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Flux fraction vs. MJD, UT, Elevation, and extinction correction, <<BR>> for Ar2, Ar1 and Ar3. |
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Back to the main NIKA2 run 72 page
Data reduction of run 72 (re-commissioning) and results
To be progressively updated, when the re-commissioning data are being analyzed.
PIIC data reduction
Beam maps new analysis
This new analysis of the beam maps extends what was done during the re-commissioning weeks (see the daily reports) Remeber that Box C of Ar2 is noisy and therefore mostof its KIDs are rejected, including the reference KID KC016. Therefore I am using KID KB013 as reference. Hence this same KID has been used as pointing KID during the observations. All pointing offsets were refereed to this KID. All maps are cenetred on this KID, although it is off-axis, and therefore all maps are slightly shifted (one-two 2mm beams) with respect to the geometrical/optical center of the f.o.v.
Available Beam maps |
|||
Scan |
Target |
Comments |
Analyzed? |
20250324s23 |
2251+158 |
decent |
yes |
20250324s37 |
2251+158 |
terrible |
Excluded |
20250324s58 |
Uranus |
ok |
yes |
20250330s301 |
1253-055 = 3C279 |
focused on Ar2 (and Ar1) |
yes |
20250330s314 |
1253-055 = 3C279 |
focused on Ar3 |
yes |
20250331s8 |
1253-055 = 3C279 |
focused on Ar2 + 0.25 mm |
yes |
20250331s10 |
1253-055 = 3C279 |
focused on Ar2 - 0.25 mm |
yes |
20250331s12 |
1253-055 = 3C279 |
focused on Ar2 + 0.50 mm |
yes |
20250331s14 |
1253-055 = 3C279 |
focused on Ar2 - 0.50 mm |
yes |
20250331s74 |
1641+399 = 3C345 |
polarimetry beam map |
no |
The best beam maps, that I combined together to produce the DAF RPPs are:
Array |
best beams maps (used and combined in the RPPs) |
Ar2 |
20250324s23, 20250324s58, 20250330s301 |
Ar1 |
20250324s23, 20250324s58 |
Ar3 |
20250324s23, 20250330s314, 20250331s8 |
Comparison of analyzed the beam maps: PDF file
Comparison of FWHM for each KID, array and beam map:
Calibration analysis
During the re-commissioning days, we took a total of more than 150 pointing and calib1_scan scand on primary and secondary calibrators. I used them to study the statistics of calibration and derive the calibration factors of the new Ar1 and Ar3. Below here, I post a series of diagrams, showing the fraction of calibrators flux retrieved, using the old calibration factor and the newly determined calibration factors.
The Ar1 and Ar3 statistics are very noisy (more than usual). In my opinion, this highlights the need to have very high quality data, in order to perform this kind of analysis. Note that several scans were taken either in sub-optimal sky conditions (large extinction correction) or during the warmest hours of the day, when the telescope was subject to strong thermal distorsions. Consequently the beams were larger than usual and distorted, which might have caused losses of main beam flux. Finally, this "noisy statistics" might indicate that the new Ar1 & Ar3 arrays are not only much more sensitive that the old ones, but also more easily affected by sky/telescope instabilities.
Results using the old calibration factors:
Flux fraction vs. MJD, UT, Elevation, and extinction correction,
for Ar2, Ar1 and Ar3.
