The Mid-infrared Instrument for JWST and Its In-flight Performance

Wright, Gillian; Rieke, G. H.; Glasse, Alistair; Ressler, Michael E.; Marín, Macarena García; Aguilar, Jonathan; Alberts, Stacey; Álvarez-Márquez, J.; Argyriou, Ioannis; Banks, Kimberly C.; Baudoz, Pierre; Boccaletti, A.; Bouchet, P.; Bouwman, J.; Brandl, Bernhard R.; Breda, David; Bright, Stacey N.; Cale, Steven; Colina, L.; Cossou, Christophe; Coulais, A.; Cracraft, M.; Meester, W. De; Dicken, D.; Engesser, Michael; Etxaluze, M.; Fox, O.; Friedman, S. D.; Fu, Henry; Gasman, Danny; Gáspár, András; Gastaud, R.; Geers, V. C.; Glauser, Adrian M.; Gordon, K. D.; Greene, Thomas P.; Greve, T. R.; Grundy, Timothy; Guêdel, M.; Guillard, P.; Haderlein, Peter; Hashimoto, Ryan; Henning, Thomas; Hines, Dean C.; Holler, Bryan J.; Detre, Örs Hunor; Jahromi, Amir; James, Bryan; Jones, O. C.; Justtanont, K.; Kavanagh, Patrick; Kendrew, Sarah; Klaassen, Pamela; Krause, O.; Labiano, Á.; Lagage, Pierre-Olivier; Lambros, Scott; Larson, Kirsten L.; Law, David R.; Lee, David; Libralato, Mattia; Alverez, Jose Lorenzo; Meixner, Margaret; Morrison, J.; Mueller, M.; Murray, Katherine T.; Mycroft, Matthew; Myers, Richard; Nayak, Omnarayani; Naylor, B. J.; Nickson, Bryony; Noriega-Crespo, A.; Östlin, Göran; O’Sullivan, Brian; Ottens, Richard; Patapis, Polychronis; Penanen, Konstantin; Pietraszkiewicz, Martin; Ray, T. P.; Regan, Michael W.; Roteliuk, Anthony; Royer, P.; Samara-Ratna, Piyal; Samuelson, Bridget; Sargent, Benjamin; Scheithauer, S.; Schneider, Analyn; Schreiber, J.; Shaughnessy, Bryan; Sheehan, Even; Shivaei, Irene; Sloan, G. C.; Tamás, László; Teague, Kelly; Temim, Tea; Tikkanen, Tuomo; Tustain, Samuel; Dishoeck, Ewine van; Vandenbussche, B.; Weilert, M.; Whitehouse, Paul; Wolff, Schuyler

doi:10.1088/1538-3873/acbe66

Cited by 92 publications

(58 citation statements)

References 50 publications

(35 reference statements)

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“…Recently, JWST/MIRI (Wright et al 2023) secondary eclipse measurements were used to provide the first observational constraints on whether or not the two innermost planets, TRAPPIST-1 b and c, had atmospheres (Greene et al 2023;Ih et al 2023;Zieba et al 2023). These studies complement previous efforts to use secondary eclipse measurements to probe atmospheric composition and thickness on hot rocky exoplanets (Kreidberg et al 2019;Crossfield et al 2022;Whittaker et al 2022).…”

Section: Introductionmentioning

confidence: 82%

Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm

Lincowski,

Meadows,

Zieba

et al. 2023

ApJL

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The first James Webb Space Telescope observations of TRAPPIST-1 c showed a secondary eclipse depth of 421 ± 94 ppm at 15 μm, which is consistent with a bare rock surface or a thin, O2-dominated, low-CO2 atmosphere. Here we further explore potential atmospheres for TRAPPIST-1 c by comparing the observed secondary eclipse depth to synthetic spectra of a broader range of plausible environments. To self-consistently incorporate the impact of photochemistry and atmospheric composition on atmospheric thermal structure and predicted eclipse depth, we use a two-column climate model coupled to a photochemical model and simulate O2-dominated, Venus-like, and steam atmospheres. We find that a broader suite of plausible atmospheric compositions are also consistent with the data. For lower-pressure atmospheres (0.1 bar), our O2–CO2 atmospheres produce eclipse depths within 1σ of the data, consistent with the modeling results of Zieba et al. However, for higher-pressure atmospheres, our models produce different temperature–pressure profiles and are less pessimistic, with 1–10 bar O2, 100 ppm CO2 models within 2.0σ–2.2σ of the measured secondary eclipse depth and up to 0.5% CO2 within 2.9σ. Venus-like atmospheres are still unlikely. For thin O2 atmospheres of 0.1 bar with a low abundance of CO2 (∼100 ppm), up to 10% water vapor can be present and still provide an eclipse depth within 1σ of the data. We compared the TRAPPIST-1 c data to modeled steam atmospheres of ≤3 bars, which are 1.7σ–1.8σ from the data and not conclusively ruled out. More data will be required to discriminate between possible atmospheres or more definitively support the bare rock hypothesis.

