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lämpömittari. Piitä lämpötilassa T bath < T c. Si 3 N 4 kerros ( lämpöeristys ). I bias. TES (Ti/Au/Bi). Nb. Nb. 300 m. R shunt. < 100 mK. Observatory, University of Helsinki ESA space science

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  1. lämpömittari Piitä lämpötilassaTbath<Tc Si3N4kerros (lämpöeristys) Ibias TES (Ti/Au/Bi) Nb Nb 300m Rshunt < 100 mK • Observatory, University of Helsinki • ESA space science • X-ray Evolving Universe Spectroscopy Mission (XEUS).Observatory coordinates instrument technology development in Finland for this future (launch 2014-15 ?) X-ray mission. Also participation in science planning. HESA TES X-ray microcalorimeter scheme • Sensitivity: ~10-18 erg cm-2 s-1 röntgen- säteilyä Terminen kytkentä absorbaattori lämpökylpy Transition Edge Sensor (TES) SQUID Change/evolution of plans: ESA-JAXA  NASA-ESA-JAXA (XEUS + Constellation-X) Back to upper level

  2. Observatory, University of Helsinki • ESA space science • Our share in XEUS (+ Constellation-X) plan NFI2 = TES microcalorimeter array • Collaboration with NL – Italy – UK - ... • Finnish group: UH/Obs. + VTT (+Univ. of Jyväskylä ? + companies ?) • SQUID readout array for the instrument by VTT • Science utilisation lämpömittari Piitä lämpötilassaTbath<Tc Si3N4kerros (lämpöeristys) Ibias TES (Ti/Au/Bi) Nb Nb 300m Rshunt < 100 mK HESA TES X-ray microcalorimeter röntgen- säteilyä Terminen kytkentä absorbaattori lämpökylpy Transition Edge Sensor (TES) SQUID Back to upper level

  3. NFI2/TES-based micro-calorimeter specifications/features Field coverage: 32 arcsec Number of pixels: 32x32 Pixel size: 1 arcsec (= 240 micron) Energy range: 0.5 - 15 keV energy resolution (FWHM): 2 eV @ 1 keV, 5 eV @ 7 keV Detection efficiency: 95% for 1-7 keV Count rate limit: 250 c/s/pixel Effective time constant: 0.1 ms • TELESCOPE AND S/C FEATURES Telescope effective area: ~ 10 m2 @ 1 keV, ja ~ 3 m2 @ 7 keV Angular resolution: 2-5 arcsec (HEW). Also: XEUS orbital plan changed: L2-point instead of LEO HESA Back to upper level

  4. More specifically in XEUS context and plans HESA • Evolution of large-scale structure – probing dark matter and energy • Coeval growth of galaxies and their supermassive black holes • Gravity in the strong field limit • what else can be done ? Back to upper level

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