Okay, good afternoon, everybody. So it's a pleasure to have this program today. To, it's an ICDP prize ceremony. And this is actually taking place in conjunction with our summer school in particle physics. And I'm very happy that his excellency, Ambassador Ahmad Pakachi, permanent delegate of the Islamic Republic of Iran to UNESCO is present with us. The prize this year was given to two outstanding cosmologists from Iran. Shant Bagaram, who is from Sheryl University of Technology in Tehran, Iran. And Muhammad Hussain Namjoo from the Institute for Research in Fundamental Sciences, IPM in Tehran. He's also a regular associate of ICDP. So, ICDP has a very long connection with the scientific community in Iran. And many Iranian scientists have come and contributed to ICDP's mission and have benefited from it. This ICDP prize was created in 1982 by the ICDP Scientific Council to recognize outstanding and original contributions in physics by young scientists from and working in developing countries. And awardees thus far have included many notable scientists from India, China, Brazil, Argentina, and many other countries. Together with today's two awardees, I think the total of Iranian scientists who received this prize is now goes up to five. In the past, in 2020, Dr. Mehdi Kargarian from Sharif University of Technology in Tehran received the prize. In 2013, Dr. Yasman Farzan, a woman scientist from Institute for Research and Fundamental Sciences in Tehran. And in 2007, M.M. Sheikh Jabari, again from IPM in Tehran. Let me just quickly read the citation of the prize. The two share the prize for their pioneering contributions to developing robust theoretical, computational, and statistical frameworks to compare theoretical predictions for various cosmological and astrophysical phenomena with high precision observational data. So I now request his Excellency Ambassador Ahmed Pakachi to say a few words. Mr. Director, ladies and gentlemen, scientists, researchers, I'm honored to participate in the special ceremony to award the ICTP prize, which for the fourth time is being awarded to young scientists from my country. At the outset, I wish to extend my thanks to Professor Atish Dabalkar, the Director of ICTP and his colleagues in particular the Selection Committee. Today, on behalf of Iranian government and nation, I would like to sincerely congratulate Dr. Shant Balram of Sharif University of Technology and Dr. Mohammad Hossein Namjoo of the Institute for Research in Fundamental Science. Their outstanding research and articles cover varied subjects, including dark matter and large-scale structure. Since its creation in 1945, science has been an integral part of UNESCO indeed it remains the only UN specialized agency with the mandate for science. Although the setting of standards and norms is one of the primary duties of UNESCO in the field of science, together with its related institutions, it provides scientists with an intellectual forum and engaged governments on scientific issues relating to the achievement of sustainable social, cultural and economic development. Ladies and gentlemen, science and knowledge play such a significant role in the world today that the progress of a nation is related to its collective knowledge. As we are aware, the progress of science is intrinsic to human progress. The rapid advances that have been made in science together with their technical applications are one of the most significant factors in the development of human society. All people should be able to enjoy the benefits of this advancements. Scientific development allows us to explore new paths of action in not only tackling the challenges of today but also preparing for those of tomorrow. I may say that we need not only more science but rather better and more ethical science and to meet these concerns, UNESCO created the program on ethics of science and technology. I would like to recall that the UNESCO Avicenna Prize for Ethics in Science was established in 2002 on the initiative of my country. It remains the only international prize concerned with the subject of ethics in science. We are living in the area of knowledge societies. However, scientific equitability is not always fully observed. Scientific education is essential for human development and the fulfillment of the active role that citizens may play in their country, notably in the eradication of poverty. Freedom of access to knowledge and freedom of research should accompany one another. Newly appeared information and communication technologies are highly effective in the exchange of scientific knowledge and it is essential to ensure full access to all such information in the public domain. Ladies and gentlemen, throughout history science has played a unifying role not only due to its problem solving methods and its extension in response to social needs but also through bridging divides by bringing together individuals and nations in active cooperation. That's why I'm delighted to be here today in the ICTP which is actively engaged with scientists in developing countries. It is a positive example of the international scientific cooperation which helps to foster a culture of peace. Thank you. Thank you very much, Ambassador, for those words. Now I request Professor Marko Simanovich to say a few words about the scientific background and accomplishments of the two prize winners today to set the context. Thank you. Well, thank you very much and good afternoon. Well, first of all I have to say that it is really a great honor to introduce the recipients of this year's ICTP prize. I have to say that as a PhD student here at ICTP I had the pleasure to attend several of these ceremonies in the past and every time this was a very special occasion. This award, I think perhaps more than any other, recognizes outstanding and original contribution from scientists in our field who work in developing countries and given the mission of ICTP to support science in the developing world, it has a very special place and a significance for this institution. As we heard, this award has been around for 40 years and if you look at the list of recipients, it is very impressive with names of some of the most brilliant scientists in theoretical physics. And we are very happy today to add two more of our colleagues from Iran to this list which is ever-growing and contains more and more names of brilliant researchers who do physics. So personally, being a cosmologist, I'm particularly thrilled to see that this award goes to two colleagues working in the same field. Cosmology has tremendously evolved in the last couple of decades from a more speculative to precision science and many discoveries have been made along the way, some of which had a very deep and profound impact, not only on our understanding of the history of the universe but also on neighboring fields, such as particle physics and more broadly high energy theory. Now with all these discoveries, many other puzzles emerged and given many upcoming observational campaigns that are going to deliver data with unprecedented accuracy, we can say that cosmology today is as active and promising area of research as it has ever been. Professor Bagram and Namjoo have made several contributions, as we heard in the citation, to developing robust theoretical computational statistical frameworks to compare theoretical predictions for various cosmological and natural physical phenomena with these upcoming high precision observational data. So let me say a little bit more details about their work. I would say that in particular, Professor Bagram's research recently has been mainly focused on large scale structure of the universe and late universe. He has been working on providing phenomenological models and developing new methods to test accelerated expansion of the universe. As you know, since the discovery of this accelerated expansion, the problem of cosmological constant has been one of the most intriguing and most important problems in theoretical physics. And with the new observations, any framework which allows us to test this to its limit is going to be a very, very important thing. On the other hand, Professor Namjoo has been more focusing on investigating the earliest stage of our universe, which is known as inflation, which is a big puzzle at the opposite side of the cosmic history at very early times. And he worked on several important things. In particular, some of his most important works include understanding in a little bit more detail under which conditions the so-called local mongosianities can rule out, for example, detection of local mongosianities would rule out single field inflation, which is an important class of inflationary models that we hope to test in the near future. And some other examples include the role of impact, the role in impact of massive fields during inflation to late time observables. And we are going to hear about it today. I would also like to emphasize that the two of them have collaborated on a couple of well-known and influential papers. For instance, they were studying the possibility of anisotropic clustering through the so-called anisotropic bias, which can be induced by primordial mongosianities, and also on possible asymmetry in the sky, introduced by modulation, by the best fluctuations that you observe in our universe, on the largest possible wavelengths. So to conclude, given the breadth and impact of their research, I think that this award is certainly more than well-deserved. I would like to personally congratulate you. And instead of me giving further details, I think that you're all eager to hear from the winners about their own work. And so I will stop here and invite you to present your research. Thank you. Thank you, Marco. So I would like to just add that this year's ICTP prize is, in fact, being given in the honor of Russian physicist Valeriy Rubakov for his fundamental contributions at the interface of particle physics and cosmology. In particular, Professor Rubakov wrote pioneering papers about barrier genesis, the mechanism which explains why the universe contains matter and not antimatter, non-perturbity methods, including his insightful work on monopole catalyzed proton decay, sometimes known as the, otherwise known as the Kalan Rubakov effect, and the brain world scenarios. Professor Rubakov was a dear friend of ICTP, wonderful person, and a member of the scientific council. He decided to remain in Russia after the dissolution of the Soviet Union. And he mentored a large number of students forming the Rubakov School in Moscow. He was a strong defender of academic freedom. And we will miss him because he passed away on the 18th of October, 2022. So this prize is being given in the honor of his memory. And I'm also very happy that today the prize will be given together with me by the hands