 Hi everybody, welcome to this event, the Hunt of the Origin of Cosmic Race from La Palma, that is jointly organized by MAGIC and CTO. Today is the International Cosmic Day, so what a great day to talk about cosmic race and how we can study them through the observation of camera race. We're going to talk in this event about the scientific part, but we are also going to talk about two projects that are trying to disentangle this mystery, this origin of the cosmic race, from what side we are going to talk about MAGIC, which is the current generation of telescopes for the ground-based gamma ray astronomy, and from the side we're going to talk about CTO, the next generation and what will be the first ground-based gamma ray observatory. And even though MAGIC and CTO are different projects, are separated at La Palma, we are very close by, we are neighbors, and so we can do a joint life connection. After some presentations, we are going to connect with Lina Max that are there at La Palma, and they are going to show us the two MAGIC telescopes and also the LST-1, which is the CTO's large-sized telescope prototype. So before starting with the presentations, just to tell you, if you have any questions or comments, you can put them already at any time of event in our social media in both CTO and MAGIC, Facebook and YouTube channels. At the end, we are going to go back then and we will try to answer all your questions. So without any further, I would like to invite Dominique, who is going to provide an introduction of MAGIC. Yes, hello Alba, hello everyone. A pleasure to be here with you today and to talk about this long-lasting mystery that we are trying to disentangle on the Canary Island of La Palma. And as you have already heard, one of the projects we are operating there and have been operating now for nearly two decades is MAGIC. So as often, I mean, MAGIC is of course an acronym, but it's also telling. So it's in the world what those telescopes do. They are the major atmospheric gamma ray imaging Cherenkov telescopes. Now that's a lot of words in one short acronym. Major, of course, those are huge telescopes. You see in the backdrop already one of those telescopes, they have a 17 meter diameter mirror. So they are basically larger than a typical house. And then atmospheric gamma ray imaging Cherenkov. So that's basically what is happening here. The way we detect high energy gamma rays at the surface of the earth, it's an indirect way. That is necessary because of the, in principle, of course, very good circumstance that the atmosphere of the earth is not transparent to gamma rays. So in a way, the atmosphere of the earth, of course, it protects us from this flux of high energy particles from the universe. And that's basically that's good for life on earth, of course, but it's a bit of an obstacle for astrophysicists trying to study those particles from the surface of the earth. And now what can we do about this? Either we can put our telescopes onto satellites and do our observations from space or we can become very creative and use this effect of the absorption of gamma rays to make ground-based observations possible by an indirect way. And this way you can see in principle here. Now to the right on this slide, there is the telescopes. Those are not precisely the magic telescopes because there exists several Cherenkov telescopes, of course, on earth, but there's a system of two telescopes, not unlike the one we operate on La Palma. And you see from the top left the gamma ray particle, so the photon entering the atmosphere of the earth. And what does it do? It produces the cascade of charged particles, electrons, those particles that make up the, together with the nuclei make up the ordinary atoms, what matter consists of. So it produces a lot of electrons that move through the atmosphere of the earth. And now those particles, they are so fast that in principle they have to pay a speeding bill. They are faster than the speed of light in the atmosphere, which is always slower than the speed of light in the vacuum. Being faster than the speed of light in the vacuum is not possible, we know since Einstein, but being faster than the speed of light in material, like air is possible, but comes with a speeding bill. And this speeding bill, it's paid in the form of a short flash of blue light. And this flash of blue light is called the Cherenkov pulse. This can be detected by those large telescopes on the surface of the earth and using fast cameras. And that's the basic principle, how we can detect very high energy gamma rays and other particles from the surface of the earth, from the Rokate-Los Mochaches on La Palma. You can see an image of one of those Cherenkov flashes in a typical camera to the lower left. So what you see is basically just a very, very short 10 nanoseconds or 10 billions of a second long flash. And this is what carries the information we so crave. Now, how do those telescopes really look that we operate? You see another picture here, the system of two telescopes, they work stereoscopically. So they both look at the same air showers from two slightly different directions. And they consist, of course, of those large mirrors, so 17 meter diameter mirror, you can see them reflecting the starlight in these images here. And you can see on those long booms in front of the mirrors, of course, you can see the cameras. Those cameras, they have to be very fast because they have to detect those nanosecond long flashes of light. And they have, of course, to be very sensitive because there's not a lot of light that is produced by these air showers. And now the information that