 Und wir wären sehr glücklich für die Feedback auf Twitter mit dem Hashtag C3T. Promoviert gerade beim Desi-Zentrum in Seuthen. Das ist unser honor to present. Der Titel ist Kosmische Teilchenbeschleuniger und ihre Spuren in der Angt-Arktis. Angt-Arktis ist um Kosmische Teilchenpartikel und die Trace in der Angt-Arktis. Und das ist Anne. Sie ist bei Desi und Seuthen. Sie ist eine Doktorstudentin. Wunderbar, dann erst mal Danke für die traumhafte Angt-Arktis. Danke, Anne, für die Introduktion. Ich stelle dir einfach vier Fragen zu kontrollieren, ob du es verstanden hast. Ja, ich werde dich fragen, ob du es verstanden hast. Willkommen zu meinem Vordergrund. Herzlich willkommen zu den Gesprächen über Kosmische Teilchenpartikel und ihre Trace in der Angt-Arktis. Es gibt zwei Names, die ich in den Vortrag geben will. Das ist der Vortrag meines Kollegen. Das ist der Vortrag bei meinem Freund. Aber er hat gemerkt, dass er jetzt in Shanghai ist. Er ist in Shanghai. Der zweite Grund, der größte Grund für diesen Vortrag über Hause, ist, dass dieses Jahr, der große Durchbruch in der Astropartikelphysik in meinem Feld für die Forschung kam, das letzte Jahr, ich weiß nicht, ob ihr das seht, der erste Mal, dass es Gravitationalwaffen vorhanden war, von den Kollisionen von zwei Neutron-Styles, dieses Jahr, dass es für den ersten Mal eine große Nase für den Eis-Kub gemessenen Neutrinos und das Eis-Kub mit dem Eis-Kub-Detektor verwendet wurde. Das ist für uns ein riesigeres, größter Ding, für uns. Ich möchte euch jetzt nicht erklären, was diese Entwicklung war, wie wir da sind und warum es so spannend ist. Warum wir auch so stolz sind. Der erste Grund, warum wir stolz sind, ist, weil die ganze Geschichte vor über 100 Jahren angefangen wurde. Denn alles begann über 100 Jahre ago mit Victor Hess, und er hat die Altitut-Radioaktivität in den Anfang des 20. Jahrhunderts getestet. Ihr könnt euch nicht wissen, dass das Radioaktivität, das war eine große Sache, das war in der Forschung, und wenn die Leute die Radioaktivität researchen, sie wollten auch, wie unsere Erde radioaktiv wäre und die Radioaktiv-Räse. Also, das ist meistens von der KA-Serie, von Tourium und Uranium, und Victor Hess hatte das Objektiv, um die Decke der Radioaktivität zu detectieren mit der Altitut, und er wollte in einem Ballon fliegen und die Decke der Radioaktivität zu detectieren von der Erde, und er wollte detectieren, wie ionisiert er ist und wie kวioe er ist, das war der Secondary signature of Radiation. Victor Hess hat das auch durchgelegt ... Victor Hess did that, did balloon flights. You see him in the picture. On the translations, you already see letters, and ... ... und unter er, okay the B's are picture references All die Referenzen sind open Access, und ihr könnt mehr informationen bekommen, um die Referenzen in der unteren Rettkante zu tracken. Zurück zu Victor Heß. Zurück zu Victor Heß. Victor Heß hat Ballon-Flights, und er hat gemerkt, dass die Radioaktivität, die Radioaktivität mit Altitüten, aber dann, es erhöht. Er ging über die Rente, über eine bestimmte Altitüte, und der Air war in Iona stärker. Bei 10.000 Metern Altitüte, es war ein Faktor von 40 Up. Victor dachte, das sei stupid. Die Radiation, die die Air, die Atmosphäre, muss aus dem Raum kommen. Das war das Erste des Kosmik-Rais. At that time, es war Altitut-Rais. Er hat gemerkt, dass da kosmische Teilchen, dass auf der Erde, und die Air ionisiert. Wir fragen uns, woher es kommt? Was ist das Kosmik-Raviation? Es gibt noch Ballon-Experimente. Heute gibt es noch Ballon-Experimente. Die Ballon-Experiment hat das gleiche Fertigkeits-Satellit als das 8MS-Satellit. Es war transportiert nach der International Space Station. Bei hohen Energien wird es in der Space itself geprägt. Es ist praktisch, und man kann es immer machen. Man muss nicht Ballons fangen. Das sind die Teilchen-Detektoren. Die Teilchen-Detektoren sehen, wie diese Teilchen-Detektoren sehen. Das ist der AMS-Satellit, das ist auf der International Space Station. Das sind die Teilchen-Detektoren, die von der Partik der Physik wie der Large-Heartron Collider gebaut wurde. Es ist eine Part, die die Velosität betrachtet. Der Korps ist ein Magnet, ein Magnet mit einem Tracking-Detektor, das Detekt die Charg-Partikel in einem Magnet und die Menge der Kurvaturen des Deflektions erhältst du die Energie und die Momentum. At the bottom there is an electromagnetic calorimeter that stops the particles and measures the energy, we get to the next point, why can't we use satellites everywhere at higher energies, just the particles don't get stopped in the electromagnetic calorimeter and the trajectories in the tracking calorimeter relatively straight. The other reason why at higher energies we can't work with satellites is because the particle flows are very low. So these satellites are very small and you won't be able to measure anything and that's not very practical that's why you use for higher energies a different way of detection that's something you do on Earth before you these particles arrive at Earth and they interact with the air molecules in the atmosphere and what happens it's some kind of air shower so a cosmic radiation particle hits the atmosphere and interacts with the molecule in the air and then there will be a whole zoo of particles like mesons and millions also photons and this here you