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The SMILES Mid-Infrared Survey

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arxiv 2406.03518 v1 pith:WVUUYSBP submitted 2024-06-05 astro-ph.GA

The SMILES Mid-Infrared Survey

George Rieke , Stacey Alberts , Irene Shivaei , Jianwei Lyu , Christopher N. A. Willmer , Pablo Perez-Gonzalez , Christina C. Williams This is my paper
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keywords micronsmiriinstrumentjwstmid-infraredsmilessurveybands
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The Mid-Infrared Instrument (MIRI) for JWST is supplied with a suite of imaging bandpass filters optimized for full spectral coverage in eight intermediate-width bands from 5 to 26 microns and a narrower one at 11.3 microns. This contrasts with previous infrared space telescopes, which generally have provided only two broad bands, one near 10 microns and the other near 20 microns. The expanded MIRI spectral capability provides new possibilities for detailed interpretation of survey results. This is an important feature of the instrument, on top of its great increase in sensitivity and angular resolution over any previous mission. The Systematic Mid-infrared Instrument Legacy Extragalactic Survey (SMILES) was designed to take full advantage of this capability. This paper briefly describes the history of infrared surveys that paved the way for MIRI on JWST and for our approach to designng SMILES. It illustrates the use of the observations for a broad range of science programs, and concludes with a brief summary of the need for additional surveys with JWST/MIRI.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. PhotoIFU: NIRCam as a Photometric Integral Field Unit for Mapping Feedback in Galaxies

    astro-ph.GA 2026-07 conditional novelty 6.0

    PhotoIFU maps stellar mass, star-formation rate, dust, and metallicity pixel-by-pixel from JWST imaging, and finds gas-outflow regions are distinct from host galaxies in three z≈1.3–3.7 systems.

  2. Calibrating Photometric Mid-Infrared Star Formation Rates for JWST

    astro-ph.GA 2026-04 unverdicted novelty 4.0

    Rest-frame 6-8um MIRI luminosity provides broken power-law SFR calibrations with 0.2-0.3 dex scatter and UV+IR composites at 0.15 dex, supporting robust use above log M* ~9 up to z~3.