of Professor Kamran Wafa. He is the holiest professor of mathematics and natural philosophy in the physics department of Harvard University. He is an Iranian-American physicist, a very distinguished string theorist. And I'm very, he not only, he has been actually a very close associate affiliate of ICTP. He has been a distinguished staff associate for many years. And he was also the member of our scientific council for many years. So I'm very happy that Kamran is here. And in fact, Kamran was here recently to inaugurate his book, which was being translated into Italian. So he has written a popular book, which you might want to read in Italian. So I now request we will proceed with the award ceremony. So I request Professor Shant Bagaram to please come forward. And now I request Professor Namjoo to come. OK, thank you. So now we proceed with the scientific presentation by the prize winners. And I just should say that following the ceremony, then you will have refreshments on the terrace. Now we go to the scientific part of it. OK, so our first speaker will be Professor Shant Bagaram. He will tell us about large-scale structure of the universe beyond the standard model of cosmology. Please. OK, good afternoon. Director of the ICTP, ladies and gentlemen, it's deeply an honor to be here and have received this prize. It's a really honor and pleasure. So I will try to, in a 30-minute talk, say what we think in these years with my supervisors and students about the cosmology. And that's the two words of the large-scale structures and beyond the standard model of the cosmology. I'm very lucky that Professor Markosomanovich gave great talks on the cosmology that makes my work very easy. So if you have questions, ask Marko in the lectures that really have the upcoming days. So, OK, I want to start the story from the 17th centuries from the Newton and the problem of the gravity and the universe. So it seems that Newton's seat in the Royal Academy of the UK and the people are coming and asking questions about, is it from 17th centuries or? So one of the guys, the Bentley, come and ask that if you apply your theory of the gravity to the universe, why doesn't sky fall over us? And what happens? And Newton didn't like these questions. And he thinks that the universe is almost homogeneous and isotropic, but that's an unknown question. So going to the 20th century, a remarkable paper by Albert Einstein that applying the gravity on the cosmology has the same question. And instead of solving the boundary problem, he said if we assume that the universe is homogeneous and isotropic, you can have a solution. There's more letters coming back between Dositer and Einstein about this. And the metric you have seen is the metric that made by Friedman, Robertson, Lometchan, Walker. And people are trying to test this idea of the homogeneity and isotropy. There are many tries from the 30s by the Shapley and the Hubble and then 50s after the World War II that the radio astronomy is developed. There's a radio telescope in Cambridge and people are trying to counter galaxies in different directions to see if this works or not. This is a modern version of looking at the universe and see if the universe is homogeneous and isotropic. This is the Sloan Digital Sky Server. They work for more than a decade and each point is a galaxy. So Marco said that if you use this assumption, you can write the cosmology very easily by the Friedman equation. And the question is how to measure the expansion rate and how much matter is in the universe. And we find that the universe is in a special case, is almost flat. This is a list from works in the 30s to recent days to just measure how much matter is in the universe. And it's 0.3 almost. It seems that the universe is flat but there is less matter. It seems that there is something ridiculous like dark energy in the universe that maybe is related to the Bentley's question that why not Sky Falls. So what we learned that the universe is very vast and very old and it's very empty. If you put the numbers and have the expansion rate, you find that there's such five protons in cubic meters. There's two great books by the Nobel Prize winners Peebles in these last two days, the Cosmos of Century and the Whole Truth that he say about the history of the cosmology and one of the greatest discoveries is the cosmic microwave background radiation, the photons that comes from the early universe. And we learned that this radiation is a black body and we know that in each centimeter cube there's 400 photons and we measured the contribution of the photons there as well. So this is the latest plot by the Planck. This is the angular power spectrum of the density of the angular power spectrum of the temperature density contrast versus the scales by Planck and you have this standard model with almost six parameters. How much baryon is in the universe? How much cold dark matter? What's the distance of us to the CMB? It measures the amount of the dark energy and three parameters that is related to the early universe. So it seems that it happens a revolution in the 1998 to 2003. We have this cosmological standard cosmological model on the CDM and you can teach the standard cosmology in a semester and you need an initial conditions that Professor Namjoo will talk about it and you can make the universe. So summing up, what we know about the universe is that the universe is all very big. It means that there is dark energy. It says that the essential force in the universe is the gravity and there is dark matter that makes the structures and the initial condition of the universe is very simple. It means the perturbations are almost Gaussian, scale invariant and isotropic and you have two assumptions that the GR is the right theory of the gravity and you have this Einstein principle of cosmology that the universe is homogeneous and isotropic. It's a great model but we don't know of 95% of it and we don't know how is the physics of the early universe. That's a great area of research because almost you know nothing about it. Okay, so what will be our plan to study the universe? Instead of asking fundamental question we can go and check how the different constitutes of this model can be changed. For example, asking if lambda, cosmological constant is the reason of the expanding universe is called dark matter right or not and the initial condition GR and Einstein cosmological principle that will be the plan. So this is my supervisor, professor Sourabh Ravra I have much depth to him. It's two decades ago when I was an undergrad student and he teach us that the structure formation is important and we are doing it for two decades. The idea is the gravitational instability is important because it makes the structures from the initial condition to the late times. So why is structure formation important? Because if you go and measure the distribution of the structures in the linear regime you can find out that there's a differential equation that the Hubble constant goes through it the pressure and how the gravity acts and there's great progress in linear perturbation theory. You have the matter power spectrum even you saw the bump of the bionic acoustic oscillation the physics of the early universe maps in the late time. So that's great but when you look at the observation or the simulations of the cosmology you see that the cosmology is not linear almost in the smaller scales and there's a cosmic web there's halos, there's filaments, there are voids and you have to look at the cosmos in the nonlinear regimes. If you ask an astronomer that what we can observe maybe I put a wrong thing here, okay thank you. So if you ask an astronomer you will say that observable is the luminosity function of the galaxies and then you have to relate it to the number density of the dark matter halos. So what we try to do thanks to the ICTP programs because I was visiting here as a junior and I worked with the great scientist Professor Ravi Ches and he introduced us about this idea of the musing of the pressure and the shecter and the works that is done by the other colleagues and the S is the Ches and Torman and the other guys. So the great idea is that instead of doing simulation you can look at the initial condition of the universe where the perturbations are almost linear and Gaussian and ask that if you evolve them how many how much of the structures will be made in the universe. So it's a good idea to make simulation but it's costly and you have different models to check and even in a specific model if you have changed the parameters you have to do the simulation again. So it's great to have some semi-analytical ideas to go with this data. So what's the pressure or exclusion set theory idea? The idea is very nice and easy. It says that the x-axis is the scale in the universe so you choose the biggest scale you can imagine and you count the structures in it and you calculate the density contrast. The y-axis is density contrast. And you start to decrease the scales to have the smaller and smaller scales so you have some trajectory for each point in the universe. So there's a critical density in the linear theory, delta C, if one of the trajectories touches this barrier it seems that there's a structure in that scale and it's important to find the first crossing. So people, the bound k-ser and f-stashu and col they use a very specific smoothing window function k-space because they know how these trajectories can be solved, they are Markov and they look at the Chandrasekhar papers in 40s and they have the solutions. So what we did with our colleagues is to make this process non-Markov if you choose any smoothing function which is more physical like the Gaussian or top hat in the real space and you have the trajectories in the... in trajectories and you can count the number of the crossing and you have the number of the structures in the universe. This works is lately done by Farnik and Mamadreza who are post-docs in Yale and Heiderberg now and we have both approximations and numerical solution for this problem. So the other thing that I did with my PhD students, Mamad, is that we asked that if we can find the number of the filaments in the universe and it's related to the saddle points in the distribution of the early universe and this is, we put the name of the excursion set theory of the saddle points. So we want to push it further by Hamid as we know the gravitational astronomy is on its way and it's important to have the merger history of the structures or progenitor history of the structures. So this excursion set theory can shows... can calculate in the first approximation the number of the conditional crossings. So you can move the barrier upper to count the number of the structures in the higher rate shift. It's trivial because you need more density contrast if you