can see it here very artificially it's a whole network of particles and these secondary particles these are the ones you measure on Earth and for this reason that's a particle from some observatory that's the largest observatory that does this nowadays they just installed water tanks and these water tanks they put cameras so what you are measuring in these cameras is the Jarenkovs radiation of the secondary particles from these air showers Jarenkov radiation I'll talk later about this in more details just keep the question what's that, just wait so besides these water tanks they also have fluorescence telescopes that they use for calibration and these telescopes they just use the effect that this whole air shower moves through the atmosphere and the particles interact all the time particles in the air and excite them and what happens in the emission is fluorescence and that's something you can just see with classical telescopes additionally they'll get an upgrade they'll get scintillators on top they already started that so they detect electrons a little bit better and for completeness there's not only RG there's also a telescope array up there in Utah that's sizably smaller but they'll also get an upgrade in particular more detectors interestingly they're still a little bit smaller than the other but I don't know why they didn't make it larger but that's okay so we have new methods in order to detect these cosmic rays and that's why we can already say a lot about it we already measured quite a lot so what I'm showing you here is the results that you know in general on the left side there's a particle flow and I brought this in order to demonstrate why it wouldn't work with a satellite so in the x-axis you can see the energy that's an electron volt that's a weird unit but it's normal for particle physicists an electron volt is the energy a particle gains if you accelerated with a voltage of one volt so for illustration I showed the energies that you get at the LHC on the y-axis you see how many particles per square meter per time unit arrive at the atmosphere so you can see in the blue area it's a lot that's one particle per square meter per second that means with my square meter large satellite you still measure quite a lot on the middle of the right area one particle per square meter per year and all the way to the right one particle per cubic kilometer per year and that's when you need like the Tetergus like the Bergeri Observatory that has just like 3.000 square kilometers next to the information how many particles according to which energy we also have directional information so on the right side you can see the direction at arrival of the particles if you wonder why it's black at the top well that's because Orges is down in Argentina and they can't measure to the north they can't see that and you can also see this dotted line that's the galactic plane and the center is the star they measure from which direction in the sky they measure more and you can see more particles arrive in the bottom right that's what's greenish so one could say okay I know now where they come from then I maybe can answer what are the sources of the particles one knows a little bit about the sources one knows that at lower energies so if you go back to the plot on the left the blue stripe that's basically all solar cosmic rays in the sun one has verified that by looking at how does it correlate with what we measure with the activity of the sun in the middle like in the right area these are the particles mainly from our galaxy how do you know that well you don't know that 100% but one knows well cosmic rays they are charged particles they are like 90% protons 9% helium atoms and the rest is like more heavier atoms and some electrons, positrons and such but they are all charged and these charged particles they get deflected by magnetic fields for example in our galaxy I just really think these pictures are very beautiful and the the path these particles the curvature depends on the energy and now the lower particles the galactical magnetic field causes that these particles don't leave our galaxy probability that they leave our galaxy is extremely low so they before that they would interact and it would be billions of years until in our galaxy medium energies our cosmic rays are likely from our galaxy at the highest energies however the particles are capable of leading the galaxy and these curved trajectories are the trajectories you see there of the highest energy particles at the highest energies we know that a cosmic rays come from far away from a galaxy far far away in my talk I'm going to talk about the highest energy cosmic rays from a galaxy far far away outside our galaxy there are a lot of objects there are there are strong objects gamma bursts and back holes we still have the problem that the cosmic rays is deflected by magnetic fields and that the direction of impact the direction of arrival for the highest energies it can't be traced in a straight line to the sources so it's even 100 years after these first balloon flights it's not clear at all where these particles originate in this and we we're trying to use other particles too because our universe doesn't send protons and helium 4 alpha particles and for the search of the sources of this high energy cosmic radiation you could take