 Velkommen alle, jeg er min grønne kredsjere til at introducere hendes klikker. Jesus Pérez Rios fra Stonybroek Universitet, som du kan se her. Ja, Jesus har været meget... Hvis man kender hans kæreste kæreste, så har han været i vejret meget. Han tog hans kæreste kæreste i Madrid i 2012. Han tog hans kæreste kæreste kæreste i Lavertois-Emigue-Conton, i Osset, ved Folier du Lille, som kæreste kæreste kæreste. I deres kæreste han til stedet, til Pendue Universitet, og i en gruppe af Chris Screams, som du kan sige om, at nogle af de her kæreste kæreste kæreste kæreste kæreste kæreste kæreste kæreste kæreste kæreste. I den samme universitet, som du fortsætter på, i en gruppe af François Rubégeau, så går du til 2016, og i 2017 og 2018 går du til Universitetet, og så går du til Rappel, for Torico, hvor du var en social professor for to år. Og så går du til Europa igen, i en gruppe af Gerd Meier, der er et fætabære Institut af Max Planckens Society i Berlin, som nogle af os kan vente, at det er en af de bedste places i Europa at være, og være der for et par år, tre år. Og så since last year, you've been at Stonely Brook University, and François has already a very long track record in, I'm saying more or less anything you can do with cold atoms and molecules, ions and so. So even he wrote a book, also an introduction to cold and also cold chemistry atoms, molecules, ions and ribbrax. So this topic you're going to hear about today is just one of the many topics that you are touching upon in your research, so please. This is, I would say, the most provocative of what we do, and it's a way to provoke you guys to do science, like to be more than what you guys do. Okay, so let's start. In a group I want to do some advertising, okay? So we do ammo physics, even though I'm going to talk about dark matter, but I will try to show you the connection, okay? And we do theory and computational, right? So we use computers to the simulations, because sometimes reality is harder than we expected. And we have four lines of research. One is cold and tropical chemistry, as Michael mentioned. We do free-boy physics, where basically we study atmospheric physics, like ozone formation, stuff like that. Then we do data science, where basically we use machine learning techniques to understand better ammo systems. And finally, this is the topic that we're going to discuss today with you guys, is physics beyond the standard model. Of course, if I mention this, it looks like highly physics, but we do ammo physics, with the hope that we can help this guy from highly physics, because they're pretty lost. This is my group. No, indeed they are lost. Everyone is lost somehow, right? So this is my wonderful group. So I have two lines. This is the upper line, the guys in the states. The lower line is the guys still in Germany, because some people don't like the states. So they prefer to stay in Europe. So what can I do? Okay, so this is my whole group. And today's talk is about the universe. Okay, so I'm pretty sure that, you know, every one of you, you go, you know, doesn't matter if you are drunk or not, you go outside, you look at the stars, you feel like, oh man, this is beautiful, right? So indeed this is kind of the motivation that the old philosophers of, even from the very beginning of human history, this is what helped us to do science, right? So all the scientific knowledge is coming from curiosity. For me, as an ammo scientist, I can see all bunch of stars of planets, like atoms and molecules, right? This is the basic building blocks of the world as we see it, right? And this is kind of the spectra of ammo physics. So we can go as cool as we like it. It's fine, we have BECs as people here doing. And also we can go higher in energy up to this energy. At this energy, you break the hydrogen atom, and then you have electrons and protons, so then we don't have atomic physics anymore. We go into the high energy region, okay? And this is how I see the world. But that's a very narrow view, and I cannot do nothing about it. I'm very ignorant. So then we have the heine physicists that say, no man, we can do even better. We can really truly understand the fundamentals of physics, okay? And this is the standard model. This is the most beautiful theory ever made by humankind, supposed to contain all the information in the universe, okay, and explain everything. That's not true, by the way. But anyway, so we are working through that. So it turns out that all this knowledge, the very beginning of human history, only contains 4% of the energy of the universe. So all the things that you guys do in your lab, all the things that I'm doing, it's only 4% of the universe. So every time they see that, they feel really sad. Really, really sad. I mean, I'm spending my whole life doing this, and I can only understand 4% of the universe, what I'm doing with my life, right? So it's kind of pretty depressing. But this is the way it goes. There's nothing about it. But here's the thing. There are two big chunks that we don't know nothing. Dark matter and dark energy. So let's start with dark matter, okay? So what is dark matter? And this talk is about how we can use, what we know from atoms and molecules to try to figure out a little bit the properties of dark matter. Okay? So let's see what is dark matter. And I will try to convince you that dark matter exists, which most people believe that they do not exist. Okay, whatever. This is a free country, right? Okay. So this is the famous thing about, that you have seen and pressured all of you about the rotation of galaxies, right? So