= NIKA Run#3 Summary of Off line processing Results =

The main document is [[attachment:Run3_Analysisv4.pdf|here]] and refers to figure

== 3 - Photometry ==

=== Evolution of the sky opacity during Run#3 ===

{{attachment:NIKA3OpacityCal/Study_atm2_4.jpg| Run#3 225GHz opacity at zenith | width=700}} 

=== Absolute photometry ===
Using pointing sources (mostly quasars), we compare the absolute flux measured with NIKA run3 with an estimate obtained using PdB measurements. The summary of the photometry is given [[attachment:Calibration_sources_NIKA2011_and_PdBv2.xls|here as a spreadsheet]] and in this figure:

{{attachment:Photometry_20111018v2.jpg| Run#3 NIKA vs PdB comparison| width=700}} 

The agreement is reasonable with the fluxes covering from 1.5 to 15 Jy.

The basic data reduction in IDL includes: deglitching, decorrelating from far away pixels and off-resonances, removing of one common mode (the average of the array), calibrating, projecting on the sky, computing a noise map, fixed-width Gauss-fitting (18 and 16 arcsecond FWHM).

In the previous results, these [[attachment:Batch2_allmapsv1.pdf|maps]] and [[attachment:Batch2_allplotsv1.pdf|plots]] were obtained by masking the central point-source so that no filtering shows up in the results.

Here are the results if no masking is used and then a compensating calibration factor 1/(0.615, 0.674) is used: [[attachment:Batch2_1_Analyze_v1.xls|see the spreadsheet]], [[attachment:Batch2.1_allmapsv1.pdf|the maps]] and [[attachment:Batch2.1_allplotsv1.pdf|the plots]]


=== Sensitivity ===

Results for the compact sources of the 20111019 night are shown here. No masking option is used (weak sources). In the case of weak sources and several scans, one can compute the noise from the dispersion of fluxes measured on the average of the map fluxes of different scans (W fluxes in the spreadsheet) or from the dispersion of the flux measurement of each detector map averaged over all scans. These two methods give consistent flux measurements. The error bar is consistent too for weak fluxes only. For stronger sources the photometric uncertainties contribute to the detector-based flux measurement too (source noise).

[[attachment:Batch3_1_weak_fluxes_v1.xls|The 20111019 flux measurements as a spreadsheet]] and in these figures as: [[attachment:Batch3.1_allmapsv1.1.pdf|maps]] and [[attachment:Batch3.1_allplotsv1.1.pdf|plots]]

Results for the compact sources of the 20111020 night are here (worse sensitivity but interesting results):

[[attachment:Batch4_fluxes_v1.xls|The 20111020 flux measurements (pointing sources) as a spreadsheet]] and in these figures as: [[attachment:Batch4_allmapsv1.pdf|maps]] and [[attachment:Batch4_allplotsv1.pdf|plots]]

and

[[attachment:Batch5_fluxes_v1.xls|The 20111020 flux measurements (weak sources) as a spreadsheet]] and in these figures as: [[attachment:Batch5_allmapsv1.pdf|maps]] and [[attachment:Batch5_allplotsv1.pdf|plots]]

== 4 - Focal Plane Geometry and Beams ==

Both RZ (Mopsic) and NP (IDL, from [[OffProcNika3?action=AttachFile&do=view&target=FP_quicklook_120207.pdf|This pdf]]) have found a distortion of the focal plane geometry well beyond the expected one.

{{attachment:OffProcNika3/avRPo1mmMeanEdge_1_9.png | average FoV 1mm RZ}}
{{attachment:OffProcNika3/NIKA2mmPh6-20111019s52_indFFmxRef1mm22_1_rpp.png | 2mm beams in PF (RZ)}}

{{attachment:FP_QLA_120207.png |  FoV 1mm&2mm NP}}

The focal plane distortion affects the beams in a correlated fashion with the Focal Plane Geometry distortion. This points towards a general optical distortion common to both detectors (an optical element is misplaced in the optical train).

== 5 - Glitches ==

4 examples of glitches as seen by all detectors, 2 on the A array and 2 on the B array. (Scan 64, A665, 20111020)

[[attachment:Glitch_study_AGl3.pdf|Glitch on A]], [[attachment:Glitch_study_AGl80.pdf|Another glitch on A]]

[[attachment:Glitch_study_BGl20.pdf|Glitch on B]], [[attachment:Glitch_study_BGl50.pdf|Another glitch on B (quite strong)]]



== 6 - Mars plateau ==

{{attachment:OffProcNika3/NIKA1mm-20111019s52_3_Jy.png | plateau@1mm uPixs Jy}}


== 7 Cosmetics ==

rms of maps per scan per kid per beam, averaged over 5 scans

{{attachment:Noise_PerKid_4C05.19_20111019_10_17v2.jpg | Noise per scan per kid per beam averaged over 5 scans}}