Okay, I think we are live. Okay, welcome everyone. Thank you for joining us for today's little physics webinar.  Today, we are presenting Searching for New Particles in the Sky by Masha Vallactar. Professor Vallactar earned her bachelor in physics and mathematics from Harvard and then she did her PhD in physics from Stanford University where she worked with Professor Savas Domopoulos. Before arriving at the University of Washington, she was a band in postdoctoral fellow at the Permanent Institute for Theoretical Physics in Canada and a James Arthur postdoctoral fellow at the Center for Cosmology and Particle Physics at New York University. She works on a variety of things and she's going to mention some of them in today's webinar but in particular, her focus is on theories beyond the standard model and on creating new ideas and direction for testing these theories. We are delighted to have her in our webinar series today and remember you can ask questions over email through our YouTube channel or Twitter and then the questions will be read at the end of the talk. So without further ado, we will turn it time over to Masha. Thanks for joining us. Thank you very much for having me. This is such a great experience so let me just get started. So today I will tell you about new ideas to look for new alternate particles and if she thinks it's not working, let me know. So, right, so I'm a particle theorist and in the world of particle theory we have what we call the standard models which have been very, very successful so some of us younger theorists may be too successful because they describe very accurately and everything that we see and understand about the fundamental particles and interactions and also the cosmological standard model which describes how the universe evolved from its earliest moments to today. And they've been very successful in capturing all of the observations we see which are quite consistent with the predictions. We have multiple measurements of the subcomponents of the universe such as gravitational waves. We have dark matter, dark energy and standard model matter which all intersect given different parameters and different measurements. We have precision measurements in the C and D and the particle physics side we've had great success with both precision measurements where our predictions with the standard model are accurate out to many, many decimal points and also with big discoveries of the final piece of the standard model which is the Higgs boson. However, of course, we all know this is not the full story and that's what I'll talk about today is how do we try to fill out these last puzzles? On the cosmological side, we know that there are these things called dark matter and dark energy just from the gravitational interactions and on the theory side we have a lot of questions about why the scales we have are what they are especially given our understanding of quantum field theory. So for example, why is the Higgs boson here at the weak scale so much lighter on the punk scale? What happens at the plug scale and maybe slightly less well-known questions like why is the electrical moment of the neutron so small? But this little question here is one of the kind of guiding principles for a lot of my work which is these three questions here. So on the theory side, there's something called the strong CP problem in the standard model which I'll describe that points to the new mechanisms that we expect new particles and interactions and on the experimental side, we know there's more stuff out there in particular mode there should be a new particle or a set of particles that makes up the dark matter of the standard model and just in general, it'll be great to have new windows on trying to look at the highest scales in the theory because as it stands, we have only explored fairly narrow range of energies in our experiments on Earth. So to answer these questions, we will talk about the QCD axion and related particles. Sorry, this panel is in the way, can we just move it? Okay, so the QCD axion as many of you know is motivated by the strong CP problem. So the statement of the strong CP problem is that in the standard model of particle physics, we have a lot of interactions that violate charge and parity, so roughly speaking, mirror symmetry. And this is a well-known feature of a lot of the interactions that we observed and have been measuring since the 50s, but for some reason, all of this violation does not propagate into the strong sector for interactions between quarks and gluons. And if you did have charge and parity violation in the strong interactions, you would give the electron, excuse me, the neutron and electric dipole moment. You can see, for example, that the presence of an electric dipole moment violates parity because here, let's look at a neutron. You have a spin, a mu and a dipole moment. If you make a transformation under parity, you would flip the dipole moment because it's a vector, so you flip it to its negative, whereas the spin is a pseudo vector because it's a cross product of two vectors, so it will remain unchanged. So clearly under parity transformation, having a spin between all the neutron heads and the dipole moment is not a good symmetry and the dipole moment will be violated. And we go out and measure it and this has been a tremendous experimental effort for many decades now. And the expected value for the neutron dipole moment, if you just had normal order one violation would be about this number, which looks small, but it's really the size of the neutron times the charge. It's two times the minus 16 centimeters for each electron charge. But the experimental upper bound is even smaller by about 10 orders of magnitude, which implies that this theta parameter, which characterizes how small the violation is, is about 10 to the minus 10 or smaller. So far we don't have an upper bound. So if this theta parameter, which is actually a sum of two different fundamental parameters in the theory that come from the gluon sector and the quark sector is a fixed parameter. This is a huge unexplained cancellation or tuning in the model. And so we'd like to have a better theoretical prediction for it rather than just saying it's a very small number. And luckily for us, there is a great way to explain it, which was proposed almost 50 years ago now, I guess, which is the axion. So instead of saying theta is just a number in the theory, like the electron charge or another coupling constant, you promote it to a dynamical field, which we call the axion. So now the axion can have a potential energy, which is shown here. So if you have some initial value for the axion field, A, you have large CP violation, but this potential has a minimum where charge and parity violation do not occur and being a dynamical field that likes to relax to the minimum of the potential. And this is a whole, I could go into lots of interesting physics here. So you ask if you have questions at the end, but basically the takeaway from this is just that there's a new particle with this potential, which is set by one high-scale parameter F here. And its mass is inversely proportional to this high-scale parameter, which sets the particle's couplings and interaction scale. So you expect a very light new particle, which interacts very loosely with everything else. And in addition to the QCD axion, people predict that many of these theories which try to complete the standard model to high scales to include gravity, can also produce many more of these types of light particles. Which are similar to this QCD axion. So if you have, for example, theories with extra dimensions, the extreme theory, you can have zero modes of fields that are propagating in the extra dimensions, which in our four dimensions look like new ultra light particles if they remain light after all is said and done. And so in addition to the QCD axion, you might, which solves the strong speed problem, you might expect there to be additional ultra light particles with similar properties that don't necessarily couple two nuance in the same way that this one does. And finally, it was realized that the axion or axion-like particles are excellent candidates for to also solve the dark matter puzzle. So although it was proposed to solve this theoretical issue of the QCD problem, it turns out that the axion's cosmological evolution is also exactly what you would need for cold dark matter of the universe. And it's not showing up here, I'm sorry, but basically there was supposed to be evolution equation for the axion field, which is basically a damped harmonic oscillator. So what happens is in the early universe, there's some initial condition for the axion value. And then as the universe expands, the friction is given by the Hubble expansion of the universe, which prevents the axion from developing a large gradient. But then once the universe sufficiently expands for the Hubble friction is small compared to the mass, the axion starts to oscillate around its minimum with a equation of state that's exactly that of a cold dark matter candidate. So to summarize, this is the granular space for axion-like particles. So the QCD axion is this green line here, which I mentioned the axion mass on the x-axis and the axion interaction scale on the y-axis are inversely proportional, so stronger interactions at larger scales. And along this line, you solve a strong CPU problem. If you have more general axion-like particles and you take some kind of more or less generic initial conditions in the early universe during a period of inflation, in the blue band you get order one of axion dark matter. So you get the right density of dark matter from just having this new particle around in the early universe without having to add any extra model building or other sectors. So these are kind of interesting parts in a granular space to focus on. And what I wanna draw your attention to is that if you have these very light particles, they automatically have very, very high interaction scales. So this FA, which sets its coupling to other particles is almost as high as the plug scale, 10 to the 18 or 19 GV, compared to most particles that we typically interact with which are much more strongly interacting. So automatically, if you are lucky enough to discover this new particle, it's not just exciting that you found a new particle, but it would also open up a window to these very high scales in theory. So the summary of why I think it's exciting to look for these new particles is that on one hand, they would address the strong fee problem. They could also make up the dark matter of the universe and they could also teach us about very high scale physics that is very difficult to probe otherwise. And so how do we look for them? And this is main part of my talk is how you can use astrophysical probes to look for these light new particles. And this is not a new idea that some of the best ways we have to look for light weekly couple of particles come from astrophysical objects. For example, if you have something like the sun and we compare how the sun produces more strongly coupled particle like the photon or more weakly coupled particle like the neutrino, you would expect that the flux of photons from the sun is much, much larger than the flux of neutrinos just because they're produced much more frequently. But the photon is actually so strongly interacting with the interior of the sun that it takes a relatively long time to get out once it's produced. So effectively you're really emitting photons from the surface of the sun because any photon that's produced in the volume is going to scatter many times and get reabsorbed and so on. Whereas neutrinos get produced from the whole volume. So even though they're produced much more rarely and there's also different processes that produce neutrinos, but just order of magnitude speaking, the neutrinos are produced much more rarely but they travel, but they are basically produced in the whole volume and they travel outward. And so the flux from the sun and neutrinos is just a couple percent of the whole emission of the solar energy, which is quite large given how weakly a couple of the neutrinos