Time series observations with the mid-infrared instrument (MIRI) on JWST
Wright, Gillian S.
Garcia Marin, Macarena
Batalha, Natalie M.
Bean, Jacob L.
Stevenson, Kevin B.
AffiliationUniv Arizona, Steward Observ
MetadataShow full item record
PublisherSPIE-INT SOC OPTICAL ENGINEERING
CitationSarah Kendrew, Daniel Dicken, Jeroen Bouwman, Macarena Garcia Marin, Thomas P. Greene, Pierre-Olivier Lagage, Mike Ressler, Nicolas Crouzet, Laura Kreidberg, Natalie M. Batalha, Jacob L. Bean, Kevin B. Stevenson, Alistair Glasse, Gillian S. Wright, and George H. Rieke "Time series observations with the mid-infrared instrument (MIRI) on JWST", Proc. SPIE 10698, Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, 106983U (6 July 2018); doi: 10.1117/12.2313951; https://doi.org/10.1117/12.2313951
Rights© (2018) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE).
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractTime-variable phenomena such as transiting exoplanets will be a major science theme for the James Webb Space Telescope (JWST). For Guaranteed Time and Early Release Science Observations, over 500 hours of JWST time have been allocated to time series observations (TSOs) of transiting exoplanets. Several dedicated observing modes are available in the instrument suite, whose operations are specifically tailored to these challenging observations. MIRI, the only JWST instrument covering the wavelength range longwards of 5 mu m on JWST, will offer TSOs in two of its modes: the low resolution spectrometer, and the imager. In this paper we will describe these modes for MIRI, and discuss how they differ operationally from regular (non-TSO) observations. We will show performance estimates based on ground testing and modeling, discuss the most relevant detector effects for high precision (spectro-)photometry, and provide some guidelines for planning MIRI TSOs.
VersionFinal published version