TOI processing

This Section kept with a low profile as this Planck release does not contain TOIs.

Overview

We describe here the how the TOIs are processed in order to be used for map production. We do not repeat the general features of the pipeline which are given in the HFI Data Processing article (REF). Here we give complementary explanations on some details. The TOI of each bolometer is processed independently of the other bolometers, so as to keep the noise properties as uncorrelated as possible. The processing involves modifying the TOI itself for what concerns the conversion to absorbed power and the correction of glitch tails. It also adds a flag TOI that masks the TOI samples that are not to be projected on maps for various reasons.

Input TOI

The input TOI consists in the AC modulated voltage output of the readout of each bolometer. The input has previously been decompressed, and converted from internal digital units to voltage via a constant factor. The TOI has a regular sampling at the acquisition frequency of facq=180.373700+-0.000050 Hz. There are almost no missing data in the TOIs, except for few hundred samples of 545 and 857GHz TOIs which are lost in the on-board compression due to saturation on the Galactic Center crossings.

General Pipeline Structure

The next figure shows how the initial ccTOI is transformed and how flags are produced:

A schematic of the TOI processing pipeline

Output TOIs and products

A TOI of clean calibrated samples (ccTOI) and a combined flag TOI (fTOI) are the outputs of the processing. The ccTOI is calibrated so as to represent the instantaneous power absorbed by the detector. It is worth mentioning how the ccTOI is changed with respect to the input TOI, beyond the harmless constant conversion factor from voltage to absorbed power. The demodulation stage allows to get the demodulated bolometer voltage. The non-linearity correction is a second-order polynomial correction based on the physical but static bolometer model. In order to avoid too much masking after glitches, a glitch tail is subtracted after an occurrence of a glitch in the TOI. Finally, the temporal response of the bolometer is deconvolved. This affects mostly the high-temporal frequency part of the TOI, although a small but significant low frequency tail is corrected too. Although flagged samples are not projected, their value influences the valid samples somehow. Hence interpolation procedures introduce some indirect modifications of the TOI. The flag TOI is a combination a dozen flags with an OR logic. Only unflagged data are projected. The exhaustive list of flags is given here: CompressionError, NoData, SSO, UnstablePointing, Glitch, BoloPlateFluctuation, RTS, Jump, PSBab. A complete qualification of the data is obtained at the ring level. If the TOI shows an anomalous behaviour during the duration of a ring, this ring is discarded from projection.

Trends in the output processing variables

Here we intend to show the trend of the systematic effects that are dealt with in the TOI processing

Noise stationarity

Noise power spectrum

rms per ring

Example of RTS detection

Flag description

Input flags

These flags are used as inputs to the TOI processing The point-source flag (PSflag) An earlier version of HFI point-source catalog is read back into a flag TOIs, at a given frequency. In practice, 5 sigma sources are masked within a radius of 1.3 FWHM > > gal flag : from apodized masks : /data/dmc/MISS03/DATA/DX5_MAP_GALACTIC_2048_masks/FREQ_galaxy_fsky_0.X0_apodised avec X = 7,7,8,9,9,9 a 100,143,217,353,545,857 GHz

> SSO flag : 4 toi, 4map, seen beam FWHM = 9,7,5,5,5,5 a 100,143,217,353,545,857 GHz

TOI : Mars, Jupiter, Saturn flagges a 2,3,3,4,4,4 FWHM

MAP : Mars, Jupiter, Saturn flagges a Factor_Source x NbBeam_freq FWHM avec Factor_per_Source1 = 1.1 (Mars) Factor_per_Source2 = 2.25 (Jupiter) Factor_per_Source3 = 1.25 (Saturn) NbBeam2Flag_list1 = 2.25 100 GHz NbBeam2Flag_list2 = 4.25 NbBeam2Flag_list3 = 4.0 NbBeam2Flag_list4 = 5.0 NbBeam2Flag_list5 = 6.0 857 GHz

en plus une petite queue pour prendre en compte la non deconvolution du signal de la planete interpolee par le signal "de fond" largeur = 10 % du diametre du flag principal Nb de SN flaggues en plus du flag principal = Factor_Source x AddSNafter1 AddSNafter1 = 10 100 GHz AddSNafter2 = 30 AddSNafter3 = 20 AddSNafter4 = 20 AddSNafter5 = 30 AddSNafter6 = 40 857 GHz

seen :

> > comment thermal decorr nettoie solar flare & elephant.

> Elephant dominent. Je prepare un joli plot de l'evolution de ce flag en fct du temps. en moyenne 3.3% des donnees mission nominale, 2,5% mission complete > > out flag = (avec et sans ps) --> identique pour bolos a & b Flag used for map making :

   UnstablePointing Flag OR FlagTOIproc OR SSOflag 4 map OR SSOflag seen
   FlagTOIproc = glitch OR saut OR flag template thermique

si PSB flag glitch = flag glitch A OR flag glitch B (car essentiellement des longs qui sont essentiellement simultanes A et B - meme si pas toujours a un niveau detectable. Flag utilise pour destriper : le meme avec en plus les sources ponctuelles

>