are. And this is actually the first place where people were predicting neutrinos to play an important role in solar processes after they were first proposed as a new particle. They were not discovered in the lab almost 20 years, until almost 20 years after they were already developed as a key component of solar evolution. So changing the neutrinos for an axion, the same thing happens and these constraints I was showing on the axion flux and grays that I'll come back to are exactly from this type of process. Or if you have a weekly couple of particles like the axion produced in the core of the sun may free stream out and it can change the heat transfer and cool the star much more quickly than what we observe. And so this produces a very strong constraint on these types of particles. And even stronger constraint comes from even denser objects like neutron stars that are produced in a supernova. So they are even, the object is so dense that even neutrinos don't see stream out while axions can. And so by looking at the neutrino flux that comes from a supernova, we can already say that there were not axions that were produced in large enough numbers to change the heat transport of neutrinos out from this neutron star. So these are some of the best constraints we have on these new light particles. You can see here in gray as a premise. So you have constraints from the sun and constraints from supernova 1987A which exclude all of this parameter space up here. And then of course there are, this is, there's some experiments here like ADMX which is at the University of Washington which are actually starting to probe really significant and interesting parameter space in the laboratory as well if these particles are the dark matter. And there's lots of ideas about how to keep extending these further. But for this talk, the moral is that we need a lot of energy density to produce like in a star or in a supernova to produce a large enough flux of these particles that they can change the dynamics of the object and we can infer that change and either make a discovery or place some constraints. But these are quite still very far from the interesting parameter space here and the next kind of densest objects that we have in the universe is a black hole. And of course that has completely different dynamics than a star or neutron star but it turns out that we can still use it to probe these new light particles. And that can be done through a process called black hole super aliens. So if you have rotating black hole those can produce clouds very weakly coupled bosons by extracting the black holes rotational energy and extend our reach in this parameter space to very, very weakly coupled particles. So we'll talk about how black holes can teach us about these particles in two parts parameter space for axiom that interacts gravitationally there'll be one set of signatures and for axioms that interact a bit more strongly you can still use black holes to test them but in a slightly different way. And this is a very different production mechanism instead of a thermal production of particles thermal energy of the star being converted to particle production. Now we have a rotational energy of the black hole that's being converted to particles but you still start with this huge amount of energy density that you can use to produce huge amounts of particles. And just to give you a sense of scale at the length scales we'll be talking about are Compton wavelengths of these particles which are kilometers to thousands of kilometers. So very long. And those are set by the sides of astrophysical black holes which are about, tends to hundreds of solar masses their radii are of the same size and we'll talk about why that is. So how do we do black hole searches for ultralight axioms before getting into black hole dynamics I want to talk about super radians which is actually a very simple process. It's the, if you have a rotating object with dissipation you can get super radians. So for example, let's start with a rotating or with a non-rotating cylinder with a lot of friction on the outside. If you have a ball that's scattering off the cylinder with a lossy surface, it'll slow down due to friction. However, if you have a rotating cylinder this ball can actually extract the rotational energy and speed up as it passes by the surface because at the place where it's interacting with the cylinder, the cylinder is actually going faster than the tangential velocity of the ball and it'll give it a kick forward. In the frame of the cylinder, basically it looks like it's slowing down the ball but in the lab frame it's actually speeding it up. So if you have dissipation, you can extract energy from rotating objects if they're speeding fast enough. And so this is a quite general kinematic statement but it turns out to also apply to black holes and wave dynamics. So if you have a wave that's scattering off a rotating object, it can increase in amplitude by extracting the angular momentum and the energy of this rotating object. Unlike the ball, here we're not increasing the velocity but we're increasing amplitude of the wave. That's how the energy is growing. And so you start with some wave packet and can come out with larger amplitude. And the growth is proportional to the probability of absorption onto the object when it's not rotating the same as for a cylinder, you need the ball to be efficiently slowed down when the cylinder is at rest yet to be able to extract the energy when the cylinder is rotating. So black holes are perfect for this because they're perfect absorbers at the horizon. So you have very high rates of dissipation and you also need rotation. So this gives rise to a secretion condition. You want the angular velocity of the wave to be slower than the angular velocity of the black hole horizon. So here's the energy over the M, I'll be calling the angular momentum number of the wave. So e to the IM5 is less than the angular velocity of the horizon. So here's a scattering process of a gravitational wave from a rotating black hole. So incoming is a blue wave and outgoing is a red wave. Just you can separate the two and you can see that outgoing wave is much, much larger than the incoming one in amplitude. So this is a full numerical GR simulation that was done by Will Ease the perimeter which shows how efficiently the black hole can give up its energy into this incoming wave of incoming gravitational waves. And that's very exciting, but it's not very interesting kind of microscopically because we need to already start with a fairly large wave to be able to extract a lot of energy and the amplification is proportional to the initial wave that comes in. But it was realized that there can be an even more exciting process which initially you was on our thought experiment by President Kipulski called the black hole bomb.  You start with a wave packet, it gets amplified, it gets reflected back from the mirror, gets amplified again and eventually the radiation pressure inside the mirror becomes so large that the mirror explodes. This was called the black hole bomb. And of course, this is not a very practical implementation but it gives rise to the next idea which is how do we actually realistically trap particles near a black hole? And that can be done just through gravity again itself. So if you have a massive particle who is massive such that the Compton wavelength is of order of the black hole size, then it will have bound states which are localized very close to the black hole. In particular, if you have just one of our potential for a black hole, which is G Newton times the black hole, mass of the black hole times the mass of the particle over R, then the scale of the gravitational potential is of order of the Compton wavelength of the particle. And if you said these scales are comparable, you have most of the particles in bound states that are localized very close to the black hole and can super radiate very efficiently. So this was known for scalar solutions around mass of scalar solutions around black holes in the 50s and 80s.  So what do these bound states look like? Well, if you're far away from the black hole, it's very simple. We all know how to solve this equation. It's a one of our potential and that gives you energy density of these particles that just follows bound states of the hydrogen atom. So you can classify the solutions by their principle and orbital quantum numbers and L and M. So you can have more angular momentum, which gives more interesting structure and less energy density close to the black hole. And so I'll be talking a lot about this parameter alpha, which is the gravitational fine structure constant in analog to the electromagnetic sine structure constant. So it's the coefficient of the one over up potential, which is G Newton times mass of the black hole times mass of the particle mu. Or you can think of it as the ratio of the black hole size or G to the Compton wavelength of the particle one over mu. The radius of these bound states is, again, the same scaling as for hydrogen atom have one over the coupling times the mass, which is the Bohr radius. And now it's a few to a few hundred black hole radii. So now it's not the same constant everywhere, but depends on the mass of the black hole and to which the particles binding to. And of course, the important difference is now the occupation number. The axioms are both on certain zero particles and you can build up as many of them as you want in these bound states. In fact, exponentially these bound states will exponentially grow in number and we'll see the occupation number can be as high as 10 to the 75 to 10 to the 80 particles. And the other important difference in the solution from what you expect from a hydrogen atom is of course that there's a black hole in the middle and that means that the boundary conditions are very different. So unlike the, when you solve the hydrogen equations, you say that the wave functions have to be regular at the proton and at infinity. Here we put a absorbing boundary condition at the black hole horizon because anything that falls onto the horizon is absorbed and that gives you an imaginary frequency in your energies. So instead of just having the energy, which is a mass minus the binding energy, which is given by alpha squared corrections, just like in hydrogen, you have this imaginary piece which is exactly the super radiance rate. If it's positive, then these bound states will grow exponentially. If it's negative, they will decay. And whether it's positive or negative is set by the super radiance condition. These bound states are non-held mystics of energies just pass to leading order over this angular momentum quantum number. And just to say these are, I'm using the language of quantum mechanics for the solution just because that's where we first see this equation, but these are completely classical states with very large application numbers. So you can think of these as classical objects. So how does this, let's talk about how this would happen in our galaxy, for example. So if new light axioms exist, then any fast spinning black hole will super radiate, which means it will lose energy in angular momentum to exponentially growing bound states of axioms. So let's say there's a new particle we haven't discovered yet, like an axion with mass, the extent of my 13 EV, very, very light.  