is recorded by the cameras, it goes to this building you see in the lower left, our accounting house control building that we actually share with CTA LST-1. So this is the next generation of Cherenkov telescopes on the Canary Island of La Palma. And it's recorded there and then sent for further processing to the participating physicists that come actually from more than a dozen countries, basically all over the world. You can see on this map of the world here, you can see the location of the magic telescopes on the Canary Island of La Palma. And you can see in blue with the countries where we have major participation of physicists from. And this collaboration, it's composed of, in total, about 300 members, physicists, technicians, administrative staff, and many others, also students, of course, that participate in this decade-long and very, very fundamental and fascinating quest for the origin of the cosmic rays. Now, what those telescopes can actually do and what is especially exciting also in the context of the mystery we try to unravel is that the lightweight structure of those telescopes, and if you remember this carbon fiber structure that you have seen carrying the mirror and the cameras, you will shortly recognize it again in very great similarity when you look at the LST-1 telescope, it enables a very rapid movement of those telescopes over the sky. So we are able to catch short events, rapidly evolving events, and of course, those might hold some clues to the origin of those mysterious cosmic rays. Among those events, what we have been successful in catching over the last years are fast brightness changes from the centers of distant galaxies. Those centers that often host supermassive black holes, so black holes with masses millions or billions of times larger than of our sun. And when matter gets accreted onto this black hole, so matter falls into the gravitational potential of these black holes, we sometimes get dramatic increase in brightness of these objects, and then we can spot those, we call them AGM flares, so AGM for active galactic nucleus, an active center of a galaxy. And when it flares up in brightness, we can quickly catch that. We have been successful in tracing cataclysmic cosmic explosions, which happen at the end of the life of very massive stars, and which we call gamma ray bursts. And we also have been able to detect eruptions of binary stars much closer inside our own Milky Way in the form of so-called Norway. So that's a short overview over the magic telescopes and some of our recent science highlights. And with that, I'll hand over, again, back to Alba for an explanation of the next generation of Schrodinger telescopes on the Canary Island of La Palma and elsewhere in the world. Thanks a lot, Dominik. So I'm going to share now my slides. I hope you can see them. So just very briefly, I'm going to make an introduction about CTO that stands for Schrodinger Telescope Array Observatory. And I would like to start answering this question. What is CTO? So I mentioned at the very beginning that CTO will be the first one-base gamma ray observatory and the world's largest and most sensitive detector for gamma rays. We're going to have two telescope sites, one on the northern hemisphere, one in the southern hemisphere. And we'll talk about them a bit more in detail in just a couple of the slides. But CTO has also other facilities. We have the headquarters at Bologna in Italy, also some offices in Heidelberg and the center for management, for the data management in Soiten nearby Berlin. Right now CTO is in charge of the design and implementation of the observatory. Once the new legal entity so-called Eric is in place next year, we are going to be responsible for the construction and operation of the observatory. And CTO actually works in close cooperation with the so-called CTA Consortium, group of scientists all over the world. As you can see here, we have groups in five different continents. And CTO and CTA Consortium work together in the definition of instrument designs and the scientific program. So here we have the two telescope sites for CTO. As I said, one in the northern hemisphere in La Palma and the Canary Island in Spain and one in the southern hemisphere in the Atacama Desert in Chile. So these two sites, actually it's the first time we have a ground-based gamma ray facility with two sites. So we are going to be able to cover the entire sky. And they are going to be focused on different science topics. For example, in the northern, we are going to focus more on astragalactic physics. So observing sources that are beyond our galaxy, while in the south, we are going to focus more on the galactic physics. So those sources that are within the Milky Way. But since today, we are going to have a live connection with La Palma. Let me just tell you some more details about the CTO northern array. It is located in the existing Roque de los Muchachos Observatory in La Palma where Max and Lena are. And in the first construction phase, the so-called alpha configuration, we are going to have 13 telescopes. You have here a rendering. This is not exactly the picture or a rendering for the alpha configuration, but you can have an idea about the telescopes that we are going to have. For example, you can see that we have different types of telescopes. I'm going to talk about this now. Here also in this rendering, you can see the magic telescope here. I don't know if you can see my mouse, but you can see the back of the magic telescope here. Magic are not part of the CTO site and array. But as you can see, we always say we are neighbors because we are extremely