WEBVTT

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<v Speaker 1>Welcome to Bedtime Astronomy. Explore the wonders of the cosmos

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<v Speaker 1>with our soothing Bedtime Astronomi podcast. Each episode offers a

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<v Speaker 1>gentle journey through the stars, planets, and beyond, perfect for

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<v Speaker 1>unwinding after a long day. Let's travel through the mysteries

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<v Speaker 1>of the universe as you drift off into a peaceful

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<v Speaker 1>slumber under the night sky.

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<v Speaker 2>Welcome to the deep Dive. Today, we're looking at something

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<v Speaker 2>that feels like it's straight out of science fiction. We

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<v Speaker 2>might be at the end of a hunt that's been

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<v Speaker 2>going on for what nearly one hundred years, the search

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<v Speaker 2>for dark matter.

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<v Speaker 3>It's the biggest piece of the cosmic puzzle, and it's

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<v Speaker 3>been missing this whole time. We're talking about the invisible structure,

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<v Speaker 3>the scaffolding that holds literally everything together, and for decades

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<v Speaker 3>it's just been well, a number in an equation, a

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<v Speaker 3>gravitational ghost.

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<v Speaker 2>That's such a good way to put it. And our

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<v Speaker 2>mission today is to really get into a new fine

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<v Speaker 2>that is so specific, so tantilizing that it has the

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<v Speaker 2>entire physics community buzzing.

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<v Speaker 3>It really does.

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<v Speaker 2>We're going to be unpacking the work of Professor Tomanoy

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<v Speaker 2>Totani from the University of Tokyo using data from NASA's

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<v Speaker 2>Fermi gamma rayse based telescope, and the claim is huge.

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<v Speaker 2>They think they may have finally seen it, or at least.

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<v Speaker 3>Seen its fingerprint. It's direct signature. We're going to connect

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<v Speaker 3>the dots today from the abstract theories of the nineteen

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<v Speaker 3>thirties all the way to this cutting edge space telescope

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<v Speaker 3>data from twenty twenty five.

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<v Speaker 2>And we're using the study itself as our guide, the

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<v Speaker 2>one published in the Journal of Cosmology and Astroparticle.

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<v Speaker 3>Physics, exactly because this isn't just about finding something new.

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<v Speaker 3>If this is right, it's the discovery of a brand

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<v Speaker 3>new fundamental particle, something that would force us to rewrite

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<v Speaker 3>the standard model of particle physics.

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<v Speaker 2>Okay, so let's unpack that. If this really is the

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<v Speaker 2>smoking gun, it means that eighty five percent of all

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<v Speaker 2>the matter in the universe is made of stuff that

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<v Speaker 2>is fundamentally different from anything we have ever seen or cataloged.

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<v Speaker 3>Right, the implications are just staggering.

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<v Speaker 2>So we have to approach this with, you know, a

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<v Speaker 2>lot of critical thinking. We need to understand not just

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<v Speaker 2>what they found, but why on Earth it's taken us

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<v Speaker 2>this long to get even a glimpse of it.

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<v Speaker 3>Precisely, to really appreciate what a massive claim this is,

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<v Speaker 3>you have to understand the decades of frankly frustration and

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<v Speaker 3>dead ends, and that journey starts way back at the beginning.

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<v Speaker 3>Why did we even think this invisible stuff existed in

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<v Speaker 3>the first place.

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<v Speaker 2>Okay, so let's set the scene. We're in the nineteen thirties.

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<v Speaker 2>Our understanding of the universe is still pretty new, but

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<v Speaker 2>it's built on these pillars of classical mechanics. You know,

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<v Speaker 2>Newtonian gravity, right, And.

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<v Speaker 3>The assumption was simple. What you see is what you get.

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<v Speaker 3>If you want to know the mass of a galaxy,

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<v Speaker 3>you just add up all the light from the stars,

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<v Speaker 3>estimate the mass of the gas and dust.

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<v Speaker 2>And that's your total mass. That tells you how much

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<v Speaker 2>gravity it has exactly.

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<v Speaker 3>And this is where the Swiss astronomer Fritz Zwicki comes in.

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<v Speaker 3>He was this brilliant though apparently very cantankerous scientists.

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<v Speaker 2>I heard that.

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<v Speaker 3>Yeah, he was studying a huge collection of galaxies called

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<v Speaker 3>the Coma cluster, and he was trying to measure how

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<v Speaker 3>fast the galaxies inside it were moving around.

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<v Speaker 2>So he's basically timing the speed of this giant cosmic dance.

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<v Speaker 3>A very very fast dance. As it turned out, he

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<v Speaker 3>did the math based on all the light coming from

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<v Speaker 3>the cluster, all the visible matter, the galaxies should have

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<v Speaker 3>been moving at a certain speed, but what he actually measured.

