Ask Ethan: What were the “dark ages” of the Universe?

Today, in all directions, no matter where we look, there are luminous sources of energy to behold. Stars, galaxies, nebulae, and even energy-emitting black holes populate the Universe wherever matter has clumped and clustered together sufficiently. Even though there are great cosmic voids that span up to around a billion light-years in diameter, they’re merely holes in the cosmic “Swiss cheese” of structure. From all directions, the light still gets in, and illuminates even the darkest corners of the Universe.

But that’s what things are like now, 13.8 billion years after the Big Bang. As we look deeper and deeper into the Universe, we see that the story gradually begins to change. Past a certain threshold, galaxies appear redder and fainter than expected: as though something were in the way, blocking that light. That effect gets more severe with distance, where only the brightest of galaxies can be perceived at all. At last, we run out of light to see, suggesting that there were “dark ages” beyond a certain point. What were those dark ages like? That’s what Predrag Branković wants to know, asking:

“How was the dark age of the universe really dark?”

The darkness was real, but there are actually three things at play, all together, that caused them. Here’s how to understand the dark ages, and why they finally came to an end.

At the high temperatures achieved in the very young Universe, not only can particles and photons be spontaneously created, given enough energy, but also antiparticles and unstable particles as well, resulting in a primordial particle-and-antiparticle soup. Yet even with these conditions, only a few specific states, or particles, can emerge, and by the time a few seconds have passed, the Universe is much larger than it was in the earliest stages. As the Universe begins expanding, the density, temperature, and expansion rate of the Universe all rapidly drop as well.

Initial light fades away

Back at the start of the Universe as we know it — during the earliest stages of the hot Big Bang — everything was brilliantly hot and dense. Not only was the Universe filled with quanta of light, photons of terrifyingly high energies, but all the other particles (and antiparticles) that the laws of physics allowed to come into existence. Given that:

• energies were tremendous, possibly as high as trillions of times what the Large Hadron Collider at CERN can achieve,
• conditions were very dense, causing enormous numbers of high-energy collisions to occur at every instant,
• and that any particles or sets of particles/antiparticles that could be created would have come into existence as a result of those collisions, so long as they obeyed Einstein’s E = mc²,

a hot, dense, energetic “primordial soup” of particles (and antiparticle) must have been what existed back then: in the beginning stages of the Universe.

But this hot, dense Universe is also expanding very rapidly, which causes it to cool. The reason is simple: photons (and all massless particles) have a wavelength, and even massive particles have a wavelength associated with them, and the size of that wavelength determines the particle’s energy. As the Universe expands, the stretching of cosmic length scales causes these wavelengths to be stretched as well, to longer and longer values. Longer wavelengths mean lower energies, and so as the Universe expands, it also cools.

As the fabric of the Universe expands, the wavelengths of any radiation present will get stretched as well. This applies just as well to gravitational waves as it does to electromagnetic waves; any form of radiation has its wavelength stretched (and loses energy) as the Universe expands. As the fabric of the Universe expands, the wavelengths of any radiation present gets stretched as well. This causes the Universe to become less energetic, and makes many high-energy processes that occur spontaneously at early times impossible at later, cooler epochs. It requires hundreds of thousands of years for the Universe to cool enough so that neutral atoms can form.

In the initial stages, practically all of the photons that existed were at extraordinarily high energies: in the gamma-ray portion of the spectrum. But as the Universe continues to expand (and cool) over time, the energy inherent to everything drops.

The heavier particles and antiparticles can still annihilate away, but it gets more difficult to create them via E = mc², since there’s less energy in each particle to have a chance of creating them.

The unstable particles and antiparticles, as the Universe expands and collisions/interactions become less frequent, begin to radioactively decay into lighter, more stable particles.

Reactions that couldn’t stably occur at higher energies — like protons and neutrons fusing into heavier elements, or electrons binding onto atomic nuclei to make neutral atoms — now occur, with the former taking place at ~a few minutes after the hot Big Bang and the latter occurring a few hundred thousand years after the hot Big Bang.

At last, the Universe, some ~380,000 years after the cosmic story began, is filled with neutral atoms, and the light left over from the Big Bang has cooled down tremendously: to about ~3000 K, with the photons making this bath of radiation up following a blackbody spectrum in their energy distribution.

At early times (left), photons scatter off of electrons and are high-enough in energy to knock any atoms back into an ionized state. Once the Universe cools enough, and is devoid of such high-energy photons (right), they cannot interact with the neutral atoms, and instead simply free-stream, since they have the wrong wavelength to excite these atoms to a higher energy level.

So all of this radiation still exists, and it’s luminous: ~3000 K would appear as bright red visible light to human eyes (if there were any humans or human eyes around back then), but the Universe is still expanding and cooling. As the Universe continues to age, it:

• expands,
• cools,
• and gravitates,

where those gravitational effects will eventually pull matter into sufficiently large clumps that stars can form. However, that will take time: considerably longer time periods than it takes for the leftover radiation from the Big Bang to continue to cool down past the threshold of being visible to human eyes.