So here the mass has a light axis and solar masses and the spin is on the y-axis where zero is short-shelved and one is extremo-curve. So the blue regions are the super radiance condition regions where the black hole is rotating quickly enough to super radiate into the different levels. So for example, NLM equals 211 is this region, 322 is this region, 433 is this region. These are the conditions here. So if you have a black hole that's born up here, 40 solar masses and spin 0.9, say in a binary merger at LIGO, then in about a year, if this new particle exists, the black hole will lose a lot of its energy and angular momentum and build up a cloud of these very light particles and saturate the super radiance condition where now the black hole angular velocity is the same as the phase velocity of the particles and the cloud. So the growth stops. And at this point, the black hole angular momentum has decreased by about 10 to the 78 H bar. So each axion has one unit of angular momentum. So L equals one and carries away one H bar from the black hole. So once there's 10 to the 78 particles, the growth stops and so that's why we have about 10 to the 78 particles in the cloud. And you also lose a little bit of mass. So it's black hole is going a bit to the left, but it's hard to see in this picture because relatively speaking, you're putting a lot of angular momentum far away from the black hole so you don't need to put that much mass. So what happens to the particles is what I'm showing on the right side here. So the number of axions is shown on the y-axis as a function of time and the black hole spin is shown again on the y-axis on the bottom panel. So over about one year time scale, the number of axions grows exponentially and then it levels off once the black hole spin is lost. And then on parametrically longer time scales, the next level will grow as shown in the dashed line here. So now it's three to two level, which has a larger angular momentum, which means it has a larger angular momentum barrier. So it sits further away from the black hole and it has less efficient absorption onto the horizon, which means the growth rate is parametrically slower. So you can see that the level is gonna be growing much longer, about a million years in this case, and the black hole spins down again. In between, you see that the number of particles is going down over time and this is due to gravitational wave emission. So you have a very large energy density in the cloud with time dependence set by the axion mass. So just like you can have a neutron star that's rotating at a certain frequency emitting gravitational waves if it's not perfectly axially symmetric. There is some energy density in the cloud with time dependence that gives rise to gravitational wave emission. In particle physics language, you can think of this as annihilation. You have two axions going into one graviton to produce outgoing gravitational wave radiation. And so axions don't have any conserved quantum numbers and you can just deplete the cloud by radiation. So here is another beautiful simulation by Will East which is showing a cloud of particles. This is actually spin one particles for technical reasons they're easier to simulate around the black hole in the center. Particles are shown in the energy density is shown in purple. And you'll see the gravitational wave radiation emitting out because it's this huge classical object that's all rotating together. The gravitational waves that are emitted are coherent and monochromatic which is a very interesting signal that's quite different from what you've already observed in LIGO mergers. So here you can see that there's a sub component of the energy density that's rotating around and that's what's leading to this gravitational wave emission. So what do these signals look like? Here I'm showing the strain each over time as shown as seen in the frame of the black hole. So what's the amplitude of the gravitational wave? It's just a very simple cosine at twice the energy of the axion. And then on Earth you'll observe it in some more complicated form but this is exactly the same as what people in LIGO and Virgo and growing collaboration across the globe are looking for when they look for say neutron stars as I mentioned. If you have a pulsar that's rotating we know it's rotating because it's meeting some electromagnetic waves or we just think there are more pulsars out there that we haven't observed yet directly. They can make gravitational wave radiation which looks very similar to this if they're not perfectly symmetric so if they have a bump for example and these are the types of searches that are already being run on gravitational wave data and we can do similar analyses of different classes to try to look for the presence of superediance in these very light particles. So there's three classes of ideas that I think are very exciting and I'll just quickly mention them here. One is if you look do a blind search across the whole sky and you look at signals from black holes that are in our galaxy. There can be thousands of these signals as I'll show in a second and these can be observed and studied in detail if we are lucky enough to see them. So these are just monochromatic lines that you'll see in the spectrum. Because the frequency is set by mostly the mass of the axiom you can also just lump all of these signals together and look for excess stochastic power in a narrow band in the gravitational waves so you can have a stochastic search or you can also try to look at known black holes. For example a merger where you know that the new rapidly spinning black hole was formed and you can try to see if there's a new signal that's coming from that rapidly spinning black hole due to this gravitational emission from the super radiant cloud. Now that is a very weak relatively speaking signal compared to the merger itself. So for this last one which would be the most dramatic you will probably need future generation gravitational wave detectors. But for now we can do blind searches so here I'm showing the number of signals we would have expected to detect in existing data that's already on tape that we looked at with these collaborators as a function of axiomass and the reason why the spread in the number of detectable signals is so large is because we don't know how many rapidly spinning black holes are nearby in our galaxy. So the range of signals goes from a few to almost a few thousand depending on what the typical spin distribution is for black holes that are produced from stellar collapse but for fairly reasonable assumptions you expect many many signals and so once we have hopefully a better understanding of black hole population properties we can use this to exclude some parts of axiom parameters piece. If you do see signals then of course that would be great studying them in detail and hopefully convince yourself that you're seeing the product of a new particle. So this is what you can do with gravitational wave searches and in the last part of my talk I want to tell you what happens if gravity is not the main driver of these of the evolution of these clouds and I'm not sure how much time I have left let me know but 10 minutes I think okay perfect thank you so so far we've assumed that the whole picture is described by only gravity so you have this new field which I've been calling the axion and it extracts energy from rotating black holes but initially I motivated this by telling about particles which interact with the standard model and also have this complicated potential that's generated so in principle we expect there to be interactions that are not just gravitational so we've been focusing on this part down here of the parameter space the question is what happens once we turn up this interaction are there changes to the dynamics and indeed there are in the first thing that turns out to matter is the quartic interaction of these particles so in addition to the mass term the potential that's produced will have higher order terms in the first and second one will be being a quartic interaction which scales as the mass squared of this coupling squared so if you have this quartic interaction you can get some new really interesting dynamics in the process that in addition to what we already discussed so from super radians you have black holes that produces a cloud of axions for example with intermomentum one oops and you can also have gravitational wave emission which gravitational waves are sourced by the energy density which is quadratic in the field so you have two powers of axion cloud of contribute to emission of gravitational wave radiation but now you have a quartic interaction so you can get these two other processes on the right so the blue cloud with intermomentum one the red cloud with intermomentum two if you start with a cloud that has intermomentum one you can take two axions and put them together and make an axion with intermomentum two but you have some extra energy left over or negative energy left over so this particle will fall into the black hole so you have two axions make one with more intermomentum with zero intermomentum that falls into the black hole you can also have axion emission to infinity so you have two infinities here you can take two axions once you've built up some number in three two two you can take two axions with intermomentum two put one back into two one one and then you have some extra energy left over so you'll have axions two infinities these are unbound particles so now you have new dynamics for a black hole energy sources one bound state two superavians but then the second level can be populated through self-interactions and you also carry away some energy to infinity through non-enrolistic axion waves so let's look at that again in this same time evolution picture so if the axions just interact gravitationally or if this FA is basically the Planck scale then what happens is what I showed you before the number of axions grows exponentially levels off because you spin down the black hole they get depleted through gravitational wave radiation over some longer time scale the next level will grow and the same process will repeat until these time scales become longer than the age of the black hole or the age of the inverse the black hole spin is basically lost in two big jumps at the end of the growth at each level and just notice that sorry here the levels are never occupied two levels are never occupied at the same time because the growth is parameterically different the growth time scale and also going a higher level the black hole loses enough angular momentum that the first level actually becomes not too pre-dead and falls back into the black hole so you can see that this level occupies the number starts dropping very quickly once the next level starts to grow the picture changes dramatically once you have a large chord itself interaction so you have this new process where now you can exchange energy between levels without talking to the black hole so now in orange I'm showing what happens when the FA scale of the axion is much higher say 10 to the 12 GB which gives it a larger chord self-interaction so the number of axions will also grow exponentially but the first level is growing it's going to start pumping the next level as it's growing so the two levels grow together and the solid line and the dashed line grow together and then because you have this process of emission to infinity you have this way to release energy from the cloud so as the black hole is pumping up these levels you're also emitting axion waves out to infinity and you have this quasi-equilibrium configuration where once you get to a large enough occupation number the number stays fairly constant over time as the black hole energy is being pumped into the cloud and the cloud is emitting axion waves over a much longer time scale the black hole eventually spins down and then you lose the source energy and eventually the number of axions will also decrease so if you have particles with stronger self-interactions what happens is the number of particles in the cloud is reduced because now you have this energy leak out to infinity and also the black hole spins down much slower because the rate of extraction of angular momentum is proportional to the number of particles in the cloud so it's going to be much longer now we have this understanding we can use insisting data of black hole spin measurements to place some constraint on particle parameter space so I told you that you have basically the main thing about superannuation is that it spins down black holes so if you have a spinning black hole you can exclude the fact that this process occurred and since this process happens it's a classical instability of these black holes so if you have a rapidly rotating black hole it'll just automatically super-adiate if you have the right particle so for example these spin measurements here are from telescope observations of black holes and binaries and