want to make structures in higher rate shifts and we try to make this idea as a test for checking the models. Sorry I'm passing this through to slide quickly to show what the problems are there and then I can answer the questions in the break if there are some. So the other works that we promote by my PhD students and master's students is looking to the one point statistics. The idea is that if you're going to the cosmic web in simulation or in observation you can stand on a specific point and ask what is the number of the nearest neighbor. This specific point can be a random point if we call it the spherical collapse, spherical contact sorry or you can go and sit on a dark matter halo or a galaxy it names not nearest number density. So it's related to correlation function that cosmologists can do the work with it by the nominal paper by Wight in the 1979 and we plot, we calculate this for different mass scales different galaxies and different red shapes and it seems that it could be a novel probe for checking the cosmologists beyond the standard model. For example you can add neutrinos and see how this j function which is the spherical contact and near distribution can change. It seems that it is related to the minimum mass but in the range of 0 to 1 it's not changed. Okay I pass through this going back to another idea is the cold dark matter problem or not. One of the ways to look at this problem I want to ask Marko if there's five minutes remaining just told me that. There's much more, okay. And even if you are tired you can say I can pause. So the other ideas is about the cold dark matter so it's important to know if the cold dark matter is the real dark matter model. One of the ideas is go to the smaller and smaller scales people are doing many simulations because the smallest mass of the dark matter can say that this dark matter is cold or it's warm or it's hot. There are some problems the people are talking it's about more than a decade that like missing satellite problems or too big to fail problem and a community says that maybe the baryonic physics is the solution but again you have to answer this question. One of the ideas that we developed by my supervisors Professor Rahvar and my postdoc mentor Professor Afshordi is the idea of the transit weak cleansing. The idea of transit weak cleansing is that if you have a source and there's many of these dark matter substructure passing through the line of sight you can find a lensing effect which is a transit which is have a time dependence so you can calculate the power spectrum of the change of the lensing. So you can ask that what are the sources that you can find because the sources in astronomy they have their intrinsic fluctuation if you have this idea if you're going to look at the strong gravitational lensing sources you can subtract the intrinsic change in light and find this transit weak lensing. However we can put an upper limit about the distribution of these dark matter structures. So another work is recently our people are talking about this fuzzy dark matter models that make this solitonic course with our joint PhD students now Dr. Maliki we go through the pattern of the lensing in the colliding cores of the dark matter if there is some quantum mechanical effects in the dark matter. So we want to relate these two ideas of beyond cold dark matter and simple initial conditions this is one of the other pillars of the cosmology and this is the work by my former student Dr. Kameli that to solution for the too big to fail problem or missing satellite problem maybe it's not the modified cold dark matter or maybe it's not the bionic physics but modified initial condition. People are talking that you can change the power spectrum in the small scales and we choose a very phenomenological model we put a bump in the power spectrum in the smaller scales and we ask how it will be changed the number density of the structures it seems that we have more structures like Milky Way but we have less in the smaller dwarf galaxies we check that this result are consistent with the paradigm and alpha test and it could be an idea if someone could simulate this model so this is important because people are recently talking about the primordial black holes as the source of the gravitational wave and if you need to make primordial black holes in the paradigm of the inflation you need to have an excess in the power in the smaller scale so maybe these two ideas can be related so we try with one of our colleagues to find the number density of the primordial black holes in the context of the exclusion set theory what we did is that if this is the shrinking cobble radius the smaller scales go first out of the horizon and come first so we have to do this mechanism of exclusion set theory from the right to the left the other works that they mainly contribute with Professor Namjoo and our mentor in the IPM Dr. Feroz Jai is the ideas related to the late time universe and the early universe such as the CMB lensing I'm not go through this the last almost last part of the talk is about the lambda or GR so recently it's five or six years we are talking about the H0 tension that if you measure the Hubble constant from the nearby supernovies is four or five much different with the one you measure from the cosmic microwave background as a one parameter of the lambda CDM so we come up with one of my best friends Dr. Khosravi in Shahid Beshti and Professor Afshordi a model known over lambda CDM that it shows a change in the gravity model and in the Hubble parameter but still not a very successful model because you have to make the prediction for the structure formation as well so we have a chance that Professor Mashun one of the guys that works with the wheeler in the 17s he comes to our university and give lectures and we learn a lot from him and he give the stories about the D-key and the wheeler and the pebbles and he works on the non-local gravity and we try to make a cosmological model from the non-local gravity the idea is brilliant so the general relativity has a couple of assumptions like equivalence principle the Lorentz invariance and locality the locality is that any observer in the university is accelerated point by point is locality like a Minkowski observer so if you have an acceleration in the universe acceleration is something absolute so it introduce a specific length and if you have some averaging process like the waves you have to take the non-local effects there's a great book by him Non-local Gravity by Afshord and people are talking about this idea from the Anishtain to the Weyl and the Minkowski and etc so in order to introduce the non-locality to the gravity we have to go to the teleparallel equivalent of the GR which is make the gravity very similar to the electrodynamics so instead of working with the metric you work with the tetrods and instead of the curvature you have distortion and we know how to make a theory non-local in electrodynamics by introducing this epsilon and mu which are the permeability of the matter if you apply an electric and magnetic field to the matter we did the same procedure with the gravity and we look at the local limit of it so if you look at the homogeneous and isotropic cosmology it's only one function of s of t so you have ability to fit with the data and solve the Hubble tension and we are very interested to learn about this more the last thing it's about the Anishtain principle cosmology the other works that is done with Dr. Mohaye in ERP that asking if really we have we are living in a homogeneous universe so I have a couple of thank you slides this is a slides from summer school in cosmology in 2008 I want to thank Professor Kreminelli for hosting me during the junior associate years and organizing these wonderful events it has a very deep impact in this year Professor Rubakov talked to us about the dark matter I have his notes and I bring it with myself it really I'm saying that it's had a great impact for a first year PhD student and the other thing which is not scientific but cultural is the Marikuri library because in the last four years I have the responsibility of the libraries in Sharif University and the Marikuri library is very inspiring and we try to make the libraries like the ones that are in the ICTP the physics department library is in the name of the Abdu Salam and the central library is trying to be some place like the library in the ICTP at last but now this I want to thank you my brilliant students that I learned very much from them they are bright and I'm very happy and I know that they make the future of Iran in the scientific very much bright and great and no need to say in a particle physics conference that the cosmology is very important and there's many discoveries that happen in the cosmology thank you very much this is the Foko Pendoliom I can host you in a conference of particle physics or cosmology there thank you very much thank you for the very nice talk and perhaps we can ask if there are some questions we have time for a couple of questions thank you for the nice talk and during your talk you explained that the small bump in the power spectrum can fit to the limon alpha forest and I wonder the shape of that bump actually important to fit the data or is it completely irrelevant no it's important so it's like a Gaussian bump that it has two variables the variance and the amplitude and you have to put constraint on both of these parameters otherwise you cannot pass the limon alpha forest thank you any other question so I have a question the excursion said mother that you mentioned so you said that it's not it was originally assumed to be Markovian and you considered the deviation from Markovianity can you explain how good of an assumption it is for it to be Markovian or is it something when is it Markovian when it is not very nice question so if you have these trajectories and you choose a top hat filter in the case space then your trajectories will be Markovian and you know the solution but it seems not a real model because if you Fourier transform the k-sharp to the real space it's like something have negative smoothing function and positives otherwise if you go to the real space and make a Gaussian smoothing function or top hat in the real space so you are not Markovian anymore Any other questions? I do not see any so maybe I would like to invite Professor Namjoo to present his own work on probing the primordial universe using heavy particles Hello everyone thank you very much for the prize and for this opportunity Shant sorry maybe I should be more official Dr. Bakram ended by acknowledgement I am going to start by acknowledgement so I should thank my wife and also my parents who have been so patient and very supportive during this whole years of education and hard working and I am also grateful