See James Webb’s MIRI instrument’s first unreleased pictures

See James Webb's MIRI instrument's first unreleased pictures

With science operations underwaythe James Webb Space Telescope (JWST) newly reveals our Universe.

This three-panel image shows the view of the Carina Nebula’s “cosmic cliffs” as seen by Hubble (top), JWST’s NIRCam instrument (middle), and JWST’s MIRI instrument (bottom). With its first science release upon us, this new era in astronomy has truly arrived.

(Credit: NASA, ESA, CSA, and STScI; NASA, ESA, and The Hubble Heritage Team (STScI/AURA))

This comes ~6+ months after its initial launch.

On December 25, 2021, as the solar array deployed 29 minutes after launch, and ~4 minutes ahead of schedule, it became clear that NASA’s James Webb Space Telescope was operational and receiving power, and well on its way towards its ultimate destination. The launch was an unparalleled success.

(Credit: NASATV/YouTube)

Four reasons necessitated the long wait.

James Webb Space Telescope

The 18 segmented mirrors must unfold, deploy, and form a single surface that’s calibrated to a positional precision of ~20 nanometers, while the secondary mirror must then focus that light precisely onto the instruments. Any failure here would have been ruinous for the telescope.

(Credit: NASA/James Webb Space Telescope team)

1.) Deployment: the observatory needed to unfold into its final configuration.

During the first month after its launch, JWST’s priority was to reach and enter a stable orbit around the L2 Lagrange point. With the Sun, Earth, and Moon always behind it, there’s no chance of any of those sources ever obscuring its view. Hubble, however, from low-Earth orbit, is prevented from observing its targets for more than 50% of its potential observing time.

(Credit:ESA)

2.) Orbital Insertion: it needed to arrive at its desired destination.

All five layers of the sunshield must be properly deployed and tensioned along their supports. Every clamp must release; every layer must not snag or catch or rip; everything must work. Once fully deployed, the 5-layer shield provides passive cooling down to temperatures of about ~40 K. Shown here is the sunshield prototype, a one-third scale component.

(Credit(Alex Evers/Northrop Grumman)

3.) Cooling: all of the components needed to reach operating temperature.

This three-panel animation shows the difference between 18 unaligned individual images, those same images after each segment had been better configured, and then the final image where the individual images from all 18 of the JWST’s mirrors had been stacked and co-added together. The pattern made by that star, a “snowflake” unique to JWST, can only slightly be improved upon with better calibration.

(Credits: NASA/STScI, compiled by E. Siegel)

4.) Calibration and commissioning: each and every component requires it.

Although the MIRI (Mid-InfraRed Instrument) of the James Webb Space Telescope achieves the lowest resolution owing to the long wavelengths it’s sensitive to, it’s also the most powerful instrument in many ways, capable of revealing the most distant features in the Universe of all .

(Credit: NASA/STScI)

This includes both the optical system and each science instrument as well.

The original “first light” image taken with MIRI, the Mid-Infrared Instrument, were taken on April 13, 2022, with the science goals of achieving better than ~1 arcsec pointing resolution and to determine the geometric distortion and scale of MIRI’s imaging and spectroscopy capabilities. Where the 7700nm and 5600nm fields overlap, MIRI’s first color image could be constructed.

(Credit: Team MIRI)

Arguably, the most difficult instrument to commission is MIRI: the mid-infrared instrument.

This six-panel view of various images taken with the MIRI instrument, during commissioning, represents some of the fields that were viewed in order to identify and mitigate many of the technical issues involved with the instrument before science operations began. The right-most image in the top row is the composite of the 7700nm and 5600nm filters from MIRI’s first light image.

(Credit: Team MIRI)

Unlike all others, passive cooling to ~40 K is insufficient for MIRI.

The MIRI imager filter wheel includes: 10 filters for imaging, a 4 filter-diaphragm, combinations for coronagraphy, one neutral density filter, one ZnS-Ge double prism for the LRS mode, one opaque position for darks, and one lens for ground testing purposes. These sets of filters enable us to view the mid-infrared portion of the spectrum as never before, but only at sufficiently low temperatures.

(Credit: NASA/JWST MIRI instrument team)

Probing the longest wavelengths, from 5-30 microns, demands operations below ~7 K.