all of these black holes circled in red would be expected to be at the bottom of these blue super-adiance curves if there is a new light axion this mass here and so we can use the combination of these observations and our understanding of what happens when you have large self-interactions to place some constraints so here are five black holes that we have spin and mass measurements of and as a function of the axion mass here on the x-axis and the self-interaction on the y-axis some range of parameter space is excluded because you would have expected these black holes that have high spins to have spun down to much lower spins than what we observe and as self-interactions increase however we know that the spin downtime increases parametrically so at some point here you can no longer place an exclusion and for if you remember the parameter space I was showing in the beginning the QCD axion here falls well into the excluded region and axion like particle dark matters kind of at the edge so it's still fairly constrained by these spin measurements and so you might think okay well then this is a very gravitational process we're given with black holes so at some point once you have no spin down there's not much else you can probe in this parameter space but as I said there is axion wave emission so there's actually a very cool signature that you can look for in future experiments which is that you have this very long period of non-autistic axion emission to infinity where all of these black holes could still be emitting axions today and sending them out throughout the galaxy and we do have so far I haven't assumed anything about how these axions interact in the standard model but if they do interact we have experiments that are being designed to look for axion dark matter which could be in the future reanalyze to look for these axion waves coming from black holes which would be very exciting so it's the same idea as for the gravitational wave emission you have an axion field parameterized by this theta angle that we started with at the beginning which will be oscillating very small amplitude over time and if these axions are both the standard model you see a flux of axion waves sent over millions or billions of years coming from nearby rapidly spinning black holes and there are experiments that are proposed to look for these the best ones are ones where the axions couple the spins of particles for reasons that I can talk about if you have questions so here I'm just showing some projections so if you have an axion mass the effect on nuclear spins on earth is shown on the y-axis so basically you can characterize it by some effect of magnetic field but the important thing is that these are all these blue regions are all amplitudes of the signal emitted from black holes like sigma-6-1 that I talked about or other black holes that we think are nearby and anything above this line would be open parameter space for axion models that so far haven't been probed in kind of the future generation experiments that are looking for axion dark matter so we could see these axion waves coming from nearby black holes depending on the details of the axion coupling so that brings me to the end of my talk so we've talked about ultralight axions and this parameter space here of how you can hope to probe these particles by looking at different objects in the sky and so we've added to this existing constraint from stars and supernova we've added black hole constraints where you extract the angular momentum of the black hole and by measuring the spins you can exclude some parts of axion parameter space but even more excitingly for the future you can hope to measure gravitational waves or axion waves that are coming from this parameter space and try to learn about the strength of the problem and the dark matter and these high scales in our universe so thank you very much for your attention and I'm happy to take questions thank you very much Masha for this wonderful webinar let me see if there are questions in the chat so I found I see one question in the youtube channel is it possible to constrain the axion mass based on the existence of magnetic fields around the super radiant black holes is it possible to constrain axion mass so there are interactions between the axions and magnetic fields so there can be some interesting dynamics there so if you have a very large axion cloud you could have a conversion from axions to photons in the background of a magnetic field that's what this experiment the ADMX does in the case of dark matter and you would in principle this process might occur but what we found and that is something that you could use to constrain or look for axions but what we found is that the self interaction processes that I described at the end of my talk are more important for typical values of magnetic fields so basically unless you really have very much stronger than expected interactions between the axion and the magnetic field given its self interaction what you would normally do is more efficiently emit axion waves rather than interacting with the magnetic field basically you don't build up enough axions for that process to be important and first you would lose these axions to the self interactions but there could be kind of interesting interactions between the axions and the magnetic fields but they just turn out to be a bit small to be observable okay thank you I think Nicolas Bernal has his hand raised yes Niko you kind of mute yourself okay thank you thank you very much for the score nice talk I'm going to have a couple of questions about this slide the first one is here you're assuming that the black will absorb axions in this gravitational cloud in the cable you have self interactions but the same could happen if there's no self interaction whatsoever right yes oh okay sorry I'm not sure if I understand your question so yeah the black hole can always absorb axions whether it's being absorbed or emitted or extracting energy depends on the super radiance condition so sorry I should have said here that these axions have zero angular momentum so then the super radiance condition says that they will be absorbed if you have some other way to mix axions or please axions into alluring the momentum state without self interactions they will also be absorbed and this can happen for example if you have a large gravitational perturbation this has been studied by some other groups like Daniel Baumann and collaborators where if you have the perturbing object you can have mixing of axions in different levels and you can have axions produced in anti-rotating levels with angular momentum minus one and those would be absorbed as well but you'd need very large basically tight binary for that to happen just to answer your question I'm not sure I'm a bit confused so for you talking in the lower left dialogue that you have so you have two axions so you have two axions and one of these goes to the black hole, it's absorbed but what about the case where there's no self interaction you cannot have these 2-2 elastic scattering however one action from who will get absorbed by the black hole or not no it's just in 2-1-1 it doesn't get absorbed so there is well in the very close horizon the wave function is constantly falling onto the black hole but if you look far away the black hole is actually spinning down and so the overall energy is growing so when you just have one axion it doesn't fall the overall rate is to increase the number of particles you have to put you have to well right so the example that you're thinking of is actually also shown in this diagram on the right so for example if you have particles with in the 2-1-1 level but then somehow the black hole spins down below the angular velocity of those particles for example if you extract more energy with the next level then these particles do get absorbed but they only get absorbed if the black hole is spinning too slowly relative to their own angular velocity so for a given angular velocity there's some range of black holes where they don't get absorbed and then there's some range of black hole angular velocities where they do get absorbed I see another two questions in the YouTube channel so the first one is by John by Bay is the super radiant in stability only for black holes or is it possible for neutron stars as well yeah that's a good question excuse me the principle as I argued in the beginning this is a very general process so it is possible also for neutron stars the two ingredients you need are that the object is rotating and that you have absorption so for black holes anything that falls onto the horizon is automatically absorbed for neutron stars if you just have axions you don't have very efficient absorption without assuming further interactions which can exist between the neutrons and the axions but once you have those interactions they are typically better constrained by other experiments for other processes so it's hard for that to be very efficient but in principle there is a rate and some people have thought about this and it's just not very large and also neutron stars can't spin as fast as black holes because they'll just eventually break apart if they spin too quickly so you can have super radiance for neutron stars but the rate at which this growth happens will be instead of tens or millions of years it will be longer than the age of the university you'll never really see a very interesting cloud around the neutron star as far as we know ok thank you there's another question on my academic brother Rohit he says nice talk can these actions be degenerate with some other environmental effects such as tidal effects yeah so I'm not sure if the question is if you see something how do you know the axions and not some environmental effects and mess up the axions which are both good questions I think it's more related to the first one yeah the cloud itself can be very much general with other stuff for example if you have some cloud of axions or an accretion based the cloud is very however it's much denser and much more close to the black hole than what you typically expect from other matter around so I didn't mention this but we talked about how there were tens of this 70 year ADE particles in the cloud but with that in terms of energy density it's basically all of that is sitting in a few tens of radii around the black hole so it's about the energy density of a neutron star that's sitting around the black hole so that's kind of hard to get another way with just standard model processes but then if you're doing some specific observation then it's kind of a case by case basis of how you distinguish that from another process like how good your resolution is on the measurement okay thank you any other question from here okay Diego you can yourself if you want and ask the question I was wondering regarding their recent observation of the black hole of the center of our galaxy looking at the evolution of this kind of image something can be inferred about the super radians yeah and it would be very cool so what I saw is that they do think that the black hole is rotating so that's interesting and so in principle yes this can happen for black holes in the center of the galaxy including the black hole in the center of our galaxy it would be more relevant for particles that have very long wavelengths because these black holes are much bigger so this would be for particles that are even lighter than the ones that I talked about but in principle the same thing goes through the issue is that the time scales are all much longer and black holes in the centers of galaxies are in a sense messier than isolated stellar mass black holes because kind of by definition to get to be supermassive black holes they had to grow through accretion and mergers so the history of these black holes is much more uncertain and so if you have these clouds they could have been disrupted over time and then had to regrow so having firm prediction for what you would see is a bit tougher but in principle you could have these clouds growing around the black hole in the center of the galaxy the observation that event horizon telescope itself is looking very very