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Thanks, Ruby, for this. Nice introduction. Glad to be here.

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And I tried to tell you something about what the LHC can really tell us about dark matter.

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Um, but before I do this, I think I have to recall of what this the evidence that we have for dark matter.

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And all these evidences are not really in a laboratory, but they come from gravitational interaction.

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Okay. And these evidences come from different sources.

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And what I think is important that you should take from this is that we can really look at different astrophysical

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observations at very different length scales in the South here at a very small scale at that spiral galaxy.

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And this is one of the first evidence for dark matter.

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So if you look at the velocity here is a function of the radius of this galaxy.

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Then what you would get from Newton's dynamic, if you go farther away than you would do,

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would tell you that you should see a velocity that falls off as one over the square root of the radius if you have a disk.

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So if this off the map, the visible matter here stops its stuff.

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But what you see is that it is really very, very different here.

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So you have first here what you would expect,

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but then that the observation that deviates from your prediction and you reach a constant instead of one of a squared off falloff.

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So this kind of tells you that there is some dark stuff, meaning that it doesn't emit light.

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Yeah, but in the end, it takes gravitational and there's more stuff in this galaxy that you can see.

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Okay. Now you can go to high to larger distances and you can look at not only galaxies, but you can really look at the clusters of galaxies.

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And one of these clusters of galaxies is called pallid cluster.

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These are two clusters of galaxies that merged and passed to each other.

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And this is what you observe if you look at the mass density contours.

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So here's the density profiles. So the masses are mostly here and here.

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And this you get from gravitational lensing. And then you can also look at that X-ray image and you see that the normal matter radiates here.

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And this is located here.

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So you see that these things at this place, which tells you that the mass density and the density of the visible limit, that doesn't really line up.

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Okay. What they can also learn from this to some extent is that these additional metal matter has essentially leafless interactions.

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So it simply pass through each other. But this other vital matter is slowed down and radiates off.

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Okay. Finally, you can go to a larger distance into the last large scale.

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And you can even try to simulate this.

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You know, what happens to the evolution of the universe if you simply put a dark matter profile and also some dark energy into it.

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And you can put it on a computer. So we have a huge number of particles.

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And then you simply solve this numerically. Okay.

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You start that early time. So, yeah. So 0.05 years.

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And then you turn on this simulation. And the idea is that you want to have at the end something that looks pretty much what we observe.

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Okay. And what you see, the final picture will depend on how much matter,

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dark matter and how much stock energy and how much normal matter you will put in here.

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Because, for example, if you have more dark matter, things will there will be more gravitation and things will clump more than they should be.

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So let's stop this. This is what you see.

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Okay. So you start with a uniform density, and then due to gravitational interactions, things start to clump.

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The universe is expanding. You don't really see this here.

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But now you see that you create some structure.

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You see these filaments that arise. And then at the end, you see that you have a lot of structure here.

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And as I said, if you put more dark matter in, you would get more.

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This all would become more clumpy. Okay. So it wouldn't really fit nicely with the observation.

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Yeah. Okay. It also depends on how you what kind of dark energy you put in.

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And if you combine these observations,

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then you can come up with really kind of an idea what is the content of the universe and the content of the universe?

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You can depicted in such a pie chart. So for a few percent of ordinary matter, this is what we are made out of.

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Okay? 23% is dark matter and the rest are essentially 75% or 74% is dark energy.

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Okay. This is the most mysterious thing that nobody really understands what this is.

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Yeah. But I will only talk about the dark matter.

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So 23 plus 3%. Okay. Because the other thing nobody understands and I don't dare to really speak about that, something nobody in the States could.

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Okay. So but what this stock mate.

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So there's, I think, convincing evidence that this dark matter has gravitational intelligence.

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But that's not enough for me, at least. Being a particle physicists, I think, is not enough for me.

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What I really want to know is, is that particular and how does this fit into a particle description?

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So what do we know? If you think about a particle, okay, we know this is already due to its name, its stock,

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its nutrients, so it doesn't interact with photons, for example, or only a little bit.

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Really, not very much. It is massive, okay.

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Because otherwise we would not see it in the evolution of the universe if water into gravitational B, but we don't really know how massive it is.

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It could be electron volt. It could be t v scale.

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Yeah. So we really have no idea. And it is still around today.

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So this means it's either fully stable or it has a lifetime that exceeds the age of the universe.

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So it must be some kind of a long lived particle that hasn't decayed so far.

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Then we can look at the standard modeller and this is already what you saw.