basically, so the rotation of stars. So basically the idea is to measure the velocity of the stars, right? And then as you are moving farther away, the velocity should be lower, right? This is what you would expect. So basically you look into the core of the galaxy as you are moving farther away, you have less stars, you have less mass. I mean, the mass is going to a constant, and then you have to go down. But indeed this is what this is observed. Okay? And that observation is, it goes with 1 over r squared. So the density is different from what you would expect from the typical visual matter. All the matter, like an image light. And this is the famous thing. Okay? Indeed, you can generalize that to any kind of galaxies. So this is a paper that got from 1991. People already knew all these things. Then in order to understand what they observed, you need to include the component of the disk of the halo and also the gas, excuse me. So again, we seem to have evidence that there is something out there that is interacting through gravity, but that's not the mid-light. It's something that we cannot see. What is that? Well, we are so original that the name that we come up was Dark Matter. Not very original because it's dark. Okay? And I'm going to tell you the story about who was the first person to come up with this name. It's a very fine story. Funny and kind of sad, too, I have to say. The real story of Dark Matter starts with the comma cluster. In the same way that you can look into the velocity of stars as a function of the distance from the center of the galaxy, you can look into the velocity of galaxies in a cluster. So basically a cluster is a bunch of galaxies that are bound through gravity. Okay? So it's a bunch of things orbiting through each other. And then if you are going far away from the system, you have more mass, and then the galaxies here will be much faster than the galaxies over here, right? So you can go and use the real theorem, which I guess that everyone knows about it. If not, it's time to learn, right? And then you can always infer from the velocity what is the mass that your system has, right? So the guys, I mean, the astronomers, not me, go look at the velocity by measuring the Doppler shift of the lines of hydrogen for instance, and then you can see what is the total mass that is in that cluster, right? That's it. This is how it works. So then what it turns out is like the mass that they need to explain the velocity is 400 times more than what they observe. This is a fact. Okay? This is not a rational fact. This is no theory. This is no prediction. This is just a fact. And indeed the guy that did this first was Fritz Swicky. Sorry. I mean, he's Swiss German, okay? But I don't know German. And this guy, 1933, looking to the Coma Cluster, proposed for the first time, doing a theory, sorry for my German, okay? But he was the first one to introduce that term. And you know what happened. No one believed on him. The whole committee believed that this guy was crazy. Was so crazy. So he was so crazy that has this wonderful quote. And I like it. A strongman started spherical bastards. No matter how you look at them, they are just bastards. And this is true. And he was very pissed off with them, okay? This is, honestly, this is, and he was very pissed off. And I'm going to tell you something. After this guy, I mean, could just start to cry and have some problem. No. The guy was the first one to observe a neutron star. So this guy did all his career at Caltech. And he's a very, very good astronomer by the way. But he has some issue with the dark matter. Then the last test is to look into the comodical scale. So right now we start from galaxies. We move to clusters, which is something bigger. And now we are going to look into the whole universe. I'm going to show you a simulation called the typical embody simulation, which is, I didn't do that. It's a very complicated simulation. Basically here what we have is a bunch of variants, so matter that make us, and a bunch of dark matter. We put it together in a random configuration, and we let the system evolve. Let's see what happens. So you let the system evolve. Matter like to clamp, and for some kind of structure. It's beautiful by the way. And now you can see what that means. Well, this is an example, but now this is this famous result for the simulation. So what we have here, this is observation. So this is like the distribution of clusters of galaxies in the universe. Okay, observation. And this is the simulation. On the model I mentioned before, so you have just a bunch of variants there, you put dark matter, which is something that interacts with gravity. And you see that you can match basically all the observations. This is pretty impressive. And we are talking about cosmological scale, size of the universe. Indeed, in order to understand this very famous figure and pressure, some of you have seen that, which is kind of the famous power spectra of the CMBO cosmic microwave background, had these wonderful peaks. So in order to explain those peaks, you need to use what the so-called lambda CDM. Lambda for the cosmological constant of Albert Einstein and called dark matter. So you need to include dark matter in order to explain this. So again, we have observational evidence that dark matter is out there. Or at least there is something dark that we need to include in our models. So now the thing is like, yeah, we know that it's out there, but what is made of? This is the one million dollar question, maybe more than one million, but important question. So