together in La Palma. So actually, as I mentioned, we are going to need different types of telescopes. And this is because CTO is going to cover an unprecedented energy range. We're going to catch gamma rays from 20 gigal electron balls up to 300 teratron balls. This is a lot of energy just to give you an idea of how energetic the light of this, how energetic the light we are going to observe is. The light we have in the offices or at home has an energy of about one electron ball. So we are talking about billions and trillions more energetic light. And to cover this broad energy range, as I said, we need different types of telescope. I'm not going into details because I don't have a lot of time, but here you have the small size telescope. These are going to be only on the south in Chile. And they are responsible actually for the highest energy age. So they are going to be responsible for observing these 300 TV. Then we have the medium size telescope and finally the large size telescope. These are actually in charge of the lowest energies even though it doesn't look like that. And we actually have already one large size telescope. We have a prototype of this LST, the so-called LST one that is located at La Palma and this is the one that we are going to see today with Lena and Max. This telescope, the LST one is under commissioning. Once this commissioning phase is finished, it will be accepted by CTO and it will become the first telescope of CTO. And while we want to build this observatory, while we see with Dominique there are already current generations working like magic, also the facilities like HES and Veritas and they've been working a lot for the past years. They've been doing great science but this field, the gamma ray, the ground-based gamma ray astronomy is extremely young. It's barely 32 years old. So there is a lot of scientific and technology potential ahead of us and that is where CTO enters. As I said, it will be the first ground-based gamma ray observatory will be the largest and most sensitive instrument to detect gamma rays. We're going to push also the electromagnetic spectrum observing up to 300 TV and with that performance, we're going to get a completely new window, new view of the sky. Also, we have two sites for the first time so we are going to get access to the entire sky and based on the knowledge from the predecessors like magic, we're going to build a state-of-the-art technology and software and we expect to detect up to 1,000 new objects. And also very important, the data on the software tools for CTO, they're going to be available worldwide so anybody are going to be able to analyze the data and do science. And just to finish, I'm not going to talk a lot about the science because I don't have time but I would like to share with you the three main topics, the three main scientific cases for CTO. Here you can see the extreme environment so we're starting Neutral Star, Black House also starting beyond the standard models, the physics frontiers now, for example, trying to disentangle the nature of that matter. But I would like to highlight the first topic because it's very related with today's International Cosmic Day. One of the main topics, scientific topics for CTO is understanding this cosmic particle acceleration, understanding where this cosmic rays come from, how they can be accelerated up to almost the speed of light, how they propagate in the universe and how this propagation affects actually the environment. And finish here, if you want more information about CTO, don't forget to visit our website and also follow us on social media, we're always putting more information. And with that, I finish and I actually would like to ask David to join me here. He will be talking about the cosmic rays actually. Hi, thank you Alba. So I think given the unenviable task to talk about 100-plus year mystery in physics and 100-plus year of physics results, so I am just going to very briefly go over cosmic rays and how we can study them, gamma rays and such instruments like LT, CTA and magic. So cosmic rays were first, we had known about, physicists had known about a low level amount of radiation just, you know, urban earth. Since the 1890s, you know, very early days of physics, they use a device called a lecture stick scope. Most physicists had assumed for a long time that this radiation came from the earth in the form of radioactive elements that had been discovered by Marie Curie around that time. And then came along a physicist named Victor Hess who had a different idea that this radiation actually came from outer space up above. So he had an idea. So he got into a hot air balloon and went up very high in altitudes, about five kilometers above earth with one of these telescopes to measure the amount of radiation as he went up. Now, five kilometers is nothing to sneeze at. It gets as cold as naked 20 degrees Celsius. So imagine doing this around 1912 in a tweaked laser going up five kilometers in a hot air balloon with a little device. These were pretty bird people. And what he discovered was that the amount of radiation as you go up higher in altitude increases. So he proved his hypotenuse to some basic science and proved his hypothesis that this radiation is actually coming from above from outer space. And he called these terms cosmic rays. And for this he won the Nobel Prize in 1936 and invented an entirely new field of cosmic ray physics. So the question that we kind of want to answer as physicists is what are these cosmic rays? We've learned a lot over the past 100 years. We learned that cosmic rays are mostly protons by 89% of them with some