Planck 2013 results. VII. HFI time response and beams

This paper characterizes the effective beams, the effective beam window functions and the associated errors for the Planck High Frequency Instrument (HFI) detectors. The effective beam is theangular response including the effect of the optics, detectors, data processing and the scan strategy. The wi...

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Published in:Astronomy and astrophysics (Berlin) 2014-11, Vol.571, p.1-31
Main Authors: Aghanim, N., Arnaud, M., Atrio-Barandela, F., Baccigalupi, C., Benabed, K., Bersanelli, M., Bock, J. J., Bond, J. R., Bridges, M., Burigana, C., Challinor, A., Chiang, H. C., Christensen, P. R., Colombi, S., Colombo, L. P. L., Curto, A., Cuttaia, F., Danese, L., de Bernardis, P., de Rosa, A., de Zotti, G., Delouis, J.-M., Désert, F.-X., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Efstathiou, G., Enßlin, T. A., Finelli, F., Frailis, M., Galeotta, S., Gratton, S., Gregorio, A., Hernández-Monteagudo, C., Herranz, D., Hivon, E., Holmes, W. A., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Laureijs, R. J., Lawrence, C. R., Leonardi, R., Leroy, C., Lesgourgues, J., Liguori, M., Lilje, P. B., López-Caniego, M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Mandolesi, N., Maris, M., Marshall, D. J., Masi, S., Matsumura, T., Matthai, F., Mendes, L., Mitra, S., Miville-Deschênes, M.-A., Morgante, G., Munshi, D., Netterfield, C. B., Noviello, F., Pajot, F., Paoletti, D., Pasian, F., Patanchon, G., Perdereau, O., Perrotta, F., Piacentini, F., Piat, M., Plaszczynski, S., Poutanen, T., Pratt, G. W., Prézeau, G., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Rocha, G., Roudier, G., Rusholme, B., Santos, D., Sauvé, A., Savini, G., Spencer, L. D., Starck, J.-L., Stolyarov, V., Sutton, D., Sygnet, J.-F., Tauber, J. A., Tristram, M., Tucci, M., Wandelt, B. D., Zacchei, A., Zonca, A.
Format: Article
Language:English
Subjects:
ASTRONOMY AND ASTROPHYSICS
Astrophysics
Beams (radiation)
cosmic background radiation
Cosmic microwave background
Cosmology and Extra-Galactic Astrophysics
cosmology: observations
Deconvolution
Detectors
Electronics
Error detection
Harmonics
Instrumentation and Methods for Astrophysic
instrumentation: detectors
Physics
Sciences of the Universe
surveys
Window functions
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Summary:This paper characterizes the effective beams, the effective beam window functions and the associated errors for the Planck High Frequency Instrument (HFI) detectors. The effective beam is theangular response including the effect of the optics, detectors, data processing and the scan strategy. The window function is the representation of this beam in the harmonic domain which is required to recover an unbiased measurement of the cosmic microwave background angular power spectrum. The HFI is a scanning instrument and its effective beams are the convolution of: a) the optical response of the telescope and feeds; b) the processing of the time-ordered data and deconvolution of the bolometric and electronic transfer function; and c) the merging of several surveys to produce maps. The time response transfer functions are measured using observations of Jupiter and Saturn and by minimizing survey difference residuals. The scanning beam is the post-deconvolution angular response of the instrument, and is characterized with observations of Mars. The main beam solid angles are determined to better than 0.5% at each HFI frequency band. Observations of Jupiter and Saturn limit near sidelobes (within 5°) to about 0.1% of the total solid angle. Time response residuals remain as long tails in the scanning beams, but contribute less than 0.1% of the total solid angle. The bias and uncertainty in the beam products are estimated using ensembles of simulated planet observations that include the impact of instrumental noise and known systematic effects. The correlation structure of these ensembles is well-described by five error eigenmodes that are sub-dominant to sample variance and instrumental noise in the harmonic domain. A suite of consistency tests provide confidence that the error model represents a sufficient description of the data. The total error in the effective beam window functions is below 1% at 100 GHz up to multipole ℓ ~ 1500, and below 0.5% at 143 and 217 GHz up to ℓ ~ 2000.
ISSN:0004-6361
1432-0746
1432-0756
DOI:10.1051/0004-6361/201321535