James Webb instruments

The cryocooler for the Mid-Infrared Instrument (MIRI), as it was tested and inspected back in 2016. This cooler is essential for keeping the MIRI instrument at about ~7 K: the coldest part of the James Webb Space Telescope. If it gets warmer, the longest wavelengths will return nothing but noise, as the telescope will actually see itself radiating at higher temperatures.

(Credit: NASA/JPL-Caltech)

JWST is pioneering a unique, closed-system cooler.

What appears as a relatively empty field was designed to study the variation in the sky background as a function of telescope pointing and across different wavelengths. This helped identify what the differences were from previously being at a “hot” to a “cold” position caused within the detector. A spiral galaxy clearly rich in polycyclic aromatic hydrocarbons pops out in green.

(Credit: Team MIRI)

It’ll keep MIRI cryogenically cold indefinitely.

This commissioning image shows a dust-rich region just a few degrees offset from the true galactic center. Scientifically, the green colors indicate the presence of organic molecules: polycyclic aromatic hydrocarbons. The data was used for measuring the level of stray light in the detectors; more than was anticipated was found in the MIRI data, particularly from 5-10 nanometers.

(Credit: Team MIRI)

MIR’s arsenic-doped silicon detectors encountered some novel issues.

This shows Hubble’s (left) and JWST’s MIRI instrument’s (right) view of the same object: galaxy NGC 6552. With an active center, the MIRI “plus sign” spike pattern clearly emerges. However, one unfortunate feature of MIRI is that when the detector becomes saturated with a too-bright source, an “afterimage” can persist for up to 25 minutes. This image was vital for helping identify what MIRI needed to do to recover from such exposures.

(Credit: Team MIRI)

These detectors saturate when viewing too-bright sourcesproducing afterimages.

This view show’s the famous Cat’s eye nebula, as seen by Hubble (L) and JWST’s MIRI instrument (R). Knowing how a saturated detector produces unwanted afterimages, it then becomes important to learn how to remove such saturation and mitigate it across the MIRI detector. Observing the Cat’s Eye Nebula allowed the MIRI team to identify precisely how to do that across all 3 of MIRI’s detectors.

(Credit: Team MIRI)

The fix is ​​thermal cycling: warming the instrument to ~20 K and cooling it back down.

This remarkable image was a “bonus freebie,” taken in parallel mode while the NIRISS instrument was being used to observe a small nebula in the Large Magellanic Cloud. In MIRI’s field of view just happened to be an asymptotic giant branch (AGB) star in the process of losing mass; the characteristic “plus” sign in its spikes, much brighter than the standard hexagonal spikes, can clearly be seen.

(Credit: Team MIRI)

MIRI’s spikes aren’t hexagonalaim display has unique “plus” shape.

Inside the arsenic-doped silicon detectors in MIRI, reflections were intended to be minimized. However, at the shortest (5-10 micron) MIRI wavelengths, up to ~73% of the light might be reflected internally, represented by the “downward” arrows at various interfaces, creating an enhanced “plus” sign atop of JWST’s standard point -spread function for its light.

(Credit: A. Gaspar et al., PASP, 2021)

Internal, short-wavelength reflections are the culprit; software is the remedy.

This image showcases the same region of sky in the Large Magellanic Cloud, all without a source bright enough to saturate the MIRI detector, in each of 9 separate filters. The instrumental aim was to generate “sky” flat field images, which are necessary to understand and achieve high values ​​for the signal-to-noise ratios that will show up.

(Credit: Team MIRI)

MIRI’s wavelength capabilities cover nine independent mid-infrared ranges.

This 10-frame animation shows each individual filter used to view the same region of the Large Magellanic Cloud (LMC), with an assigned color RGB composite used to bring out various features available to MIRI’s unique view. The final-frame image, the full RGB composite, is featured as the header image for this article.

(Credit: Team MIRI; processing by E. Siegel)

Now fully commissionedMIRI is revealing the mid-infrared cosmos.

This view showcases the difference between the JWST’s NIRCam and MIRI views, with NIRCam’s being far sharper and revealing more objects. The MIRI view reveals dusty details that no other wavelength can, however, including the abundance and composition of dust inside, which relates to a galaxy’s star-forming and life-forming potentials. In the MIRI view, red = gas-rich; blue = gas-poor (but still present); green = organic molecules, especially polycyclic aromatic hydrocarbons.

(Credit: NASA, ESA, CSA, and STScI)

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