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Starts With A Bang

The trick to instantly identifying JWST images

If you can identify a foreground star, the spike patterns are a dead giveaway as to whether it’s a JWST image or any other observatory.
jwst Abell 2744 450 million
This image shows a portion of JWST's NIRCam imager's views of galaxy cluster Abell 2744: Pandora's cluster. One of the most distant galaxies yet discovered, whose light comes to us from just 450 million years after the Big Bang, is highlighted in a white box, while foreground stars within our Milky Way show their bright diffraction spikes in JWST's cameras.
Credit: NASA, ESA, CSA, Tommaso Treu (UCLA); Processing: Zolt G. Levay (STScI)
Key Takeaways
  • From the ground and from up above in space, there are a large number of great observatories, past and present, capable of taking glorious, detailed images of the Universe.
  • However, many of them come either mislabeled or unlabeled, without correctly identifying which observatory or telescope they came from.
  • Even though there are many different ways to “colorize” these images for human consumption, there’s no way to hide the unique “spike” pattern on JWST-imaged stars.

From Earth and across space, our telescopes continually image the Universe.

m81 group
This multiwavelength view of the two largest, brightest galaxies in the M81 group shows stars, plasmas, and neutral hydrogen gas. The gas bridge connecting these two galaxies infalls onto both members, triggering the formation of new stars. If each star were shrunk down to be a grain of sand, this group would be 36 million km away, but the two galaxies would be separated only by a little over 400,000 km: the Earth-Moon distance. The galaxies comprising the M81 group will likely be the very last ones to recede from our reach in our dark energy-dominated Universe.
Credit: R. Gendler, R. Croman, R. Colombari; Acknowledgement: R. Jay GaBany; VLA Data: E. de Block (ASTRON)

Beyond their scientific value, these images are visually alluring.

galaxies without dark matter
Galaxies, when we examine their stars inside, range from ultra-diffuse to ultra-compact, depending on where their stars are located. While some ultra-diffuse galaxies are rich in dark matter, we’ve now discovered both independent sets of dark matter-free ultra-diffuse galaxies predicted to exist. In this view of the Virgo Cluster, data from multiple ground-based observatories are combined to reveal features that no single observatory can reveal on its own.
Credit: Sloan Digital Sky Survey, Canada-France-Hawaii Telescope and the NGVS team

They don’t, however, represent what the unaided human eye sees.

hubble stars andromeda halo
This image, perhaps surprisingly, showcases stars in the Andromeda Galaxy’s halo. The bright star with diffraction spikes is from within our Milky Way, while the individual points of light seen are mostly stars in our neighboring galaxy: Andromeda. Beyond that, however, a wide variety of faint smudges, galaxies in their own right, lie beyond. Individual stars can be resolved in galaxies up to tens of millions of light-years away, but that represents only one-in-a-billion galaxies overall. This image showcases both the power and limitations of Hubble.
Credit: NASA, ESA, and T.M. Brown (STScI)

Hubble, for instance, often includes ultraviolet and infrared light: information invisible to humans.

Hubble wavelength range
Hubble’s scientific instruments analyze different types of light ranging from ultraviolet (UV) to infrared (IR). This graphic shows which wavelengths each instrument studies, out to a maximum wavelength of just over 2 microns (2000 nanometers). Beyond that, thermal noise dominates, making meaningful observations impossible.
Credit: NASA

Observations from ALMA occur in radio light, and must be “translated” into human vision.

unreachable
Looking back through cosmic time in the Hubble Ultra Deep Field, ALMA traced the presence of carbon monoxide gas. This enabled astronomers to create a 3-D image of the star-forming potential of the cosmos. Gas-rich galaxies (imaged by ALMA) are shown in orange, whereas Hubble’s details are shown in violet. You can clearly see, based on this image, how ALMA can spot features in galaxies that Hubble cannot, and how galaxies that may be entirely invisible to Hubble could be seen by ALMA.
Credit: B. Saxton (NRAO/AUI/NSF); ALMA (ESO/NAOJ/NRAO); NASA/ESA Hubble

Similarly for X-ray observatories, like Chandra, we assign colors to visually interpret the data.

X-ray galactic center
Black holes, pulsars, superheated gas, and magnetic fields can all be identified from their X-ray signatures in images of the galactic center. As taken with the Chandra X-ray observatory, this image showcases many of those features.
Credit: NASA/CXC/UMass/Q.D. Wang

JWST images, although spectacular, have a variety of algorithms for assigning colors.

JWST JADES
This image shows the region of study of the JWST Advanced Deep Extragalactic Survey (JADES). This area includes and contains the Hubble eXtreme Deep Field and reveals new galaxies at record-breaking distances that Hubble could not see. The colors on JWST images are not “true color” but rather are assigned based on a variety of choices. This image, released in December of 2022, has since been augmented by follow-on observations within the same region of space, with spectroscopic observations required to determine the distance to these galaxies.
Credit: NASA, ESA, CSA, M. Zamani (ESA/Webb); Science credits: Brant Robertson (UC Santa Cruz), S. Tacchella (Cambridge), E. Curtis-Lake (UOH), S. Carniani (Scuola Normale Superiore), JADES Collaboration

Images unveiled by various collaborations frequently leverage different color palettes.

