Notes made for September 2008 session for P617
Observing
- Start the correlator (DFB3):
- login to pkccc3 as corr/*
- > sdfb3
- Start TCS
- login to a Sun (sagitta) as observer/
-
> atcsver > tcs
- to get latest version of TCS, and start it
- select Digital Filter Bank (time-binning)
- select Expert mode
- configuration file is p617
- cycletime = 4s
See whiteboard for passwords.
Looking at scans
To examine data:
- Copy from the correlator computer:
> scp corr@pkccc3:/data2/SDFB3_2/2008-09-29_hhmm-P617.rpf .
- Load into the pol format:
> pload 2008-09-29_hhmm-P617.rpf > gcopy 2008-09-29_hhmm-P617 2008-09-29_0753-P617
- Look at the data (uncalibrated). This example shows scan number 3.
> showscan 2008-09-29_hhmm-P617 -s 3
showscan asks for:
- a plot device: the first plot is not useful so give carriage return
- a channel number, then a plot device
Graphics device/type (? to see list, default /NULL): /xs
(for a screen plot)Graphics device/type (? to see list, default /NULL): filename.ps/ps
(for hard copy)> lwp filename.ps
from the unix prompt.
Producing sdfits files
- Load data: pload <filename>
- Provide unit bandpass table
Syntax :bpass <filename> -u
- Convert to Single Dish FITS . Use calscans to do this. It will output the part of the spectrum specified in the file <filename>/freqtab.dat, which contains a list of frequency bands to be formed. calscans assumes all bands have the same width and so expects a set of evenly spaced frequencies. Frequency separations should be no less than the channel separation; if more, the output bands are the averages of several input channels. The
-s
switch gives the output as RR,LL,RL,LR (instead of IQUV). The-t
switch prevents any translation from telescope to sky corrdinates (parallactic angle tracking).
Syntax :calscans <input file> <output filename> -s RL -t
> pload 2008-09-29_hhmm-P617.rpf > bpass 2008-09-29_hhmm-P617 -u > calscans 2008-09-29_hhmm-P617 output.sdf -s RL -t
Last modified 16 years ago
Last modified on 09/30/08 16:04:49