The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope. IV. Aperture Masking Interferometry
- Creators
- Sivaramakrishnan, Anand
- Tuthill, Peter
- Lloyd, James P.
- Greenbaum, Alexandra Z.
- Thatte, Deepashri
- Cooper, Rachel A.
- Vandal, Thomas
- Kammerer, Jens
- Sanchez-Bermudez, Joel
- Pope, Benjamin J. S.
- Blakely, Dori
- Albert, Loïc
- Cook, Neil J.
- Johnstone, Doug
- Martel, André R.
- Volk, Kevin
- Soulain, Anthony
- Artigau, Étienne
- Lafrenière, David
- Willott, Chris J.
- Parmentier, Sébastien
- Ford, K. E. Saavik
- McKernan, Barry
- Vila, M. Begoña
- Rowlands, Neil
- Doyon, René
- Beaulieu, Mathilde
- Desdoigts, Louis
- Fullerton, Alexander W.
- De Furio, Matthew
- Goudfrooij, Paul
- Holfeltz, Sherie T.
- LaMassa, Stephanie
- Maszkiewicz, Michael
- Meyer, Michael R.
- Perrin, Marshall D.
- Pueyo, Laurent
- Sahlmann, Johannes
- Sohn, Sangmo Tony
- Teixeira, Paula S.
- Zheng, Sheng-hai
Abstract
The James Webb Space Telescope's Near Infrared Imager and Slitless Spectrograph (JWST-NIRISS) flies a 7-hole non-redundant mask (NRM), the first such interferometer in space, operating at 3–5 μm wavelengths, and a bright limit of ≃4 mag in W2. We describe the NIRISS Aperture Masking Interferometry (AMI) mode to help potential observers understand its underlying principles, present some sample science cases, explain its operational observing strategies, indicate how AMI proposals can be developed with data simulations, and how AMI data can be analyzed. We also present key results from commissioning AMI. Since the allied Kernel Phase Imaging (KPI) technique benefits from AMI operational strategies, we also cover NIRISS KPI methods and analysis techniques, including a new user-friendly KPI pipeline. The NIRISS KPI bright limit is ≃8 W2 (4.6 μm) magnitudes. AMI NRM and KPI achieve an inner working angle of ∼70 mas, which is well inside the ∼400 mas NIRCam inner working angle for its circular occulter coronagraphs at comparable wavelengths.
Additional Information
© 2023. The Astronomical Society of the Pacific. JWST is a partnership between NASA, ESA, and CSA. The NIRISS instrument was funded by the Canadian Space Agency and built in Canada by Honeywell. AS and AZG acknowledge support from the NSF, NASA, and the STScI Director's Discretionary Fund, J.S.B. acknowledges the full support from the CONACyT "Ciencia de Frontera" project CF-2019/263975, PGT is grateful for support from the Australian Research Council grant DP1801034089, and BJSP under DE21010163.Additional details
- Eprint ID
- 119905
- Resolver ID
- CaltechAUTHORS:20230308-468102500.10
- NSF
- NASA
- Canadian Space Agency (CSA)
- CF-2019/263975
- Consejo Nacional de Ciencia y Tecnología (CONACYT)
- DP1801034089
- Australian Research Council
- DE21010163
- BJSP
- European Space Agency (ESA)
- Space Telescope Science Institute
- Created
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2023-05-23Created from EPrint's datestamp field
- Updated
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2023-05-23Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)