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V255M

v255m

Setup v255m.5cm-icrf: nif=4

Setup v255m.5cm: nif=2

Mode changes:
300 00:00:00 v255m.5cm
300 00:07:00 v255m.5cm-icrf
300 01:00:00 v255m.5cm
300 05:30:00 v255m.5cm-icrf
300 06:15:00 v255m.5cm
300 11:15:00 v255m.5cm-icrf
Ftp: ftp://ftp.atnf.csiro.au/pub/people/vlbi/v255/v255m

Comments:

The basic method and frequencies for this experiment are the same as for the earlier v255 experiments (Jul, Mar 10 and earlier). The frequency setup for this session is identical to July. As for July the setup for the ICRF observations is to be 2 IFs with different polarizations, rather than 2 IFs with a single polarization which was used prior to September 09 (this avoids recabling at Hobart/Ceduna and significantly simplifies the setup changes). The times for the setup changes are given above.

The purpose of these observations is to obtain the final epoch for proper motion/parallax observations of the methanol maser sources G9.62+0.20/G8.68-0.37. G9.62+0.20 should show a strong peak at a sky frequency of around 6668.2 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. Unlike the sessions prior to September 09, we wont need to recable during the run though. 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 v255k.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 please phase-up the maximum number of antennas the conditions allow for, there is no requirement for a larger synthesised beam for this source (unlike yesterdays v255l).

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. To switch between single frequency and and dual frequency setup you need to stop the recorder and change channel selection in cdisko as per the following table.

Observing times for Parkes :
0000 - 0020 : Fringe finder/delay setup (+ 1 ICRF source)
0052 - 1017 : ICRF runs and Target sources (target sets at 1017 at Parkes)
1130 - 1155 : Final ICRF run

Hart :

Hart should use the v255m.5cm setup for both the maser and ICRF observations.

Observing times for Hart :
0537 - 0615 : Second ICRF run
0758 - 1155 : Target source rises at Hart at approximately 07:58 UT

Observing Logs

Parkes onsource flagging
ATCA onsource flagging
Mopra onsource flagging
Mopra Tsys (plot)
Parkes Tsys

Weather

ATCA Weather
Mopra Weather
Parkes Weather