the standard approach we look at what is particularly bright, we look at the photons that are emitted from the universe and the only thing about light is that we know lights from every day but light as information sources is extremely versatile you see the galaxy in the optical range here which you can see with your eye if you look at the Milky Way and this is already quite impressive but electromagnetic radiation has a lot of other wavelengths in ranges that I can't detect and if we look at the Milky Way in all sorts of wavelengths we get a much more diverse picture of this object one can get a lot more information and extract much more information and the nice thing is each wavelength range tells us something about different properties of the Milky Way in this case for example in the radio range you see emission lines of atomic hydrogen so you can do by radioastronomy you can look at warm clouds of gas that have lots of atomic hydrogen you also see the molecular hydrogen H2 in the radio range look at somewhat colder dust clouds in the infrared range dust is in emitting light that's excited by starlight and then re-radiates in the infrared range and at the highest energies we have that was really interesting we are looking for the sources of these highest energetic cosmic rays those are charged particles at a very high energy accelerated to a very high energy and in this and while they are accelerated they are radiating all the time when they get deflected when they interact so in the X-ray and the gamma ray range you get those could be those give us hints was the sources of the cosmic radiation are so they could but they are diverse problems with light the first problem is at the highest energies the light doesn't get very far in our universe there is something like the cosmic background radiation and that fills our entire universe that's a relic from the early primeval times when the when the universe was opaque and suddenly it became transparent and that gave the microwave background from a certain energy the photons interact with the cosmic background radiation and then they don't appear at the earth anymore and that means you see it in the graph to the right where you see the energy of the photon why axis and why axis is how far the photons get what you see is that at 10 to the 14 or 10 to the 15 electron volts the photons go only to the galactic center so a few kiloparsec and that's just not far enough so so we want to get cosmic rays from far from galaxies far far away they don't get far enough the light doesn't get far enough so light as information carrier high energetic light is an indicator of high energy particles but those don't have to be protons or helium cores necessarily so it could also be electrons so it's not unique so we can't uniquely discriminate which what the source that produces cosmic rays and the last practical point is that if I want to measure light and it has to be dark and on earth it's a problem and the telescope needs to be oriented correctly or we have to use satellites so those just not very good very accurate so are there other carriers of information too in our search for the sources of cosmic radiation and now we get to the third messenger to the retinos now I want to put a little insert or standard model in country to protons that's not in everybody's mind so it's a short excursion into the standard model of particle physics the complete matter is built out of leptons and quarks of leptons and quarks of the first family up and down quarks and protons and neutrons and those form the nuclei of atoms and around them are electrons and so we get our atoms all of our atoms and up and down are quarks and also in leptons there's the electron neutrino there's not just the first particle family from which which the matter around us is there are two more versions of this there's the same in terms of charge they're just heavier in each of these particle families there is a neutrino neutrinos don't constitute in our matter in that sense but in radioaktive they are important and they play an important role what properties have neutrinos they're not charged they have almost no charge 3-4 years ago there was a Nobel prize for the proof that neutros have finite mass that they don't have zero mass but it's still infinitely small infinitely small and they only interact weak interaction that's why they're often called ghost particles and how weak this interaction is is you can visualize by thinking about how many neutrinos impact the body per cubic centimeter per second 65 billions of neutrinos and obviously you don't notice that the interaction is really non-existent or it's only very rare so now we know what neutrinos are now we need a connection to the cosmic rays no if in astrophysical sources there are cosmic rays then they interact with other cosmic rays with other protons and helium atoms and from this interaction there will always be in principle always very often they will have neutrinos they have 5% of the primary energy so if you have a very high energetic cosmic rays then we will have also very high energetic neutrinos but like of a factor of 100 less but in contrary to light that means that if a source emits neutrinos then we will be very certain that they also cosmic rays because if not there would be no way of them being created so they