to all my collaborators who helped me a lot to be able to contribute to science okay so this pointer is not working I need to keep rest so I am going to tell you about how possibly we can probe the primordial universe the tool that I am going to use is the heavy particles I am going to tell you what heaviness would mean here it has some technical meaning my talk would be based on these papers in collaboration with these nice guys and this is the outline of my talk I am very briefly going to talk about inflation, introduce inflation to non cosmologists and very briefly alternatives to inflation then I will tell you how massive fields or massive particles are going to help to probe the primordial universe and this comes under the name of under the name of primordial standard clock so again I will tell you why we have chosen this terminology the massive fields at the early universe are called primordial standard clock it becomes clear later on why this is so and then I will tell you about the properties of the signals that we expect to get out of these primordial standard clocks so inflation what is inflation inflation is an accelerated expansion of the universe at very early times when the universe was very young perhaps a tiny fraction of second old the inflation itself had happened for again a tiny fraction of second but there is a dramatic change to the universe as a result of inflation inflation becomes much much bigger after inflation compared to what it was before inflation ok so why do we need inflation we seem to need inflation because what we observe today has some particular properties this is an example if you look at the universe in different directions you see that the universe is almost at larger scale is almost isotropic meaning that for example if you count the number of galaxies looking at that direction and compared to the number of galaxies in that direction you get more or less the same thing the same number so this means that the universe is isotropic and if you add to it the Copernican principle which states that we are not in a particular position in the universe you can conclude that the universe is also homogeneous so the universe is both isotropic at largest scales another observable that we can look at and get basically the same conclusion is the cosmic microwave background which is a microwave light that is coming to us from distant places this is basically the oldest light and the most distant places that we can even in principle observe this is the cnb map what is actually showing you is the perturbations the anisotropy on the cosmic microwave background but these perturbations are pretty small so at leading order we can conclude that again this cosmic microwave background radiation is isotropic so what is the problem here is the problem if you want to have such a homogeneous and isotropic universe you need to have a very particular initial conditions for your universe a small change in the initial conditions would lead to a very different universe compared to what we see today so it seems that without inflation we are going to have a problem in the initial conditions the initial conditions of the universe need to be finely tuned but this is the work of inflation that washes out basically the sensitivity of observable universe to the initial conditions so in a large fraction of the space of all possible initial conditions what you get at late times as long as inflation was there would be basically the same and this was the main reason for the growth in 1981 to introduce inflation so how inflation can happen this is a kind of weird behavior of the universe like it's an accelerated universe with positive acceleration and for this thing to be realized you need to have a kind of classical scalar field at least one classical scalar field that is rolling on top of an almost flat potential then the inflationary phase can be realized so yeah this is this is the inflationary scenario it has been very successful it can disentangle the observable universe from the initial conditions sort of but this is not the only success of inflation this classical scalar field that is rolling on this potential has also some quantum fluctuations the quantum effects are always there it's not avoidable and this is pretty helpful because also provides us a nice mechanism for generating the fluctuations that we see at very large scales including the fluctuations that we see in the CMB for example right so what is the mechanism these quantum fluctuations are there during inflation and these fluctuations are straight out from small scales to very large scales and the small scale fluctuations become large scale fluctuations during inflation and then these large scale fluctuations can be considered as primordial seeds for the fluctuations that we see and observe at late times so this is a nice link between what we learn from the quantum field theory to what we observe at large scales so these fluctuations will be a bit technical but don't panic I'm not going to go through the details just showing you a flavor of what kind of theoretical framework we are dealing with so we need to do cosmological perturbation theory as I've told you the two leading order the universe is homogeneous and isotropic so the line element for that universe is pretty simple is also simple and this is just a scale factor that quantifies the size of the universe as the universe expands this A of T the so-called scale factor becomes bigger but now we want to add fluctuations, small fluctuations so the metric would change it would change in different ways including that kind of change we introduce a new parameter zeta which is called curvature perturbation up to some gauge freedom that I'm going to ignore in this talk and then since you are dealing with Einstein's equations you need to also perturb the other side of Einstein's equation which is the matter sector so the matter sector should also be perturbed the scalar field the perturbations of the scalar field and basically you can derive equations of motion for these fluctuations or write down the action for them in particular for zeta for the curvature perturbation and this I'm going to work with this parameter zeta because it is directly related to the fluctuations that we are going to see at later times zeta as a random variable or more precisely as a quantum field you can calculate different correlation functions including this two-point correlation function or power spectrum or you can go to higher orders and calculate the higher order correlators like the three-point correlation function and so on what are the predictions of inflation as long as the inflation in model remains sufficiently simple here is the prediction of the inflationary scenario it predicts that the fluctuations have to be almost scalar invariant and almost Gaussian and this prediction works remarkable well in describing our universe this is the this is the most recent data the power spectrum the two-point correlation function of fluctuations on the cosmic microwave background and this red line is the theoretical prediction this theoretical prediction contains a lot of information a lot of physics including the predictions of inflation it's not just inflation but inflation is also included and you see that they match pretty well the data and the theory match pretty well so this is the success of inflation and perhaps that's the reason that most people believe on inflation but pros and cons come together there are some objections to inflation as well here is a list of objections to inflation it's a complete list but just to mention a couple of them people claim that the simplest model models of inflation has been disfavored by most recent data thousands of models of inflation are there why? because the physics governing inflation is unknown we don't know what is the potential under which the scalar field is evolving or whether we have one scalar field or more than one scalar field the particle physics theory of the inflationary universe is unknown some models of inflation lead to the multiverse and the major problem is there it's not even sometimes clear whether the fine tuning problem is solved if inflation had occurred then yes we are going to solve the fine tuning problem in cosmology but the question is that do we need another fine tuning for inflation itself to happen or not some people claim that the inflationary scenario is not falsifiable the singularity problem is still there the initial singularity cannot be resolved by inflation so I don't necessarily buy these arguments but the point is that some people based on these arguments against inflation decided to think about alternatives and they actually came up with some interesting ideas one example is a matter contraction scenario in which you have temporality contracting universe at early stages and if such a contracting universe is filled with a non-relativistic matter you can conclude that the predictions for perturbations for the fluctuations is almost the same as the predictions of an inflationary universe and there are other scenarios as well another example they are not as beautiful as inflation but still there are some proposers and as long as the observation is concerned they are almost indistinguishable so now I'm getting closer to the main topic of my talk here is two fundamental questions that I want to ask how can I probe inflation as I have told you the physics governing inflation on now so how can I probe directly the physics behind inflation and even more important or more fundamental is inflation really the true story of the universe or we should think of alternatives so I'm going to skip that slide because it's a bit technical just to mention what is the question here I'm going to tell you that I can't probe the primordial universe using the massive particles but the question is do we expect them to be there and the answer is yes we do expect them to be there there are several theories that predict that they should be there and if we assume that massive particles are present at the early universe we can use them to probe the primordial universe so how these particles are going to generate some signal for us it's pretty simple I can just tell you about it without showing equations so it's based on the resonance mechanism so this is the massive particle and massive here means that the mass should be larger than the Hubble parameter larger than the expansion rate of the universe at early times then I'm going to call such a particle as massive and if the mass is sufficiently large this massive field is going to oscillate with frequency mass and this is a universal thing it is independent of the evolution of the universe that's why we call it standard clock primordial standard clock it ticks like a pendulum and it is standard in the sense that the