close to the horizon so it's a bit difficult for that to be to give us information but you could try to look for other observations like gravitational waves once we have lower frequency detectors or things like that. Thank you. Okay, so Nicolas has another question please Nico. Thanks. I was wondering what did you instead of having a physical black hole with a few firm masses you have a super light primary black hole and what not action but heavy heavy particles? Yeah in principle you could I mean this process is kind of there's one overall scale which is the mass of the particle and then there's this dimensional parameter which is the ratio of the black hole size to the particle wavelength so you can just scale it up or down in principle you could look at primordial black holes I think there was even a paper recently about trying to produce new particles from primordial black holes this way the issue is that well we haven't seen any primordial black hole so then it would be kind of a you know you wouldn't be able to say anything without making assumptions about the primordial black hole population but you could do the exercise and see what you get but absolutely you could look for heavier bosons or even heavier axions right we have a lot of parameter states of axions to go so you could look for really tiny black holes in fact one of the first papers I showed by that wire that studied this process just in kind of he was a general relativist so he was just solving the equations around the black hole without thinking about how it would apply to new particles he has a little sentence at the end of the paper that says oh by the way if you had really tiny black holes you could this could happen with pions which is actually not correct because pions are very strongly so you'd have all of this kicking in very early on but in principle people and also they decay quickly but yeah okay and also I mean all what you say completely they apply to any super like not only axions I think the only point where you really use the fact that they're axions is when computing the third interaction right correct yes well I also use the fact that they're spin spin zero you could also do this for spin one particles and but that has it has the same qualitative effects but different quantitative calculations yeah but yeah it's very general okay so you could do the same for spin one or spin two yeah it would be horrible I guess yeah so we did do it for we have studied the spin one case it's actually kind of fun because you have the spin and it's a bit more complicated in terms of the solutions but you could have like same similar bound states but now you have an angular momentum spin vector so just like in an atom you could have like a total angular momentum number and or bro angular momentum number and they could be pointing in different directions so you get more complicated bound states and spin two is a little hard because automatically you would have some scale of self-interaction that kicks in typically or some new states that come in for theory to be consistent so then the range where this is valid is fairly narrow because you build up such huge field densities that you're going to start producing other states or any interactions involved okay thank you okay I think we're way past the hour this discussion it's amazing thank you Masha thank you everyone for thanks for the great questions yes our next webinar would be in about two weeks it's going to be by George Wonk about the recent EHD image so stay tuned and then we hope to see you soon Masha thank you very much for this wonderful talk and then see you around bye bye thank you okay I think we are not live anymore


Hey everybody, it's Bob Lorenz. I'm in my home office thousands of miles away. It's enjoy my yes network colleague We are practicing the ultimate social distancing, right? We're doing it, right? Yes, we are Doesn't get further than this. So hope everybody else is as well. You're being safe. You're with your families I think that's kind of the sort of the byproduct of this right that you're spending more time at home With your family face-to-face conversations, right? I think it's really important that people recognize how important it is to be following the steps and making sure you are Self-isolating with your family away. I'm gonna say this Bob I'm actually seeing this as a little bit of a blessing in disguise an opportunity to sort of slow down from the crazy routine of lice But the rat race so to say and then all of a sudden you get this moment where you're stuck with your family and the Four walls looking at each other for the first time in a long time No plane to catch no car waiting for you no studio to get to all of a sudden you've got now this quality family time So I'm seeing and treating it as a little bit of a blessing in disguise and it's great at this moment in time to spend of course This time with the family. It's unfortunate the circumstances that we're under but I hope everybody's following so Yeah, I hope so too. I think it will make things a lot easier You always heard that term flattening the curve, but it is important You know, I always think about this because I have had to go out a couple times to go get groceries that kind of thing and it's after I've Isolated for five six days, right? And so I'm wondering like did I just reset my clock or am I doing the right things when I'm out to make sure? Okay, you know what you're fine. You're doing exactly what you need to do, but I'm confident of that We have some gloves. We have hand sanitizers that sort of thing So again not getting out there very often only do it if you have to I think that's the important thing But you know the one thing is we do have to eat right so you got to eat you got to get to the grocery store You got to also keep yourself, you know saying make sure that you craft your mental health in situations like this Bob Because it's never easy when you're on your own Maybe you're you don't have family around you you're on your own you haven't deal with a situation in isolation Making sure that you're taking care of yourself trying to keep in some sort of a routine Doing a workout reading a book taking a class online that you probably didn't think you had the time to do Those types of things to keep your your head stimulated and going keep aggressively working out making sure you look after your body Eating the right foods and things like that because it's so easy Bob to slip into this path of sitting on the sofa Watching the symptoms for 24 hours a day. Have you have you been spying on things? We've been doing here because I will say this that our eating habits have slipped a little bit You know you stay at home. You get in a little bit of that comfort food routine, right? Yeah, for example, we had chili last night, which isn't a bad thing it's just probably how much you eat but We have fallen into that habit. So now after a little more than a week of this Like I gotta get back on track the wife got out the workout bands yesterday that kind of thing So you sort of get that mindset back, but it takes a while You know what Bob? I can't believe that I'm getting this opportunity to sit and having a one-on-one discussion with you Because most of the time we're crossing paths at the yes studio I'm on my way to do a game the NYC FC coverage. You're doing a Yankees pre-game or post-game. We're in your office There's obviously 10,000 balls of candy sitting there So I'm coming in to get candy and I see you there.  But I gotta think you've already given us great ideas like I never honestly thought about taking an online class I think that itself. It's like a cool thing. It was like, oh, that'd be a good thing to spend a couple hours a day Doing so staying positive. What kind of positive things are you doing through this? Well staying positive is is obviously an outlook I think I have in life and I always try to take the best of whatever situation or whatever cards have been dealt to me It's always happened throughout my career And I think it's natural when you're a former athlete and a lot of the viewers who are Yankee fans or Nets fans or Liberty fans Who are watching this right now probably are seeing me for the first time They don't know who I am and they don't know I was a former professional soccer player who's working now on the sports broadcast and For my CFC and you know as an athlete You're sort of drilled in to have that positive mentality to be able to pick up yourself from low Situations when you're losing in a game to be able to get the teammates around you G'd up and ready to rock and roll for the second 45 minutes And in that mentality always carried its way through in my life. It comes from my parents as well Bob You know my mom and dad very positive people They are there are people who are obviously in the danger zone right now because they're in the 70s now My father 69 I shouldn't say 70 might kill me But yeah, there are not danger zone so trying to keep them obviously gone is important for me right now And having this positive vibe this positive energy. I think it's easy for me to be able to spread news It's easy for me to have an interaction on social media Everybody out there can reach me on my social media to have an interaction right now Twitter has probably been more positive than I've ever seen Twitter before Facebook's great everybody's telling their story Instagram's great everybody's sharing their pictures I think it's phenomenal social media right now in a moment in life where we're all stuck at home We're in self-isolation. We're all doing the right things. We're showing on social media exactly what we're doing We're sharing ideas everybody's getting creative and for me. It's just it's amazing to see It makes me so happy to see this positivity out there on social media for the first time in a long time Yeah, it's great because as you know, it's social media has really kind of deviated over the years And it's it was became a dumping ground in some ways especially Twitter as you know the instant feedback the instant everything That's what's nice. And I hope like you said this is sort of a reset for all of us in a way It's maybe a reset for all of us on social media as well Kind of take a look at the big picture like you said some of the garbage just throw it out You don't need to address it. Let's stay positive. Let's look at all the good things And I do want to say this if people don't know you from anything else Your line that you used on the one game the savages What's when there were savages in the box, right? You quoted the year, but I love that Was that just forget it that just happened? well, you know since I've obviously started working at the network I followed the Yankees closely and You know, I followed it more and more and as you as you fall in love with it more and more You follow it more and more the stories in front and behind the camera on the field off the field, you know for me It's like it's something I'm waiting for that story I'm waiting for that that's something special to come out so that I can grab it and sort of make it mine and This just it fell from the heavens. It was unbelievable First of all that clip went viral when he went crazy It was for me a great opportunity to be able to grab that line But there was only one situation Bob where I could use it because we only have one box, right? Box and and that goal has to happen inside that box And it has to be someone who is scoring a goal regularly to say he's a savage inside that box So I knew because it was so close to when the incident took place I knew that I had to have one game that if this was gonna happen I was going to say it so when the goal happened You know, I couldn't wait to say it but it was just natural for me because I just I knew it was there The player scored and when he scored I couldn't wait to get the line and as soon as I did You know, everybody was just looking at me like you're crazy. Like you're a believable They loved it and but for me it was a special moment as well because the player deserved it It was a great goal and he is a savage inside that box Saber took his opportunity in that line. I wish I could