helium atoms thrown in about 1% are electrons and 1% are actually every other element that includes things like carbon, calcium, iron, all the way up to, I forget exactly what the heaviest moment is, but they go very heavy, well past iron. We also know that the abundance of the amount of materials that we see in these cosmic rays is very similar to what we see in our own solar system. So this implies that at least some of these cosmic rays are coming from inside our own galaxy, our own galaxy. We also know that cosmic rays cover an immense range of energy. As Alda said, we use this as a unit called an electron bolt which in itself is a very small unit of energy. Cosmic rays go all the way from a few GEV, that's 10 to the 10 EV, all the way up to 10 to the 20 EVs. That's 10 quintillion electron bolts. These are the ultra high energy cosmic rays. To put 10 quintillion, because that's just, I'm sorry, 100 quintillion in the number, that makes sense. That's the equivalent of kicking a football at 50 kilometers per hour. Remember to also put this in some sort of context that the largest particle accelerator on Earth, the Large Hadron Collider, can change the switch length only makes, accelerates protons up to 10 to the 12, seven times 10 to the 12. So only a fraction of what we see in cosmic rays. But for all that we've learned, we still don't know quite a lot about cosmic rays. In fact, one of the biggest mysteries of cosmic rays is where they come from. We do not think that these cosmic rays come from a single object, like say one star or one black hole within our galaxy, that they come from a type of objects, a class of objects. One of the main issues and problems with cosmic rays is that they have underneath charge to them and charge particles when they interact with magnetic fields like this picture, of the magnetic field measured over our own galaxy, they deflect. And as you can see here in this video, when you put a magnet up to a beam of electrons, it bends. So these cosmic rays, as they're flying through the galaxy or hitting these magnetic fields, bouncing every which way. And since they have a, the galaxy is full of magnetic fields of different directions and strengths and everything, these cosmic rays are bouncing around the galaxy like a pinball machine, like a pinball and a pinball machine. Fortunately, we have what's such a device that allows us to really know where cosmic rays are coming from with those cosmic rays. This is why we do the science that we do. So gamma rays, which are just as Alba and Dominique said, are just light, just very high energy light, but light doesn't have a charge like say a proton or electron does. So the gamma rays can travel straight through the galaxy and point us back towards where the cosmic rays. And we also know through lots of science that when cosmic rays indirect with matter, such as interest in gas or even visible light through processes that have fun names as inverse compton scattering or pi zero protection, that they will create very high energy gamma rays. And that the gamma rays will only have a fraction of the energy that the original cosmic ray did. And these gamma rays are perfect for such telescopes as are, as Ajay has to bear a toss these very high energy telescopes and for these future observatories like CTA. So gamma rays, you know, will night will travel straight line, as you can see here in this animation, while the cosmic rays will bounce around. So we can use gamma rays as a trigger for bear think that cosmic rays are being accelerated to try to figure out where the cosmic rays are coming from. So we have a lot of candidates and ideas for where cosmic rays are coming from. One of the strongest candidates we have are where it calls supernova magnets. These are leftover gas and dust accelerating very quickly from the depths of massive stars. From either hundreds or thousands or even tens of thousands or hundreds of thousands millions of years ago. We have some nice pretty images here, one such example as the Casio-PA on the left. And these explosions create shock waves that expand into the interstellar medium, the dust and the gas. And these travel and the shock waves travels hundreds of kilometers per second, which creates an ideal location to produce cosmic rays. And we know that from observations from telescopes like magic and has some veritas and soon to be CTA, that these supernova magnets can produce gamma rays. And that these gamma rays are coming from the protection and acceleration of cosmic rays. Unfortunately, the answer still is not 100% clear because we also know from studying these sources that they produce high energy cosmic rays. That the cosmic rays only go up to a couple of TV, a couple of tens of TV, that's 10 to the 12 EV energy. So, and also that most supernova remnants only create cosmic electrons. So we're still missing 99% of cosmic rays, the origin of 89% of cosmic rays. We also know that supernova remnants can leave behind fast rotating neutron stars, which we call pulsars, which have extreme environments, crazy high magnetic fields. And that these pulsars can create huge outflows of cosmic electrons. And such a class example that we often use in our field is the crab medulla. But again, these are only creating cosmic ray electrons. So we'll still have a mystery that our galaxy of where the cosmic ray protons are coming from, where they're being accelerated. Another such source that was mentioned earlier by Dominic and Alba are active galactic nuclei. These are cores, dense cores of galaxies, millions and even billions of light years away. And we think that these are the origin of