frequency of the oscillation is independent of the evolution of the universe on the other hand you have another thing which is let's say Zeta the curvature perturbation which is also oscillating at early stages of its evolution but the frequency of this oscillation is quite different from the previous oscillation and this oscillation has a time dependent frequency at some certain point these two frequencies would match and then you get a resonance of course this resonance is not a disaster it's a good thing because you're going to observe such a resonance effect at late times so what kind oh okay yeah let me tell you about two types of standard clock that we should deal with since this massive field has to oscillate there are two ways to excite the massive field so that it starts oscillating maybe the simplest way to think about this is the classical way in which case you have a sharp phase transition which triggers the massive field and it starts oscillating around the minimum of the potential but if this phase transition did not happen we still have quantum fluctuations right quantum fluctuations are unavoidable they are there and these excitations of the quantum field can also play the role of standard clock so we have two types of standard clock and they have basically different signals so we can distinguish between them so a bit of technicality here again just to quantify how the universe behaves at early times I'm gonna assume that the scale factor behaves like t to the power of p and for different values of p I have different behaviors of the universe if p is larger than 1 I have inflation if p is 2 third I have matter contraction if p is something between 0 and 1 I have slow contraction etc so what I'm looking for is a signal that is p dependent so it encodes the information about the time evolution of the universe at early times so if I show you a signal that is p dependent then I'm done I have a prediction it depends on the time evolution of the universe at early times and this is the signal that you can basically calculate using the idea of the resonance mechanism you see that this is a signal in the Fourier space so a signal is a function of k you have an overall amplitude right which can be scale dependent but besides that you have an oscillator factor this is the important factor here and you see that the frequency of oscillation is changing with scale and how it changes with scale is p dependent the change in the frequency of these oscillations would be p dependent so it can if you can observe such a signal then you can distinguish between inflation and alternative scenarios you can discover how the universe was evolving at early times this is just a visualization of the same signal and you see that you see that they are different for different scenarios right the signal is different for different scenarios there are two ways to think about the massive fields at early universe one is the primordial standard clock that I've just told you the other is that if you for some reason convince that you know what was the evolution of the universe then the question is that do you care about these massive fields to be present at early universe or not the answer is yes you should care about that because even if you don't care about this p dependence here you should still care about the physics of early universe right so because this frequency also depends on mass of the particles so you can do if you can observe such a signal at late times you can basically do the spectroscopy of the early universe this is the so called cosmological particle collider okay so how we are going to observe them is it actually an observable thing or not as I've told you at leading order the current data is telling us that the primordial fluctuations should be almost scale invariant okay whereas what I've shown you as the signal is changing with scale so it is not scale invariant this means that we should look at the higher order corrections to our first order theory and we should look at the more precise data to be able to observe such an oscillatory signal but already in the Planck data there are some interesting candidates it's not that significant because as you see the error bars are pretty large here but we can hope that in the near future when we get better data we might be able to either put strong constraints on such signals or even discover them and in particular the near future observations of large scale structures by Euclid and LST is very important for that particular purpose we have shown that you can put much stronger constraints than Planck you can put much stronger constraints than Planck using the LST or Euclid data these are kind of forecasting right we still don't have the actual data yet but the difference between Planck and Euclid or LST you see that the contours are much smaller for LST and Euclid as compared with Planck data this is the concern that you can in principle put on the such kind of oscillatory feature on the power spectrum just a few words about the things that I'm currently working on it seems that besides the observational constraints that we can put on the different scenarios of the early universe there are also some theoretical I'm almost done there are also some theoretical constraints that in particular alternative scenarios not inflation alternative scenarios should satisfy if they want to work and be consistent with observations these are coming these new constraints that we are working on are coming from the existence of massive fields at early stages of the universe okay we have seen that there are some instabilities and deviations from perturbativity of the theory as a result of the existence of these massive particles if you consider for example matter contraction scenario this is still a work in progress okay in this talk I was trying to advocate the possibility of distinguishing between inflation and alternative to inflation using massive particles and I have argued that the massive particles are also pretty important to discover the physics governing the early universe's dynamics if you believe that inflation was the true story you can still use the massive particles to discover the physics behind inflation and the future prospect of discovery of these particular signals this oscillatory signal is very promising thank you very much for this nice talk I will ask again if there are some questions thank you for your great speech professor as a non cosmological physicist I have an ambiguous issue here you mentioned the standard clocks we have two standard clocks in quantum and classical and they measure something is this thing are comparable I mean when you measure something with classical clock is it comparable with that in the quantum clock or not comparable I mean are they in the same space or scale or not completely different okay if the question is that are they distinguishable or not yes they are distinguishable they can appear at the same scale depending on some details of the the model of the universe but they are very distinguishable because for example for the classical standard clock you need to have a phase transition and the phase transition itself would also have some non-trivial signal that you can in principle observe whereas for the quantum version you don't have such a signal the other thing is that I didn't tell you much about it but if you look at the three-point correlation function of the fluctuations because of the conservation of momentum you have at this triangle right of three momenta and for the classical standard clock if you change the size of this triangle you see these oscillatory features whereas for the quantum standard clock you need to change the shape of this triangle then again you see some oscillatory features but this is as a result of the quantum standard clock so they are very different they basically generate very different signal thank you any other question thank you for the nice talk so usually these cosmo collider signals with heavy particles have some exponential suppression that's right the signal you were talking about first of all is this the power spectrum or the three-point function it depends for the quantum standard clock it is hard to see in the power spectrum unless if you have alternative scenarios it's not going to work for inflation so for the quantum standard clock you expect to see these effects at higher order correlation functions including the three-point correlation function but this is not the case for the classical standard clock it can also appear with large amplitudes at the power spectrum but you are right for the quantum version of the standard clock you have this Boltzmann suppression but then this means that how large the coupling is what is the model that you are considering so the amplitude of the signal is model dependent you need to be lucky enough so that these oscillates signals are large enough so you can observe them in the future any other questions? thank you for the talk I wanted to ask about the phase transition that you just mentioned in regards to standard classical clocks what kind of observable would that produce like gravitational waves or other cosmological observables and if there are prospects for detection of these signals you are talking about the phase transition that you need for the classical standard clock this is again about the evolution of the early universe and since we don't know the physics of the early universe we can just imagine what possibly can happen this is one way for this phase transition to be realized at the early universe this is a let's assume that it is an inflationary universe right and this is the scalar field that is rolling on a potential this is the the field space a two-dimensional field space so it is not just a scalar field we have two scalar fields driving inflation and initially you have at the ridge of this potential but you can fall down to the value of the potential then it is a kind of phase transition and this phase transition is something that I was talking about right and this phase transition would trigger the massive field to oscillate and this is the trajectory of the field in the field space you see that there are some oscillations here any other question hello professor so thank you for hearing your talk my question is about like since I am working in extra-dimensional stuff so if ever there is an extra dimension predicted by string theory or some minimal extension of the standard model and you talk about massive particles like for example the right-handed neutrinos or the actions dark photons that could propagate to an extra dimension so my question is like I would like to hear your opinion the dynamic of the extra dimension the size of the extra dimension at the early stage of the universe could you comment about this one thank you I am not sure I got the question I am not expert on the extra dimension stuff but the thing is that the theory is that predict extra dimension would also this is the usual thing that also predicts existence of massive fields if you are living on a lower-dimensional space-time so yeah this physics would also tell you that you should expect to have massive fields at early universe and whether okay one question is that is this distinguishable from a theory which has no extra dimensions but has some additional particles massive particles my guess is that they are not distinguishable but again I am not expert on that are there any other questions okay if not let us thank the speaker again


