In-orbit performance of Herschel-HIFI
By P. Roelfsema, F. Helmich, D. Teyssier, V. Ossenkopf, P. Morris, M. Olberg, R. Shipman, C. Risacher, M. Akyilmaz, R. Assendorp and 89 more. 2012
219 citations recorded by the source corpus.
Aims. In this paper the calibration and in-orbit performance of the Heterodyne Instrument for the Far-Infrared (HIFI) is described. Methods. The calibration of HIFI is based on a combination of ground and in-flight tests. Dedicated ground tests to determine those instrument parameters that can only be measured accurately using controlled laboratory stimuli were carried out in the instrument level test (ILT) campaign. Special in-flight tests during the commissioning phase (CoP) and performance verification (PV) allowed the determination of the remaining instrument parameters. The various instrument observing modes, as specified in astronomical observation templates (AOTs), were validated in parallel during PV by observing selected celestial sources. Results. The initial calibration and in-orbit performance of HIFI has been established. A first estimate of the calibration budget is given. The overall in-flight instrument performance agrees with the original specification. Issues remain at only a few frequencies.
Subfields: Astronomy and Astrophysics, Spectroscopy
View Paper: https://www.semanticscholar.org/paper/7f9b8d1de8b0860a333ce3335a291b2650112396
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Citations in the corpus
- FIRST DETECTION OF WATER VAPOR IN A PRE-STELLAR CORE (2012, methodology): “…within the GILDAS package:16 the line intensity units were converted from antenna to brightness temperature (TB) using a beam efficiency of 0.76 (Roelfsema et al. 2012); the H and V spectra were analyzed individually and found similar within the noise (therefore, the two spectra were averaged).”
- A Herschel [C ii] Galactic plane survey - I. The global distribution of ISM gas components (2013, methodology): “We applied a main-beam efficiency of 0.72 to transform the data 2 http://www.iram.fr/IRAMFR/GILDAS from an antenna temperature to a main-beam temperature scale (Roelfsema et al. 2012).”
- Water in star-forming regions with Herschel (WISH). II. Evolution of 557 GHz 110-101 emission in low-mass protostars (2012, methodology): “Figure 7 shows the correlation between ∫ TMB d /(Tpeak × Δ (25”