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Published July 12, 2008 | Published
Book Section - Chapter Open

The data processing pipeline for the Herschel/SPIRE imaging Fourier Transform Spectrometer

Abstract

We present the data processing pipeline to generate calibrated data products from the Spectral and Photometric Imaging Receiver (SPIRE) imaging Fourier Transform Spectrometer. The pipeline processes telemetry from SPIRE point source, jiggle- and raster-map observations, producing calibrated spectra in low-, medium-, high-, and mixed low- and highresolution modes. The spectrometer pipeline shares some elements with the SPIRE photometer pipeline, including the conversion of telemetry packets into data timelines and the calculation of bolometer voltages from the raw telemetry. We present the following fundamental processing steps unique to the spectrometer: temporal and spatial interpolation of the stage mechanism and detector data to create interferograms; apodization; Fourier transform, and creation of a hyperspectral data cube. We also describe the corrections for various instrumental effects including first- and secondlevel glitch identification and removal, correction of the effects due to the Herschel primary mirror and the spectrometer calibrator, interferogram baseline correction, channel fringe correction, temporal and spatial phase correction, non-linear response of the bolometers, variation of instrument performance across the focal plane arrays, and variation of spectral efficiency. Astronomical calibration is based on combinations of observations of standard astronomical sources and regions of space known to contain minimal emission.

Additional Information

© 2008 Society of Photo-Optical Instrumentation Engineers (SPIE). The authors wish to acknowledge Andres Rebolledo, Peter Kennedy, Zhaohan Weng, Yan He, Karim Ali, Yu Wai Wong, and Alim Harji for their contributions to the development of the SPIRE spectrometer data processing modules. The authors would also like to thank Christophe Ordenovic and Dominique Benielli for their contributions to the first level deglitching and Telescope/SCAL corrections. The figures that show the SPIRE astronomical footprint for the different spatial sampling modes were provided by Ivan Valtchanov. The funding for the Canadian contribution to SPIRE was provided by the Canadian Space Agency and NSERC.

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