This is the routine run my lmap_markII to derive a crude LRS2 wavelength solution. It uses a variety of more general tools, but I run it here using files made by lmap_markII that take care of a lot of the biikkeeping associated with LRS2. For instance, which amplifier images have dispersion running red-to-blue or blue-to-red, etc...
% % lmap_waver -h usage: lmap_waver fullfits [-v] [-h] [-f frame] [-F font] [-c color] arg1 = fullfits (raw) image name Additional options: -h = just show usage message -v = run in verbose/debug mode -F = specify font size of ds9 markers -c = specify color of ds9 markers -f = specify ds9 frame to be used
The product files are dumped into a local subdirectory that has the name $device_wsol. So, an image named 20200530T020734.3_056LL_twi.fits will produce a local wavelength directory named "056LL_wsol". Here is an example:
% % pwd /home/sco/LRS2_wavesols/20200529-30/uv/056LL_wsol % ls 20200530T020734.3_056LL_twi.fits 20200530T020734.3_056LL_twi_uv_ALL_wsol.parlab 20200530T020734.3_056LL_twi.Image.Info 20200530T020734.3_056LL_twi_uv_ALL_wsol.table 20200530T020734.3_056LL_twi_uv_ALL_wsol.curveThe FITS file is a bias-correcte LRS2 image. The *.Image.Info file is an ASCII dump of information that can be access in a script with the routine config_val_get. The table file contains viusually set (with ds9) spectral feature positions and other data used by downstream wavelngth solutions codes.