JWST’s early, massive galaxies agree with ΛCDM cosmology

Since JWST’s launch, astronomers have used it to investigate the young Universe.

The Cosmic Evolution Early Release Science Survey (CEERS Survey) broke the record for largest deep-field image taken by JWST, previously held by the first lensing cluster image released. This small patch of sky, near the handle of the Big Dipper, contains some ~200 luminous disk galaxy candidates found within the first ~3 billion years of the Universe’s history. The deepest views of the early Universe have given astronomers and astrophysicists much to ponder.

With unprecedented technical capabilities, JWST has already broken Hubble’s cosmic distance record.

The viewing area of the JADES survey, along with the four most distant galaxies verified within this field-of-view. The three galaxies at z = 13.20, 12.63, and 11.58 are all more distant than the previous record-holder, GN-z11, which had been identified by Hubble and has now been spectroscopically confirmed by JWST to be at a redshift of z = 10.6.

Numerous ultra-distant galaxies have been uncovered, revealing a rich, early Universe.

This animation switches points of view between the Hubble Ultra Deep Field and the JWST view of an overlapping region of space. Because of the difference in telescope size and resolution, the JWST views are downsampled by about a factor of 4 in resolution to make these two images match.

These youthful galaxies appear massive, evolved, and are rapidly forming stars.

The galaxies that are members of the identified proto-cluster A2744z7p9OD are shown here, outlined atop their positions in the JWST view of galaxy cluster Abell 2744. At just 650 million years after the Big Bang, it’s the oldest proto-cluster of galaxies ever identified.

Although data is still incoming, many question whether these galaxies conflict with our consensus cosmology.

This collection of several different JWST “pointings” from the CEERS photometric survey contains Maisie’s Galaxy, a high-redshift galaxy candidate that was recently spectroscopically confirmed to be at z=11.4, placing it just 390 million years after the Big Bang. It also contains four separate, nearby galaxies at a confirmed redshift of 4.9, indicating a galaxy proto-cluster just 1.2 billion years after the Big Bang.

The initial conditions of our Universe are known: imprinted in the Big Bang’s leftover glow.

The large, medium, and small-scale fluctuations from the inflationary period of the early Universe determine the hot and cold (underdense and overdense) spots in the Big Bang’s leftover glow. These fluctuations, which get stretched across the Universe in inflation, should be of a slightly different magnitude on small scales versus large ones: a prediction that was observationally borne out at approximately the ~3% level. By the time we observe the CMB, 380,000 years after the end of inflation, there’s a spectrum of peaks-and-valleys in the temperature/scale distribution of fluctuations, owing to interactions between normal/dark matter and radiation.

The equations that govern gravitation and structure formation are also highly certain.

The largest-scale observations in the Universe, from the cosmic microwave background to the cosmic web to galaxy clusters to individual galaxies, all require dark matter and dark energy to explain what we observe. While the equations that govern the evolution are well known, as are the magnitudes of the initially overdense regions in our Universe, obtaining the necessary small-scale resolution to tease out the masses and properties of the smallest, earliest galaxies remains difficult.

Therefore, we should successfully predict how massive structures can be all throughout cosmic history.

Over time, gravitational interactions will turn a mostly uniform, equal-density Universe into one with large concentrations of matter and huge voids separating them. Because simulations are limited in the number of particles they can handle at once, the largest-scale cosmic simulations are inherently limited in their ability to resolve individual, early galaxies. However, the great underdense regions, the cosmic voids within our Universe, are well-understood.

One underappreciated limitation of modern simulations, however, is resolution.

This snippet from a medium-resolution structure-formation simulation, with the expansion of the Universe scaled out, represents billions of years of gravitational growth in a dark matter-rich Universe. Note that filaments and rich clusters, which form at the intersection of filaments, arise primarily due to dark matter; normal matter plays only a minor role. The larger-scale your simulation is, however, the more that smaller-scale structure is intrinsically underestimated and “smoothed-out.”

Prior simulations had difficulty reproducing massive, evolved galaxies so early.

While the web of dark matter (purple, left) might seem to determine cosmic structure formation on its own, the feedback from normal matter (red, at right) can severely impact the formation of structure on galactic and smaller scales. Both dark matter and normal matter, in the right ratios, are required to explain the Universe as we observe it. However, even state-of-the-art simulations like Illustris, shown here, struggle to reproduce the small-scale structure within the cosmic web.

With both greater mass resolution and spatial resolution, however, the Renaissance simulations offer a different perspective.

Although this table might appear to be just a jumble of numbers, the key to high resolution is the final two columns: lower masses and smaller spatial separations lead to higher-resolution simulations, which means more reliable predictions for structures at lower masses, on smaller scales, and at earlier times. Note how superior Renaissance is to all others in these regards.

The unprecedented resolution highlights just how much mass the most initially overdense regions accumulate.

Regions born with a typical, or “normal” overdensity, will grow to have rich structures in them, while underdense “void” regions will have less structure. However, early, small-scale structure is dominated by the most highly peaked regions in density (labeled “rarepeak” here), which grow the largest the fastest, and are only visible in detail to the highest resolution simulations.

Rare but strongly overdense regions grow to contain the earliest, most massive galaxies of all.

The three simulated regions highlighted earlier, using the Renaissance suite, lead to predictions for how massive galaxies should be in those three regions (orange, blue, and green lines). The 5 earliest galaxies revealed so far with JWST, with error bars shown, have about a probability of “1” of occurring within the observed regions. If they were truly rare, they’d be brighter and more massive, as shown by the ~10^-3 and ~10^-6 likelihood curves.

Even with modest, completely realistic star-formation rates, JWST’s most distant galaxies are perfectly typical within our standard ΛCDM cosmology.

Three different but still realistic estimates for sustained star-formation rates are given by the three lines, with model galaxies as revealed by simulations shown with shadings and the actual, JWST observed galaxies shown atop them. Note the 100% overlap.

Surprises and new records still await JWST, but claims like “JWST broke cosmology” were all premature.

This composite image from 7 of JWST’s NIRCam filters shows the central part of galaxy cluster Abell 2744: Pandora’s Cluster. The three main cluster components are highlighted with insets, with foreground and background objects, totaling some ~50,000 of them, present in this 0.007 square degree patch of sky.

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