User Tools

Site Tools


lbaops:lbasep2015:v490d

v490d

Description Measuring the proper motions of the Large and Small Magellanic Clouds
Antennas At-Cd-Hh-Ho-Mp-Pa
Start 268 12:00:00
Stop 269 01:00:00
PI S.P. Ellingsen

Setup v490d.1cm-icrf: NIF=4

Station Modes At Cd Ho Mp Pa
Channel 1 IFP#1-LO 22000 - 22016 MHz USB RCP
Channel 2 IFP#1-HI 22016 - 22032 MHz USB RCP
Channel 3 IFP#2-LO 22500 - 22516 MHz USB LCP
Channel 4 IFP#2-HI 22516 - 22532 MHz USB LCP
DAS 1 Skyfreq 22016 & 22516 MHz
Bandwidth 16 MHz
DAS Mode vsop.pro (telescope)
Station Modes Hh
Channel 1 22000 - 22016 MHz USB RCP
Channel 2 22016 - 22032 MHz USB RCP
Channel 3 22500 - 22516 MHz USB LCP
Channel 4 22516 - 22532 MHz USB LCP
Bandwidth 16 MHz
DAS Mode Mark5

Setup v490d.1cm: NIF=2

Station Modes At Cd Ho Mp Pa
Channel 1 IFP#1-LO 22211 - 22227 MHz USB RCP
Channel 2 IFP#1-HI 22227 - 22243 MHz USB RCP
Channel 3 IFP#2-LO 22211 - 22227 MHz USB LCP
Channel 4 IFP#2-HI 22227 - 22243 MHz USB LCP
DAS 1 Skyfreq 22227 MHz
Bandwidth 16 MHz
DAS Mode vsop.pro (telescope)
Station Modes Hh
Channel 1 22211 - 22227 MHz USB RCP
Channel 2 22211 - 22227 MHz USB LCP
Channel 3 22227 - 22243 MHz USB RCP
Channel 4 22227 - 22243 MHz USB LCP
Bandwidth 16 MHz
DAS Mode Mark5

Mode changes:
268 12:00:00 v490d.1cm
268 13:08:00 v490d.1cm-icrf
268 13:59:53 v490d.1cm
268 17:31:22 v490d.1cm-icrf
268 18:14:39 v490d.1cm
268 21:46:08 v490d.1cm-icrf
268 22:30:01 v490d.1cm

Ftp: ftp://ftp.atnf.csiro.au/pub/people/vlbi/v490/v490d


Comments:

Due to popular demand V490 has copied the basic strategy used for the V255 series of methanol maser astrometry experiments. There are two different frequency setups, the “ICRF” observations to calibrate the tropospheric delay has 2 IFs with different polarizations. The second setup (the one used for the majority of the time) has a single IF with dual polarisation. The times for the setup (mode) changes are given above.

The purpose of these observations is to obtain the fourth epoch for proper motion observations of water masers in the SMC and LMC.

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 both Hobart and Ceduna the LOs should be set to 706 MHz (IFP#1) and 206 MHz (IFP#2) for the 4 x 16 MHz setup and 495 MHz for the 2 x 16 MHz setup. For Hobart use 16.37 GHz as the Agilent frequency and for Ceduna use 17.47 GHz. For the 4×16 MHz setup 880.2 and 900.2 MHz should give coherence in IF#1 and IF#2 respectively, while for the 2×16 MHz use 888.64 MHz to check coherence (these tones apply for both Hobart and Ceduna).

The level into IF#2 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 v490d.1cm setup - it doesn't matter if the system temperature measurement doesn't work for the second 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 antennas CA01 through CA05 for this experiment. The sources 0100-760, 0601-706 and 0530-727 should all be suitable for phasing the array (in addition to the fringe finder sources) and have been marked with the AUTOPHASE_DETERMINE intent in the vex file.

The information below for Parkes has been copied from the v490b experiment and may need to be updated.

Parkes LO can be controlled using the “losched” command. It assume the initial setup has been made usign a normal lo_setup file. Run if as pksobs on joffrey:

> losched v490b.losetup

v490b.1cm frequencies at Parkes can be setup using the 2013Nov_13MMd.cmd and v490b.1cm-icrf using 2013Nov_13MMe.cmd

Observing comments for each antenna:

Observing Logs

Weather

Monica log information - EXPERIMENTAL:

lbaops/lbasep2015/v490d.txt · Last modified: 2015/12/18 16:38 (external edit)