User Tools

Site Tools


lbaops:lbasep2009:v255g

Differences

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

Link to this comparison view

Both sides previous revision Previous revision
Next revision
Previous revision
lbaops:lbasep2009:v255g [2009/09/01 18:04]
sellings
lbaops:lbasep2009:v255g [2015/12/18 16:38] (current)
Line 20: Line 20:
  
 ^Station Modes                 | At Cd Ho Mp Pa | ^Station Modes                 | At Cd Ho Mp Pa |
-^Channel 1          | '' ​ IFP#1-LO 6300 - 6316 MHz USB LCP''​ | +^Channel 1          | '' ​ IFP#1-LO 6300 - 6316 MHz USB RCP''​ | 
-^Channel 2          | '' ​ IFP#1-HI 6316 - 6332 MHz USB LCP''​ |+^Channel 2          | '' ​ IFP#1-HI 6316 - 6332 MHz USB RCP''​ |
 ^Channel 3          | '' ​ IFP#2-LO 6642 - 6658 MHz USB LCP''​ | ^Channel 3          | '' ​ IFP#2-LO 6642 - 6658 MHz USB LCP''​ |
 ^Channel 4          | '' ​ IFP#2-HI 6658 - 6674 MHz USB LCP''​ | ^Channel 4          | '' ​ IFP#2-HI 6658 - 6674 MHz USB LCP''​ |
Line 40: Line 40:
 The method and frequencies for this experiment are identical to those for v255f earlier in this session. ​ The frequency setup for this session is identical to February, the only difference is that the setup for the ICRF observations is to be 2 IFs with different polarizations,​ rather than 2 IFs with a single polarization as previously (this avoids recabling at Hobart/​Ceduna and significantly simplifies the setup changes). ​ Unlike for previous epochs we will change the setup for the ICRF observations in the middle of the run, as well as for the beginning and end.  The times for the setup changes are given above. The method and frequencies for this experiment are identical to those for v255f earlier in this session. ​ The frequency setup for this session is identical to February, the only difference is that the setup for the ICRF observations is to be 2 IFs with different polarizations,​ rather than 2 IFs with a single polarization as previously (this avoids recabling at Hobart/​Ceduna and significantly simplifies the setup changes). ​ Unlike for previous epochs we will change the setup for the ICRF observations in the middle of the run, as well as for the beginning and end.  The times for the setup changes are given above.
  
-The purpose of these observations is to obtain the fourth ​epoch for proper motion/​parallax observations of the methanol maser sources ​G9.62+0.20 ​and G8.68-0.37.  Previous epochs were v255a (Mar08), v255b (Aug08) and v255f (Feb09). ​ We will observe both masers and phase calibrators with dual polarization 2x16 MHz bandpasses, but the correlator output will be high spectral resolution around the masers (G9.62+0.20 ​should show a strong peak at a sky frequency of around 6668.MHz during these observations) and standard continuum for the phase reference source. ​ The idea is to have a mode which expands the number of suitable phase reference sources available for spectral line sources. ​+The purpose of these observations is to obtain the third epoch for proper motion/​parallax observations of the methanol maser sources ​NGC6334F ​and NGC6334I(N).  Previous epochs were v255c (Nov08) and v255d (Feb09). ​ We will observe both masers and phase calibrators with dual polarization 2x16 MHz bandpasses, but the correlator output will be high spectral resolution around the masers (NGC6334F ​should show a strong peak at a sky frequency of around 6668.28 MHz during these observations) and standard continuum for the phase reference source. ​ The idea is to have a mode which expands the number of suitable phase reference sources available for spectral line sources. ​
  
 During the ICRF runs we have sometimes had to exclude certain antennas (particularly Parkes) from observations of some sources in order to get a good spread of azimuths and elevations. During the ICRF runs we have sometimes had to exclude certain antennas (particularly Parkes) from observations of some sources in order to get a good spread of azimuths and elevations.
Line 52: Line 52:
 ==== Parkes, ATCA, Mopra :  ==== ==== Parkes, ATCA, Mopra :  ====
  
-NOTE: the setup for the 4 x 16 MHz (ICRF sessions) differs from previous epochs, we now record dual polarization for both the ICRF and maser setup.  ​This may require stopping the recorder ​and changing modes in cdisko?+NOTE: the setup for the dual frequency ​(ICRF sessions) differs from previous epochs, we now record dual polarization for both the ICRF and maser setup.  ​ 
 + 
 +Setup DAS1 for 6316 MHz and DAS2 for 6658 MHz for the entire run. For then single freq setup, select channels 5-8 in cdisko. For the dual freq (ICRF) setup, select channels 1,2,7,8. You will need to stop and start cdisko to make these changes at the designated times. 
 + 
  
 Ftp: [[ftp://​ftp.atnf.csiro.au/​pub/​people/​vlbi/​v255/​v255g]] Ftp: [[ftp://​ftp.atnf.csiro.au/​pub/​people/​vlbi/​v255/​v255g]]
lbaops/lbasep2009/v255g.txt · Last modified: 2015/12/18 16:38 (external edit)