JWST deep field vs hubble
This region of space, viewed first iconically by Hubble and later by JWST, shows an animation that switches between the two. Both images still have fundamental limitations, as they were acquired from within our inner Solar System, where the presence of zodiacal light influences the noise floor of our instruments, and cannot easily be removed.
Credit: NASA, ESA, CSA, STScI, Christina Williams (NSF’s NOIRLab), Sandro Tacchella (Cambridge), Michael Maseda (UW-Madison); Processing: Joseph DePasquale (STScI); Animation: E. Siegel

From even a visual inspection, however, there is one key to identifying JWST images.

JWST Hubble compare
This composite blinker image was constructed by rotating our first view from the White House release of JWST’s first science image and pasting it atop the previous Hubble image. The number of new features revealed are spectacular, but the difference between the Hubble pattern of diffraction spikes and the new JWST pattern is clearly visible for the foreground Milky Way star above the center of the image.
Credit: NASA/JWST team, via PBS/White House briefing; NASA/ESA/Hubble (STScI); composite by E. Siegel

That key is the pattern of diffraction spikes that appear around point sources, such as stars.

JWST initial alignment star
JWST’s diffraction spikes, seen in great detail around the star 2MASS J17554042+6551277, are the same spikes seen in the first successful alignment image. The science data, as evidenced by the glorious detail of background galaxies, has helped revolutionize what we know about the Universe in, thus far, under one full year of science operations.
Credit: NASA / ESA / CSA / STScI

Whereas many observatories, like Hubble, produce “diamond spike” patterns, JWST’s spikes are unique.

cluster core pandora's cluster abell 2744
This view of two of the three main foreground cluster components of Pandora’s Cluster, Abell 2744, are “separated” on the sky by the lone bright foreground star within the Milky Way in this field of view. Even with just a selection of filters applied to this, the intracluster starlight and several thousand galaxies are on full display here, as is JWST’s unique spike pattern for bright point sources.
Credit: NASA/ESA/CSA/STScI, UNCOVER and GLASS collaborations

There are six large spikes and two smaller spikes to every bright point source in JWST images.

JWST LMC calibration image
This remarkable image of features in the direction of the Large Magellanic Cloud 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, exhibiting the characteristic 8-spiked pattern unique to JWST images.
Credit: Team MIRI

This includes:

  • active black holes in the MIRI images,
MIRI Stephan's quintet
The MIRI view of Stephan’s Quintet showcases features that cannot be seen at any other wavelength. Its topmost galaxy – NGC 7319 – harbors a supermassive black hole 24 million times the mass of the Sun, which the MIRI instrument overexposes to reveal the characteristic JWST diffraction spike pattern. It is actively accreting material and puts out light energy equivalent to 40 billion Suns. MIRI sees through the dust surrounding this black hole to unveil the strikingly bright active galactic nucleus.
Credit: NASA, ESA, CSA, and STScI
  • foreground Milky Way stars in deep NIRCam images,
NIRCam sparkler
This NIRCam view of a selection of the gravitationally lensed region surrounding galaxy cluster SMACS 0723 contains multiple lensed galaxies, including the thrice-appearing Sparkler galaxy, highlighted here. The “sparkles” have been identified as star-forming knots of gas appearing atop already-existing globular clusters. Below the left-center of the second image of the Sparkler galaxy, a foreground star within the Milky way shows the characteristic diffraction spike pattern for JWST.
Credit: NASA, ESA, CSA, STScI; Annotation: E. Siegel
  • and even bright moons within planetary systems.
neptune triton jwst
This portion of JWST’s NIRCam image of Neptune focuses on its giant moon, Triton. Appearing blue in this assigned color image, Triton brightly reflects the near-infrared light emitted by the Sun to the tune of ~70%. By comparison, Neptune only reflects a tiny fraction of the incident sunlight in the infrared, as methane, one of Neptune’s primary components, is a spectacularly successful infrared absorber. The eight-spike pattern unique to JWST is clearly visible around Triton.
Credit: NASA, ESA, CSA, and STScI

The honeycomb-patterned hexagonal mirrors, plus the three main support struts, are the culprits.

nightmare snowflake
The point spread function for the James Webb Space Telescope (JWST), as predicted back in a 2007 document. The four factors of a hexagonal (not circular) primary mirror, composed out of a set of 18 tiled hexagons, each with ~4 mm gaps between them, and with three support struts to hold the secondary mirror in place, all work to create the inevitable series of spikes that appear around bright point sources imaged with JWST. This pattern has been affectionately called the “nightmare snowflake” by many of JWST’s instrument scientists.
Credit: R. B. Makidon, S. Casertano, C. Cox & R. van der Marel, STScI/NASA/AURA

Originally called the “nightmare snowflake,” these beautiful spikes are JWST’s telltale signature.

silly annotation JWST diffraction spikes
This rather silly annotation of the bright star at the center of JWST’s first alignment image showcases that although the six brightest hexagonal spikes cannot be avoided, the central diffuse light from the point source and the spurious striations coming out of the weaker 7th and 8th spikes (stemming from one of JWST’s struts) could potentially be improved. This 8-spiked pattern, with six large and two smaller spikes, is unique to JWST’s configuration.
Credit: NASA/STScI; annotations by E. Siegel

Mostly Mute Monday tells an astronomical story in images, visuals, and no more than 200 words.


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