Planckearly results. VI. The High Frequency Instrument data processing

Abstract

We describe the processing of the 336 billion raw data samples from the High Frequency Instrument (HFI) which we performed to produce six temperature maps from the first 295 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545 and 857 GHz with an angular resolution ranging from 9.9 to 4.4 . The white noise level is around 1.5 μK degree or less in the 3 main CMB channels (100-217 GHz). The photometric accuracy is better than 2% at frequencies between 100 and 353 GHz and around 7% at the two highest frequencies. The maps created by the HFI Data Processing Centre reach our goals in terms of sensitivity, resolution, and photometric accuracy. They are already sufficiently accurate and well-characterised to allow scientific analyses which are presented in an accompanying series of early papers. At this stage, HFI data appears to be of high quality and we expect that with further refinements of the data processing we should be able to achieve, or exceed, the science goals of the Planck project.

Cloud Structure of Three Galactic Infrared Dark Star-forming Regions from Combining Ground- and Space-based Bolometric Observations

“…For our combination purpose, we use the Herschel SPIRE extended emission products from the data base. The Planck353 GHz images, which are in units of K CMB ,are converted to Jy beam −1 (Planck HFI Core Team et al 2011aTeam et al , 2011bZacchei et al 2011). …”

Search for C ii emission on cosmological scales at redshift Z ∼ 2.6

“…The Low-Frequency Instrument (LFI) (Bersanelli et al 2010;Mennella et al 2011) implements pseudo-correlation radiometers to observe over 3 frequency channels at 30, 40 and 70 GHz. The High-Frequency Instrument (HFI) (Lamarre et al 2010;Planck HFI Core Team et al 2011) uses bolometers and observes over 6 frequency channels at 100,143,217,353,545,and 857 GHz. We use the 545 GHz intensity map to trace the redshifted C ii intensity over the sky, while additionally using the 353 and 857 GHz maps to constrain the CIB and SZ emission and clustering. The maps have beam full-widths at half-maximum (FWHMs) of the order of a few arcmin.…”

“…In this paper, we measure the intensity of C ii diffuse emission by performing an Monte Carlo Markov Chain (MCMC) analysis fitting for C ii and cosmic infrared background (CIB) emission jointly using cross-correlations between high-frequency intensity maps with LSS tracers. Specifically, we measure angular cross-power spectra of overdensity maps of both spectroscopic quasars at redshift z = 2.6 and CMASS galaxies at redshift z = 0.57 from the SDSS-III Baryon Oscillations Spectroscopic Survey (BOSS) (Eisenstein et al 2011) with the {353, 545, 857} GHz intensity maps from the Planck satellite (Lamarre et al 2010;Planck HFI Core Team et al 2011) to fit jointly for the C ii intensity and 3 CIB parameters. The spectroscopic quasars are limited to redshifts z = 2 − 3.2, which comprise the redshift range of C ii emission within the 545 GHz band, while the redshifts of the CMASS galaxies are too low to correlate with C ii emission in the Planck maps.…”

Bicep2. Ii. Experiment and Three-Year Data Set

“…We have simulated the effect of cosmological T E correlations as a bias on the beam centers and find it well below 5 . The same beam-fitting procedure has been repeated with Planck 143 GHz maps (Planck Collaboration et al 2013b;Planck HFI Core Team et al 2011) instead of WMAP templates. The results are identical to within 15 for all Bicep2 detectors.…”