LMS-files

This option was included in order to create a full set of observing scripts (Target.acq, Target.spec, Target.flatcal, Target.lambdacal, Telluric.acq, Telluic.spec), using LMS files (created by the LUCIFER MASK SIMULATOR). After the upload of the lms-file using the regular upload function, the file is automatically treated as a LMS-script, if the last extension of the file ends with ".lms". It then hashes the keywords 'TEL.TARG.ALPHA/DELTA', 'INS.TARG40.ALPHA/DELTA' (coordinates of target/guide respectively),'LCEN', 'CAM', 'GRAT', 'FILT' and 'MASK_ID', as well as '#userdate', and '#INS.MASK.NA' (PI_name and filename respectively) from the script and translates them to scripting language, generating an acquisition script (standardvalues for acqusition script: DIT=10, NDIT=4, NEXPO=1, save_mode=integrated, readout_mode=o2dcr, OFFSET=-5 -5, ACQUISITION=5 5) and asking the user for value input for the spec-script (so all chosen options, except for DIT,NDIT,NEXP which can be entered in the respective field, just change the spec-script). After hitting the submit button the spec-script is tested with the scriptchecker and the entire lucichk output is printed. All the other files are tested by the lucichk separately and the number of errors/warnings as well as a link to the entire lucichk output is printed on the bottom of the output page. Using the values from the spec script, a standard flatcal and lambdacal script is generated (using NDIT_flat=NDIT_lambda='1', NEXPO_flat=5*NEXPO_lambda=5, readout_mode=o2dcr, save_mode=normal). The times were probed on the telescope and should be reliable for the standard filter/grating combinations (cf. Appendix B).

The tell.acq script offsets the telescope, after imaging the object in the center again, to the first position of the slit which was given on the Form-page. The default values there give the two most extreme cases (highest and lowest x-position on detector), if the value "INDEF" is chosen, the fields are ignored. Then the .spec script takes a spectrum of the object in the first chosen slit and moves then the telluric to the other chosen slits respectively. In addition to just move the telluric through the different slits, dithering of the telluric in every single slit can be done. After the last dithering the star is then moved to the center(!) of the next slit (new_pos=delta_slit-SUM(all dither)).

In order not to saturate the detector a filter combination suggestion is given for the telluric acq-script based on the spectral class of the star. Only for G,K type stars the J magnitude is fainter than the Ks magnitude, so that we chose:

Telluric Type	Filter combination
G & K	J & Paschen_beta
Rest	Bracket_gamma & Ks

NOTE: Any value that needs to be changed in the automatically created scripts has to be edited manually in the files generated by the script creator.