right now I hope to convince you that we have evidence that dark matter is needed to understand galaxies, cluster of galaxies and cosmology. So even in all scales you can explain dark matter. And also you can come up with the idea of modifying gravity, right? That's an alternative. However, those theories can only work in one of them. Of course, this one always will fail. You can only use modified gravity to understand the CMBO. And this one, it will work. So you can modify gravity like with a you have a potential kind to make this guy work. Maybe this guy too, but this one is a problem. So far dark matter is the best theory that we have to understand the universe as the way we see it. Without counting dark energy that's a different business and not for today, okay? That's even harder. I would like to mention this. When I put distance in parsec, even I don't know what is a parsec, right? I know it's big, but I don't know how big it is. So a galaxy is pretty large, right? Way bigger than Europe, right? 10 to 17 kilometers is the size of a galaxy. So we go from 10 to 17 to 10 to the 23 kilometers. So from this scale to 6 kilometers, and still we need dark matter. The same model that can explain everything in this order of magnitude. This is pretty robust evidence that we need this guy. And with that, I would like now to pass about how we detect our matter. Of course, we don't detect our matter because no one ever sees it, right? Otherwise, you will get an overprice. So this is the typical approach. From high in physics, it's like either you do a beam experiment like having high energy particles colliding with some kind of material and then you see you lost some kind of momentum. If you lose some kind of momentum, it means like there is some kind of invisible particle that you are creating. Okay? So that particle should be beyond a standard model. Then we have the typical synone experiment, which is liquid synone. And then if there is an event such that your synone gets ionized, then you will see an assimilation signal. So like kind of spark. This is how we detect synone. Synone experiment. This is the typical approach right now. However, there is something that we have to keep in mind. This is the permitted space for dark matter. And this is one of the main problem. The mass goes. I mean the mass of dark matter can go from 30 to our masses to 10 to minus 22 EV. Okay? So we are talking about more or less 30 hours of magnitude. Parameter space. And when you go to accelerators, you can only, only, I mean there is a huge chunk of it, okay? But usually you are going to affect this range. What about the rest? What you can do with, I mean we need new approaches, new machines, new methods to try to explore different mass ranges of dark matter. And one of them is molecules. So why molecules? Because first, molecules are part of the universe, right? So we are here, made our molecules. And also thanks to the wonderful machining that you guys have in the lab, you can control molecules very well. Much better than anyone in the world. So you can prepare guys in a particular quantum state. You can look into interference. You can look at all kind of different effects. All these things that you guys study are very sensitive to small changes. Dark matter is a small change. So then, if you have full control of your system, you are basically sensitive to any kind of weird stuff. And that's the point why molecules are important. Thanks to you guys. And this is the outlook of my talk. I will try to mention what is the principle of the detection. And then I will show you our proposal for very simple excitation. And finally we talk about the migtal effect, which is a kind of funny thing. The principle, the principle is fairly simple. Indeed, I start in this business thanks to this paper. These guys, of course, was part of the PRD, high energy journal. I was reading that and was like shocked. I always thought, naively, that dark matter is dark, so why should I care, right? It's fine. This is a first statement. Dark matter is mostly dark, but at some point it's not dark. Indeed, these guys propose, like for instance, you have a, let's assume, that you have an H2 gas, a gas of hydrogen, so that you can control everything. Let's put it underground, no background, nothing. Then the principle, hydrogen, should be stable, right? But if one of the hydrogen atoms, sorry, hydrogen molecules breaks down, maybe due to the interaction with neutrinos or maybe with dark matter. So these guys propose that as a way to detect it. And this is something that motivates me. So then in this paper, 2012, there was the idea, like if dark matter interacts with a molecule, basically it could happen at vibrational or rotational excitation. And turns out that the typical energy scale for molecular excitation is going to be very good for light-dark matter. As a result, since the energy spacing of molecules is very small compared with atoms, we have a system that can complement what we can do with typical high-energy physics approach, and then we can explore even more. That is why molecules can be very interesting for high-energy physics. It's not because they like molecules, they don't care about molecules, they don't care about the system, they only care about having a system sensitive to new stuff. The systems that they are used to work, they cannot go to low masses, because the energy of those systems are very high. But molecules are preferred for that. I here with this plot, I just want to convey the general knowledge. Like we have dark matter colliding with your