This is a significant complication for data analysis especially where accurate flux deck densities are required. It is strongly recommended to regularly observe a compact calibrator that is part of the ATCA calibrator monitoring program to provide amplitude calibration bootstrapping. Such a source should preferably be within approx 10 degrees of your target sources. Your phase calibrator will often be suitable.
 +
 +It is also possible to use the ATCA local interferometry data to provide this calibration for a source that is not in the monitoring program. Please consult with observatory staff before committing to this strategy.
  
 ===== Wiki ===== ===== Wiki =====
lbaops/lbascheduling.1569483762.txt.gz · Last modified: 2019/09/26 17:42 by cormac