these cosmic rays that come from outside our galaxy. There's cosmic rays from inside and outside our galaxy. And we know that these cores are very bright and gamma rays. We see tens and dozens of these active galactic nuclei in the air and in the sky. And their key science started for the CTA North Observatory. They can create large jets, which spew out material and matter, as you can see in this animation, and could create cosmic rays that the highest energy is Earth. But then again, we still don't see these key signatures that we're looking for to create cosmic ray protons. We think that most of these are very easily to accelerate cosmic ray electrons. So we're still missing a lot, so missing the origin of these cosmic ray, the majority of cosmic rays is protons that we're trying to find. But that's where CTA can come in and help. And the current generation of IOC of the very high energy gamma ray telescopes, because these will have unprecedented sensitivity as Aldo just showed towards observing gamma resources and unprecedented sensitivity and ability to detect gamma rays will solve this hundred plus year of history that we're all working on. Thank you. Okay. Thanks a lot, David. Yeah. Yes, thanks a lot for this super nice context on cosmic rays. I think that after having a look to the project, to the telescopes and the science in presentation, it would be time to watch them live from La Palma. So I would like to invite Lina and Max. Hi, Lina. We cannot hear you. Wait, now maybe. Can you hear us? Yes, I can hear you, but we cannot hear Lina. Maybe you are muted, Lina. Oh, I'm sorry, the classic problem. No problem. So I leave you guys to show us the LSE one and the magic telescopes. Yeah, okay. So Max is showing us around this and he's at this moment inside the area of the LSE telescope I've already told us about. We see here on the right, this is the camera tower and you see this bow from the telescope. There's, yeah, the camera located and yeah, the camera is at this moment safely parked on top of this camera tower. Yeah, and there we have the mirrors of the telescope. So we have a very large area of mirrors. It's like 400 meters and this mirror has to be, yeah, like bent a bit in a parabolic shape and you can't do this in one piece or you can't do a mirror in this size in one piece. So what we do usually is that we use this, a lot of smaller mirrors and arrange them in this parabolic shape. And we see here, I think it's 198 mirrors we have here in hexagonal shape, yeah. And so yeah, Max is standing directly in front of the large size telescope. So as Alba already told, this is the prototype for the LSE telescopes, large size telescopes for CTA. And Max is showing us now the rails where the telescope can rotate. And we see here that all of those rails are covered with plastic, yeah, plants. This is because you maybe have heard of it. We had a volcano eruption here on La Palma, which is still ongoing. I think like 50 or 60 days now. And the ash is raining down on the observatory. So if the wind blows all the ash from this volcano to our observatory, the ash is raining down and covers nearly everything. Yes, every bush, every stone, and of course all telescopes are covered in ash and yeah, we have to protect especially those rails with these plants so that there's not that much ash coming down on the telescopes. At this point, maybe I can say, so the problems we have here in the observatory are quite little compared to the problems the people have living close to the volcano. So all our thoughts are with them and yeah, we are really, yeah, try to supporting them wherever we can. Okay, so now back, Max is showing us the LST tower again where the camera is resting. So this white thing up there. And then we see here the containers where, yeah, the operator sits on the left here. We have the container, there's so some, yeah, just some computers and some tables where we can sit and operate the telescopes. And now Max is opening the fence. All our telescopes are surrounded by fans that know, yeah, visit or tourists which come up the site sometimes can entering the telescope area because it would be quite dangerous if some person randomly spends near the telescopes and then the telescope is moving. So we have a lot of, yeah, a lot of fences here who protect the telescopes and especially the tourists. Okay, now here we see the fact telescope. We haven't here about the fact telescope. Now this is a very small telescope compared to this big LST and the big magic telescope. This has just a diameter of I think 4.5 meters. Then this was a prototype for new camera technology. Yeah, and this was a very successful project, yeah. And yeah, exactly. So we see here this white thing on the right is the camera and there's, you see this black cover so this is the ash on the camera. We haven't removed it yet. Yeah, okay, and yeah, in the background you see very nicely this huge LST telescope. So I think on the video, you might not see it but it's really, really big. Okay, so here we see other telescopes on the side. So we have more than 60 telescopes in total and this is Rocker, the Los Machachos. So this is a very big observatory and we have not just our drink of telescopes here but also a lot of optical telescopes. You see, yeah, I think the Githi see the Gran. I don't know the name of this telescope. It's the Githi. Gran Telescope, your canary. That is the name. So Max knows all the facts. I don't know. Yeah, okay, and if you, Max, if you go a bit to the right then we might see no other way around, maybe to the right. Then I can show you. So in the back there, so stop. There would be the