have cussed there, but I didn't Keep it clean. It is it is cable. Oh, it is satellite, you know, you can pretty much do whatever you want. Well, good You're being a pro good to see I do want to implore our viewers at yes to look for Ian's Promos that he did for NYCFC this year. Those are I mean was that kind of a manifestation of that like it It sort of grew out of that because there I mean the energy that you have the calls that you have with the players They give you by the way I knew when the players were coming in that I had to surprise them. So first and foremost, they didn't know I was there Oh, good. No, we told all the promo guys and the NYCFC guys We were going to do this promo. We only got five minutes with each player So we had to make it quick and the first thing I said to each player because I do have personal Relationships with the players as you know working around sports you you get these personal relationships So I told them don't laugh. Whatever you do don't laugh because if they laugh It's natural and and that's what I wanted I wanted them to try and hold it as long as possible and then have this natural outburst of laughter So when I'm screaming in your ear as you know, Bob when I come into your office with that energy For me it was it's so important. So we got great content there and the commercials available You can see it. That's actually pinned on the top of my Twitter handle right now So anybody who wants to catch it they can see it at Joy Paulie and on all my social media platforms So anybody's welcome like I said before they can talk to me about any sport I love New York sports in general. I love sports in general So I'm across all of it at the moment and of course, that's my passion in life I've got a question for you Bob because while I have you here I guess you have also got this positivity comes out of you you're a great person and I admire that about you You're very friendly. You're welcoming and you've been great towards me But what is it about sports broadcasting that you love so much that comes across to all of us who are watching you? Well, I think probably and by the way I want to say this that positivity that I have that a lot of that came from my family and my parents as well Just kind of instilled in me. I was also the youngest of four kids So I was always a guy trying to you know, get attention and do whatever I could to make him laugh or yeah, whatever I think it's because sports has such passion and think about it every game you 162 baseball games There's passion. There's something exciting that can happen in each game That's so a half a year of excitement and then you translate it to football soccer Basketball hockey whatever else sport you're passionate about so on a daily basis you can have that excitement I think the other thing I've always told people that I love about sports broadcasting is Is it most everything we do is live? So you get one chance to get it right? Ian gets one chance to kick that ball for the game winner, you know what I mean? You don't get a do over you get that one shot at one moment in time and for live broadcasting That's what we have we have one chance to get it right without a safety net and there's there's a juice about that There's an energy about that that to this day and I've been in this business now 87 years something like that You know like we we know especially for a Yankees audience We're so passionate about this team and it's ingrained in them for a hundred years We can't fake it. We can't not give the effort because they're gonna notice So that in itself is kind of exciting, you know, I mean absolutely you have to nail it every time Something about the New York sports public the viewer that I love so much. They want you To be under pressure. They want you to be the latest and greatest breaking news and they want to put you on the spot They want to see you be honest and that is something I love about sports broadcasting because you know I've worked for Fox and I've worked for other networks where Of course, there's this fluff that goes around what the analysts and the host talk about But sometimes and I've noticed this especially in soccer and some certain other sports that they've covered That there's a lot of fluff and it's too much fluff I like to see brutal honesty if I'm working with somebody I'm gonna come down hard on them if they're not telling the truth and I know they're not telling the truth They've not done their preparation I'm gonna make sure that I let them know that's unacceptable and that's what the New York public expect They want to see you be brutally honest be prepared give them that straight That's all they ask for and you do exactly that I mean you're you're fortunate to work with so many great analysts as well, Bob Is there one particular analyst that you've worked with or maybe it's a co-commentator or someone who you've had in studio? It stood out to you that was just one of the best there where even you learn from well because I've worked so much with them Both Jack Curry and John Flaherty What I wanted to and I'm gonna actually circle back and ask you a question.  It's the same thing 30 40 50 years later It doesn't matter you have to be prepared those guys always are They make my job very easy and what impressed me most about them Was the minute Flaherty came off the field and into the studio or the booth the minute Jack came from being a writer And I knew he had some TV experience, but to joining us Seamless you would never have known that it was there and it wasn't their first day in television or in front of a camera You never would have known it. It was just like boom. Let's go. We're off and running. That's impressive That's good stuff because they were prepared right from day one So what I wanted to ask you was the transition from playing to sports broadcasting. Was it seamless for you? Was it easy in a way?  Well, there's a lot out there that people don't know about my transition over to sports broadcasting Obviously I played professional soccer for 14 years, but when I was young 21 years old I got hurt in a game and Missed the next game. So the next game instead of just sitting in the stadium watching the game like most people would do I actually asked if I could do the broadcast. Could I do maybe the radio or could I do a pregame or something like that? Because I was already falling in love with sports media in general Sky Sports in the UK where I grew up in case you couldn't tell why the accent. This is not a San Diego accent You know, I'm in San Diego, but this is not a San Diego accent grew up in the UK Sky Sports took over the world and and soccer in general where it's a religion over there And I fell in love with two or three broadcasters who I was learning from just watching them And I didn't even realize it Bob and that's what our viewers do as well They're watching and they're listening and they're learning and they don't even realize it So I did exactly that. So when I became a pearl, I knew that my post career would Hopefully be jumping into sports media. So 21 years old I took liberty to ask for an opportunity to go into the commentary booth and do color commentary And they said yes, so I actually have two or three clips from that first ever game. I great Oh, I have to share with you. You'll love it. I'll put it on my Twitter as well It is just the the most strongest broad Scottish accent just raw material that you'll ever hear But it gave me this buzz and it goes back to what you were talking about earlier on When that camera goes on that red light goes on you either have it or you don't many people could try to learn it Yes, absolutely, and it does take experience to get better in it But I feel like there's certain people who are just natural in front of the camera and they've just got it And I realized pretty early that I had something I had something that I could maybe try to build And make it special and I did it before I finished my career by the time I finished my career I'd already done 40 broadcasts. That's all I was edible. Good. I was ready to rock and roll So I don't mean to interrupt you but every time you maybe either had a break or had an injury where you couldn't play You jumped up into the booth and did a game. Well, there's another thing you don't know about me Bob Is they used to pick up the red card, you know the suspension? So I used to set out a lot of games and and I did get hurt every now and again It sort of held me back in my career, but that was my my moment I went into the booth and and got some experience. So by the time I finished I'd already had 40 games 40 broadcasts. So I knew that was what I wanted to do Yeah, and then I got my opportunity a year after I retired from pro sports It was only 29 when I retired so I was 30 years old when I got my opportunity and I grabbed it with both hands It was not about money was not about anything other than opportunity to gain experience, you know So that's priceless as you know. Yeah. Oh, I tell people all the time. It's about reps You know, you're better if you take 50 swings in the batting cage than zero 500 swings 5,000 swings you're gonna be a better hitter. You're gonna be a better broadcaster everything It's not getting those reps which leads me to the next question when you do look back at that first game that you did Could you tell the difference? Could you look at it and say I remember that look look how nervous I look there Look how haltingly I talked or something like that because I think back to some of my first broadcasts and I probably thought I was really smooth But I probably looked like I was being held hostage or something like Yeah, I mean going back and listening to it now, of course I think you have a tendency to speak very fast when it's your first broadcast because you're nervous and you want to impress and Sometimes you forget your lines or where you are in your production sheet and you're just like oh, I gotta catch up here I've just got to make something up until I find where I'm at So there was certainly a nervousness in my voice and I was speaking way too fast and the viewer wants confidence And that's what I've recognized Through my experience and I'm only eight years in which is relatively young into a sports broadcasting career or broadcasting career in general So for me, it's it's just about that that repetition getting the experience and just coming across Very confident because the viewer the audience your fans the people tune in simply just to watch you Bob Lorenz people do They tune in just to watch you because you're smooth You're a smooth criminal in front of that camera. They love that they feed off that they feed off the energy and the positivity and I Think confidence is very important for sports broadcasting in particular because you want to give each individual supporter Who's tuning in a confidence and and they want to believe what you're saying that this guy knows what he's talking about So is there has there ever been a moment that stood out to you in your broadcasting career? That has been an outstanding blooper like a moment where you've gone all my word I can't believe that just happen now I know there's been many of course this natural it's live television But is there one in particular that stood out to you? Well, there's there's two things and I Mean I'll tell you the first one It was one where I just rolled my eyes when I realized what had happened. It was in my second TV job We were coming out and I had a weekend sports show And we were coming out of break and they immediately with five seconds to go. They told me. Oh You don't have your opening animation. Just go and We're still in black and you can hear me quietly Drop a four-letter word that begins with And I was like And I replayed it and I'm like Did that make air and they're like May have but it was it was real subtle. It wasn't like I was more of like Anyway, that was lost to the ages the other one which you can you don't see me But as I was working Turner for the Super Bowl when it was in Atlanta Yeah, and I was working my my CNN football partner was Trev Alberts and he was talking to Bruce Smith The all-pro the Hall of Famer at a separate they were talking at a plasma and Bruce got hot Dehydrated he collapsed on that on live TV While Trev was talking to him. Well, most people didn't realize is he landed About two feet from me, but you don't see me on camera So I'm hearing his like his breathing and I'm like, oh my god So Trev tossed to me I had to go to break and then we regrouped and got Bruce off the set and got him hydrated and But that's one of those things where it wasn't a blooper per se But it's like one of those things like those moments where you're like whoa. Yeah, what just happened? How about you? I've had a couple.  