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We have these various particles. Nothing in the standard model of particle, unfortunately, fits this profile here.

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So there's no particle that we have in the standard model that has these properties.

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Okay. Good. This means that essentially we have to go beyond this standard model and introduce new physics.

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Yeah, and that's what I tried to tell you about.

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So what we want to do is really we want to somehow fill in this question area.

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So we want to we know it into X gravitational, but we have no idea.

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We don't know it's mass, we don't know it's spin. We don't know it's life time.

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We do not know if it has weakened the x if it isn't the X with WS or SATs.

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Yeah, we don't know that.

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We don't know if it X if the Higgs, we do not know if it interacts with blocks and gluons with leptons, if it's a tell me relic.

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Yeah, we really don't know that. I mean, we have essentially no knowledge about it, a part that it intersects gravitationally.

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So this is something that, you know, you need to do experiments in order to fill this in here.

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And I will tell about various experiments a little bit about essentially all combining those experiments.

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I think you can really feel or tick all these boxes and fill in what the what it is.

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Good. So what are the particular probes of dark matter?

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They are essentially free ways to search for dark matter before a human built detector.

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So the first search strategy strategy is called indirect detection.

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So the idea is here you have a dark matter particles, which I will always call ICS, or if you speak Greek, it would be exciting.

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And then you assume and this is this this is due to all of this methods that you can look at that there must be some intersection between the stock,

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MIT, the particles and the standard model particles. So there must be some coupling, otherwise we can never see it.

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Okay. And I.

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I simply parameterised this by this blob is a kind of a black box, and something happens there, but we don't really know what happens now.

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And the first thing is that you have these dark matter particles and you annihilate them and you generate some standard model of particles,

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for example, photons. So you have this thing and there's a small copying somehow of the stock method, two photons, and then you look for photons.

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And this is, for example, what is Fermi's telescope a satellite is doing.

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So it looks and tries to detect something. For example, it looks for gamma ray lines.

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So this would be a line of bump sticking out of a background, essentially flat background.

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Okay. The second possibility is now you can somewhat take this blob and turn it around.

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Yeah. And the second possibility is called direct detection.

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What you would look at there is a scattering of dark matter on standard model particles.

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Okay. And this is something you can do, for example, in lacks detect the way Oxford is involved.

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So the idea is that the standard model particle comes in here.

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His cat thus on in the detector produces a photon.

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And then you have electric field here and you have photo multiplier sitting here.

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Yeah. And then you get some a cascade of this photon of electrons and then you detect this.

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Yeah. So you start with a very small signal, and then you look at how this involves the time.

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And this the electrons move up here. They produce largest kinetic.

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And from the way how this is how did this signal and this signal relate you?

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Can someone feel something about the energy of this that has been put from this particular into the detector?

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The last thing is you can again to undo the diagram around and you start with standard model particles

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and this is what collider switches to and the you you take protons or it could also take electrons,

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smash them together and then you look at what happens.

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Yeah. And you look for dark matter particles. Okay.

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And this is what is done at the LHC yet. So some people might have thought that they are already some hints of dark matter.

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And these hints came from both indirect and direct detection experiments.

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So there are many of these experiments and some of them had some small deviation from what is expected.

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For example, this is Fermilab collaborations.

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One has to say that this collaboration didn't really claim evidence, but theories that analysed the data did, and they found a bigger number about it.

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So let me tell you what. This yeah. So they look at events essentially, and they look at a model, a photons at a certain energy.

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And and this is kind of the background that you would get.

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And then you see a little bump sticking out.

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I mean, it's very not really I mean, it's not a huge bump, as you can see.

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So this if the experimental collaboration analyses this data, they find the evidence a local significance of something like Three Sigma.

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Yeah.

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So this is certainly not proof that this is something, but it's I mean, could be a hit, but one should not really take this maybe extremely seriously.

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And a second a second evidence or potentially hint for dark matter is comes from CDM SE, for example.

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So they have, they look at this a direct detection experiment.

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They see that there are three events of really a lot of events that could be dark matter.

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Okay. What they should also see is that essentially that detectors only sensitive up to this line.

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That's only sensitive to here. And these events sit right there.

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Okay. I'm not an experimental physicist, but I assume that, you know, and this is also very vague.

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It's very, very difficult to understand the to take their value,

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understand the detector well here at the border of your detection, it's probably very difficult.

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Yeah. And another thing is that one has to say is that the other experiments are a little bit of in conflict with this observation.

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Yeah. So they don't really fit together if you put them all in the same plot.

