| | 46 | === Producing sdfits files === |
| | 47 | 1. Load data: pload <filename> |
| | 48 | 1. Provide unit bandpass table [[BR]] |
| | 49 | Syntax : {{{bpass <filename> -u}}} |
| | 50 | 1. 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).[[BR]] |
| | 51 | Syntax : {{{calscans <input file> <output filename> -s RL -t}}} |
| | 52 | {{{ |
| | 53 | > pload 2008-09-29_hhmm-P617.rpf |
| | 54 | > bpass 2008-09-29_hhmm-P617 -u |
| | 55 | > calscans 2008-09-29_hhmm-P617 output.sdf -s RL -t |
| | 56 | }}} |
| | 57 | |
| | 58 | |