So welcome back everybody to this afternoon's session. So sorry for the small delay due to small technical reasons. So we are going to proceed. I don't know if the second speaker or the first one if Francis Dejeune is around, because we could not identify him. If it's not the case then we will ask the second speaker, Nana Cruz to share her screen and then proceed with her presentation. And she's not in meeting. Nana is not around? No. Okay. Francis also is not there. No. Okay. Any of the following ones? Semi. Semi. Yes, I'm around. Okay, good. Then you can share your screen and then proceed with your presentation. Okay.  So in total 25. Please, all the guests will be good to mute your microphones. Okay. Can I start? Yes. My name is Adiso Semi. I'm assistant professor in computational data science program at Adisa University. Sorry, Adiso, can we see your face please? Okay, sure. It's much easier to follow a talk with the face to the name. Okay. I'm just, okay. Can you hear me? Perfect. Thank you. Okay. My research interest is to study the organization of convection in the organization of the mechanism of organization of convection in tropical region. So today I'm going to present to you my recent work on relationship between precipitation extreme and convective organization inferred from satellite observations. Since I will use convection several times, let me define what convection is for people who are not from atmospheric physics. So convection refers to any motion driven by the buoyancy and in the atmosphere is manifested as a vertical motion of air parcel due to atmospheric instability driven by surface heating and relative cooling of the atmosphere. Convection refers as deep when parcel originating is a watery layer exceeds the trade in virtual layer. So as you can see it in the graph in the picture, we see deep convective clouds. And this deep convective clouds are aggregated together, and therefore cloud clusters so whenever I'm talking about organization of convection, please try to picture this image, this image. So, deep deep convection exhibits a wide range of spatial and temporal organization, and they are ubiquitous in tropical in the tropics. As you can see it here in infrared image showing the inter tropical convergence on it is it, and that circles the globe around the equator. It is indicated by bands of deep clouds. Deep clouds which are quite in the image. This has been related to variability of weather and to the occurrence of extreme rain rainfall events. So observations and numerical simulation have been used to investigate role of convective aggregation in climate. So, our question is, how is organization of convection related to precipitation extremes. Up to now, there is no consensus among modeling studies enhancement of some some simulation found enhancement in extreme precipitation when applications become more organized, while others could not find an increase in precipitation extremes with organization. Here we are going to use observations of tropical and apply a new diagnostics diagnostics to link between convective organization and aggregation. So aggregation of convection and extreme precipitation. Here is the outline of my talk. First, I'll talk about characterization of precipitation field, then spatial distribution of deep convection in satellite observation. I'll discuss about the link between organization of deep convection and extreme precipitation in local and domain range. Here, latitude and longitude and latitude domains of 10 degree by 10 degree are considered to be mesoscale domains. Since this size is comparable to the domains of most cloud resolving model simulation, model studies of convective organization. In the figure, we are seeing a brightness temperature TV is brightness temperature. And the other one is precipitation field. So, both of them are this snapshot is taken at the same time. So, for a given brightness temperature we have the corresponding precipitation field. So, within the 20 degree south and 20 degree north tropical based, we consider a one degree, a one degree of a moving box of 10 degree by 10 degree. So the, this box is moving every one degree. So we have a brightness temperature for each one degree and precipitation field. So, we have like a total of 14,400 boxes for a given snapshot in the in this tropical belt. So, when we characterize precipitation and fit. First, we obtained the data from trim 3B 42 product, and this has a special spatial resolution of 0.25 degree by 0.25 degree. We consider it is this mesoscale domain, which is 10 degree by 10 degree. And the total precipitation PT is a combination of precipitating region PR and non precipitating region. So we have precipitating and non precipitating region and precipitating region further divide classified into weekly precipitating region and strongly precipitating region. According to this paper. We, we consider strongly precipitating region as whenever they have value greater than two millimeter per hour. So, we define here PT and PR to be PT is the total domain scale and PR is the local scale precipitation respectively. So we can write PT as a product of fractional area of precipitation region and intensity of precipitation region and the precipitation region can be written as a sum of weekly precipitating region and strongly precipitating region. So AR shows the fractional area covered by weekly precipitating region. AR is the total precipitating region. When we say AW is fractional area covered by weekly precipitating and AS is fractional area covered by strongly precipitating region. So, there are, there are more than 546 million mesoscale domains 10 degree by 10 degree domains when we consider all three are the data over a period of 1998 to 2000 day. And we remove, we remove all the domains for which more than 1% of the area is covered by undefined precipitation data. So, when we do this, this reduce the total number of 10 degree by 10 degree domain by 20 27% so here we are showing the PDF, the PDF of total precipitating total precipitating and precipitating region. This is the domain scale precipitating. This is the local scale precipitating. So the dark light that it is clearly shown that the local scale precipitating, precipitating precipitation is much higher than the domain mean precipitation. Then from this we calculate the 99th percentile. So in this paper the 99th percentile, the values greater than the 99th percentile are considered as extreme precipitation. So the domain as a domain scale as a domain is domain scale precipitation, which is PT has a 99% of 1.18 whereas the local scale. 90 precipitation 99% of the local scale precipitation is 4.25. So all values greater than 1.18 is considered as extreme precipitation for the domain scale for the domain scale, whereas all precipitation greater than 4.25 are considered as extreme precipitation for the local scale. So their value is PT 99 and PR 99 respectively. So whenever we see PT 99 it refers to the domain scale extreme precipitation and when we are seeing PR 99 we have to we have to connect it to the local scale extreme precipitation. So this precipitation extreme. So what we are showing here is a frequency of occurrence of the two scales. The first one is the PT, the domain scale, the lower one is the local scale extreme precipitation. So what we are seeing is for a given grid, we are calculating the frequency of occurrence of extreme precipitation in the direction of time. So most of the domain scale extreme precipitation events occur over warm pools of tropical and western Pacific Indian Ocean where one pool of tropical western Pacific and Indian oceans. Whereas the local scale extreme precipitation mostly occur over tropical. The other important parameter is number of convective centroids. So from this brightness temperature field. We identify the local minimum, like for a given three degree, three by three grid, a grid set pixels. First we identify as a local minimum and once we identify the local minimum we compare it with value with the threshold value. And in our case, 240k is considered is our threshold value. If it is less than the threshold value that point will be considered as our convective centroid. As you can see in the figure, all these great points are the convective centroids. One thing here, here we have the same number of convective centroid, but their special distribution is completely different. This one seems more organized than this one. Similarly here, the number of centroid is 105 in this, and here also is 104, but this convective entities are distributed differently for these two cases. So in order to quantify the different spatial distribution, we introduce a matrix called I work on organization index. So what this index is do once it will calculate, it will calculate the nearest neighbor distance between the convective centroids first. So every time it will calculate the nearest neighbors distance, then we'll take the cumulative density function of this distance. So we have NNCDF, which is nearest neighbor cumulative density function. So this curve shows the nearest neighbor distance and we have the corresponding nearest neighbor cumulative density function. So the black curve shows the one that we calculated. The blue curve is an assumption that it is calculated from the theoretical value of Poisson's distribution. It assumes that the distribution is random. So we use randomly random distribution. We compare these two curves. So the one which is actually calculated the NNCDF and the other one is Poisson's nearest neighbor cumulative density function. So what we found is the blue curve shows if the distribution of the convective centroids are randomly distributed, we would have found the curve to lie on the blue line. So that shows the distribution is randomly is random. But if it is below the blue line, we say that it is regularly distributed and if it is above the blue line, then it is considered as more organized. So to quantify this value, we integrate the area under the black curve. So it will give us a specific value that enable us to quantify the level of organization. So we applied this for all the domains to