The Infrared Imaging Spectrograph (IRIS) for TMT: final design development of the data reduction system
- Creators
- Surya, Arun
- Zonca, Andrea
- Rundquist, Nils-Erik
- Wright, Shelley A.
- Walth, Gregory L.
- Anderson, David
- Chapin, Edward
- Chisholm, Eric
- Do, Tuan
- Dunn, Jennifer
- Gillies, Kim
- Hayano, Yutaka
- Johnson, Chris
- Kupke, Renate
- Larkin, James
- Nakamoto, Takashi
- Riddle, Reed
- Smith, Roger
- Suzuki, Ryuji
- Sohn, Ji Man
- Weber, Robert
- Weiss, Jason
- Zhang, Kai
- Others:
- Guzman, Juan C.
- Ibsen, Jorge
Abstract
IRIS (Infrared Imaging Spectrograph) is the near-infrared (0.84 to 2.4 micron) diffraction-limited imager and Integral Field Spectrograph (IFS) designed for the Thirty Meter Telescope (TMT) and the Narrow-Field Infrared Adaptive Optics System ( NFIRAOS ). The imager will have a 34 arcsec x 34 arcsec field of view with 4 milliarcseconds (mas) pixels. The IFS consists of a lenslet array and slicer, enabling four plate scales from 4 mas to 50 mas, with multiple gratings and filters. We will report the progress on the development of the IRIS Data Reduction System ( DRS ) in the final design phase. The IRIS DRS is being developed in Python with the software architecture based on the James Webb Space Telescope science calibration pipeline. We are developing a library of algorithms as individual Python classes that can be configured independently and bundled into pipelines. We will interface this with the observatory software to run online during observations and we will release the package publicly for scientists to develop custom analyses. It also includes a C library for readout processing to be used for both in real-time processing (e.g., up-the-ramp, MCDS) as well the ability for astronomers to use for offline reduction. Lastly, we will also discuss the development of the IRIS simulation packages that simulate raw spectra and image readout-data from the Hawaii-4RG detectors, which helps in developing reduction algorithms during this design phase.
Additional Information
© 2020 Society of Photo-Optical Instrumentation Engineers (SPIE). The TMT Project gratefully acknowledges the support of the TMT collaborating institutions. They are 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, the Department of Science and Technology of India and their supported institutes, and the National Research Council of Canada. 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 Natural Sciences and Engineering Research Council of Canada, the British Columbia Knowledge Development Fund, the Association of Canadian Universities for Research in Astronomy (ACURA) , the Association of Universities for Research in Astronomy (AURA), the U.S. National Science Foundation, the National Institutes of Natural Sciences of Japan, and the Department of Atomic Energy of India.Attached Files
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Additional details
- Eprint ID
- 107239
- Resolver ID
- CaltechAUTHORS:20201221-120012677
- TMT partner institutions
- Created
-
2020-12-21Created from EPrint's datestamp field
- Updated
-
2021-11-16Created from EPrint's last_modified field
- Caltech groups
- Thirty Meter Telescope
- Series Name
- Proceedings of SPIE
- Series Volume or Issue Number
- 11452