molecule, something will happen and then we have different scenarios. Make that vibrational excitation and then a typical experiment. Or a mental setup that may work, hopefully. Let's see how it works, the vibrational excitation. This is pretty simple. So simple that I is always fun to explain. The idea is the following. Let's assume that we have CO gas, okay? Carbon monoxide, something you can buy in a bottle. You put it in a place such that all the guys are in the ground state. You isolate the guy, you put on the ground everything is good. So, in principle, all the guys should be in the ground state, because there is nothing there that can populate the guy to excited state. Which are cold enough, so you are in thermal equilibrium. Now, let's assume that this is a dark matter event, like colliding with your molecule. Now the molecule will be excited to some vibrational state. So, what happened next? So, the idea is the following. You have that tank full of CO, then you just need to detect the photons, because the guy will be excited, and when they excite, every time they excite, that means you have one, two, three, four, or whatever, you will get photons out. You have to detect them basically surrounding your thing. You're always supposed to see darkness, right? You're supposed not to see any photon, because the guys are in the ground state. But if something excited guy, then you will see the signal of the photons. However, there is something that we have to take care of. Black body relations are there, right? Something that can mess you up. You have to take care of. But there is something that we can work it out. As a result, we can put constraints on the temperature that we need and the density. So, we need to have the gas fairly cold, cold 50 Kelvin, way hotter than what you guys are used to. But this thing is supposed to be big, like meter side. I mean, a clear start of one meter side is not trivial. And the density cannot be too high either, because the density is too high, basically, what can happen, like you can quench the excitation via collision with another molecule. And we want to avoid collisional quenching, right? So we want to have pure photonic emission. Okay? So now I'm going to describe the two main processes that can happen. Let's start with this one. This one we call the cascade process. And it's in a condition such that the guy goes to this state, for instance. And then the density is such that it's solo, that the guy has time to decay to another, another, another. So basically the guy is cascading, because there's no collision. It's very low density. The guy keeps going down and down. And then every time you go down, you meet a photon with different frequency. This is the cascade signal. It can happen, on the other hand, that you can be in the opposite regime. You can still have an excitation to the same state. But turns out now you have collisions. These collisions are going to quench your system, right? So you start with guy N, zero. Now this guy will go with one. This guy will go one down. So you reduce one, you go up, one, like that. And there's something cool. You can keep doing that with another guy, another guy, another guy. But at the end, they will go to the V-equal one. So we choose the density or the pressure, whatever you prefer, such that you cannot quench this guy. So all the things will accumulate until you get the V-equal one. So you have a V-equal two end. You have N excitation in the V-equal one. And then you will emit it and get it down. And collect it with your IR photo detector, single photo detector. Okay, that's another business for an auto, how to design these things. But that basically are the two ways how we can detect the signals. Here's an example of how it looks like. A typical signal. Here we have the vibrational state of the CO. And this is the rotational state of CO. Let's assume that the guys start over here. So in this region, the vibrational quenching is very inefficient. So the guy will have cascade. Going cascade like that. At this time, now, the collisions are effective. Because now you're in a vibrational state where it can quench easily. So then the guys start to quench, quench, quench. And then you accumulate. And then you get all these guys out. This is another effect. First time you have another event here. This is what you have. So basically, in the way how we design these things, no matter what happens, you have photons out. You can read them. And more than once, you can measure coincidences. And in that way, you can get almost background free signal. And this is the benefit of using molecules, in particular CO. We use CO, because CO doesn't like to quench. CO is a very weird molecule. Even CO has a lower cross-section for quenching than H2. CO is amazing. It doesn't like to quench. Which is something that we like, too. And this is the end what we get. So this is our prediction. Here, what we have in the y-axis, is the cross-section between that matter. It doesn't matter what kind of model it is. Because we are not interested in that. We are not interested in, like, what is the minimum cross-section between something colliding with our nuclei, such that we can be sensitive, too. As a function of the mass of that thing. And here, in gray, we have things that has been already ruled out by astrophysical observations, seen on experiments, some other things. And you can see this, a big chunk of the parameter space that has not been ruled out. Using our setup, we can be sensitive to this region with something decent. Like 20 centimeter side. An area of 1 