Just as heated materials will glow red, but will fail to glow red if they’re below a certain temperature, this blackbody radiation left over from the Big Bang will cease to be visible after the wavelength has lengthened by a specific amount. As the glow of the Big Bang fades away, the last appreciable amount of photons leave the visible spectrum when the Universe is a little more than 3 million years old: about 3.62 million years, to be precise. Once it reaches that point, the Universe has entered the dark ages.

The overdense regions that the Universe was born with grow and grow over time, but are limited in their growth by the initial small magnitudes of the overdensities, the cosmic scale on which the overdensities are found (and the time it takes the gravitational force to traverse them), and also by the presence of radiation that’s still energetic, which prevents structure from growing any faster. It takes tens-to-hundreds of millions of years to form the first stars; small-scale clumps of matter exist long before that, however. Until stars form, the atoms in these clumps remain neutral, requiring ionizing, ultraviolet photons to render them transparent to visible light.

It takes time to form stars

Before any stars form, there will still be reactions inside atoms and between atoms occurring, and while those reactions will produce light, it won’t be visible light, but rather radio waves. The biggest culprit here is the humble hydrogen atom: the most common element in the Universe. If you were to take every atom that exists in the Universe at this time and count it, you would find that about 92% of all of your atoms were plain, normal hydrogen: with a proton for its nucleus and with one electron orbiting it. About 8% of the atoms would be helium-4, a few hundredths of a percent would be helium-3 and deuterium (hydrogen-2), and about one atom in a billion would be lithium-7. Nothing else, at this early epoch, yet exists.

But when hydrogen forms, containing both a proton and an electron, there’s a 50/50 chance that the quantum spins of those particles — the proton and electron — will be aligned, or facing in the same orientation as one another, and a 50/50 chance that they’ll be anti-aligned, or facing in opposite directions from one another. If they happen to form anti-aligned: great, that’s the lowest energy state, and no further transition will occur. But if they form aligned, with a half-life of about ~9 million years, they’ll spontaneously transition to the anti-aligned state, emitting a single photon in the process.

When a hydrogen atom forms, it has equal probability of having the electron’s and proton’s spins be aligned and anti-aligned. If they’re anti-aligned, no further transitions will occur, but if they’re aligned, they can quantum tunnel into that lower energy state, emitting a photon of a very specific wavelength (21 cm) on very specific, and rather long, timescales. The precision of this transition has been measured to better than 1-part-in-a-trillion, and has not varied over the many decades it’s been known. It is the first light emitted in the Universe after the formation of neutral atoms: even before the formation of the first stars, but also thereafter: whenever new stars are formed, ultraviolet emission ionizes hydrogen atoms, creating this signature once again when those atoms spontaneously re-form.

That transition, known as the spin-flip transition of hydrogen, will produce a photon of approximately 21 centimeters in wavelength every time. This happens to every proton and electron that spontaneously form a neutral hydrogen atom at any point: 50% of them will form in the spin-aligned state, and then those atoms will eventually all undergo this spin-flip transition, emitting long-wavelength photons in the process. However, because these photons are too long in wavelength to fall into the visible light portion of the spectrum, the Universe will remain dark.

We’re going to have to wait until stars form, until clumps of matter in the Universe get dense enough to start emitting their own light — first a little bit via gravitational contraction and then a lot from nuclear fusion — before there’s any way to “light up” this darkness. According to our best, highest-resolution simulations, the very, very first proto-stars ought to begin forming when the Universe is between about 50 and 100 million years old (at a redshift between z ~ 30-50), where nuclear fusion should ignite in their cores.

But, as the very first stars form, the Universe still remains dark, as all of those neutral atoms formed back when the Universe was just 380,000 years old now serve a second, less desirable purpose. In the dense regions that surround these newly-forming stars, they’ve combined to form molecular gas, and that neutral matter absorbs and blocks the starlight, keeping the Universe dark.

An artist’s conception of what the Universe might look like as it forms stars for the first time. As they shine and merge, radiation will be emitted, both electromagnetic and gravitational. The neutral atoms surrounding it get ionized, and get blown off, quenching (or ending) star formation and growth in that region. These stars will be short lived, with fascinating and important consequences.

Light-blocking matter needs to be “boiled” away

This is the big problem now: all of those neutral atoms that we formed so long ago are now very effective at absorbing the starlight that’s being produced. Even though the first stars should be:

• made exclusively of hydrogen and helium,
• very high in mass, about 25 times the mass of the “average” star that forms today,
• extremely hot, with surface temperatures between 20,000-100,000 K,
• incredibly rich in their production of ionizing, ultraviolet radiation,
• and very short lived, dying in cataclysmic explosions after only a few million years,

there is so much neutral matter compared to the small number of stars that form early on that their radiation cannot penetrate very far. After traveling only a few thousand light-years, at most, it’s been entirely absorbed — or, as astronomers say, “extincted” — by the intervening neutral matter.

