The infrared imaging spectrograph (IRIS) for TMT: overview of innovative science programs
- Creators
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Wright, Shelley A.
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Larkin, James E.
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Moore, Anna M.
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Do, Tuan
- Simard, Luc
- Ádámkovics, Máté
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Armus, Lee
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Barth, Aaron J.
- Barton, Elizabeth J.
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Boyce, Hope
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Cooke, Jeffrey
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Côté, Patrick
- Davidge, Timothy
- Ellerbroek, Brent
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Ghez, Andrea M.
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Liu, Michael C.
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Lu, Jessica R.
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Macintosh, Bruce
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Mao, Shude
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Marois, Christian
- Schoeck, Mathias
- Suzuki, Ryuji
- Tan, Jonathan C.
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Treu, Tommaso
- Wang, Lianqi
- Weiss, Jason
- IRIS Team
Abstract
IRIS (InfraRed Imaging Spectrograph) is a first light near-infrared diffraction limited imager and integral field spectrograph being designed for the future Thirty Meter Telescope (TMT). IRIS is optimized to perform astronomical studies across a significant fraction of cosmic time, from our Solar System to distant newly formed galaxies (Barton et al. [1]). We present a selection of the innovative science cases that are unique to IRIS in the era of upcoming space and ground-based telescopes. We focus on integral field spectroscopy of directly imaged exoplanet atmospheres, probing fundamental physics in the Galactic Center, measuring 10^4 to 10^(10) M_⊙ supermassive black hole masses, resolved spectroscopy of young star-forming galaxies (1 < z < 5) and first light galaxies (6 < z < 12), and resolved spectroscopy of strong gravitational lensed sources to measure dark matter substructure. For each of these science cases we use the IRIS simulator (Wright et al. [2], Do et al. [3]) to explore IRIS capabilities. To highlight the unique IRIS capabilities, we also update the point and resolved source sensitivities for the integral field spectrograph (IFS) in all five broadband filters (Z, Y, J, H, K) for the finest spatial scale of 0.004" per spaxel. We briefly discuss future development plans for the data reduction pipeline and quicklook software for the IRIS instrument suite.
Additional Information
© 2014 SPIE. The TMT Project gratefully acknowledges the support of the TMT collaborating institutions. They are the Association of Canadian Universities for Research in Astronomy (ACURA), the California Institute of Technology, the University of California, the National Astronomical Observatory of Japan, the National Astronomical Observatories of China and their consortium partners, and the Department of Science and Technology of India and their supported institutes. This work was supported as well by the Gordon and Betty Moore Foundation, the Canada Foundation for Innovation, the Ontario Ministry of Research and Innovation, the National Research Council of Canada, the Natural Sciences and Engineering Research Council of Canada, the British Columbia Knowledge Development Fund, the Association of Universities for Research in Astronomy (AURA), the U.S. National Science Foundation and the National Institutes of Natural Sciences of Japan.Attached Files
Published - Wright_2014p91479S.pdf
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Additional details
- Eprint ID
- 58434
- Resolver ID
- CaltechAUTHORS:20150623-085515363
- Gordon and Betty Moore Foundation
- Canada Foundation for Innovation
- Ontario Ministry of Research and Innovation
- National Research Council of Canada
- British Columbia Knowledge Development Fund
- Association of Universities for Research in Astronomy (AURA)
- NSF
- National Institutes of Natural Sciences of Japan
- Created
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2015-06-23Created from EPrint's datestamp field
- Updated
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2021-11-10Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)
- Series Name
- Proceedings of SPIE
- Series Volume or Issue Number
- 9147