centimeter square. It can be done right now. It can be hard, but it can be done. Then, of course, in this business, you always can go to futuristic things, right? Let's assume that now we have a volume of 2 meter side. That may be too futuristic to be true. But anyway, we can do it, right? We are theoreticians. We go to 2 meters. And then the area is 1 meter square. In that case, for the photoetectronus, we can go as low as this. So we can be sensitive to a huge chunk of the parameter space, which again is something that you cannot do with other systems. Another benefit of molecules is the spin. We can play with different isotopes, right? You have carbon 13. You can have different isotopes of oxygen if you like it. As a result, you can be sensitive to a spin, independent or spin-dependent interaction. You can interact with the spin of the neutron, the spin of the proton. As a result, you can be sensitive to even more than matter models. That's for regression. Now we are going to go to the MIGDAL effect. How many of you know what is the MIGDAL effect? No one, right? It's okay. I mean, you don't have to know. I didn't know until a year ago, okay? So it's fine. So this is something that is funny. MIGDAL effect. MIGDAL was like, I worked a baby in 1930, something. I tried to get the baby what is in Russian. I don't understand Russian, so I cannot show to you guys. So the idea was the following. He was envisioning the following problem. I have an atom. But the nuclei are going to be radioactive. I'm going to decay through a beta decay. So now the guy goes to a beta decay. So then the neutron goes to a proton. We have a neutrino and an electron. So basically, your guy will get out one electron. An electron will fly out. As a result, your nuclei will get a recoil. Right? Because your electron is going out, then you have a recoil. If the recoil happened too fast, even you can ionize the atom. That's the MIGDAL effect, because your charge, your nuclei is moving on time. So you have an independent apple moment, right? So that's kind of like a microwave field. So you can ionize and even excite electrons. This is the MIGDAL effect. He did it, of course, for this particular nuclear right of decay. But now we can do it without matter. Now the question, what we have. And what happened, instead of having a right to decay, we have done matter colliding with an atom, let's say. But the recoil is so fast. So the recoil is so fast that it can even ionize or excite your atom or your molecule in this case. And this is what we study. So what we did here is we generalized the idea of MIGDAL to molecules. Okay? And it was pretty fun, to be honest. The idea is like instead of going from one state to another in an atom, now we go from one potential energy curve to another. And now we have different reverberation states, as you know, different states. Okay? And then this recoil can give you from one guy to another. Let's see how that goes. In order to calculate the probability, sorry, this is a bunch of math, but you should be able to handle it, okay? If not tell me please, I will try to make it simple. This is fairly simple. In order to calculate what is the probability to end up in one electronic state, is the following. It's just the overlap between the initial wave function, which you control at your initial state that you're preparing your gas, right? To the final state. And now you have these two guys over here, which is basically playing wave, which is basically like when you have a kick, and these guys are moving. You have different coefficients, that depends on the properties of the nuclei. Okay? And Q here is the momentum transfer. That's the momentum that the dark matter is transferring to your guys. So now we can write the position of my nuclei in the interest of the center of mass, the relative distance, and the position of the electrons. I do that. I put it back. And this is what I got. I got the probability to come separated, as expected in two terms. One is pure nuclear, which is just a bunch of vibrational coupling. We don't care like kind of Frank-Conton factor business. But then we have an electronic coupling here. Let's see how that looks like. I'm pretty sure some of you already know the answer. Right? People doing quantum optics should know that. So what we have here is like this guy. Basically. It's the same as this. We have a penalty over here, which is the mass of the electron versus the mass of the molecule. So usually you will get this like zero. This is very small, but in our case we care. Then we have the momentum transfer, and then we have this guy over here. This guy over here is the transition dipole moment between the excitation. So this is basically the same as having like a typical transition between that guy and that guy. Okay? And then we have the same selection rules that you have for E1. The same selection rules like a dipole allows transition. But the transition is triggered by a dark matter event. Okay? Now the middle effect has another term. And it's the following. We can never forget that the electronic state is not a pure state. What do you mean? Like pure, like what we call the state is a single sigma. It's not really a single sigma. We have some component with other guys, right? The quality of the quantum number that you have depends on the validity of the Bohr-Hemmer approximation. But we can always go beyond Bohr-Hemmer, and then we can use non-adiabatic effects. When we have non-adiabatic effects, basically we have a final wave function plus some kind of new component from other guys. Because we