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Okay. So I think it's fair to say that given this large backgrounds in both cases and also the fact that in the case of both indirect detection,

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direct detection, you cannot really switch off.

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And on the second meaning, we cannot really control influx of dark matter.

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Yeah. So we have no control of the experiment itself.

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It's very difficult that you can say that this is really a hint of dark matter where essentially possible.

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And this is, of course, something that you can't do it, the LHC, because it can essentially turn the protons off and on the beam off and on.

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I can't regulate the flux of dark matter or indirectly if it's there.

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So this is something it's a really more controlled environment if you want.

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Okay, good. So the idea that the production of dark matter there she is as follows.

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Yeah, if dark matter particles sufficiently light meaning they should be below the

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TV because otherwise we don't have enough energy to produce simultaneously.

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And if the couple two quarks influence, we should be able to produce them at the LHC.

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So you should see them in the atlas detector. Essentially, if you are lucky.

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And by studying the dark matter production, proto proton collisions we are testing.

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What we really do is we test the inverse of the process that kept that metal in trouble equilibrium in the early universe.

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If you're very lucky, we will not only find dark matter so these x particles,

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but there might be a really other states of toxic OC that somehow talks to this dark matter particles

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and they are no longer present in the universe because otherwise they would be if they would be stable.

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It would also be consist of dark matter. But they have decayed already.

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But they could be could give a link between this hidden sector, between the toxic and the standard model.

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Okay. So there might be even more than only one particular might be a whole slew of particles, and one could in principle see all of them.

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So how do you see the invisible OC? So if the diameter, the particles interact the index very weakly.

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Okay, this is already clear. So you will not though what will happen is they will fly out of the detector.

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So you will produce important you fly out. This is pretty much what you what happens to neutrinos.

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Yeah. For example, if you produce neutrinos, the intake so weakly that they fly out of the detector and you don't see anything.

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Okay. A way to see them.

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They are essentially two techniques. One way to see them is that you look at missing momentum.

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So how does this work? You look at addition to standard model radiation.

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So for example, this initial standard model particle in the initial state radiate off a photon.

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Okay. Okay. And then you look also, if your event contains some missing momenta.

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Let me show you an event that shows this quite clearly. Okay.

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So this is the atlas detector again. So the beam is going into the black blotted out, but.

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And this is sliced up. Okay. So you see this thing here is transverse to the beam.

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Okay. And you see that there's a spray of particle here, which is called a chip.

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So these are gluons and quarks, and they have energy and momentum.

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And you measure this energy of momentum here. Okay. What is also see is that there's nothing here.

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Okay. So there's some kind of problem because it looks like that energy momentum is conserved.

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There's something here, but nothing here. Okay, good.

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Of course there's something here. Uh, and this is this missing momentum?

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Yeah. So by measuring this. Yeah, what is called a more low trait event.

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Event that is essentially only one gluon or one chip.

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You can infer that there must be something here. And this, for example, is probably a neutrino.

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You produced two neutrinos in the fly out of the detector, but it could also be dark matter.

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Okay. You don't know. The second possibility is slightly more complicated.

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But it's also very interesting because what you would do here, you would not directly produce this stock, met this or this state,

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but you would produce a partner state, and then this partner state would decay into the standard model and the dark matter.

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Okay, this is another possibility and you will see later that this is, for example, realised in supersymmetry.

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Okay, good. So this is the other possibility then this depending on how this popped the case has not this very nice and clean signature.

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Yeah. You have more activity in the detector. You have what, threats and so on.

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Yeah. So it's maybe more difficult to really pin that down.

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Good. So, like, Juan and, uh, uh, Julia told you we have seen the hicks and the hicks essentially was banned.

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Ponting. Yeah I saw. He has again this craft that has been showing this is the events is a function of the invariant mass of

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the photocopier and you see this little nice pom pom and if you saw many you see it's a clear signal.

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If you do this for the SAT, if you have two sets and indicate to two leptons, you do not even have to assume hidden.

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The band really sticks out of the background. Okay.

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And. To give you an idea, I now compare this situation to what it will look like if you see dark matter.

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Okay. Also notice that this is a linear scale here.

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So it's a number of events in the media landscape. So this is what you see if you have a linear scaling.

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So here, yes, the missing energy or the missing momentum.

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Red is the standard model background.

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This is essentially if you produce in this case, a set plus a chart and this set decays to neutrinos, then you see a dark matter signal, which is hot.

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You can see this is this green stuff, okay?

