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NIKA run#3 October 2011Report on data analysis

February 2012F.-Xavier Désert on behalf of the Nika team

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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)