I like to go to the last red line before they go cute.  I work with here She's across Fox and Turner and and does on she does everything and I always love to make her laugh because she's like a school child in the classroom that can't control herself Like she's just uncontrollably laughs So when I make our laugh before they go cute go they got to start reading the autocue the Teller and she can't read because she's laughing so Trying her hardest so she's a you have to talk you have to talk on air We're live and I have to take over and start the show for just because I made a laugh so much We did have one I have well actually have two situations where you know very well with baseball rain delays and Soccer it's not so common because they play through rain. They'll play through snow. They'll play through anything It's like it's like football. They just play. Yeah, and I was covering Los Angeles football club just helping them out. They just started new football club here the soccer team and They wanted to do their broadcast. So I thought okay first game. I'm gonna go down. It was July Team was playing away in Houston. So they were on the broadcast and this is like YouTube TV or something like that I don't know what it is and I'm like, okay. All right. Here we go. So I do the broadcast I'm already exhausted by the time I get there because it's during the World Cup They're in Houston and it's Houston. They have this rain delay They don't have the luxury of playing in the dome or anything like that this thing is like on delay because there's lightning near the stadium So for one and a half hours, we had to stay live on air while this game was in delay for one and a half hours And there's no commercial break longer than 60 seconds So you're just talking for an hour and a half and I'm thinking okay That's a one-off. It's never happened in my career hour and a half crazy situation. They were like, yeah We look forward to inviting you back Ian. Anyway, they did invite me back They were also playing against Houston, but this time it was in Los Angeles and I thought nothing can go wrong We did a pre-production show where they were making fun of me being the weatherman holding an umbrella The sunshine and I'm like, yeah, haha was fun. It was great the crew's awesome there You'll never guess what happened during this game in Los Angeles They had a lightning delay again during this game We had a delay for another hour in the game So we had to talk for another hour in the middle of the game. Nobody could believe it So that was one story that stood out to me. I've had multiple stories in my young career But it's certainly one of them I bet this one for you Bob because I know a lot of people in New York and around the tri-state area They are aspiring Sports broadcasters, they look up to people like yourself and and they want to know whatever information they can get Do you have a tip? Do you have some advice or what would your advice be to a young broadcaster who's at home? Even right now. They're stuck at home. They've got a microphone They've got a camera Is there a piece of advice that you would give to someone who's young maybe going through this situation right now? Honestly, we already talked about it repetition.  I mean, maybe if you're this would be a tip If you're hanging out you're self-quarantine and your buddy is next door, but you can't go hang out with him Do what we're doing right now and do it as if it's a sports show or it's a talk show or you know, you'll get comfortable with What you say and cadence and how long you talk and if you play it back you realize wow I just prattled on for three minutes. I don't need to do that. I can speak for a minute 30 seconds It'll be fine. I would think something like that with the technology they have today Which was certainly not available when I was growing up.  I mean you you're God knows how older than me Bob But as you've gone through I mean when you started back in the day now you see the technology It's made such a difference to the viewer as well, right? They get to see a better product Wow, absolutely everything digital everything 4k or getting there Yeah, we had the old, you know what next time you're in the office I've got a bunch of old three-quarter inch tapes from back in the day And I still need to go through by the way and I mean the video quality was just horrible And now I mean people are spoiled by everything that they can shoot everything they can see Yeah, it's it's a great era for technology So if you're a kid you want to be in broadcasting I would take advantage of it Just kind of do what we're doing right now Everybody talks about the candy in your office, right? And for me, I knew about it It was like a myth that was out there Everybody talked about go see Bob go talk to Bob go check out his office. You hungry go to Bob's office I'm thinking like what is going on First time I stepped into your office candy is everywhere. What's the story behind the candy? Why you got so much candy in your office? It just like being friendly? Well, yeah, normally Ian won't stop and talk to me. So it's a way to suck him into my world Have a conversation I get lonely No, uh, you know what you just started out as one of those things Like I think I threw a few bowls of M&Ms out then people started coming in and I started expanding the base and now I have like four kinds of M&Ms Reese's peanut butter cups twizzlers. I try and throw something healthy like almonds out there We have one guy Glenn who left Skittles. So we throw Skittles out there now So yeah, just started is you know something nice to do and It's funny though I will tell you this when I come back from let's say Yankee season ends that I Get a couple weeks off and I do a next game. I commit those bowls are decimated They are wiped out.  I can't tell you how great it is to have this opportunity It's unfortunate in the situation that we're in the circumstances people in isolation But content like this is so vital so important to get it out to the people right now because this looks like it could be a long road for people Well, you're a legend for me to get this opportunity to sit and have a conversation with you It's an honor for me and I can't thank you enough because in my young career already There's there's five or six people. I really look up to to look to learn from Every time they go on air See if there's a little nugget that I can take and and maybe make it my own And you're one of those guys bob and and thanks for everything you do Your is a pleasure to know you as a friend but to to get to work alongside you. It's an honor, man Ian I feel exactly the same way you embody everything that's good about this business and again You've been in this business a short time compared to me But your energy your passion It's off the charts and I love it. So I can't wait to see you in person, but let's do this again if we have to This way right I'm here Anytime you want to talk about it the latest news the greatest news because I know there's a lot of fans out there Who want to have this content they want to hear about what's going on with the Yankees What's happening with the nets? The liberty of course my cfc We can introduce maybe a few more soccer stories to those supporters who are out there who don't know the game So well and absolutely and moments like this, you know, we create some content for people who are just craving something right now We're here for you and follow us follow social media everything you can And in terms of just doing what we're doing now You know people want sports to come back, right? So I know you're getting a little stir crazy We all are we keep doing the things the social distancing staying inside Uh, it's going to speed up that process and it's going to get soccer back faster baseball back faster Everything's going to come back faster the things that we love will come back faster if we just do these We're able to get past this Yeah, but YouTube brother take care keep safe look after the family and I can't wait to see you in person under different circumstances YouTube see you soon


The pervasive problem of irreproducibility of pre-clinical research poses a significant threat to the translation of clinical trials generated by CTSA hubs. Stakeholders have proposed solutions to address this issue, but their efforts have been largely unsuccessful due to a lack of focus on the processes of research rather than the products, as well as the absence of consideration of the incentives that drive the research enterprise. To address this issue, CTSA hubs should leverage the principles of team science and the science of team science, SOTS, to develop strategies that promote reproducible research practices from the beginning of the project through its completion. These strategies should include building team-based best practices and identifying observable behaviors that indicate a culture of reproducible research. This article was authored by Betsy Rowland, Elizabeth S. Burnside, Corinne I. Voiles, and others.


Right Tim and Jaco back from the school cast and it's 64 things, 64th, okay and it is we've been around the world, I'm enjoying it, it's around the world, it's a musical theme, we had it in the commos last week, it commonly ups stuff up, so this week is round the world press-ups, I've got no idea what this is, I'll show you one, check out the news, they're not part of the school uniform, these are, you know that they're good, because they're real pantheon, go on, so press-up position and then you've got to go round the world, so you've got to walk yourself around all the way there and then round, is there any license for artistic impression in this or can you of course, yeah additional grades that we're given for artistic impression, so once you've done one then you work your way back and then it's how many can you do in 30 seconds, 30 seconds, yes so we'd like Tim to get a pen somewhere, yes, I've got to get out of the way alright, this is from press-up, ready, three, two, go, are you looking at this hips-up, that looks like some sort of weird cramp fit you're in a conversation on artistic impression, but you're running out of time I'm not honest, you can't say artistic impression and then criticise you for optimisation, how many can you do, two, ten seconds, ten seconds, we didn't go all the way, you're only going to do dark rep then, there you go 30 seconds, do we count in three reps on that, stricter with the rules please David, you need to set the boundaries if you don't want me to go off I need to cast it, yeah. Unprepared as well. All right, ready? That can be. Three, two, one. Go. Ten seconds. The socks look splendid. The socks look great. You've got to have a 360 view of them actually as you go around. I think you still can. I still can. No. Twenty seconds. You're not? No. I've done more than three, so it doesn't matter. Yeah. I can have an idea of what grades you can do. Three. Two. Get along. Yeah. Yeah. Yeah. Yeah. Yeah. Yeah. Yeah. Get along. One. Ask. So send us in your incentives, guys. I would like to see some artistic impression now. Follow them. Don't break the rules. I'd like to see some reps. Okay. See if you can beat Tim. You only need three to beat Tim this week. So those grades are below. If you've got any questions, you can comment. See them in the comments below as well. If you haven't clicked subscribe, that's up by Tim's. If you haven't got our free beginners guide, that's up there. Get that. That's free. That's a no-brainer. And then for last week's challenge, that's down there. So until next time. Class dismissed.


