What is Dark Matter ?

Matter” doesn’t just mean it’s stuff.

What physicists classify as matter must behave like the matter we are made of, at least for what its motion in space and time is concerned.

This means in particular dark matter dilutes when it spreads into a larger volume, and causes the same gravitational attraction as ordinary, visible, matter. It is easy to think up “stuff” that does not do this. Dark energy for example does not behave this way.

It’s not going away.

You will not wake up one day and hear physicists declare it’s not there at all. (Well, you will, but those claims are rare, and those physicists are wrong.) The evidence is overwhelming: Weak gravitational lensing demonstrates that galaxies have a larger gravitational pull than visible matter can produce.

Additional matter in galaxies is also necessary to explain why stars in the outer arms of galaxies orbit so quickly around the center. The observed temperature fluctuations in the cosmic microwave background can’t be explained without dark matter, and the structures formed by galaxies wouldn’t come out right without dark matter either.

Additional matter in galaxies is also necessary to explain why stars in the outer arms of galaxies orbit so quickly around the center. The observed temperature fluctuations in the cosmic microwave background can’t be explained without dark matter, and the structures formed by galaxies wouldn’t come out right without dark matter either.

Even if all of this was explained by a modification of gravity rather than an unknown type of matter, it would still have to be possible to formulate this modification of gravity in a way that makes it look pretty much like a new type of matter. And we’d still call it dark matter.

Rubin wasn’t the first to find evidence for dark matter.

Though she was the first to recognize its relevance. A few decades before Vera Rubin noticed that stars rotate inexplicably fast around the centers of galaxies, Fritz Zwicky pointed out that a swarm of about a thousand galaxies which are bound together by gravity to the “Coma Cluster” also move too quickly.

The velocity of the galaxies in a gravitational potential depends on the total mass in this potential, and the too large velocities indicated already that there was more mass than could be seen

However, it wasn’t until Rubin collected her data that it became clear this isn’t a peculiarity of the Coma Cluster, but that dark matter must be present in almost all galaxies and galaxy clusters.

Dark matter doesn’t interact much with itself or anything else.
If it did, it would slow down and clump too much and that wouldn’t be in agreement with the data.

A particularly vivid example comes from the Bullet Cluster, which actually consists of two clusters of galaxies that have passed through each other.

In the Bullet Cluster, one can detect both the distribution of ordinary matter, mostly be emission of x-rays, and the distribution of dark matter, by gravitational lensing.

The data demonstrates that the dark matter is dislocated from the visible matter: The dark matter parts of the clusters seem to have passed through each other almost undisturbed, whereas the visible matter was slowed down and its shape was noticeably distorted.

The same weak interaction is necessary to explain the observations on the cosmic microwave background and galactic structure formation.

It’s responsible for the structures in the universe.
Since dark matter doesn’t interact much with itself and other stuff, it’s the first type of matter to settle down when the universe expands and the first to form structures under its own gravitational pull.

It is dark matter that seeds the filaments along which galaxies later form when visible matter falls into the gravitational potential created by the dark matter.

If you look at some computer simulation of structure formation, what is shown is almost always the distribution of dark matter, not of visible matter. Visible matter falls into, and hence, is assumed to follow the same distribution at later times.

It’s probably not smoothly distributed.

Dark matter doesn’t only form filaments on supergalactic scales, it also isn’t entirely smoothly distributed within galaxies — at least that’s what the best understood models say.

Dark matter doesn’t interact enough to form objects as dense as planets, but it does have ‘halos’ of varying density that move around in galaxies.

The dark matter density is generally larger towards the centers of galaxies. Since dark matter doesn’t rotate with the disk of stars we observe, solar systems like our own constantly move into a “wind” of dark matter particles.

Physicists have lots of ideas what dark matter could be.

The presently most popular explanation for the puzzling observations is some kind of weakly interacting particle that doesn’t interact with light.

These particles have to be quite massive to form the observed structures, about as heavy as the heaviest particles we know already. If dark matter particles weren’t heavy enough they wouldn’t clump sufficiently, which is why they are called WIMPs for “Weakly Interacting Massive Particles

Another candidate is a particle called the axion, which is very light but leaves behind some kind of condensate that fills the universe.

There are other types of candidate particles that have more complex interactions or are heavier, such Wimpzillas and other exotic stuff.

Macro dark matter is a type of dark matter that could be accommodated in the standard model; it consists of macroscopically heavy chunks of unknown types of nuclear matter.

Then there are several proposals for how to modify gravity to accommodate the observations, such as MOG, entropic gravity, or bimetric theories. Though very different by motivation, the more observations have to be explained the more similar the explanations through additional particles have become to the explanations through modifying gravity.