nika run#3 october 2011 report on data analysis february 2012
DESCRIPTION
NIKA run#3 October 2011 Report on data analysis February 2012 F.-Xavier Désert on behalf of the Nika team. Basics. Run #3 motivations : Test cryocooler Test the new magnetic shielding Test photometry with a new method Test an improved 1mm channel Moreover Show the ability to go deeper - PowerPoint PPT PresentationTRANSCRIPT
F.-Xavier Désert IRAM NIKA 8 February 2012 p. 1/21
NIKA run#3 October 2011Report on data analysis
February 2012F.-Xavier Désert on behalf of the Nika team
F.-Xavier Désert IRAM NIKA 8 February 2012 p. 2/21
Basics
Run #3 motivations : – Test cryocooler– Test the new magnetic shielding– Test photometry with a new method– Test an improved 1mm channel
Moreover– Show the ability to go deeper– Use New beam splitter
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Characteristics
• 2 channels readout with 2 independent coaxial cable pairs and electronics
• 2x150 timeline outputs at 22 Hz• about 80 @2mm, 90@1mm valid kids
(+10 off resonance at 2mm)• FWHM: 17”• Pointing accuracy determination:
<2 arcsecond per detector• Array pointing accuracy: < 1arcsec
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Raw data
Raw data file necessary for Quick Look Analysis and instrument control
IDL routine transforming to fits file (Juan, Xavier)
Imported to IMBFITS (Albrecht, Robert) according to an agreed-upon format (doc)
Real-time of fits files was not available during the campaign
Fits files will be available during the next run and after each scan, via a C-program interfaced with data acquisition program
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Systematic effects
Common glitches– simultaneous, one sample affected, widely
varying intensity, seen on the off resonance ---> electronic cross-talk
plateau on Mars – ---> attributed to the same effect (cross talk)
Jumps in the data aligned in a straight oblique line on the 2 arrays drifting in time across the line – ---> A flying bug is a likely culprit. This occurs
rarely.No other jumps : the magnetic shield worked
wonders.
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Focal Plane Geometry
Linear fit to the expected position Mopsic method (Robert) IDL-based multi-beam fitter (Nicolas, Juan,
Alain)Polynomial distortion enoughLarger than expectedBeam width is larger than expectedBeam and distortion are correlated →
optical effect
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FPG kid position 4 scans
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FPG kid FWHM
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FPG optics
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Photometry
Relative photometryRf_dIdQ method provides a big
improvement with respect to 2010 runA new improved method based on
polynomial fitting using I, Q, dI, dQ is tested. – Cannot be real time, but after each scan
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3rd degree Polynomial
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3rd degree Polynomial
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Relative Photometry 10 hours later
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Absolute Photometry Calibrated on Uranus
Tau correction incorrect and based on taumeter (Xavier and Phil working on real time total power estimation of opacities)
Neptune, MWC349, quasars
Has been tested on the 18 and 19th Oct data
Compared with PdB (Samuel) or RJ for Uranus
Neptune
Neptune
3C84
MWC349
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Map making
In-house Real timeMopsic after-scan real timeoffline processing
– IDL custom routines (IPAG)– Blast-based routines (Cardiff)– IDL based noise decorrelation method (LPSC)– Selenepix (IAS)– Scanamorphos (IAP)
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M82
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Sky and Electronic noise Decorrelation
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Sensitivity
NFA 2mm Flux from final det avg is 9.5 +- 0.8 mJyNFB 1mm Flux from final det avg is 24.2 +- 7.6½ hour, 7 scans1
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Sensitivity
APM sourceNFA Flux from final det avg is 1.6 +- 0.6 mJyNFB Flux from final det avg is 1.2 +- 2.2
NEFD (mJy.s1/2 /beam) A&B 22.7 81.0Total Exposure Time (s) 3024Valid data integration time (and ratio with Exp Time) 2963 0.980Total Telescope time (and ratio with Exp Time) 4173 1.380
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2011 run #3, Spectral bandpasses(dot=run #2)