Planck early results. V. The low frequency instrument data processing

We describe the processing of data from the Low Frequency Instrument (LFI) used in production of the Planck Early Release Compact Source Catalogue (ERCSC). In particular, we discuss the steps involved in reducing the data from telemetry packets to cleaned, calibrated, time-ordered data (TOD) and fre...

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Detalles Bibliográficos
Autores: Zacchei, A., Maino, D., Baccigalupi, C., Bersanelli, M., Bonaldi, A., Bonavera, L., Burigana, C., Butler, R. C., Cuttaia, F., De Zotti, G., Dick, J., Frailis, M., López-Caniego Alcarria, Marcos, Barreiro Vilas, Rita Belén|||0000-0002-6139-4272, Cruz Rodríguez, Marcos|||0000-0002-4767-530X, Curto Martín, Andrés, Diego Rodríguez, José María|||0000-0001-9065-3926, Herranz Muñoz, Diego|||0000-0003-4540-1417, Martínez González, Enrique, Vielva Martínez, Patricio|||0000-0003-0051-272X
Tipo de recurso: artículo
Fecha de publicación:2011
País:España
Institución:Universidad de Cantabria (UC)
Repositorio:UCrea Repositorio Abierto de la Universidad de Cantabria
Idioma:inglés
OAI Identifier:oai:repositorio.unican.es:10902/28453
Acceso en línea:https://hdl.handle.net/10902/28453
Access Level:acceso abierto
Palabra clave:Methods: data analysis
Cosmic background radiation
Cosmology: observations
Surveys
Descripción
Sumario:We describe the processing of data from the Low Frequency Instrument (LFI) used in production of the Planck Early Release Compact Source Catalogue (ERCSC). In particular, we discuss the steps involved in reducing the data from telemetry packets to cleaned, calibrated, time-ordered data (TOD) and frequency maps. Data are continuously calibrated using the modulation of the temperature of the cosmic microwave background radiation induced by the motion of the spacecraft. Noise properties are estimated from TOD from which the sky signal has been removed using a generalized least square map-making algorithm. Measured 1/f noise knee-frequencies range from ~100 mHz at 30 GHz to a few tens of mHz at 70GHz. A destriping code (Madam) is employed to combine radiometric data and pointing information into sky maps, minimizing the variance of correlated noise. Noise covariance matrices required to compute statistical uncertainties on LFI and Planck products are also produced. Main beams are estimated down to the ??10dB level using Jupiter transits, which are also used for geometrical calibration of the focal plane.

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