need to see how this electronic state covers for the rest. Using the second-reperation theory, we see that we can compute that excess or that combination wave function like that. And this delta V is just the gradient of the nuclear wave function times the gradient in the real direction. So when you apply that, at the end what you get is like the new chunk of wave function that is shared with other electronic states. Is this thing over here, where this guy is the non-adiabatic coupling term, which is basically, as you expect, it's just the coupling within your electronic state and the gradient of the electronic state. Sandwich, this is what you get. And this is what we calculate, or I calculate how the physicists don't care about how to do that. This is what I do, this is my job. So this is the amplitude for the transition. And how we calculate that is through quantum chemistry. So what I do is I try a different basic set that makes sense for the molecule at hand, this case, CO and two, whatever. Then I optimize the geometry, I choose a different method, I use MRCI, and then type of calculation. Then we do a single point and then we do an electronic cover map. We have to a single point to calculate numerically the gradient and the overlap is necessary to know what is the probability, because we have the sandwich between the wave function and the gradient of the wave function at a different point. And this is what we have as a result. So this is for instance for CO. This is the so-called delimodulation. This is the modulation that you will expect to have in a dark matter signal just because we are, just because the rotation of Earth. So we have a delimodulation, and you think it's very large for both cases. For the center of mass, this case, and also for the non-diabatic coupling. And what is more important is this graph. In this graph I'm showing the neutron, I mean the dark matter, or in this case, anything colliding with your nuclei as a function of the mass of that thing. And as you can see here, this is the state of the art. This is what people have prepared as the best thing. Now they are trying to use silicons. They predict to use semiconductors to detect dark matter, because then after a dark matter event you can excite an electron from the valence band to the conducting band. Okay? So our guy, N2, is over here, not very good, but CO, is as good as semiconductors. So when I'm saying like if you use a CO, the detector as the one that we propose, we can beat or it be as good as semiconductor devices. And they have a different technicalities, but we are competitive with them. So again, molecules are really good and can be a potential good candidate to detect our matter in this range of mass. But you know what is even more funny. MIGDAL proposed the MIGDAL effect in 1930 something. No one ever measured that effect in atoms or molecules. That's funny. Yeah, that's right. No one ever, I don't know how to explain this, no one ever tried to systematically study how MIGDAL effect appears. One way to do it is through neutrons. Neutrons is the closest thing that we have to a dark matter, right? Kind of. It's neutral, so do not interact with the charge. Right? Basically do not interact with anything. As long as you are far away from any nuclear resonance for a fission of fission, you are good to go. And this is what we are trying to do. So we are proposing now in the Overreach National Lab, we are trying to design an experiment such that we can really measure the MIGDAL effect and with that calibrate or proposal to build the real detector for that matter. The idea is the following. We have a gas of CO molecules and we have a neutron beam, very low energy. He has to go low energy because we don't want to buy an ICO. So the neutrons have to be low. That's not a problem, you guys can't do it. There's only two things. Three or four labs in the state that can do that. It's a very complicated and expensive thing and you have to go there. So there's nothing that you can build in your lab with neutrons. So the idea is like now we're going to go from here to there. But the benefit of the MIGDAL effect, then only about the coupling, like you go to a state with different symmetry. So what it means is like, when you excite a guy, it may decay to an intermediate state and this signal is unique. This photon is of resonance with any transition from the ground state to another guy. What it means is like you have a background free detection scheme. Then you put all this with UV photo detector which are fairly simple, way easier than IR photons to detect. So it's using photo multipliers that can work. And then the good thing is like we can do it even at room temperature. Because we only care about vibrational excitation. We don't care about rotation. So even if the gas is in rotation, we don't care. We are good to go. And then we can do it in high pressure. We don't care about collision. As long as we don't quench the electronic state. So we have to be sure like the lifetime of this guy is way longer than the typical collision of time. Sorry, the other way around. Otherwise the guy will decay. Okay? So now to conclude. I hope to convince the Murgurs at gas phase are potential to become an effective thermal detector. We are sensitive to spin and spin independent. The Murgurs are making that effect incorporating non-alibatic effects. An important thing is like we have a daily modulation as I mentioned also directionality. I didn't put a point of that because you guys don't care much about directionality. But the good thing is like if you