Galactic gas can help unveil what dark matter is made of
Warm versus cold
Dark matter cannot be seen directly. We know it exists because we can see the gravitational effects it has on the surrounding matter. There aredifferent theoriesabout what dark matter may actually be. The standard model suggests it is cold, meaning it moves very slowly and only interacts with other matter through the force of gravity. This would be consistent with it being made up of particlesknown as axions or WIMPS. Another theory, however, suggests it is warm, meaning it moves at higher speeds. One such particle candidate is thesterile neutrino.
If dark matter is cold, a Milky Way-type galaxy could harbor one or two subhaloes weighing as much as 1010Suns, and most likely hundreds with masses of around 108Suns. If dark matter is warm, haloes lighter than around 108Suns cannot form easily. So tallying light mass dark haloes can tell us something about the nature of dark matter.
Halo imprints
We believe that the existence of lower mass haloes can be revealed by carefully planned observations. Astronomers have already got pretty good at this game of hide and seek with dark matter haloes and have devised observations to pick up the damage they leave behind.
To date, observations have targeted mostly the changes in the distribution of stars in the Milky Way. For example, the Large Magellanic Cloud, a smaller galaxy orbiting ours, seems to have a dark matter halo which is massive enough totrigger an enormous wake– driving the stars from across vast regions to move in unison.
A few of the smaller dark matter haloes thought to be whizzing inside the Milky Way may occasionally pierce through large stellar features, such as globular clusters (spherical collection of stars), leavingtell-tale gapsin them. Dark matter haloes can also affect how light bends around astrophysical objects in a process calledgravitational lensing.
But the signals left in the stellar distributions are weak and prone to confusion with the stars’ own motions. Another way to probe the effect of haloes is by looking at the galactic gas it affects. Galaxies haveplenty of hot gas(with a temperature of around 106degrees Kelvin) which extends out to their edge, providing a wide net for catching these dark matter haloes.
Using a combination of analytical calculations and computer simulations, we have shown that dark haloes heavier than 108solar masses can compress the hot gas through which they are moving. These will create local spikes in the density of the gas, which can be picked up by X-ray telescopes. These are predicted to be minute, of the order of a few percent, but they will be within the reach of the upcomingLynxandAthenatelescopes.
Our models also predict that the spikes in the density of thecooler galactic gas(with a temperature of around 105K) will be even more significant. This means that the cooler gas can record the passage of dark matter haloes even more sensitively than the hot gas.
Another promising way of observing the dark-matter-induced fluctuations in the gas is via the photons (light particles) from the cosmic microwave background – the light left over from the Big Bang. This lightscatters offthe highly energetic electrons in the hot gas in a way that we can detect, providing a complementary approach to the other studies.
Over the next few years, this new method can be used to test models of dark matter. Regardless of whether dark matter haloes below 108solar masses are found in the numbers predicted or not, we will learn something useful. If the numbers match up, the standard cosmological model would have passed an important test. If they are missing, or are far fewer than expected, the standard model would be ruled out and we’ll have to find a more viable alternative.
Dark matter remains a mystery, but there’s a huge amount of work going into solving it. Whether the answer will come from instruments on Earth or astrophysical probes, it will no doubt be one of the most important discoveries of the century.
This article is republished fromThe ConversationbyAndreea Font, Astrophysicist,Liverpool John Moores Universityunder a Creative Commons license. Read theoriginal article.
Story byThe Conversation
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