The Mid-Infrared Instrument for the<i>James Webb Space Telescope</i>, X: Operations and Data Reduction

Chen, C. H.; Anderson, Rachel E.; Azzollini, R.; Bergeron, Louis; Bouchet, P.; Bouwman, J.; Cracraft, M.; Fischer, Sebastian; Friedman, S. D.; García-Marín, M.; Glasse, Alistair; Glauser, Adrian M.; Goodson, G. B.; Greene, T. P.; Hines, Dean C.; Khorrami, M. A.; Lahuis, F.; Lajoie, Charles-Philippe; Meixner, Margaret; Morrison, J.; O’Sullivan, Brian; Pontoppidan, K. M.; Regan, Michael W.; Ressler, Michael E.; Rieke, G. H.; Scheithauer, S.; Walker, H. J.; Wright, Gillian

doi:10.1086/682260

Cited by 14 publications

(6 citation statements)

References 18 publications

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“…The data were reduced with the standard JWST calibration pipeline (data processing software ver.2022_2a, calibration software ver. 1.5.3;Gordon et al 2015;Bushouse et al 2022) and up-to-date reference files from the Calibration References Data System. The images in this work, including HST, are aligned to the Gaia Data Release 3 catalog (Gaia Collaboration et al 2016.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

GOALS-JWST: Unveiling Dusty Compact Sources in the Merging Galaxy IIZw096

Inami

Surace

Armus

et al. 2022

ApJL

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We have used the Mid-InfraRed Instrument (MIRI) on the James Webb Space Telescope (JWST) to obtain the first spatially resolved, mid-infrared images of IIZw096, a merging luminous infrared galaxy (LIRG) at z = 0.036. Previous observations with the Spitzer Space Telescope suggested that the vast majority of the total IR luminosity (L IR) of the system originated from a small region outside of the two merging nuclei. New observations with JWST/MIRI now allow an accurate measurement of the location and luminosity density of the source that is responsible for the bulk of the IR emission. We estimate that 40%–70% of the IR bolometric luminosity, or 3–5 × 1011 L ⊙, arises from a source no larger than 175 pc in radius, suggesting a luminosity density of at least 3–5 × 1012 L ⊙ kpc−2. In addition, we detect 11 other star-forming sources, five of which were previously unknown. The MIRI F1500W/F560W colors of most of these sources, including the source responsible for the bulk of the far-IR emission, are much redder than the nuclei of local LIRGs. These observations reveal the power of JWST to disentangle the complex regions at the hearts of merging, dusty galaxies.

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Section: Observations and Data Reductionmentioning

confidence: 99%

GOALS-JWST: Unveiling Dusty Compact Sources in the Merging Galaxy IIZw096

Inami

Surace

Armus

et al. 2022

ApJL

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“…• What is the minimum length of an integration? 5 groups is the recommended lower limit to obtain good flux calibration with the Space Telescope Science Institute (STScI) calibration pipeline 13 . 3 nonsaturated groups are the minimum number to achieve high-precision TSO (time series observations 14,15 ).…”

Section: Miri Observationmentioning

confidence: 99%

Observing recommendations for JWST MIRI users

Marín¹,

Rieke

Ressler

et al. 2018

Observatory Operations: Strategies, Processes, and Systems VII

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The Mid-Infrared Instrument (MIRI), a result of the collaborative work of a consortium of European and US institutes, is the only Mid-IR science instrument on the James Webb Space Telescope (JWST). The combination of MIRI s sensitivity and angular resolution over the 5-28.5 µm wavelength range will enable investigations into many different science topics, ranging from the local to the high-redshift Universe. The MIRI team has defined and published a set of "Recommended Strategies" to help observers optimally plan and execute their science programs. Some of these recommendations are generic and applicable to any science case; others are tailored to specific observing modes. Here we summarize key generic recommendations for MIRI observers, with emphasis on detector usage. All this information is available to observers as part of the James Webb Telescope User's Documentation System and will be updated as needed.

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“…13 It consists of four Integral Field Units working simultaneously (Gordon et al 2015). Consistent with Glasse et al (2015), the reference extended source detection limits 12 (10σ, 10,000 s) for the four channels are 1.8 × 10 −20 W m −2 / arcsec 2 (4.87  λ  7.76 μm; R ∼ 3500; FoV ∼ 3 0 × 3 9), 9.0×10 −21 W m −2 /arcsec 2 (7.45  λ  11.87 μm; R ∼ 2800; FoV ∼ 3 5 × 4 4), 5.0×10 −21 W m −2 /arcsec 2 (11.47  λ  18.24 μm; R ∼ 2700; FoV ∼ 5 2 × 6 2) and 1.9 × 10 −20 W m −2 /arcsec 2 (17.54  λ  28.82 μm; R ∼ 2200; FoV ∼ 6 7 × 7 7).…”

Section: Mrs Overviewmentioning

confidence: 99%

“…20 The minimum integration time available for the MRS is ∼30 s (SLOWMode readout time; Ressler et al 2015). In this paper we consider a minimum exposure time of 0.1 hr, because observations with a lower integration time would be very disadvantageous in term of overhead (see Table6 in Bouchet et al 2015; see also Gordon et al 2015) so we expect that it is unlikely they will be planned. Delvecchio et al (2014) on the basis of the same surveys, respectively.…”

Section: Pointed Observationsmentioning

confidence: 99%

Exploring the Evolution of Star Formation and Dwarf Galaxy Properties with JWST/MIRI Serendipitous Spectroscopic Surveys

Bonato

Sajina

Zotti

et al. 2017

ApJ

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The James Webb Space Telescope's Medium Resolution Spectrometer (MRS), will offer nearly two orders of magnitude improvement in sensitivity and >3× improvement in spectral resolution over our previous space-based mid-IR spectrometer, the Spitzer IRS. In this paper, we make predictions for spectroscopic pointed observations and serendipitous detections with the MRS. Specifically, pointed observations of Herschel sources require only a few minutes on source integration for detections of several star-forming and active galactic nucleus lines, out to z=3 and beyond. But the same data will also include tens of serendipitous 0z4 galaxies per field with infrared luminosities ranging ∼10 6 -10 13 L ☉ . In particular, for the first time and for free we will be able to explore the L IR <10 9 L ☉ regime out to z∼3. We estimate that with ∼ 100 such fields, statistics of these detections will be sufficient to constrain the evolution of the low-L end of the infrared luminosity function, and hence the star formation rate function. The above conclusions hold for a wide range in the potential low-L end of the IR luminosity function, and account for the PAH deficit in low-L, low-metallicity galaxies.

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The Mid-Infrared Instrument for theJames Webb Space Telescope, X: Operations and Data Reduction

Cited by 14 publications

References 18 publications

GOALS-JWST: Unveiling Dusty Compact Sources in the Merging Galaxy IIZw096

GOALS-JWST: Unveiling Dusty Compact Sources in the Merging Galaxy IIZw096

Observing recommendations for JWST MIRI users

Exploring the Evolution of Star Formation and Dwarf Galaxy Properties with JWST/MIRI Serendipitous Spectroscopic Surveys

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