Correcting the extended-source calibration for the Herschel SPIRE Fourier-transform spectrometer

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Valtchanov, I.
Hopwood, R.
Bendo, G.
Benson, Christopher S.
Conversi, L.
Fulton, T.
Griffin, M. J.
Joubaud, T.
Lim, T.
Lu, N.
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Oxford University Press
We describe an update to the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) Fourier-transform spectrometer (FTS) calibration for extended sources, which incorporates a correction for the frequency-dependent far-field feedhorn efficiency, ηff. This significant correction affects all FTS extended-source calibrated spectra in sparse or mapping mode, regardless of the spectral resolution. Line fluxes and continuum levels are underestimated by factors of 1.3–2 in the spectrometer long wavelength band (447–1018 GHz; 671–294 µm) and 1.4–1.5 in the spectrometer short wavelength band (944–1568 GHz; 318–191 µm). The correctionwasimplementedintheFTSpipelineversion14.1andhasalsobeendescribedinthe SPIRE Handbook since 2017 February. Studies based on extended-source calibrated spectra produced prior to this pipeline version should be critically reconsidered using the current products available in the Herschel Science Archive. Once the extended-source calibrated spectra are corrected for ηff, the synthetic photometry and the broad-band intensities from SPIRE photometer maps agree within 2–4percent – similar levels to the comparison of point-source calibrated spectra and photometry from point-source calibrated maps. The two calibration schemes for the FTS are now self-consistent: the conversion between the corrected extended-source and point-source calibrated spectra can be achieved with the beam solid angle and a gain correction that accounts for the diffraction loss.
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Instrumentation , Spectographs , Space vehicles , Instruments - Techniques , Spectroscopic
Valtchanov, I., Hopwood, R., Bendo, G., Benson, C., Conversi, L., Fulton, T., ...Wu, R. (2017). Correcting the extended-source calibration for the Herschel-SPIRE Fourier-transform spectrometer. Monthly Notices of the Royal Astronomical Society, 475(1), 321-330. doi:10.1093/mnras/stx3178