ATNF VLBI Wiki

Setup v255o.5cm:

Setup v255o.5cm-icrf:

Mode changes:
205 19:00:00 v255o.5cm
205 19:10:00 v255o.5cm-icrf
205 20:00:00 v255o.5cm
205 23:30:00 v255o.5cm-icrf
206 00:15:00 v255o.5cm
206 04:00:00 v255o.5cm-icrf
206 04:50:00 v255o.5cm
206 10:00:00 v255o.5cm-icrf
206 10:45:00 v255o.5cm
206 15:15:00 v255o.5cm-icrf

Ftp: ftp://ftp.atnf.csiro.au/pub/people/vlbi/v255/v255o

The basic method and frequencies for this experiment are the same as for the earlier v255 experiments (Mar 11, Oct10, and earlier). The frequency setup for this session is identical to v255n in March 2011. As for March 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 second epoch for proper motion/parallax for Mon R2 and the fourth 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 19 - 4 UT and should show a modest peak at a sky frequency of 6668.1 MHz. The G329.03-0.20 run from 4 - 16 UT and should show a modest peak at a sky frequency of around 6669.0 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.

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 v255o.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.

For the ATCA phase-up all available antennas CA01 through CA05 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.

2000 - 2026 : No target sources visible, no observations with Parkes
2026 - 2236 & 0136 - 0231 : 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.

Observing times for Hart :
0231 - 0450 : Mon R2 and then ICRF observations
1010 - 1045 : ICRF observations
1221 - 1600 : G329.03 observations followed by ICRF observations at end.

Observing times for Sheshan :
Not participating in fringe checking, only observes in v255o.5cm mode
1936 - 0450 : Sheshan involved in nearly all Mon R2 and G188.95 observations and some of the ICRF observations.

òÀÔ-

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

ATCA Weather
Mopra Weather
Parkes Weather

Mopra Tsys
Parkes Tsys
ATCA Tsys