calculate. So all our domains have number of convective points and we can also quantify the level of organization. So here, for instance, the number of convective centroids are 34 but they are differently distributed. This one appears to be more organized than this one. So our index captured this information correctly. And we introduced this in our previous paper with Adrian Tonkin's, we applied it in the cloud resolving model and it successfully captures the evolution of the organization. And now we are applying it to the observation data. And here also we have like the number of convective points are the number of convective centers are 104 and the distribution is looks like randomly distributed. So as you can see it here, the curve seems closely overlap to each other. So, so this is our space, the organization in the level of organization and the number of convective points. So, for a given, for a given snapshot, we have for a given brightness snapshot, we have the corresponding precipitation. So we will get the number of convective points here, and we have the corresponding precipitation value from the precipitation field. In this order, the number of convective point is inversely related to the organization, but it's not always true but usually when we have more number of convective points that it is, we found to be less organized. So here also nicely captures the information. Then we study the link between the mean precipitation and convective organization. So we for each group of N, so we have a group of we classified our data into a group of number of convective points. So for each group of N, we have level of organization and corresponding value of mean precipitation. So this the level of organizations are indicated by by the dots like the blue one shows weak weekly organized the green is is less organized and strongly organized and highly organized is dark, dark rate. So, for a given number of convective point we have this different category, it is classified into different quartiles, and we can see also their corresponding precipitation value. So, for both total precipitation, I mean for domain scale precipitation PT and for local scale precipitation PR. And as we can see here in both cases, as the number of convective, as the number of convective centroid increase, the precipitation also increase. So, we see that stronger clustering is associated with weaker mean precipitation. So, yeah. Now, let's see the link between precipitation extremes and convective organization. So, for a given, for a given. So, this is similar to the previous one, but what we are showing here is the extreme precipitation. This is that. Sorry, allow me to interrupt you just five minutes left please. Okay, okay. So, this is the domain scale x extreme precipitation, and this is the local scale extreme precipitation. So what we are seeing here is for a given in, there is no systematic relationship between extreme precipitation domain scale extreme precipitation and level of organization. So it's not clear in this case, but when it comes to local scale extreme precipitation. It increases systematically. So that with the increase of organization, we see higher efficiency of precipitation. So it increase systematically with a degree of convective clustering. We further see this with the fractional area of precipitation. So, here, we see the fractional area for the domain scale precipitation, and this is a fractional area of local scale precipitation. So, the AR also increase with the number of convective point, but when we see the strongly precipitating region, a which is defined by AS fractional area of strongly precipitating region seems to be related with level of organization. Higher level of organization seems to have to be linked with higher values of AS. So, this is true for both cases for the domain scale and and for the local scale precipitation. So, the fractional area covered by heavy precipitation increases with level of organization in all the missile scale domains where extreme events occur.  So that's why we were not able to see the link between domain scale extreme precipitation and level of organization because then then precipitating area has a stronger weight. So, in conclusion, extremes in domain scale precipitation, which occur mostly over the ocean warm pools primarily depends on the total number of convective centroids within the domain extremes in local precipitation, which occurs mostly over land depends on the degree of convective clustering. Observations are just a strong link between the intensity of extreme rainfall at the local scale and organization of deep convection, especially over land. So this is our key message. So we are, we can see it in the observation that there is a link between level of organization and extreme precipitation and at the level of local scale, which is important information especially for the modeling. This enables them to predict better if we understand the mechanism. So, finally, I have, I have done most of this work in collaboration with San Dream Pony when I was doing my postdoc at CNRS and LMD lab and also I would like to thank Adrian Tomkins from ICTP who helped me to develop a reliable organization index and this is my current institute. Thank you. Good. Thank you for your very nice talk. The talk is now open for questions. Any question? Yeah, Ali. Thank you for your very interesting talk and for injecting some climate physics into this very diverse meeting. I have two questions for you. The first one is in regards to, you know, these convection pictures that you showed. I assume that these are, they're dynamical processes, right? Yes. So these things change over time. So, in some of these density plots that you had, is this something that you get by averaging over a certain amount of time or is it a, yeah, how do you build that figure basically? So, what we did is for a, for every snapshot, like, so we calculated for a period of 1998 up to 2010. So, we consider all of them in the same books. So we put the data in the same books and we do the calculation from those data. But what is, okay, so you, you, you lump a lot of data over many, over a long times into the, into it. What is, how much, what variation is there in those patterns? I mean, there, there, obviously, there are different variation like journal variation, seasonal variation on one. So, we will consider all these things. Our interest here is just to see how they are related, like for a given, a given period, like we have the brightness temperature, and we have station one. So, how are they related? Is there a connection between the level of precipitation and the organization or the characters? This is similar to what we were doing in the modeling. So, we wanted to see how they are, how these two things are related. I see. Okay. Okay. Thanks. Thank you. Yes. Any other questions? You can write in the chat or If nobody asks, I will. Before. You had two questions. So I was, yeah, I was waiting for someone else to. So, is there, okay, I'm, I'm a completely ignorant to this, but is there any correlation between these extreme precipitation events and pollution, so aerosols? Like what is there any connection or is it completely meaningless to even ask that question? Actually, it's a different area. So I didn't look at the impact of the pollution. I mean, there are people who are working on the, on this aerosol impact. I can't give you accurate answer for this. Okay. Thanks. Good. I would have one question. Thanks for the nice talk. So you see a clear difference in between tropical convection over land to over oceans, right? Yes. Yes. And organization matters for the extreme precipitation over land, more than over ocean. Was the surprising to you? Yes. Okay. Yes, it's, it's surprising. Actually, our assumption was always, we thought that we always find organization enhance the extreme precipitation. So I would accept so as well. Yeah. But, but we were not able to see this over the warm oceans. So, in the warm oceans, what dictates extreme precipitation is the number of convective points, not how they, how they organized. When there is more number of convective convective entities, then it tends to have a higher level of extreme precipitation. But over land, there is a local dynamics, which will make it be more intensive. Yeah, I would also expect that the dynamics of convection over land is kind of more complex, even you can get supercells and maybe score lines more often. Yeah. Yes, you are. You're right. So, somehow, still, it doesn't solve this. So, some models found this enhancement related with organization and the others were not able to see it. So, our result is somewhere in the middle. So we are saying both of you are correct. So, what we are seeing over land is similar to those people who found higher extreme precipitation with organization. And for those who are not able to see the impact of organization on extreme precipitation is similar to what we have seen it over the ocean. Thank you. Okay. Good. Professor Tomkins, did you have a question? No, it's okay. I let it drop. It's fine. I think it's being covered. Thank you. Okay, sorry, I didn't see you. It's just now that. No, no, it's okay. I don't want to hold things up. It's okay. Thank you. But we have some time if you want one, two minutes is okay for us. I was just really wondering a little bit, actually, if you thought more about the implications for climate modeling with larger scale models. I mean, is this something that you think should be incorporated somehow into global models of climate where really we don't really have any representation on the sub grid scale of convective organization but they do manage to reproduce organization, should we say on the result very large scales. So do you think, because when you talk about the organizational index, you haven't mentioned very much, whether it's the smaller or the larger scales that dominate. So I was just wondering if you could talk a little bit about those scales and whether it's something you think should be focused upon in GCMs or do they already represent it. Yeah, I think the main message here is we have to understand the mechanism properly so that so that we will integrate this information in the GCMs. So we are asking to understand this mechanism in depth as it has been done in the modeling world. So we are asking for more understanding of that process to enable us to integrate this information in the GCM so that they can forecast extreme precipitation better. So, yeah, do you get your question or. Oh, sorry, I'm muted. Yeah, no, thanks. Okay. So, I think that I really appreciated your talk you can see that it drove many interrogations so now thank you very much for your talk and then we are moving now to the next speaker from Stellenburg University in South Africa. Professor Daniel McKinney.