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But if you get furious, that's easier. You simply turn to logarithmic scaling and everything becomes completely obvious.

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That's all. You see that now there is in the tail region and that's a qualitative search area.

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You see that there's a clear and large deviation.

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Okay. Of course, it's very misleading because now this is ten to the minus two.

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Yeah. So there's essentially no event there. But yeah, that's how it is.

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So. And this tells you that this is really it.

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I mean, it's really more complicated than the Higgs. Yeah. In some way, yeah.

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Because you really have to understand this background even better than you did in the case of the.

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Of the Higgs. Good. So the question is really, if I experimentalists,

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how well can I measure the few events sitting in the tail and the furious should ask how they calculate these small numbers.

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Yeah. So the question is really how precise do I have to know all these things?

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And of course, the fear is usually we don't do this, but I didn't find a different picture.

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And it's sorry for this. Okay, so how so?

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What do we have to know? What do we need to know?

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I mean, one thing is that we really need precise predictions, meaning precise standard model of prediction.

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And they involve a lot of ingredients. So you need the expertise of different people.

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So you need the expertise, for example, of someone that knows how to compute this here, the pot and distributional functions,

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which tell you essentially if you ask for a Coke and that given momentum, how likely is to find this Coke in the proton?

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Okay. But then what happens is then you have some kind of a hot scattering process.

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So here I show there's a standard model event that would give rise to a jet and missing energy.

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So you produce a set both on and on, for example, and then they set the case to neutrinos.

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Those fly out of the detector. And you have to compute this.

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Either you can compute this at three level or if you are really good, I like to it, for example,

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then you can do this at Newport are you add new ones and so on, but it's not enough.

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So then what happens is that these gluons radiate off more gluons and also quarks.

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And this is called a potentially. Yeah.

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So typically you have some numerical code that does all this, so it computes all the emissions of additional gluons in a certain approximation.

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Okay, finally, what you need is you don't see a clue one and you don't see the quark in the detector.

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What you see at the end, pions, leptons and photons are.

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So you have to modernise this cluster, these events.

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Yeah. So out of the gluons, you have to make chips hot or nice, everything, and then even have to include decays of these things.

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Yeah. So you see, it's a very complicated process. It involves a lot of calculation, different techniques.

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Yeah. And but you really need it because otherwise you will never be able to sum up, figure out what this is seeking out.

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What is the background? Okay. Good.

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What you also need, of course, is you also need a theory to describe this dark matter into action.

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Yeah. So you need the standard model in order to tell you what the background is.

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But you also have to you need an idea of what this dark metal fury can look like.

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And the idea is that, well, it's probably very likely that with this free search strategy strategies, if you only take one of them.

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Yeah. You cannot really figure out, even in the case of a discovery, what are these, all these properties,

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what is the mass of the dark matter, the spin of what this how does it intersected so on?

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You probably need more of the all of this experience, all of this search strategy to really fill in all the gaps.

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And then the idea is that there's a certain complementarity.

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Yeah. That if you find evidence for dark matter in one type of search, then if you have a field,

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you can also predict what you would expect in the other kind of search.

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And then you can see that whether you see something or not.

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And in this way, by combining this information, you can try to kill mortals or say this is not the correct description and so on.

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Okay. In fact, there's really no lack of theoretical models because, I mean, furious or rather creative.

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And so there can be a lot of theories of physics beyond the standard model.

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There's, of course, supersymmetry. There are some kind of extra dimensional furious with either of warped X that I mentioned

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or a universal X that I mentioned as the as things called little hicks models.

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It could, of course, be an action. This, for example, would be something that you would not be able to detect at the LHC.

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So a very briefly coupled particle. Yeah, yeah. So you would need a different experiment for this could be also some kind of neutrinos.

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There's some asymmetric dark matter that some have worked on.

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So there's really a really a variety of ideas of new physics.

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And very many of these various, in fact, do have a dark matter candidate.

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Yeah, it's not difficult to make a new physics model and to have a dark matter candidate

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is actually the only thing is that you need a symmetry set to symmetry.

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So asymmetry between X and minus x and then this is a stable particle and this is easy to cook up in essentially every model's okay.

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So you can either look it in this way, but this is you see the cartoon that was made by Tim Tait is a very.

252
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Yeah, yeah. It would be better if you have some kind of a guideline and I think you can cook up

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a guideline so you can somehow look at the spectrum of dark matter fairy space.

254
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So let me explain this a little bit. Okay.

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What you can do is you can really look at a complete model, a complete theory that contains the dark matter and in general, also a lot of other stuff.