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Section: Introductionmentioning

confidence: 82%

Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm

Lincowski,

Meadows,

Zieba

et al. 2023

ApJL

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“…The complete details of the CEERS program will be presented in Finkelstein et al (2023, in preparation), and the program data can be found at doi:10.17909/z7p0-8481 and at https:// archive.stsci.edu/hlsp/ceers. This source is one of the first to be observed and published with four JWST (Gardner et al 2023) observing modes: NIRSpec (Böker et al 2023), NIRCam (Rieke et al 2023), MIRI (Wright et al 2023), and NIRCam/ Wide-Field Slitless Spectrograph, or WFSS (Greene et al 2017). We describe these observations below and provide a summary of information about this source in Table 1.…”

Section: Datamentioning

confidence: 99%

A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars

Larson,

Finkelstein,

Kocevski

et al. 2023

ApJL

100

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We report the discovery of an accreting supermassive black hole at z = 8.679. This galaxy, denoted here as CEERS_1019, was previously discovered as a Lyα-break galaxy by Hubble with a Lyα redshift from Keck. As part of the Cosmic Evolution Early Release Science (CEERS) survey, we have observed this source with JWST/NIRSpec, MIRI, NIRCam, and NIRCam/WFSS and uncovered a plethora of emission lines. The Hβ line is best fit by a narrow plus a broad component, where the latter is measured at 2.5σ with an FWHM ∼1200 km s−1. We conclude this originates in the broadline region of an active galactic nucleus (AGN). This is supported by the presence of weak high-ionization lines (N V, N IV], and C III]), as well as a spatial point-source component. The implied mass of the black hole (BH) is log (M BH/M ⊙) = 6.95 ± 0.37, and we estimate that it is accreting at 1.2 ± 0.5 times the Eddington limit. The 1–8 μm photometric spectral energy distribution shows a continuum dominated by starlight and constrains the host galaxy to be massive (log M/M⊙ ∼9.5) and highly star-forming (star formation rate, or SFR ∼ 30 M⊙ yr−1; log sSFR ∼ − 7.9 yr−1). The line ratios show that the gas is metal-poor (Z/Z ⊙ ∼ 0.1), dense (n e ∼ 103 cm−3), and highly ionized (log U ∼ − 2.1). We use this present highest-redshift AGN discovery to place constraints on BH seeding models and find that a combination of either super-Eddington accretion from stellar seeds or Eddington accretion from very massive BH seeds is required to form this object.

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“…Owing to its proximity in the Large Magellanic Cloud (LMC), astronomers have been able to follow the evolution of this SN across the entire electromagnetic spectrum as it evolves into an SN remnant (SNR). The first JWST observations of SN 1987A were carried out as part of guaranteed time observation (GTO) program 1232 (PI: G. Wright), using NIRSpec (Jakobsen et al 2022) as well as the MIRI medium-resolution spectrometer (MRS; Wells et al 2015) and Imager (Bouchet et al 2015;Wright 2023). These observations provide unprecedented information about the IR emission from the system and make it possible to address a wide range of scientific questions regarding the ejecta, circumstellar medium (CSM), and compact object.…”

Section: Introductionmentioning

confidence: 99%

JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock

Larsson

Fransson

Sargent

et al. 2023

ApJL

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We present initial results from JWST NIRSpec integral field unit observations of the nearby supernova SN 1987A. The observations provide the first spatially resolved spectroscopy of the ejecta and equatorial ring (ER) over the 1–5 μm range. We construct 3D emissivity maps of the [Fe i] 1.443 μm line from the inner ejecta and the He i 1.083 μm line from the reverse shock (RS), where the former probes the explosion geometry and the latter traces the structure of the circumstellar medium. We also present a model for the integrated spectrum of the ejecta. The [Fe i] 3D map reveals a highly asymmetric morphology resembling a broken dipole, dominated by two large clumps with velocities of ∼2300 km s−1. We also find evidence that the Fe-rich inner ejecta have started to interact with the RS. The RS surface traced by the He i line extends from just inside the ER to higher latitudes on both sides of the ER with a half-opening angle ∼45°, forming a bubble-like structure. The spectral model for the ejecta allows us to identify the many emission lines, including numerous H2 lines. We find that the H2 is most likely excited by far-UV emission, while the metal-line ratios are consistent with a combination of collisional excitation and recombination in the low-temperature ejecta. We also find several high-ionization coronal lines from the ER, requiring a temperature ≳2 × 106 K.

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The Mid-infrared Instrument for JWST and Its In-flight Performance

Cited by 92 publications

References 50 publications

Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm

Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm

A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars

JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock

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