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Observational Prospect of NIREBL

Observational Prospect of NIREBL. ISAS/JAXA T. MATSUMOTO, S. MATSUURA, and T. WADA. Issues to be observed. Spectral shape Confirmation of the spectral gap at ~1 m m real? Other spectral features? Fluctuation Spatial correlation over the wide range of angular scale

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Observational Prospect of NIREBL

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  1. Observational Prospect of NIREBL ISAS/JAXA T. MATSUMOTO, S. MATSUURA, and T. WADA

  2. Issues to be observed • Spectral shape • Confirmation of the spectral gap at ~1mm real? • Other spectral features? • Fluctuation • Spatial correlation over the wide range of angular scale • Search for the large scale structure at high redshift • Absolute measurements • Avoid ambiguity of the model ZL • Rocket experiment • ASTRO-F • SPICA • Out of zodiacal cloud mission

  3. ASTRO-FFormation and evolution of galaxies, stars, and planets First dedicated infrared mission of ISAS 70cm cooled infrared telescope Advanced Infrared Survey 50 times higher sensitivity, 10 times better spatial resolution, has longer wavelength band, than IRAS Instruments IRC(Infrared Camera) 512x412 InSb array camera, 1.5”/pixel band imaging: K, L, and M bands low resolution spectroscopy: R-30 slit 2x50 pixel, R-15 4x50 pixel 256x256 SiAs array FIS(Far Infrared Surveyor) Launch target : August, 2005 Orbit : sun synchronous orbit, 750km altitude Mission life: ~1.5 year (liq. He holding time) + 2 years (dedicated to NIR Observations) ISAS/ESA collaboration: 10% of the pointing observations are opened to ESA scientists

  4. Observation of NIREBL with ASTRO-F • Advantages of IRC/ASTRO-F observation • Point-source rejection by high-resolution imaging observation • Limiting magnitude at the K band is ~20 mag. for one pointing obseravation (~10 min.) • This corresponds to ~30 nW m-2 sr-1 for 1 pixel (5s) • Almost all galactic stars and faint galaxies can be identified • Discrimination of the fluctuation of the zodiacal light • Observation of the same field at the different time epoch • Observation plans • 1. Detection of the NIREBLfluctuation over the wide range of angular scale • Wide area survey towards north ecliptic pole (NEP) is being proposed. • Coordination with galaxy deep survey group • 2. Detailed study of the spectrum of IREBL • Low resolution spectroscopy at different ecliptic latitudes (2~5mm) • Spectrum without contamination of stars and galaxies can be obtained • We welcome participation of theoreticians even in planning stage!

  5. IRC SURVEY STRATEGIES Depth and Area 1 10 1000 ? 100 0.02 100 Number of Pointings 10 1 Area (sq. deg.)

  6. Expected fluctuation and detection capability of IRC/ASTRO-F(Cooray et al., submitted to Ap.J.)

  7. IRC background measurements around NEP 1. Wide-band deep imaging in K, L and M bands * in unit of surface brightness (lIl) ** FOV of the IRC camera frame is 10’x10’ *** number of pixels available for the background analysis = total number of pixels – (confusion factor) x (number of galaxies) = 1.7x10^5 – (3pics x 3pics) x (number of galaxies) 2. Spectroscopy

  8. Out of zodiacal cloud mission Infrared observation without the zodiacal light provides decisive result for the NIREBL!

  9. Possible mission concept of out of zodiacal cloud mission! Scientific objectives Accurate measurement of spectrum and fluctuation of IREBL Instrumentation Telescope 5cm dia. lens system Wavelength range 0.8-2.2mm Pixel FOV ~10’ Detector HgCdTe Cooling system radiation cooling Weight 3 kg

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