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Description Astrometric Observation of Methanol Masers: Determining Galactic Structu
Antennas At-Cd-Ho-Mp-Pa-Hh
Start 299 00:00:00
Stop 299 12:00:00
PI S.P. Ellingsen

Setup v255l.5cm-icrf: nif=4

Station Modes At Cd Ho Mp Pa
Channel 1 IFP#1-LO 6300 - 6316 MHz USB RCP
Channel 2 IFP#1-HI 6316 - 6332 MHz USB RCP
Channel 3 IFP#2-LO 6642 - 6658 MHz USB LCP
Channel 4 IFP#2-HI 6658 - 6674 MHz USB LCP
DAS 1 Skyfreq 6316 & 6658 MHz
Bandwidth 16 MHz
DAS Mode (telescope)

Setup v255l.5cm: nif=2

Station Modes At Cd Ho Mp Pa
Channel 1 IFP#1-LO 6642 - 6658 MHz USB RCP
Channel 2 IFP#1-HI 6658 - 6674 MHz USB RCP
Channel 3 IFP#2-LO 6642 - 6658 MHz USB LCP
Channel 4 IFP#2-HI 6658 - 6674 MHz USB LCP
DAS 1 Skyfreq 6658 MHz
Bandwidth 16 MHz
DAS Mode (telescope)

Mode changes:
299 00:00:00 v255l.5cm
299 00:10:00 v255l.5cm-icrf
299 01:00:00 v255l.5cm
299 05:30:00 v255l.5cm-icrf
299 06:15:00 v255l.5cm
299 11:15:00 v255l.5cm-icrf



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 second epoch for proper motion/parallax observations of the methanol maser sources G329.031-0.198, G329.029-0.205 and G329.066-0.308. G329.03-0.20 should show a modest peak at a sky frequency of around 6669.14 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 only phase-up CA01 through CA04 for this experiment. This is so that the synthesised beam is around 1 arcminute. 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. 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.

v255l.5cm Channels 5-8
v255l.5cm-icrf Channels 1,2,7,8

Observing times for Parkes :
0000 - 0015 : Fringe finder/delay setup
0050 - 0921 : ICRF runs and Target sources (target sets at about 0921 at Parkes)
1125 - 1200 : Final ICRF run

Hart :

Hart should use the v255l.5cm setup for both the maser and ICRF observations.

Observing times for Hart :
0534 - 1200 : Target source rises at Hart just in time for second ICRF run.


Observing Logs


lbaops/lbaoct2010/v255l.txt · Last modified: 2015/12/18 16:38 by