Let me start by saying that it's always a pleasure to participate in ITU events and meet new people and once again this session it provided an opportunity to engage with different experts even if we know some of the companies very well already. For me the major takeaway and I think for everybody on the on the panel in fact was the overwhelming conclusion that a mix of technologies is required if we're going to bridge the digital divide. Now that is nothing new and it's very much what we as an association have been saying for many many years but and this is what surprised me every time we hear it it appears as if it's a penny drop moment of realisation or a new conclusion that without this discussion the experts would not have reached and I think that is something that we should all be surprised by. It is absolutely nothing new that geographies, economies, markets, demographics they are different in every country they're different on different continents. There is no one-size-fits-all so I'm always quite taken aback when I hear sweeping statements like fixed wireless access or 5G has the potential to bridge the digital divide and in the face of the pandemic and the urgency to connect people I think it's really time to pragmatically address the real obstacles to bridging the divide and one of which is precisely the constant need to push back on this kind of binary approach that assumes that there's one technology at the centre and in that context I found Rakuten's question Miro Salem their head of AI his question was both surprising and refreshing especially coming from a mobile network operator. He asked we have to ask ourselves are we really serious about the problem? He said you know we can go to the moon we're even heading for Mars but we can't do this and he highlighted that the core problem is one of economics and for me he couldn't be more accurate it's not about spectrum it's about having the infrastructure to connect to in the first place and that comes down to economic viability and he also said it's a question of evolution and going step by step so the surprise for me was that you had both satellite and mobile both very genuinely calling for a more serious and a more pragmatic approach to connectivity for all. 5G fixed wireless access has the potential to provide fixed access in areas where fiber is not available and yes it can connect lots of users like schools, hospitals, people at home at the same time but when you look at where it is being deployed in reality then you see that it is in fact only in not spots but within urban areas it is difficult to extend it outside of urbanized areas because it requires a connection to the backbone so to reach into lower density areas you can't really see it as an alternative no but you really should be seeing we should be seeing the technologies as complementary because we cannot affordably extend fixed wireless access without for example satellite backhaul and why well there max we are back to the question of economics but there is another relevant consideration here and that's mobility there are so many examples of satellite enabling healthcare on the move or mobile banking or mobile hotspots especially in developing countries and with fixed wireless access the clue really is in the name it's fixed so you don't have the mobility that we expect from a 4G 5G connectivity experience and to that again to that extent again it's not an alternative but I think that the question in itself max potentially pitches one technology against another and that is something that we really must avoid because as we said is a mix of technologies and hybrid solutions that are going to be the answer to future connectivity you're right NGSO systems have brought a lot of attention to the satellite sector and indeed people finally now they understand what is satellite broadband how does it work and I do believe that an important part of this spotlight on satellite is having well-known figures like Elon Musk behind projects like the Starlink Leo broadband program however while Starlink is becoming increasingly well known it is about connecting users directly to satellite broadband in the way that all of us understand broadband connectivity so either we use our mobiles or computers or another device to just connect straight to broadband and with Starlink indeed you are doing precisely that but as I said while Starlink is about that for now it is still far away from being for developing countries because the price point is just too high and that's because of the complexity of the user equipment for Leo broadband systems but most importantly I would note that connecting users directly to the internet is in fact not what most Leo broadband systems are about they are mostly about enabling higher capacity lower latency solutions as part of an integrated satellite terrestrial network to address key market segments that have specific latency requirements for example so if we want to now if we want to talk about satellite broadband connecting users directly in emerging economies then we really need to look at what's happening today and there you have great examples based on GSO systems in fact for example in Mexico where you have I think it's 1.8 million previously unconnected people using the internet thanks to satellite powering wi-fi hotspots across I think it's 2,500 sites or Kenya where one of our members has connected 245 schools and they're providing maths literacy and life skills teaching for marginalized girls again thanks to satellite powered wi-fi sure satellite has the potential to bridge the digital divide and that too within a much shorter timeframe than any other standalone solution but it's not going to depend only on NGSO systems that that would be an erroneous assumption first of all it will happen based on multiple systems across all all orbits as we see it's happening today and secondly it will definitely include hybrid so we mean satellite terrestrial solutions working in concert together that involve either backhauling wi-fi or cellular alongside the direct connectivity but most importantly it's going to depend to my mind on the ability of policymakers to really foster and encourage the use of a mix of technologies and move away from just aiming for really high speeds based on terrestrial 5g for all or some such utopian notion which which ignores economic realities so in the session we had an MNO highlight precisely this issue and in the market we see a variety of terrestrial actors investing in satellite systems as well so there is definitely an organic movement in this direction but it's going to take time not because of the lack of technology solutions but because we need time to change mindsets and policy making and put appropriate frameworks in place. Really important question the ITU's mission is to connect the world and this marries very well with the mission of ISOA and its members which is also to ensure complete connectivity in support of a more equal resilient inclusive society and so both have a very essential role to play the private sector has so much ground experience rolling out networks dealing with regulators securing licenses and for satellite this can be so different from one country to another because of I think the level of understanding around the technology and a technology which is also evolving in leaps and bounds so we see some governments who are very familiar in how to regulate and license satellite and they're making really good use of it to connect their people but we see other countries who have a way to go yet they are not as aware they have not used it yet so they don't know yet how to exploit it so while the private sector can provide useful benchmarks as to what works well what can be done better we need the ITU to take this invaluable information and package it in the form of recommendations and guidance to member states and in the last two years when we look at what your organization has done I mean the ITU has done precisely that they've issued guidelines to support countries when facing national emergencies when facing pandemics and advising them how to achieve last mile connectivity so all of these things on the one hand they have an operational component that is informed by industry but that needs to influence the policy which is where the ITU takes the lead so for me the relationship between industry and the ITU really is symbiotic and fundamental to ensure the success of our respective missions for me these events provide a what I would call a structured networking environment around a topic of common interest and as I said we meet new people every time and with each event we actually learn based on shared perspectives new perspectives that come from different stakeholders but I think what I would highlight which is really unique about the ITU is that it provides a platform which convenes both public and private sectors in a dialogue with each other on an equal footing and that is something that we have to be so appreciative of if we consider a WRC I mean I know I've said this before but we are looking at the world's largest and most successful consensus building process which actually manages to amend an international treaty every four years which other organization can do that and it can't be done without the close interaction and working with industry and it requires also the cooperation of governments similarly what the ITU does with its study groups and by us as industry participating in those study groups and events like the ITU digital world that just happened industry has such an important platform on which it can convey really vital important information to administrations like the importance of leveraging solutions like satellite to achieve their own objectives and also so they understand how we contribute to the UN SDGs so for me the ITU is totally unique in the richness of the platforms it provides both in terms of participants the equal footing that it places them on and in terms of the content that it deals with and from my perspective as as Isoa as the recognized representative body for the satellite community we will continue to renew our commitment to working with the ITU


I was born in Pennsylvania. I was part of a large family, but I'm the youngest of six children. I was born and raised in Dallas, Texas. I've only had a brother. My parents started dating when my mother was a sophomore in high school. My father was a senior, and then they got married. We were actually planning their 50th wedding anniversary when my mother passed away. We've been together 24 years. We were in San Diego when we met. Tony was in the military. And we had gone to a country in western bars to learn how to line dance and two-step. And Tony was there, and Tony came down and said, Will you be my partner? And he was. We sat down at our first date. I told him I loved him, and I wanted to be with him for the rest of my life. And he got back up and went in the bathroom. I was like, huh? We did a lot of fun things, and that's one of the reasons why I knew he was my soulmate was because when we were together, time went fast, and when we were apart, time went slowly. We all got very close, whole family. And the next thing I know, you know, the family has pulled me into their family. So I mean, it's just, his family was there for me. We have nieces and nephews. They've always come down and spent time with us. We really did consider adopting. But at the end of the day, we couldn't both be their parent. And so we started worrying about what would happen. And so I would like to think that, you know, people like Tony and I would have been great parents. We both have careers that mean a lot to us, and so we put a lot of energy into our careers. I am a realtor. And I'm a professor of English education. He loves his students. I love my students. We both, I think, in our lives and careers have taken risks that we felt like we could take because we always knew that no matter what, I had this unconditional love at home that was never going anywhere. Yes, we love each other tremendously. And it shows in a million different ways, like Tim finishing my sentences for me. We are better together than we are separate. I want the ability to make that official. I don't want to go to Maryland and get married and then come home and not be married. I want the real thing. Well, we're Virginia, so we want to get married in Virginia. I served my country. I was injured while serving my country, and it's very important to me to know that I am a part of this country. Tony and I are both really patriotic. My dad fought in World War II, so we were both brought up to love this country, and Tony, that's one of the reasons why Tony joined the military. We've lived our lives with dignity and honesty and openness. We are a married couple, and we would like to be recognized as a married couple. Tony's my soulmate. I love Tony with all my heart and soul. He is my support. He's my backstop. What marriage means to us is that we stand by each other no matter what happens. That when one of us falls, the other person's there to pick him up. The rest of the stuff is just window dressing. Marriage puts us together for the rest of our life. And it really means something substantial because it's been such a long drive to get here.