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<v Speaker 2>Was just wrong. They were moving too fast.

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<v Speaker 3>Way too fast, so fast in fact, that the gravity

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<v Speaker 3>from all the visible stars and gas wasn't nearly strong

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<v Speaker 3>enough to keep them from flying away.

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<v Speaker 2>Wait, so, based on the laws of physics, the entire

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<v Speaker 2>coma cluster should have just disintegrated.

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<v Speaker 3>It should have flown apart billions of years ago. The

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<v Speaker 3>galaxies were moving with so much energy that the cluster's

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<v Speaker 3>own gravity couldn't possibly hold them in orbit. It was

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<v Speaker 3>a massive paradox.

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<v Speaker 2>So Zwicki had a choice. Either Newton's laws of gravity

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<v Speaker 2>are completely wrong, or there's a whole lot of mass

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<v Speaker 2>in that cluster that he just can't see.

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<v Speaker 3>And that's the conclusion he came to. He was confident

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<v Speaker 3>in his measurements. He reasoned there had to be some

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<v Speaker 3>other source of gravity, an enormous amount of unseen matter

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<v Speaker 3>holding it all together. He called it dunkle material, dark matter.

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<v Speaker 2>And people didn't exactly jump on board with this idea,

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<v Speaker 2>did they.

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<v Speaker 3>Oh, not at all. He was largely ignored, even ridiculed.

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<v Speaker 3>The idea that maybe ninety percent of the universe was

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<v Speaker 3>made of some invisible, unknown substance was just too radical.

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<v Speaker 3>People thought, you know, it must be an error in

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<v Speaker 3>his calculations, or some dust were not accounting for.

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<v Speaker 2>Just a weird anomaly exactly.

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<v Speaker 3>The idea was just shelved for decades. It was a

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<v Speaker 3>theory way ahead of its time.

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<v Speaker 2>But the evidence didn't go away. In fact, it came

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<v Speaker 2>back with a vengeance in the nineteen seventies with astronomers

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<v Speaker 2>like VERA. Rubin and Kent Ford.

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<v Speaker 3>And that was the pivot, That was the moment this

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<v Speaker 3>went from a weird idea to a fundamental problem in physics.

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<v Speaker 3>Reuben and Ford weren't looking at giant clusters. They were

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<v Speaker 3>looking at individual spiral galaxies like our own Milky.

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<v Speaker 2>And they were measuring how fast the stars were rotating

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<v Speaker 2>around the center of the galaxy.

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<v Speaker 3>Right, and you'd expect something similar to our solar system.

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<v Speaker 3>Mercury moves really fast, Earth is a bit slower, and

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<v Speaker 3>Neptune way out of the edge is just crawling along.

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<v Speaker 3>The further you get from the central mass, the slower

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<v Speaker 3>you go.

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<v Speaker 2>But that's not what they found in galaxies.

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<v Speaker 3>Not even close. They found that the stars way out

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<v Speaker 3>on the fringes of the spiral arms were moving just

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<v Speaker 3>as fast as the stars near the core. The rotation

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<v Speaker 3>curves were flat, which is impossible unless unless there's a

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<v Speaker 3>huge invisible halo of mass surrounding the entire visible galaxy,

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<v Speaker 3>extending far beyond the stars. Its gravity is what's keeping

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<v Speaker 3>those outer stars in their high speed orbits, stopping them

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<v Speaker 3>from flying off into space.

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<v Speaker 2>So after forty years, Zwicki was vindicated. This wasn't just

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<v Speaker 2>a quirk of the Coma cluster. It was everywhere. Every

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<v Speaker 2>galaxy seemed to be embedded in this massive, invisible halo

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<v Speaker 2>of dark matter.

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<v Speaker 3>It went from being a curiosity to a cosmic necessity.

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<v Speaker 3>And that raises the billion dollar question that physicists have

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<v Speaker 3>been wrestling with ever since. If this stuff makes up

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<v Speaker 3>eighty five percent of all matter, why can't we see it?

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<v Speaker 3>Why is it so incredibly elusive?

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<v Speaker 2>And the answer gets down to the fundamental forces of nature.

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<v Speaker 2>It's all about what it doesn't do.

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<v Speaker 3>It's all about the electromagnetic force. That's the force that

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<v Speaker 3>governs light, electricity, magnetism, basically everything that makes matter visible

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<v Speaker 3>and interactive particles interact with photons, which are particles of light.

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<v Speaker 2>They can absorb light, reflect it, emit it.

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<v Speaker 3>But dark matter particles, whatever they are, they just don't

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<v Speaker 3>seem to play that game. They have no electric charts.

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<v Speaker 3>They just ignore light completely.

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<v Speaker 2>So a particle of dark matter could pass right through you,

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<v Speaker 2>right through the Earth, without hitting a single thing. It's

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<v Speaker 2>completely transparent, which.