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But there’s a little bit of hope here! When ultraviolet photons strike these intervening neutral atoms, the atoms absorb the light, but at the cost of becoming ionized themselves. In other words, even though there are a tremendous number of neutral atoms in the Universe initially — somewhere around a whopping ~10⁸⁰ of them, give or take a few — at this late of a stage in the expanding Universe, once you ionize a neutral atom, the “electron” and the “nucleus” it was kicked off from are unlikely to recombine (either with the originals or with another nucleus or electron that’s been ionized) and form another neutral atom further down the road.

More than 13 billion years ago, during the Era of Reionization, the Universe was a very different place. The gas between galaxies was largely opaque to energetic light, making it difficult to observe young galaxies. The James Webb Space Telescope (JWST) is peering deep into space to gather more information about objects that existed during the Era of Reionization to help us understand this major transition in the history of the Universe.

This means that all we have to do is wait for enough stars to form in enough regions of space, cumulatively, to emit sufficient amounts of ionizing, ultraviolet radiation in order to eliminate these neutral atoms, and to turn them into ions: with free electrons and bare atomic nuclei. These atoms, which began as an ionized plasma and only became neutral 380,000 years after the Big Bang, must become reionized in order for the starlight to break free. As a result, we call this process “reionization,” and it’s only when it successfully finishes that we’ll state that the dark ages have come to an end.

Although this process begins when the Universe is very young, it is a gradual process that takes a very long time to complete. According to the best measurements we can make, a typical region in space only becomes fully reionized after some ~550 million years have passed, but becomes “mostly” reionized, where 90% or more of the atoms in their vicinity have been converted into ions, a couple hundred million years earlier. Some regions will get serendipitously reionized a little bit earlier, while others will take longer than average; variations can be a few hundred million years, in general. But it’s only when all of the neutral, light-blocking matter is gone that we can say, “The dark ages have come to an end.”

At last: the darkness ends

Although we have simulations, like the one shown above, to show us how the Universe behaves on average, we have to look to the Universe itself to actually measure how much light gets absorbed along each various line-of-sight that we look at. When Hubble discovered what was (at the time) the farthest galaxy ever, GN-z11, astronomers found that even though its light was coming to us from only ~400 million years after the Big Bang, there was only a very small amount of light-blocking neutral matter in front of it. In other words, this was one of those serendipitously “greater than average” regions, where reionization happened faster than normal.

All of the remaining earliest galaxies discovered, including all the ones seen by JWST, are behind a thicker veil of light-blocking, neutral atoms. The earlier back in time we look, the more difficult it is to see them, and there can be no doubt that even with its longer-wavelength sensitivity and superior light-gathering power, there are no doubt many galaxies that are behind such a thick veil of neutral matter — so deep in the dark ages — that JWST itself will be forever unable to reveal them. The question of when the first stars truly formed, and when the dark ages first began to “brighten up” with starlight of any kind, may not be answerable by JWST.

Only because the most distant galaxy spotted by Hubble, GN-z11, is located in a region where the intergalactic medium is mostly reionized, was Hubble able to reveal it to us at the present time, breaking the prior record held by EGSY8p7. Other galaxies that are at this same distance but aren’t along a serendipitously greater-than-average line of sight as far as reionization goes can only be revealed at longer wavelengths, and by observatories such as JWST. At present, GN-z11 has been relegated to the 9th most distant galaxy known as of 2024: in the JWST era.

However, one of the more interesting things that both simulations and observation seem to indicate is this: while it’s the biggest, brightest, most luminous and most massive early galaxies that JWST is most sensitive to and most easily able to detect, it turns out that those objects are not primarily responsible for reionizing the Universe! Instead, it’s the far more numerous but much smaller, fainter, and lower-in-mass galaxies and star-forming regions that are responsible for the overwhelming majority of ultraviolet, ionizing photons: at least 80% and up to 95% of them by some estimates.

The dark ages began after the light from the hot Big Bang faded away from view, and the Universe remained entirely dark until the first stars began to form: a process that took tens or even 100+ million years to occur. But even once stars were present, there was so much neutral matter around that needed to be ionized that the Universe wouldn’t become fully transparent to starlight — i.e., reionized — until approximately 550 million years had passed since the Big Bang in most places, and it would take even longer in a few other regions. So that’s the story of the Universe’s dark ages, including how (and why) they came to an end. Be grateful for JWST; it’s the best tool we have for peering behind this dusty veil of neutral matter, and actually probing this “era of reionization” for ourselves!

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