Updates: 14.05.2012 (Korhan)
4.4 Mid/Far-IR
The Mid-Infrared Instrument (MIRI)
The Mid-Infrared Instrument (MIRI) on JWST will provide direct imaging and medium resolution spectroscopy (R~3000) over the wavelength range 5-28.3 micron. Coronagraphic imaging at 10.65, 11.4, 15.5 and 23 micron, and low resolution spectroscopy (R~100) over the wavelength range 5-10 micron. "MIRI" is expected to make significant contributions to all four of the primary science themes for JWST:
- Discovery of the "first light".
- Assembly of galaxies: history of star formation, growth of black holes, production of heavy elements.
- How stars and planetary systems form,
- Evolution of planetary systems and conditions for life.
MIRI will use the Lyman break technique to identify objects at increasing redshifts up to z = 30 or higher. More detailed follow-ups are being planned for the brightest first light source candidates by MIRI.
MIRI will use near-infrared spectroscopy at R = 100 will be needed to verify the photometric redshifts and will observe spectroscopic follow up at R = 1000 aimed at measuring the Balmer line intensities will provide star formation rates and estimates of the dust content. It's being planned to obtain high signal-to-noise, R = 1000, near-infrared spectra of QSOs or bright galaxies identified in other surveys.
Wide-Field Infrared Survey Explorer - WISE
MID-IR survey
Science
- Asteroids
- Brown Dwarfs
- AGNs
- Ultra-Luminous Galaxies
References
MIRI Science-Requirements
What can be done with DAG
- The DAG can study detect bright far objects or QSOs in a dedicated deep or ultra-deep survey and this can be provide a basis for MIRI.
- The DAG telescope can make spectroscopic follow-up observations in greater resolutions, if DAG has a high-resolution spectroscopic instrument in near-infrared.
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