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| For example, one can remove/mask common glitches. One can remove a common mode. Here are some examples on one scan: | == Crosses on Mars == For example, one can remove/mask common glitches. One can also remove a common mode (obtained by summing all detector timelines after masking the source). Here are some examples on one scan: {{attachment:Cross_Mars_20120604_205_2mm_det7.jpg|Cross_Mars_20120604_205_2mm_det7| width=400}} {{attachment:Cross_Mars_20120604_205_1mm_det126.jpg|Cross_Mars_20120604_205_1mm_det126| width=400}} The (faint) line is a simple Gaussian fit with a linear baseline which goes along nicely to the data points. The parameters of the fit are written on the plots and show 12 arcseconds at 1 mm. One can also construct a film of the Mars crossing {{attachment:KidCartoon_Mars_20120604_205_A.gif|Cross_Mars_20120604_205_2mm}}{{attachment:KidCartoon_Mars_20120604_205_B.gif|Cross_Mars_20120604_205_1mm}} |
Cross and Focus analysis
FXD 4-Sept-2012
Back to the offline processing of NIKA run 4
Here we show some results on the cross and focus scans. We use the focal plane reconstruction by NP on the last scan of the run #168_20120604 in order to go further than simply analyzing one kid at a time.
Crosses on Mars
For example, one can remove/mask common glitches. One can also remove a common mode (obtained by summing all detector timelines after masking the source). Here are some examples on one scan:
The (faint) line is a simple Gaussian fit with a linear baseline which goes along nicely to the data points. The parameters of the fit are written on the plots and show 12 arcseconds at 1 mm. One can also construct a film of the Mars crossing