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<v Speaker 3>Makes it invisible to every telescope we've ever built. We

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<v Speaker 3>only know it's there because we can feel its gravity.

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<v Speaker 3>We're trying to study a ghost.

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<v Speaker 2>So if you can't study it with light, you have

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<v Speaker 2>to find another way. You have to hope it interacts

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<v Speaker 2>with one of the other fundamental forces, even if it's

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<v Speaker 2>just a tiny, tiny bit.

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<v Speaker 3>And that's exactactly the strategy that led scientists to the

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<v Speaker 3>leading theory, to the whimp hypothesis.

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<v Speaker 2>Okay, so if dark matter ignores the electromagnetic force, scientists

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<v Speaker 2>had to place a bet which of the other forces

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<v Speaker 2>might give us a clue, and they landed on the

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<v Speaker 2>weak nuclear force.

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<v Speaker 3>That's right, And this led to the dominant candidate for

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<v Speaker 3>what dark matter could be for a long long time.

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<v Speaker 3>The WIMP. It stands for a weekly interacting massive particle.

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<v Speaker 2>And it wasn't just a random guess, right. This idea

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<v Speaker 2>came out of other bigger theories in particle physics.

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<v Speaker 3>Exactly. It emerged naturally from theories like supersymmetry, which proposed

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<v Speaker 3>that every known particle has a heavier super partner. The

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<v Speaker 3>lightest of these super partners would be stable massive and

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<v Speaker 3>would interact via the weak force. It was a perfect

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<v Speaker 3>dark matter candidate just waiting to be discovered.

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<v Speaker 2>So let's break down the name weekly interacting Why is

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<v Speaker 2>that part so important?

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<v Speaker 3>Well, the weak nuclear force is one of the four

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<v Speaker 3>fundamental forces, but as its name suggests, it's incredibly feeble

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<v Speaker 3>and only works over very short distances. It governs things

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<v Speaker 3>like radioactive decay.

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<v Speaker 2>So if dark matter particles interact through that force, it

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<v Speaker 2>would explain why they're so hard.

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<v Speaker 3>To detect, it would. It means they would stream through

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<v Speaker 3>normal matter through us through planets almost all the time

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<v Speaker 3>without ever hitting anything. An interaction would be an incredibly

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<v Speaker 3>rare event. It solves the elusiveness problem perfectly.

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<v Speaker 2>Okay, so that's the weekly interacting part. What about massive.

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<v Speaker 3>That's crucial for a couple reasons. First, they need to

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<v Speaker 3>be massive enough to clump together under gravity and form

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<v Speaker 3>those giant halos around galaxies that we see the effects

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<v Speaker 3>of light. Particles wouldn't do that.

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<v Speaker 2>And the second reason, the second.

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<v Speaker 3>Reason is key for actually finding them. If they are massive,

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<v Speaker 3>say hundreds of times heavier than a proton, it gives

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<v Speaker 3>us something to look for. It gives us Einstein's famous

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<v Speaker 3>equation E equals mc square.

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<v Speaker 2>Ah. Okay, mass can be converted into energy, and this

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<v Speaker 2>brings us to the really clever part of the whole search,

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<v Speaker 2>the annihilation sign.

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<v Speaker 1>Right.

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<v Speaker 3>If trying to catch a single wimp is nearly impossible,

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<v Speaker 3>what if we could see what happens when two of

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<v Speaker 3>them collide? Okay, the theory predicts that WIMPs are their

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<v Speaker 3>own antiparticles. So when two WIMPs zipping around in the

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<v Speaker 3>dense center of a galaxy happen to crash into each.

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<v Speaker 2>Other, they annihilate. They just vanish, poof.

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<v Speaker 3>They're gone. But their mass can't just disappear. It gets

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<v Speaker 3>converted instantaneously into a shower of pure energy, and that.

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<v Speaker 2>Energy creates other particles that we can detect exactly.

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<v Speaker 3>It produces a whole cascade of familiar standard model particles.

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<v Speaker 3>The heavier the original wimp, the more energy is released,

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<v Speaker 3>and the heavier the particles that are created, things like

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<v Speaker 3>quarks or even w and z bosons.

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<v Speaker 2>Now those are heavy unstable particles. They don't stick around

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<v Speaker 2>for long.

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<v Speaker 3>Do they not at all. They decay almost instantly, and

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<v Speaker 3>in that decay process, in that chain reaction, they produce

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<v Speaker 3>the final stable thing we can actually look for.

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<v Speaker 2>From Earth gamma race, high energy, high.

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<v Speaker 3>Energy gamma rays. That's the smoking gun. The whims disappear,

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<v Speaker 3>they create these heavy unstable particles, and those particles immediately

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<v Speaker 3>fall apart and release a flash of gamma ray light.

