Optical technologies in ESA programmes - Congrex
Optical technologies in ESA programmes - Congrex
Optical technologies in ESA programmes - Congrex
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European contribution: SAFARI<br />
1.<br />
2.<br />
3.<br />
4.<br />
5.<br />
6.<br />
7.<br />
Cryogenic imag<strong>in</strong>g spectrometer (FTS, 35 - 210 um).<br />
Herschel class <strong>in</strong>strument (c.f. SPIRE, PACS).<br />
Cold assembly < 50 kg (IOB). Warm electronics < 30 kg (SVM).<br />
Selection of detector technology impacts design (~ 6000 px:<br />
TES, KID, Si bolometers, Photo-cond.); planned by mid 2010).<br />
Phase A study conducted assum<strong>in</strong>g adoption of TES.<br />
Additional <strong>in</strong>ternal cooler required by TES, KID and Si-<br />
Bolometer (Sorption Cooler + ADR � ~ 100 mK).<br />
PFM delivery to JAXA required by end 2015.<br />
CRITICAL AREAS:<br />
1. Detector array and read-out electronics development<br />
(compet<strong>in</strong>g: KID, TES, Si-Bolometers, Photoconductors � key<br />
decision by mid-2010).<br />
2. Internal cooler (~100 mK, SC+ADR, unless PC’s selected).<br />
3. FTS scann<strong>in</strong>g mechanism (operat<strong>in</strong>g <strong>in</strong> cryo conditions).<br />
4. Constra<strong>in</strong>ed mass and cool<strong>in</strong>g power resources.<br />
5. Compressed development schedule (FM by 2015).<br />
Optics <strong>in</strong> <strong>ESA</strong> <strong>programmes</strong> | Roland Meynart | ICSO �ό��� 2010 | 05 October 2010 | Earth Observation | Slide 48
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