The Galactic magnetic field

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Table of contents

I Scientific context and PILOT instrument 
1 Scientific Context 
1.1 Infrared astronomy and polarization of light
1.1.1 Thermal emission
1.1.2 Polarization of an electromagnetic wave
1.2 Cosmic Microwave Background (CMB)
1.2.1 The Big Bang
1.2.2 Polarization of the CMB
1.2.3 Observational bias
1.3 The interstellar medium
1.3.1 The Galactic magnetic field
1.3.2 Interstellar dust
1.3.3 Thermal emission of dust
1.3.4 Polarized emission and extinction of galactic dust
1.4 Observations of polarized emission from dust
1.5 PILOT scientific objectives
2 PILOT instrument 
2.1 Description of the instrument
2.1.1 The gondola
2.1.2 Optics
2.1.3 The Half Wave Plate
2.1.4 Detectors
2.1.5 The cryostat
2.1.6 Filters
2.1.7 Internal Calibration Source (ICS)
2.1.8 House-Keeping Electronics
2.1.9 Stellar Sensor
2.2 Polarization measurement with PILOT
2.3 PILOT data format
2.3.1 Pilot Instrument MOdel (PIMO)
2.3.2 Data File Format
2.4 PILOT flights
2.4.1 First Flight
2.4.2 Second Flight
II Inflight performances PILOT 
3 Time constants 
3.1 Data-reading time delay
3.2 Time constant of the ICS
3.3 ICS ground tests
3.4 Glitches in-flight measurments.
3.4.1 Glitches detection method.
3.4.2 Time constant measurement.
3.5 ICS in-flight measurments
4 Pointing reconstruction 
4.1 Stellar sensor
4.2 Focal plane geometry
4.3 Sky Coordinates Calculations
4.3.1 Coordinate systems
4.3.2 Euler angles
4.3.3 Quaternions
4.3.4 From Euler Angles to quaternions.
4.3.5 Coordinates calculations
4.4 Issues in pointing reconstruction
4.5 Compact sources method
4.6 Maximum correlation method
4.7 The barycentric method
4.8 Preliminary pointing model
4.9 Coordinates versions
5 Noise properties 
5.1 Noise sources
5.1.1 Photon noise
5.1.2 Thermal noise
5.1.3 Johnson-Nyquist noise
5.1.4 Flicker noise
5.1.5 Readout noise
5.1.6 Environmental noise
5.2 Ground calibrations
5.3 Calculation of noise levels and power spectra
5.4 Noise levels and spatial distribution
5.5 Noise power spectra
5.6 Half-pixel difference noise power spectra
5.7 Temperature fluctuations at 300 mK
6 Response and Background of the detectors 
6.1 Background
6.1.1 Backgroung level
6.1.2 Background polarization
6.2 Responses
6.2.1 Temporal variations
6.2.2 Response Variations with Background
7 Optical quality 
7.1 Ground tests
7.2 In-flight PSF
7.3 Simulated PSF
III Map making 
8 Polarisation measurement 
8.1 Stokes parameters
8.2 Angles definition
8.3 Mueller matrices
8.4 Measurement and determination of Stokes parameters
9 Map-Making and preliminary results 
9.1 Map-making algorithms
9.1.1 Scanamorphos
9.1.2 ROMA
9.2 Data processing pipeline
9.2.1 Time constant deconvolution.
9.2.2 Deglitching
9.2.3 Atmospheric subtraction
9.2.4 Responses correction
9.3 Simulations
9.4 Preliminary results
9.4.1 I,Q,U maps
9.4.2 Polarisation angles
9.5 Work in progress.
Conclusions and perspectives (english version)
Conclusions et perspectives (version fran¸caise)
A Experimental Astronomy paper 
B SPIE conference paper