are a jackpot for our work so they can travel extremely far because they interact very scarcely and it would really prove that they are really cosmic rays in these sources so we want to measure neutrinos and that's a little bit complicated so dass they get so far because they rarely interact so in a present year one detector, that's the ice cube detector in principle that's the neutrino detector for very high neutrino energy and that's the highest sensitivity for lower energies there has been a talk here in the congress but I think that was in day one that was coming under there are also other detectors that cover these high energies also in the future so I want to name them that would be KM3net that's being built in the Mediterranean and but for now we concentrate on the ice cube detector it's a detector that's one cubic kilometer large that's an incredibly large project over 250 scientists are in there and that's a beautiful example for a project that's crossing borders what ice cube does it detects the terrain cause radiation of interacting neutrinos so you never detect neutrinos themselves but you detect the lab tones that come from the interaction with neutrinos so in the bottom right you see I want to explain this picture so you have the electron neutrino that comes in the top left and that interacts with the neutron in the bottom left they exchange an interaction particle and what happens the electron neutrino turns into an electron and what I measure is this electron and the terrain cause radiation also so now an excursion to what is Trenkov radiation Trenkov radiation is a sonic boom just but for light this is if a particle in a matter propagates faster than light in a matter that's possible then Trenkov radiation happens and it's still the particle is not faster than light in vacuum it's only faster than light it's still slower than the vacuum speed of light this is still this hard speed limit we also know this from nuclear reactors which is the upper right picture the blue glow that is the same effect that's Trenkov radiation so if we want to detect an electron neutrino how does that work the electron neutrino gets into the detector it does an interaction an electron and the electron produces Trenkov radiation and we want to detect the Trenkov radiation so they build a giant detector for that one cubic kilometer and lots of cameras that detect that blue light of the Trenkov radiation 5.160 cameras on ropes and every 17 meters there is a camera module for blue light those lines are built with 125 meters distance and it starts from a depth of one and a half kilometers and goes down one more kilometer there are not only these 86 wires or strings that are spaced 125 meters apart so there is a core which is a spaced tighter to do other measurements and on the top there is in principles a detector like the OJ observatory those are ice tanks to detect cosmic radiation ice cube like OJ wants to do an upgrade they want to increase the volume by a factor of 10 and they want to do some improvements to the deep core so we want to detect this Trenkov radiation and for that every 17 meters on some strings there are optical modules and it's so impressive how this is built so I brought some photographs which drill 2,5 km deep into the ice and how they did it after they drilled through the snow for the ice itself you use hot water drills because if hot water meets ice the ice melts in principle they got a column of standing water and into that standing water columns they lowered their strings with the detectors and that worked extremely well from 2004 to 2010 they built this and obviously you never can retrieve the additional optical modules if one of them fails but more than 98% of these things are still functional this is really impressive this is how it looks this is all under extreme conditions so south pole in the Antarctic and try to build a giant detector so if you would stand in the ice this would look like something like that and before we deal with the neutrinos how is such an what comprises such an optical module in principle these digital optical modules are just cameras for blue light the card is the white blob you see on the picture to the left that's a photo multiplying tube if light if light impacts it's transformed into electrical charge I want to show you two interesting things this mu metal grid to shield the earth magnetic field there's a mu metal grid and what I found extremely funny is this flasher board left in the graph so each of these digital optical modules besides the main board that does the data acquisition and sends data up it has a light source in itself by which it can generate flashes of light and to calibrate the adjacent module so these digital optical modules measure the chairing of radiation how this looks if an electron neutrino goes into the core it does an interaction an electron is produced and the electron does a chairing of radiation so in the video links you see what the light signal looks like in the eyes on the right side you see how the detector perceives that so so left something starts that happens when the electron gets produced and the special thing about electrons is that they interact all the time while they interact with the ice and you get a whole shower of electrons that make a chairing of cone and in the end there is a big