The data processing pipeline for the Herschel SPIRE Fourier Transform Spectrometer

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dc.contributor.authorFulton, T.
dc.contributor.authorNaylor, David A.
dc.contributor.authorPolehampton, E. T.
dc.contributor.authorValtchanov, I.
dc.contributor.authorHopwood, R.
dc.contributor.authorLu, N.
dc.contributor.authorBaluteau, J.-P.
dc.contributor.authorMainetti, G.
dc.contributor.authorPearson, C.
dc.contributor.authorPapageorgiou, A.
dc.contributor.authorGuest, S.
dc.contributor.authorZhang, L.
dc.contributor.authorImhof, P.
dc.contributor.authorSwinyard, B. M.
dc.contributor.authorGriffin, M. J.
dc.contributor.authorLim, T. L.
dc.date.accessioned2019-12-13T03:15:51Z
dc.date.available2019-12-13T03:15:51Z
dc.date.issued2016
dc.descriptionSherpa Romeo green journal. Permission to archive final published versionen_US
dc.description.abstractWe present the data processing pipeline to generate calibrated data products from the Spectral and Photometric Imaging Receiver (SPIRE) imaging Fourier Transform Spectrometer on the Herschel Space Observatory. The pipeline processes telemetry from SPIRE observations and produces calibrated spectra for all resolution modes. The spectrometer pipeline shares some elements with the SPIRE photometer pipeline, including the conversion of telemetry packets into data timelines and calculation of bolometer voltages. We present the following fundamental processing steps unique to the spectrometer: temporal and spatial interpolation of the scan mechanism and detector data to create interferograms; Fourier transformation; apodization; and creation of a data cube. We also describe the corrections for various instrumental effects including first- and second-level glitch identification and removal, correction of the effects due to emission from the Herschel telescope and from within the spectrometer instrument, interferogram baseline correction, temporal and spatial phase correction, non-linear response of the bolometers, and variation of instrument performance across the focal plane arrays. Astronomical calibration is based on combinations of observations of standard astronomical sources and regions of space known to contain minimal emission.en_US
dc.description.peer-reviewYesen_US
dc.identifier.citationFulton, T., Naylor, D. A., Polehampton, E. T., Valtchanov, I., Hopwood, R., Lu, N., ... Lim, T. L. (2016). The data processing pipeline for the Herschel SPIRE Fourier Transform Spectrometer. Monthly Notices of the Royal Astronomical Society, 458(2), 1977-1989. doi:10.1093/mnras/stw343en_US
dc.identifier.urihttps://hdl.handle.net/10133/5627
dc.language.isoen_USen_US
dc.publisherOxford University Pressen_US
dc.publisher.departmentDepartment of Physics and Astronomyen_US
dc.publisher.facultyArts and Scienceen_US
dc.publisher.institutionUniversity of Lethbridgeen_US
dc.publisher.institutionBlue Sky Spectroscopyen_US
dc.publisher.institutionRutherford Appleton Laboratoryen_US
dc.publisher.institutionHerschel Science Centreen_US
dc.publisher.institutionImperial College Londonen_US
dc.publisher.institutionChinese Academy of Sciencesen_US
dc.publisher.institutionNASA Herschel Science Centreen_US
dc.publisher.institutionUniversité d'Aix-Marseilleen_US
dc.publisher.institutionCardiff Universityen_US
dc.publisher.institutionUniversity College Londonen_US
dc.publisher.urlhttps://doi.org/10.1093/mnras/stw343en_US
dc.subjectMethodsen_US
dc.subjectData analysis - Space vehiclesen_US
dc.subjectInstruments - Techniquesen_US
dc.subjectSpectroscopicen_US
dc.subject.lcshFourier transform spectroscopy
dc.subject.lcshHerschel Space Observatory (Spacecraft)
dc.titleThe data processing pipeline for the Herschel SPIRE Fourier Transform Spectrometeren_US
dc.typeArticleen_US
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