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P2.7

v12	v13
27	27
28	28	Comments
29
30		MB: Given the adjustment of SOULD LBT wrt to elevation should already have been done previsouly, I'd say it would be best to have also a look up table at least for TT where dichroic and in-TT are adjusted to compensate flexures [okay. in that case, we may need more time. lets discuss.]
31
32		LM: this topic needs discussion, but in principle, this can be done together with the NCPA tests (2.6). Basically, when changing the elevation of the telescope, re-acquire the on-axis source with SOUL and record how much the Pyramid WFS moved from one elevation to another one in order to re-center it on the source (maybe this already exists). After SOUL acquired the on-axis source, look for it on the TECCAM and use our internal mirrors (IN-TT and DM) to re-center the PSF and pupil on the hot pixels. If big adjustments of our mirror positions are required, we can build the look-up table (--> define "big"). Flexures of the RR or ARGOS source affect the result.