Let's go down everybody got Kyle here with latent sports cards and we are ripping two boxes for air w both going to be contenders optic basketball Good luck my friend Eric.  We got a red ice uniform to Jabari smith jr Not numbered in a first class ticket of mark williams rookie for the hornets Got a season ticket base of cj mcullum and our hollow is pg Little paul george hollow and this one is blue season ticket of anthony edwards to 99 so ant-man blue And on the back nice one. We got variation to 99 red rookie ticket auto of jeremy sohan Nice one there for you eric wimby's new teammate Should be uh, I think wimby being on the team of help open up some of these guys nice one there Sohan variation tickets to 99 And box number two tealaw trying to ice it tealaw is icing it Calvin redemption here this one is going to be a hoop dreams hollow of Peyton watson rookie For the nuggets got a lottery ticket hollow jaden ivy and red ice hoop dreams jalen williams Well j will That's right base is kevin herter Got hollow season ticket that one is going to be rudy gobear and red trade murphy not numbered season ticket for the pellies Don't do that and redemption It is jalen durin nice one there rookie variation season ticket red That'll look exactly like the sohan to 99 there on the variation season ticket red How you durin nice one there for these sixers as well All righty there eric that'll do up here two boxes some pretty nice autos there by man We will get those right out. See you. Thank you


Hello Java developers! My name is Matt Raebel and today I'd like to show you how to build Java microservices with Spring Boot and Spring Cloud. Let's giddy up! This screencast is based on a blog post that I wrote called Java microservices with Spring Boot and Spring Cloud. If you scroll down past the beginning, you'll see there's a github repo at Octadev, A0, Java microservices examples, and a git clone command. We're going to start with that. We'll do this in our downloads directories. Once that's done, we'll open it up in IntelliJ and I'm going to open up the webflux example. The configuration that we're going to do to make it work with A0 will also work with the MVC example. This readme breaks down how to actually get everything up and running. The API gateway talks to a backend car microservice that just returns a list of cars. Then the API gateway filters out the cars that aren't cool and returns those as another list. There's two different APIs in play and we're going to use OAuth to protect both of them. With A0 CLI, which I already have installed, you can run A0 login, authenticate as a user. It'll prompt you for consent for all the things that the CLI can do with your tenant. Then you're all set there. It's all hooked up with your tenant. Also, just to show you, I have Java 21 installed. You don't need Java 21 to work with Spring Boot 3.2, which is what I'm using, but you do need 17. I just wanted to show you that I am using the latest one there. The first thing I'll do is create OIDC app on A0. Go into the webflux directory here and run A0 apps create. We're going to call it kickass cars, microservice for cool cars. Just a regular web app has callback URL that's standard for the Octa Spring Boot starter and the logout URL to logout. Then we're going to copy the issuer of the client ID and the client secret and the audience into a .env file. If you look at the API directory, there's already an example one here. We can just copy that one, paste it, chop off the .example. The issuer is right up here and the client ID and the client secret. Then rather than specifying the same issuer twice, we can just go here and do it like that. Now we can start the Eureka server, which is just a basic Spring Boot app with enable Eureka server on the main class. Go into discovery service, clear that and gradle boot run. You can also do boot run lowercase, works fine. Then in the car service, we're going to need the issuer and the audience as well. Copy this one, paste it back to here, grab the issuer and start up the car service. Then finally the API gateway. Now we can make sure all apps are running by going to 8761. You can see we have the API gateway in the car service. Then if we were to log in with localhost 8080, it'll take us to OZ0. We can use our credentials here. If you don't have credentials, you can click the sign up or log in with Google. That'll work just fine. Now it's returning my name. If we looked in the API gateway, that comes from the home controller. Set up this decay here. You'll see it's just printing out my full name from the OIDC user object. If we go to slash home, it actually prints it out from the car service. This is the car service right here. It prints out all the claims that are in the JWT. If we look for the other home controller in the car service, you'll see what that looks like. What's happening is in the application.yaml for the API gateway, it is proxying with Spring Cloud Gateway and using a token relay filter to pass the access token down to the car service. This is how we're mapping that home down to it. Also in the API gateway, we have a cool car controller which uses web client and circuit breaker and talks down to that car service to grab that list of cars and filter out the ones that aren't cool. If we go back here and just do cool cars, you can see that it's filtered out the ones that aren't so cool. The other feature is we could get an access token with print token here. I'll print that to our console and then we can grab it. We could set that in a terminal as token equals. Then we'll use HTTPIE to talk to the car service without filtering out any cars. Let's do authorization, bear a token, and you'll see it's got the ones that aren't so cool in there. It proves that access token works within the microservices architecture as well as outside of it. One of the cool things that's automatically supported by Spring Security is refresh tokens. To get a refresh token, you have to pass in an offline access scope. Let's modify the API gateway, ENV file, to use a different audience, one that expires the access token every 30 seconds. By default, I think it's an hour or something like that. I don't want to wait an hour. We're going to create a new audience or a new API in AusZero that expires a lot quicker. To make that new property scopes work, we have to modify the application.properties in the API gateway. These are actually read using spring.env, that's already configured in the project. That's why you have one in your .env, you need it in your properties file as well. Here we are. Then we added some debugging to show the access token getting refreshed. We need to create an API on AusZero using AusZero APIs create. The name is fast expiring the identifier as this HTTPS fast expiring API in the token lifetime is 30 seconds. We'll go ahead and create that. Then we can restart the API gateway. Pull this into its own window here. Put that on the right. Then if we were to log in an incognito window, you'll see when it prompts us for consent, it also has that allow offline access. That's how you know you're getting a refresh token too. Once that happens, it prints the access token to the console. You can see this expires that value here. We'll use this timestamp converter to put it in our own time. Currently 30242 expires at 30257. We'll wait for that to expire. Now if we refresh, we should get a new access token. If we look back at our console, you'll see sure enough, this was the last one that expired at 257. HTTPS posts to the token to get a new one. This one's at 334. We're getting a new refresh token. Spring Security handles that all for us. As long as it has that refresh token in the beginning, it goes and gets a new access token. It's the most secure way of doing things because you want your access token to expire quickly because you can't revoke them. You can revoke refresh tokens. If you want to learn more, there is a demo script in this same project. It's written in ASCII Doctor. If you have the ASCII Doctor plugin, you can see a nice pretty view here. It basically builds everything step by step. It shows you how to do it from the very get go and creating all the projects using start.spring.io. Also, we have a microservices lab. If you're looking for something a little more formal, this steps through very similar to the demo script. I created the demo script first and then created the lab from that. It just steps you through everything with nice, concise steps. It looks a little prettier. You don't need the ASCII Doctor plugin to make it outward. Thanks for watching. I hope you learned a fair bit. If you want to create it all yourself, go check out the blog post. Try the demo script. Try the lab. If you like this screencast, I post a lot of them or I try to. I post frequent tutorials on Twitter. You can find me at MRABLE. I'm also on LinkedIn at MRABLE and on GitHub at MRABLE. You can find my whole team at Octadev on Twitter and subscribe to our YouTube channel because we have a lot of good content about identity and full stack applications and microservices. Enjoy. Have a great day.