IRAS Explanatory Supplement
IV. In-Flight Tests
B. Spectral Passband Verification
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- Verification of the Relative Consistency
- Verification of the Nominal Inband/Out-of-Band Transmission
The product of the transmission efficiency of the optical filter stack and the detector efficiency defines the effective wavelength passbands and the nominal out-of-band rejection performance of the detectors. This is described in Section II.C.5 and Tables II.C.4 and II.C.5. The detector passbands were verified before launch at the component level, but not at the system level. In-flight tests were performed to test the consistency of the passbands and out-of-band rejection within each band and to verify the nominal passbands. There was no direct in-orbit verification of the effective transmission characteristics of the detector/filter combination.
B. 1. Verification of the Relative Consistency
The consistency of the transmission characteristics within each band was checked by a two step procedure. First, all detectors were carefully calibrated relative to NGC 6543, which, for the purposes of this test, may be considered as a 150 K blackbody with spectral lines. The second step was to measure with each detector a number of sources with much hotter or colder spectral flux density distributions than NGC 6543.Numerically, the approach was to measure, in each wavelength band, the flux Si,j from test source i on detector j. The average of Si,j over the detectors in the wavelength band, <Si>, then gives the best estimate of the flux from the source in that wavelength band. The statistical distribution of the ratio
(IV.B.1)
The stars probe the short wavelength rejection and the short wavelength transmission cuton of the detectors in all bands. The two 50 K sources probe the longwave cutoff and longwave rejection in the 12 and 25 µm bands and the inband transmission of the 60 and 100 µm bands. Significant changes in the band pass characteristics of an individual detector relative to the band average transmission would be detectable as a statistically abnormal member of the Ri,j data set.
The results of this test indicate that deviations in the flux estimates from the mean are typically less than 10%, with a worst case value of 16%. Table IV.B.2 gives the typical and worst case value of the absolute deviation of Rij from unity in each band for the stars and the cold sources. In spite of their wide temperature range, there was no difference between the hottest and the coolest star.
B.2. Verification of the Nominal Inband/Out-of-band Transmission
The nominal response of the filter/detector combination and results of preflight tests at the component level are summarized in Section II.C.4. In-flight verification was required for two reasons. First, it was not possible to test fully the detector/filter combinations before the flight even at the component level. This applies in particular to the spectral response of the 100 µm detectors. Furthermore, a number of problems could have resulted in a degradation during system integration or during the flight.
Potential problems with the spectral response can be divided into two categories, those that represent systematic deviations from the nominal characteristics of all detectors in a band and those that result in a random scattering in one or several detectors in a band from the band average. Problems likely to result in random scattering are cracking or delamination of the filters, photon leaks around filter mounts etc. Extensive in-flight tests, described in the previous section, indicate that the detectors had rather similar passbands, thus eliminating random, but not necessarily systematic, effects.
An attempt was made to address the problem of systematic deviations of the nominal inband and out-of-band transmission of the four bands in a semi-quantitative way, by using observations of stars with widely different temperatures, asteroids and the planet Uranus to probe different portions of the passband.
| Hot test source | Cold test source | |||
|---|---|---|---|---|
 Vir, | B1 IV | Te=24000 K | Neptune | Te=55 K |
| CMa, | A1 V | Te=10000 K | ||
| Car, | F2 II | Te=6900 K | UGC11348 | Te=50 K |
 Peg, | M2.5 | Te=2800 K | ||
| |(Ri,j - 1)| | ||||
|---|---|---|---|---|
| Band | Stars | Planet/Galaxy | ||
| µm | Typical | Worst Case | Typical | Worst Case |
| 12 | 0.02 | 0.09 | * | * |
| 25 | 0.02 | 0.07 | 0.05 | 0.14 |
| 60 | 0.03 | 0.09 | 0.06 | 0.12 |
| 100 | 0.10 # | 0.13 # | 0.06 | 0.16 |
| * not detected | # low signal-to-noise ratio | |||
The following hardware related issues affect the various bands:
- 12 µm band: Rejection of 15-23 µm depends on an interference filter. A weak upper limit on the mean transmission in this region is based on the non-detection of Uranus in the 12 µm band.
- 60 µm band: Rejection shortward of 27 µm depends on a combination of blocking filters and the Ge:Ga detector response. Very high short wave blocking is required in the case of stars. Based on the semi-quantitative analysis of observations of hot stars, cool stars and asteroids, the shortwave blocking is consistent with the design specifications given in Section II.C.4.
- 100 µm band: Rejection shortward of 50 µm depends on a combination of blocking filters and the Ge:Ga detector response. The comments in 'b' above apply. The longwave cutoff is determined by the detector cutoff at approximately 120 µm. The detector response, including this cutoff was not measured on the actual flight detectors and the cutoff may vary a few microns from one detector to another.
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