Changes between Version 10 and Version 11 of docs/CommissioningPlan/P2.7

Timestamp:

01/31/21 15:43:40 (4 years ago)

Author:

lmarafatto

Comment:

--

docs/CommissioningPlan/P2.7

@@ -31 +31 @@
 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.]
 
-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. 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. Flexures of the RR or ARGOS source affect the result. 
+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.