sphere right okay there was visible on the right looks like the next picture is shown as blobs attached to the digital modules to the camera modules the bigger the blob the more energy has been deposited in that volume and the color code is a time code it shows when light was measured so that's what it looks like if an electron neutrino looks the muon neutrino the detector looks different muon neutrinos produce muons and not electrons and muons don't interact as nicely as electrons they have a longer lifetime so they just go through the detector on a relatively straight line they leave a relatively straight trace and they also see that straight trace in the digital modules on the right side they can imagine what the advantages and disadvantages of these particles are so muons have a extremely good angular resolution at 0.2 degrees angular resolutions but these muons fly out of the detector so they are already coming from outside so they deposit a part of their energy outside the detector so you cannot catch the entire energy and take and find out how much energies is deposited as opposed to the electrons where the sphere deposits the whole energy in the detector but the angular resolution is very bad because this looks very nice the biggest problem in the real in reality is the background in ice cube ice cube measures about 10 astrophysical neutrinos with this extremely high energy that we want per year so in one year at the same time they are measuring 100.000 of atmospheric neutrinos and 10 billions of atmospheric muons so there is an extremely high background in the detector so in reality if you look at 10 milliseconds in the side of ice cube this is what you get is that it is highly impressive that you get any useful data out of the background here and the green lines the impinging green lines are atmospheric muons so there are different veto systems so only you only take events once through the earth until the impact on the detector so you sort out atmospheric muons or you define the outside layer of the detector as veto so what happens in the veto region we don't accept as an event so you can use atmospheric muons so if it is in the atmosphere so at 300 Tere electron volts there is almost no atmospheric neutrinos anymore so you are relatively certain that this is the real thing that we want to see so actually ice cube has identified some neutrinos as astrophysical neutrinos since 2012 the first big success was the first 28 neutrinos in und bis heute hat man so Größenordnung 100 neutrinos gemessen until now we have measured about 100 so you can do some things like we can draw how many neutrinos per energy interval we have but now we also have built this detector because we want to find the sources of this high cosmic rays so what are the sources now so what you do is that you usually look measure one of these neutrinos and I see this direction is there like a very strong known astrophysical object like Quasar but we didn't find anything in these directions so we found this whole new flow of astrophysical neutrinos but now we didn't know where did they come from so more of a additional riddle than solving the question we posed so and that's where we get to now what's been published this year so the first time a neutrino has been measured and we could identify the source of this neutrino so this neutrino could be identified to a blazar which is known from measurements of photons so in our world this looks like this these news and of course much more of these and of course I added the nature astronomy article of our workgroup and not any other source but the main part to take away from this is a neutrino a very high energetic neutrino and this neutrino could be this neutrino came of the direction where Quasar is that at the same time was also very active so a simple excursion what is a blazar in principle it's the core the active galactical core of a galaxy very far away it's a supermassive black hole and it has a jet and this jet is pointed towards the milkaway or the earth I wanna say another word to this so these these active galactic nuclei there is a lot of words for these don't get confused by these they are all historically term from history wise and real blazar is just an active galactical core with a jet that points in our direction so these blazars have a very characteristic radiation in their electromagnetic spectrum and every couple of years they become active and stay excited for a couple of months what exactly is this radiation that's a little bit more complex diese zwei wunderschönen and these two videos are also from desi my institute and they are made there and along this discovery they were made so how does this core look from up close and what does emit radiation so first you have this a black hole and there is this disc around and this disc emits light in the ultraviolet spectrum and the radiation that leaves that heat up clouds that are above this disc so these clouds become excited and emit emit line emission that's the so called broadline region and they are very wide just because these clouds move and the Doppler effect widens up this radiation and around there is a dusk torus and that covers up most of this and most of all these cores have this jet that is powered from the accumulation of matter and moves with relativistic velocities within this