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

Trevor R. Fulton; David A. Naylor; Jean-Paul Baluteau; Matt Griffin; Peter Davis-Imhof; Bruce M. Swinyard; Tanya L. Lim; Christian Surace; Dave Clements; Pasquale Panuzzo; Rene Gastaud; Edward Polehampton; Steve Guest; Nanyao Lu; Arnold Schwartz; Kevin Xu

doi:10.1117/12.789850

Translator Disclaimer

12 July 2008 The data processing pipeline for the Herschel/SPIRE imaging Fourier Transform Spectrometer

Trevor R. Fulton, David A. Naylor, Jean-Paul Baluteau, Matt Griffin, Peter Davis-Imhof, Bruce M. Swinyard, Tanya L. Lim, Christian Surace, Dave Clements, Pasquale Panuzzo, Rene Gastaud, Edward Polehampton, Steve Guest, Nanyao Lu, Arnold Schwartz, Kevin Xu

Author Affiliations +

Proceedings Volume 7010, Space Telescopes and Instrumentation 2008: Optical, Infrared, and Millimeter; 70102T (2008) https://doi.org/10.1117/12.789850
Event: SPIE Astronomical Telescopes + Instrumentation, 2008, Marseille, France

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.

Citation Download Citation

Trevor R. Fulton, David A. Naylor, Jean-Paul Baluteau, Matt Griffin, Peter Davis-Imhof, Bruce M. Swinyard, Tanya L. Lim, Christian Surace, Dave Clements, Pasquale Panuzzo, Rene Gastaud, Edward Polehampton, Steve Guest, Nanyao Lu, Arnold Schwartz, and Kevin Xu "The data processing pipeline for the Herschel/SPIRE imaging Fourier Transform Spectrometer", Proc. SPIE 7010, Space Telescopes and Instrumentation 2008: Optical, Infrared, and Millimeter, 70102T (12 July 2008); https://doi.org/10.1117/12.789850

ACCESS THE FULL ARTICLE