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Okay. So these are models like, for example, the minimal supersymmetric standard model,

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like universal extra dimensions and also like little Higgs field where you have a potential dark

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matter candidate and then you have a slew of other particles that are not needed for dark matter,

259
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but maybe for maybe good for other purposes. Okay, then you can make it less complicated.

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And that would explain this. You could talk about simplified models.

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Yeah, this can be, for example, said primordial, obvious and heavy part of the suppose on a dark photon you can talk about squawks l Higgs particle,

262
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and then there's even a even less complete option and the even simpler option that do talk about effective field theories.

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And also we'll discuss this a little bit. So let me talk about this part of this spectrum, which are the complete series.

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Okay. And complete.

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Really, it's complicated. So what you have to do is you have to.

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At least add another layer to the standard model.

267
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Yeah. So he has a standard model. And in this picture I added the particles that you have in the minimal supersymmetric standard model.

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Okay. So for each particle you get a super partner and this is the same and you also get the additional excess.

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Okay. So you have really an enhanced spectrum of particles.

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Okay. In total. It turns out if you look at how many parametres this adds to our models, it's more than 100.

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Yeah.

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And fortunately, many of these are hundreds have essentially to be zero because otherwise it would be in conflict with other observations we made.

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So it boils down that in the images. M Typically what you have to consider are 20 additional parameters that can be relevant for dark metaphysics.

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But you already see that there are 20 parameters, and depending how I choose this,

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you can get it can get very different observations and very different.

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Collider Animal ology. Okay, so what is how can you take, for example, production of Dark and the Emesis and they are very many ways.

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But let me talk tell you about one way to do it.

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Okay. So one way to do is that you have the proton and you strip of some gluons,

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and these gluons produce the the supersymmetric partner off the top, which is called the top squawk or the stop.

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Okay. And you produce them. And these are dedicated to top quarks and dark matter.

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So missing energy. Okay. And this is one possibility.

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And now you can try to look or people look for this in the atlas again, for example.

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And this is a really simplify fix now quite a bit, because this can depend on a lot of parameter.

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But I only show this up kind of a slice of this higher dimension with paramount dysplasia.

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So here's the stop mass. Okay.

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And here is the literally enormous mass and all the other masses I don't show which could in principle contribute to this.

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What you can see is that, first of all, these different coloured regions correspond to different search strategies.

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Okay. You really look at different final states, okay?

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And you see that even if you do this, then there are some gaps here.

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Yeah. Which you cannot probe. So all this coloured things, these are excluded, essentially.

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Yeah. While everything right is not excluded.

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Yeah. And even in such a very simple situation, due to kinematic reasons, there is no exclusions here.

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Okay. If you look at the overall scale that we can probe or that the LHC in run one was able to probe,

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then you see that if this dark matter particle is heavier than around 250 GV, then it's all and probed.

295
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Okay. And then I should put this into the context that the,

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the fact that they did the most massive standard model particle, that being the top quark is 175 TV.

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Yeah. So you see in this case, you really did not probe very heavy objects.

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Yeah. So it's only a little bit that you got that you have already probed in the standard model.

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So what are the, what are the possible improvements of this.

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So people started this is the Atlas simulation. And what you essentially see is that by running the LHC, it's high luminosity.

301
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Yeah. At the end of its run, you will be able to to push this up to 600 feet.

302
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You've also got gain effect of more than two. Yeah, but 600 TV is still not really a huge scale, right?

303
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It's not free TV. Okay. This tells you also that this is very complicated.

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And yeah, people at work have to work very hard on it.

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Good. So let me now go to the other end of complexity.

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And this is effective field for you read descriptions and this is really effective means easier because what you

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really do is that you assume that the dark matter particles are the only new states that you can produce at the LHC.

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Okay, so what you assume that you are new model has a spectrum like this.

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So here's a standard model. Yeah.

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Here a little bit up in the mass is this dark matter candidate and then there's a mass gap and then you have heavier states.

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Okay. But they are not accessible at the LHC directly.

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And in such a way you can describe this production of dark matter in an effective way.

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And the idea is that you there's a systematic way to remove these particles and capture their interactions with the dark matter in a systematic way.

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And essentially, the idea is that you do what you did for the Fermi theory.

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Yeah. So if you are at low energies, you cannot see the W, but it looks to you like a for point into actions.

316
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And the same thing you can apply here. Okay.

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So let me walk you through this exercise here. So let's take a simple model where you couple quarks to a new proposal, one which I call a warner.

