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lbaops:lbanov2011:v255p [2005/04/07 08:23]
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lbaops:lbanov2011:v255p [2015/12/18 16:38] (current)
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 ===== Comments: ===== ===== Comments: =====
  
-At Cd Ho Mp PaDual frequency setup requiredWill need special ​DAS setup+The basic method and frequencies for this experiment are the same as for the earlier v255 experiments (Jul 11, Mar 11,  and earlier). ​ The frequency setup for this session is identical to v255o in July 2011.  As for July the setup for the ICRF observations is to be 2 IFs with different polarizations. ​ The times for the setup (mode) changes are given above. 
 + 
 +The purpose of these observations is to obtain the third epoch for proper motion/​parallax for Mon R2 and the fifth (hopefully final) epoch for proper motion/​parallax observations of the methanol maser sources G329.031-0.198,​ G329.029-0.205 and G329.066-0.308. ​   
 + 
 +The Mon R2 observations run from 12 - 21 UT and should show a modest peak at a sky frequency of 6668.25 MHz.  The G329.03-0.20 run from 21 - 9 UT and should show a modest peak at a sky frequency of around 6669.2 MHz during these observations. 
 + 
 +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. 
 + 
 +===== Observing comments for each antenna===== 
 + 
 +==== Hobart, Ceduna :  ==== 
 + 
 +The 4 x 16 MHz bandpass setup requires feeding two separate LOs into IFP#1 and #2 on the DAS/frequency ​translator. ​ For Hobart the LOs should be set to 468 MHz (IFP#1) and 810 MHz (IFP#2) for the 4 x 16 MHz setup and 810 MHz for the 2 x 16 MHz setup. ​ For Ceduna, if you set the agilent to 11.1 GHz rather than 11.4 GHz, then you can use the same LOs as at Hobart. 
 + 
 +The level into IF#1 will change significantly between the two setups. ​ Set the level into the DAS so that it is within range for both setups. ​ Setup the system temperature measurement so that it works for both IFs for the v255p.5cm ​setup - it doesn'​t matter if the system temperature measurement doesn'​t work for the first IF during the ICRF observations as these are only to calibrate the delay. ​ Please don't change the attenuation into the DAS when the setup changes as that may change the delay. ​  
 + 
 +==== Parkes, ATCA, Mopra :  ==== 
 + 
 +For the ATCA phase-up only antennas CA01 through CA04 for this experiment. G329.031 and G329.029 are separated by about 30 arcseconds and the observation of G329.03-0.2 is at the mid-point of these two masers. 
 + 
 +Setup as for a 2p-4IF experiment (dual DAS with huygens cable for entire experiment) with DAS1 tuned to the lower frequency and DAS2 to the upper frequency. Use the new features in cdisko version 4 to automate the changes of channel selection as per the following table. 
 + 
 +| v255p.5cm | Channels 5-8 | 
 +| v255p.5cm-icrf | Channels 1,2,7,8 | 
 + 
 +==== Parkes :  ==== 
 + 
 +1305-1515 & 1836 - 1931 : Only one of the two target sources (Mon R2) above the horizon at Parkes (G188.95 has set), Parkes will miss about 50% of scans during these times. \\ 
 + 
 +==== Hart : ==== 
 + 
 +Observing times for Hart : \\ 
 +1931 - 2150 : Mon R2 and then ICRF observations (misses perhaps 25% of ICRF sources) \\ 
 +0317 - 0345 : ICRF observations\\ 
 +0505 - 0900 : G329.03 observations followed by ICRF observations at end (misses perhaps 25% of ICRF sources) \\
  
 ===== Observing comments for each antenna: ===== ===== Observing comments for each antenna: =====
lbaops/lbanov2011/v255p.txt · Last modified: 2015/12/18 16:38 (external edit)