volcano ash if there would be any volcano activity at the moment or volcano activity we see. So then the great clouds come up in the right here. So behind this is still there. Okay, so then I think we can go to the magic telescopes. Okay, and here we have the magic two telescopes. So this is the second telescope that was built and inaugurated in 2009. And yeah, it is quite similar to the LSD telescopes. So we have, again, this big mirror dishes with a diameter of 70 meter for the magic telescopes. And of course, this camera bow and the camera resting at the tower at the moment. And if you look very closely, you might see that, for example, the mirrors of the magic telescopes are in a squared shape, whereas the mirrors of the LSD telescopes, the large size telescope is in a hexagonal shape. So if you ever come here, yeah, you can decide by the first look which telescope is the LSD and which telescopes are the magic telescopes. Okay, so yeah, here it is in principle the same. We are the same stuff with the covering of the drive. So we also have to cover the motors and the drive for the magic telescopes to protect them from falling ash. And now it's shaking a bit, but Max is going up the camera tower. And from this point, we will have a great view of the size and on like around. You see Max now in the mirror, he has a safety first wearing a helmet and so some of these neon jackets so that we are safe here. So we see his reflection in the mirrors as I said, 17 meter in diameter. Okay, and now he turns around. So this is the camera which is parked at the tower now. Okay, and then in the back there, you see the LSD telescopes and there where this reddish roof is, I am sitting under this roof and talking to you right now. Yeah, and here you have the very nice view from the rocket as much as us. At the most times we are above the clouds so you see the clouds there. And this is one of the reasons why we are here on top of a mountain or on top of the rocket because we are above the clouds and we have a very great view and the very clear sky most of the times. So Max is going down now and we again see the LSD telescopes. Okay, and there's the reflection of the camera in the mirrors of magic two. And I think we now might go to magic one. So there's this containers everywhere. There's all the electronic stuff. This shouldn't get wet. So we put them in this big containers. So we left the fence behind. Also magic one and two are surrounded by fences to protect any visitors from just going near there. Okay, and so now we are closer to the magic one telescope. So this is the first telescope that was built and that was I think finished in 2004. And now Max is entering the fence of the magic one telescopes. And these both or both these telescopes are in principle quite identical. You might see if you have a look at the mirrors we see now that the mirrors are a bit, yeah, not plain but a bit foreign back. And this is the major thing where you can distinguish between a magic one and magic two from the first side. Yeah, but in principle the camera and all the electronic stuff is mostly identical. And we point these telescopes to exactly the same position in the sky. And as Dominic already told us there are measuring in stereo mode. So they are measuring or taking data from this rank of showers from two different positions and from this two different images. Yeah, we can learn a lot about the shower and about the particle and the direction it came from. Okay, so Max is now going back and yeah, we see again the LSD telescopes in the counting house where I'm sitting. This white dome that you can see there, there we have a laser which we are shooting into the atmosphere where we can measure the atmosphere. And for example, or we can measure their clouds, mainly this is the main reason why we need it. So we want to know there are clouds in the sky or clouds covering the source we want to see and we can measure that with the slider under this big white dome there. Okay, and then I think we are at the end of our tour. If Max hasn't any additional thoughts and then we would like to show you a very short video of our time-lapse Max did yesterday or the day before yesterday and where we can see the LSD at night and the stars moving behind that, okay. So I think, ah, yeah, there we are. So we see here the LSD, this is a time-lapse. It's about two hours in 20 seconds and you have this bright thing behind the LSD. This is the moon going down. Yeah, and we see very nicely the sky, the stars moving in the back, some flashlights where our colleagues went there and yeah, have some flashlights. So and I think at this point, we are finished with our little tour. Thanks a lot, Lina. Well, I would like to invite all the speakers to join us here and meanwhile, let me tell you that the time-lapse is amazing and thanks a lot for walking us through the observatory. It's nice to see it even if it is remotely. Hopefully we will come back a lot of us there soon. So I don't see any comments or questions on our social media. I hope it was everything super clear, the science, the understanding why we want to what we need to observe gamma rays to shed sunlight on the origin of cosmic rays and also I hope it was clear, the projects Magic and CTO and the LSD one that we are seeing now with Max there. So let's finish here and let me thank all the audience and Marina who is in the back stage, moving everything, making it run. And that's it. See you in the next event. We will do magic and CTO together. Thank you and have a good and safe time wherever you are and have a good and safe time at La Palma. Ciao, ciao. Bye-bye. Bye-bye.