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So it's a heavy version of the set.

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And then you set copies to the stock matter. You write down an expression for this, and this is very simple.

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The expression is simply g squared, which is the coupling he had cupping here.

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And then there's a propagate that which gives you P squared minus M set one squared.

322
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Okay. And then there's some kind of a structure which classifies you this kind of kind of action.

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Okay. Now the idea is that what you do in the case of Fermi Fury,

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you assume that this moment he much smaller than this mass and then you can simply do an expansion of.

325
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Yeah, which is not even an expansion. You simply set piece square to zero here and you get something like this here.

326
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Yeah. Okay. Um, that's the idea.

327
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And then at the end, what this mathematical expression has also a counterpart is some kind of a diagram.

328
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So you have a local index here, and this local index will be suppressed by one of the mass, a mass scale, if you wish.

329
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This is the coupling in the Fermi Furia, which is also a mass, a dimension, a parameter.

330
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Okay.

331
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And the nice thing if if this and fury such an effective description is that the information on the heavy states is encoded in a single coupling,

332
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namely this object. So all what is happened here, you kind of parameterised by one coupling.

333
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Okay. And what is happening here? This is paralysed by this local index.

334
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But this is independent of the heavy physics. So you separate it.

335
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These scales. Okay, good.

336
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So what? Now you can do this, and you can do this for very different operator's interactions.

337
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And roughly speaking, what the LHC can probe is this mass scale of 700 TV.

338
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Okay. And you also see that the LHC bound is very good at the best, somehow for very light, dark matter.

339
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And then at some point, if it becomes too heavy, you can simply not have not enough energy to produce this and your balance goes down.

340
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So everything below this is again excluded by LHC.

341
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And now in this effective fear, there's a very simple comparison between LHC, a balance and direct detection balance.

342
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So you can take this balance on the suppression scale, on this mass scale and compute from this the dark matter nuclei on cross section.

343
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Okay. And this is what you find. This is the found that this everything there is forbidden.

344
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And in the case of direct detection, this is excluded by direct detection.

345
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And what you see is that at some point, because the direct detection measures, the nuclear recoil energy.

346
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Yeah. And you cannot measure arbitrarily small nuclear recoil energy is.

347
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Yeah, at some point there's no balance here.

348
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And this is where the LHC is most sensitive to the cross-sectoral area and provides them the strongest balance.

349
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Okay. For other indications is even the LHC can even do much better than a directly Texas uses for spin dependent interactions.

350
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And this is due to the fact that for such an actress you lose the coherence.

351
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So you have scattering on not the whole nuclei but on each of the particles.

352
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Yeah. Okay. And then you see that here.

353
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The LHC balance doesn't really change a lot, but direct detection moves from here to here and it's you're doing much better.

354
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Then the last point I want to discuss, and this is simply that it is also very active here.

355
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Oxford is involved in this activity to define and simplify dark matter models.

356
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And the idea is here that you can also make this a little bit more interesting and you consider

357
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models to contain dark matter and the most important step mediating the intersections.

358
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Yeah. So from this very heavy states, you pull one down a little bit and you make it accessible at the LHC.

359
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Okay. So this means that you can not only produce this guy, but you can also produce this guy at the LHC.

360
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Okay. And this has the advantage that I'd like effective field theory is this simplified model.

361
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This really can describe the full kinematics of the dark matter production at the LHC.

362
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Yeah. The effective you cannot not because for example,

363
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if you probe this mass of this of this resonance that you produced, you will see deviation from the kinematics.

364
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Okay, this you have to pay a price for this.

365
00:39:04,150 --> 00:39:11,200
So in this case, having what instead of a one parameter, you have a few parameters, but it's still not 20.

366
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So typically three or four parameters to describe this.

367
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Okay. Let me summarise so dark matter implies physics beyond the standard model.

368
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And in order to understand dark matter, you need to have a theoretical new theoretical concepts.

369
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And these can either be complete models like the MSM, but it's also fruitful to think about less defined, more hazy sketches of FURIA.

370
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Okay, the structures at the LHC in underground experiments, in astrophysical observations,

371
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they naturally target different parts of the dark, met the fury space, and they complement each other.

372
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Okay.

373
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Once we really have a detection, then I think it's fair to say that we really need all these techniques to figure out what the dark matter really is,

374
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to fill out all the, um, to tick all the boxes and to tell us all these parameters.

375
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And I think that the LHC can really bring these sketches of dark matter to life if we are lucky.

376
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Thank you very much.