jet there is turbulence that cause particles to accelerate mostly electrons and protons and these particles the image electromagnetic radiation that's what we can see so back to our discovery on the left on the top you can see this one neutrino event it's very remarkable how this happened they have this alert system it's a muon neutrino so it has a very good energy we can reconstruct so they published an alert hey we have this 300 tera electronwald neutrino please point all your telescopes optically, x-ray whatever in this direction and see if you can find something and indeed for the first time from the same direction that this neutrino came from there's also gamma rays that have been measured in particular from a blazar that's been known for quite a while and it's been active for a couple of months already so additionally what it did ice cube has been since 2012 the accumulated data has decreased okay it's dates a little bit farther back than 2012 because before the detector was finished they already had some parts of the detector active in the meanwhile they found that in the period from 2014 to 2015 there has been another accumulation of neutrino measurements from the direction of this quasar so about 10-15 neutrinos along the lines I want to say a couple of things within this period between 2014 and 2015 this blazar wasn't more active than usual in terms of gamma rays it was just very calm but apparently it admitted more neutrinos so during this event in 2017 that's shown in the top a lot of our nicely explainable with the models we have and also be able to simulate so this historical flair that's what we call the emission in 2014 and 2015 was quite a bigger challenge so with the models that we have we need quite across parameter fine tuning to be able to explain this also i've seen models that try to explain this by saying there's probably a star that flies into this jet and that's the source of this neutrino production so you need very exotic models and you have quite some difficulties to explain this increased activity but what remains is that for the first time die Quelle eines hoch energetischen neutrinos vermutlich zu identifizieren to possibly identify the source of a neutrino i want to highlight two of these headlines so what does it mean it means not what's set on the left it doesn't mean that we found the mystery space the origin of the mystery space radiation but we found one possible source that possibly emitted one single neutrino it doesn't mean that all neutrinos come from plazars like these TSX in reality their account is very limited furthermore we can learn from that in the swan source there were possibly protons but it doesn't mean that all cosmic high energy rays come from this source or only come from sources of this kind that's not what it means but it's a start and that's the first time that with these large neutrino detectors we can do astronomy and in this sense the headline on the right that's a little bit closer it's a little bit closer to home it is a breakthrough because this started with upgrades and like for ice cube it's going to be continued we're going to have more measurements we can improve our models and hopefully in the future we'll hopefully be able to answer the question where do cosmic rays come from and with that I thank you for listening Annie Alter touched down on the spot aesthetic pictures nice colors calm talk and very calming talk what SIVA just missed we have learned something that if you had said before fluorescent telescope that's a telescope that glows in the in the back so it's a fluorescence not a fluorescent telescope so we have open microphones just line up and people stand up all the way in the back signal angel waves we have a question out of the internet just shoot 2-3 slides ago you had this graph temporal evolution was der gap what is the gap between 2015 and 2016 in fact this is just an analysis so the gap to be quite honest I have to look at read up in the in the paper assuming that it's just a gap in the analysis so they did 2 analysis so they did the gaussian analysis the box shaped analysis and maybe they limited the time window but I don't know exactly it's not a measurement gap but it's an artifact of the interpretation I can't really answer exactly I know it even less thank you the internet applaud thank you very much for the talk it's a very nice talk it's my question so you said neutrinos are slower than light if we detect such a neutrino do we have the chance to to know from the source using light in our lifetime so that light is essentially speed of light so they have to be coincident so the minuscule difference so the masses are so minuscule that they are basically detected simultaneously technology makes it possible to switch to microphone number 4 are there any possibilities to influence so whether neutrino flies through mass or interacts with this mass nope so this is just a probabilistic process you cannot influence that you can put more matter in front of it in the hope that more matter makes leads to earlier interaction but no but not in principle not with neutrinos so all questions seem to have been answered was it your first talk for such a big crowd was that your last talk in front of such a big crowd next time if my colleague isn't in Shanghai i might give it again anni so that was anni