align your molecules and let you feel or something like that. Then you can see where the momentum transfer happened. And then you can see where the direction of that matter. Because we don't know what is the direction of that matter. We know that we are moving in the galaxy, right? Because the solar system is moving with the sun. In the arm of the galaxy we know what is the velocity but we don't know what is the direction of that matter. And that's something that can help us. And to that I would like to say like maybe we can work together. At least I'm doing that, I'm having a lot of fun. I hope that you guys can also do that. Indeed, Michael already did something about habit and spectroscopy. And so far so good, right? I guess he cannot complain. And now I will use five minutes. This is another thing that we do. So we just published a few reports on this thing. This is one of the models for that matter, okay? Or a physical instrument model. Like this is again an assumption. Okay, you can believe it or not. It's up to you. Standard model particles, everyone believe on that, right? Then we have the so-called hidden sector. Hidden sector is a bunch of weird things that we did in the dark side. We don't know. I mean, we cannot see them. But somehow these are portals that look like very science fiction, right? But this is a real model, okay? There are some portals, different ways to connect the unknown to the known world. Because somehow in our world we should see some evidence of this unknown world. And the portals we can put constraints on how important are these guys. It's something that Michael did. So the idea is like, let's say you have a bunch of molecules in our system. But if there's something out there, there's some kind of vibration or field going through that. So basically your molecules will feel it. So now you go and do hypersignal spectroscopy, your atoms and molecules, you should be able to see or to measure the effects of these weird things that you're not aware of. In this case we choose positronium, which is a fairly simple system. It's just a bound state of a positron and an electron, fairly simple. Okay? And what happened is the following. We have the singlet and the triplet. Triplets are long-lived and singlet. These guys annihilate superfast. They're not good. But then what happened is like in the experiment they can measure these transitions very, very accurately. It's just a way that Michael did in his experiment. But now we can also put constraints on different models like action like particles that fit for what you want. Because they can measure these really well. And then based on that we can see how this thing can be realistic or not. This is an example. Let's assume that we have a scalar interaction. I'm going to assume that they have something out there which interacts with a scalar field. Okay? Then this is what we got. So we have the p-s bound, so the positronium bound. And this is the G2 of the electron. So the geomitiv factor of the electron. The geomitiv factor of the electron is much better than positronium. So long story short, you want to put constraints on this. Use G2 of the electron, not positronium. It's not good. We can go and assume and then we have the following. We have the same as before. These guys were worse. But then we have this dashed line. This dashed line is like if we use reverse states of positronium. You can also do that. Okay? People can do that. But we don't get much. Okay? So the thing is like, if you really want to compete with this guy, they should be able to measure lines in positronium with 100 Hz precision, which is way beyond they can do right now. Right now, the velocity can do 100 kHz. Not the best. So long story short, it's hard that positronium is going to be useful for a physical and a standard model with this scalar model at least. Okay? Then we can do the same for action like particles, which is kind of a spin-spin interaction. And again, long story short, G2 is much better than the positronium. In this case, again, we have to go like very, very high precision, something that now they cannot do it. Maybe in 10 years they could, but maybe it's no point to go for different speedings. And just to finalize, I would like to advertise this. Right, Michael? Do you remember that? I invite him to contribute to this, but he keeps forgetting. It's fine. So we start, I mean, this is a field that now is growing, at least in the States. There is even in demo, there is a new topical group about high precision. And basically, there is a bunch of people experiencing the addition, they measure things really, really accurate. And with that, they can put constraints on many crazy things that you can imagine. One of them is their model. So based on that and also my, I mean, what we like, we start this Cambridge Elements and fix it in the standard model without becoming a regular system. And this is open to anyone to contribute. Okay, it's kind of, these Cambridge Elements is like something in between a chapter and a review. It has something about your personal view of the field and has something about a review of the field. And this is open to anyone. I invite Michael, I hope that he can contribute someday. And this is just a way to advertise what we are doing in this direction. I would like to touch that AIMO and Hanging Physics can work together holding their hands, I hope. And just to finalize, I would like to say that I would like to thank Professor Michael Duesen for the invitation all of you and the funding. And I feel like a kidney can't stop. Thank you very much.