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Session startup

Use the official Parkes vnc sessions on joffrey:1 and joffrey:2. Run cdisko and DAS in joffrey:2. The recording machine is different to the DAS control machine! See below

Start the following (in different virtual desktops).

Parkes control


  • showtel
  • 2 spare xterms for commands (atsnap, lorun below)

DAS control

  • ssh vlbi@pkvsi1 then das1
  • ssh vlbi@pkvsi1 then das2

LBADR control

  • ssh vlbi@pkvsi2 then cdisko2

For DAS and cdisko usage and control see here

Experiment Startup

Receiver Selection

The telescope should be parked before you change recever otherwise the translator can get stuck. Run atsnap park in an xterm on joffrey

Select required receiver in “operfcc” and click “place selected receiver on axis”.

OUTOFDATE?? Turn on Focus cabin camera while changing receivers, and remember to turn
it off again as it is a source of RFI

Click on the reciver name below for receiver specific setup notes.

Receiver Wavelength
Multi 21cm/1.4 GHz
H-OH 18cm/1.6 GHz
Galileo 12cm/2.4 GHz
METH6 5cm/6.7 GHz
Mars 3cm/8.6 GHz
13mm 13mm/22 GHz

You MUST select the receiver before starting atsnap below, otherwise pointing will be wrong.

IF setup

As observer on one of the suns run

cd ~/lbalorun SETUP.cmd

(where SETUP is the name of the correct session setup file, e.g 2011Mar_HOHa.cmd). Someone must have set this up first.

The Switch Matrix is only needed when Mark5 recorder is used (see the Mark5 setup notes | ). The DAS are not connected through the switch matrix

Antenna schedule

The antenna schedule should be copied automatically. If it is missing, download the .psn file from the atnf ftp area (see experiment wiki). As pksobs on joffrey run atsnap, with the name of the .psn file. E.g.

atsnap vc001.psn

The .psn files will be in ~pksobs/lba

DAS setup/Attenuation

Make sure that levels on the VLBI DAS are within range (ie the IF Level is mid range).

If not, adjust attenuation on the loGUI.

Use the C12 attenuators 1&2 for coarse setup (acts on both IFs), use the C40 1,2,3,4 attenuators for fine setup. Usually only the C40 attenuators should be adjusted.

Before adjusting attenuation, click the “refresh” button on loGUI near the bottom left

If you need to change the attenuation, you may want to update the lorun .cmd file.

Cal Control Unit

Tsys is measured by sending a 200 Hz signal to the receiver and a detector connected to the analog output of the VLBI DAS. On the “Stanford Research Systems” signal generator in rack#4, check the frequency is 200 Hz and amplitude is 5V.

Start the “Cal Control Unit” from PKMC gui. Ensure all relevant receivers are connected to SRSFG as well as the “DAS BE” and “MARS BE” if Mars is being used.


If the polarisation is swapped, a quick remedy is to swap the DAS inputs at the bottom of rack 2 in the equipment room upstairs. Swap the A1/B1 and A2/B2 short patch cables between the DAS OUT and DAS IN. However when observing remotely this may not be possible. For dual polarization experiments just make a note in the wiki. For single pol experiments just make a different channel selection in cdisko to select the other polarisation.

Generating a test tone

If you need to check that you are observing at the right frequency, you can use the vertex radiator to generate a test tone using the following procedure:

  • Find the LO HP 8648D in the lower half of rack 7 (upstairs) and ensure it has RF OFF.
  • Connect the “Vertex 2” port (also labelled “LO”) at the top of rack 6 to the HP 8648D RF output.
  • Connect the “Vertex 1” port (also labelled “DC”) to the power supply unit about midway up rack 7. You can use any of the ports labelled “2”, “3”, or “4”.
  • Turn on the rack 7 power supply unit by first moving down the switch (towards the “ON” label) above the port used to connect to the “Vertex 1” port, then moving down the switch next to the “+24V” label on the right of the unit. There should now be a green light next to each of the switches you just moved.
  • Set the frequency of the HP 8648D LO to an appropriate harmonic frequency. For example, to generate a tone at 8420 MHz, choose the 20th harmonic of 421.0 MHz (ie. set the LO frequency to 421.0 MHz).
  • Set the RF level of the HP 8648D LO to a very low level, no higher than ~ -12 dBm.
  • Turn the RF ON for the HP 8648D LO, to generate the tone.


Post observations

Onsource flagging

Get the on source flagging file for the whole session. Log onto a Solaris machine (e.g. pavo) as observer and run “antfg”: pavo-101% antfg <year> <dayno start> <dayno end> This creates an AIPS style flagfile as ./antflag


pavo-101% antfg 2006 316 323

This creates a flagfile covering range of days 2006/316-323 inclusive. This file should be copied to Epping and put in the vlbi ftp area /pub/people/vlbi/cal/parkes/logs with the name MonthYear, using a 3 letter abbreviation for the month. E.g.:

> scp antflag vlbi@athena:/nfs/ftp/people/vlbi/cal/parkes/logs/Nov2006.antflag

Note that the flag data for an entire session should be contained in a single file. A CGI script extracts the needed entries for individual experiments.


For observations from 2008 and onwards

Tsys values are recorded in


These should be mirrored to Sydney, using the following command logged in to a Marsfield Unix machine as vlbi.


For data pre 2007 (Nov 2007 and earlier)

A program SYSTEMP runs on the Vax YOWIE, reading the Synch Demod attached to the AT samplers, near the DAS inputs (upstairs control room).

The inputs to the synch Demod are set up by the user - in recent years I have been using the analogue outputs of the DAS Fine Tuner (FT) for this purpose. This isn't ideal but is the best we have. (See notes below).

The program writes 15-second averages to the file;


where each use of the program creates a higher version of this file.

These can be FTP'd by logging-in to YOWIE (as VLBI, usual pw), Appropriate local Parkes (Solaris) machines to use as an intermediate storage location include sagitta, pavo, pisces, perseus or orion.

$vlbi> sd obs$data:[systemp]
$vlbi> ftp <target_machine>
	ftp> put SYSTEMP_G.LOG;356 systemp.355

Once the files are on the Parkes Solaris system you can produce something more usuable with the utility pks_tsys;

sagitta% ~rey052/bin/pks_tsys
 SYSTEMP input file [SYSTEMP.LOG] : systemp.355
 TSYS  output  file [TSYS] : v215a.tsys
 Integration interval [  5.000min] :
 Diode scale factors [ 1.0000 1.0000] :

which averages the raw numbers with a specified interval (default 5 minutes) and scales the values with user-specified calibration factors. These factors need to be determined from calibration observations e.g. “SPOT”.

The file created looks like;

 ! PRKS Tsys data from file: systemp.355
 ! Tcal A/B =   1.0000  1.0000 *  1.0000
 318 09:12:35.2       30.4401      29.6506 !  0.17  0.20 19
 318 09:17:29.6       30.3742      29.7018 !  0.29  0.31 18
 318 09:22:24.0       30.4703      29.6044 !  0.15  0.13 19

which should be close to the format needed for AIPS. The numbers after the “!” are the RMS values for each channel and the number of values in the average.

lbaops/parkesnotes.txt · Last modified: 2016/09/30 22:53 by ste616