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<v Speaker 2>And the beauty of this is that the energy of

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<v Speaker 2>that gamma ray is directly connected to the mass of

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<v Speaker 2>the original wimp that started the whole thing.

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<v Speaker 3>That's the fingerprint. It's a direct line. If you can

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<v Speaker 3>measure the precise energy of the gamma ray, you can

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<v Speaker 3>calculate the mass of the dark matter particle that created it.

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<v Speaker 3>It's no longer a ghost. It has a specific measurable property.

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<v Speaker 2>So the whole strategy for the last few decades has

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<v Speaker 2>been find the place where dark matter is densest, point

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<v Speaker 2>a gamma ray telescope at it and look for a

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<v Speaker 2>specific spike of energy that can't be explained by anything else.

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<v Speaker 3>That's the game plan in a nutshell. And there's one

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<v Speaker 3>place in our neighborhood that is by far the most

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<v Speaker 3>promising hunting.

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<v Speaker 2>Ground, the center of our own galaxy, the Milky Way.

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<v Speaker 3>All the models show that our galaxy is sitting inside

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<v Speaker 3>this enormous, sort of football shaped halo of dark batter,

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<v Speaker 3>and the density of that halo gets highigher and higher

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<v Speaker 3>the closer you get to the galactic core.

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<v Speaker 2>More density means more whimps packed into a smaller.

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<v Speaker 3>Space, which means a much higher chance that two of

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<v Speaker 3>them will actually collide and annihilate. It's the brightest spot

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<v Speaker 3>on the dark matter map.

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<v Speaker 2>But it's also an incredibly messy and violent place. Astronomically speaking,

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<v Speaker 2>You've got a supermassive black hole, exploding stars, pulsars, all

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<v Speaker 2>sorts of things throwing out high energy radiation.

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<v Speaker 3>And that's the monumental challenge. How do you listen for

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<v Speaker 3>the faint, specific whisper of dark matter annihilation amidst the

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<v Speaker 3>deafening roar of a thousand other cosmic fireworks going off

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<v Speaker 3>at the same time. That was the problem Professor Tatani's

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<v Speaker 3>team had to solve, and solving that problem required an

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<v Speaker 3>instrument built for exactly this purpose. The data that Tatani's

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<v Speaker 3>team analyzed came from NASA's Fermi Gamma ray space telescope.

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<v Speaker 3>It's been orbiting Earth for years, mapping the sky in

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<v Speaker 3>the highest energies of light, so let's.

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<v Speaker 2>Get right to it. The team sifts through all this

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<v Speaker 2>data from the Galactic Center, What specific signal did they

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<v Speaker 2>make managed to pull out of all that noise?

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<v Speaker 3>After a very very careful analysis, they isolated a gamma

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<v Speaker 3>ray signal with a remarkably specific energy. The photons they

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<v Speaker 3>found were clocked at twenty gig electron vaults.

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<v Speaker 2>Okay, twenty gv let's ground that number for a second.

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<v Speaker 2>We hear these terms, but what does twenty billion electron

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<v Speaker 2>vaults actually mean? How energetic is that?

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<v Speaker 3>It's immense? For perspective, the light our eyes can see

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<v Speaker 3>has an energy of maybe two or three electron vaults.

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<v Speaker 3>A medical X ray might be a few thousand. We're

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<v Speaker 3>talking about photons that are billions of times more energetic

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<v Speaker 3>than visible light.

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<v Speaker 2>So it's an extremely high energy.

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<v Speaker 3>Signature, an incredibly high energy signature, And that's the first clue.

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<v Speaker 3>An energy that high can really only come from a

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<v Speaker 3>very energetic event, like the annihilation of a really massive particle.

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<v Speaker 3>The more mass you start with, the more energy you

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<v Speaker 3>get out.

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<v Speaker 2>So the energy level is the first perfect match. But

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<v Speaker 2>the second clue, and maybe this is even more important,

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<v Speaker 2>was the signal shape and location.

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<v Speaker 3>Absolutely, if this was just say a pulsar, a spinning

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<v Speaker 3>neutron star, you'd expect to see a single bright point

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<v Speaker 3>of light. But that's not what they saw.

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<v Speaker 2>What did they see.

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<v Speaker 3>Tatani described it as a distinct halo like structure. It's

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<v Speaker 3>not a point. It's a diffuse glow that's brightest toward

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<v Speaker 3>the galactic center but extends outward, fading gradually.

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<v Speaker 2>That's the clincher, isn't it. That shape is a dead

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<v Speaker 2>ringer for the theoretical models of the dark Manner halo itself.

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<v Speaker 3>It's an almost perfect spatial match. You have a signal

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<v Speaker 3>with the right energy showing up in the right place

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<v Speaker 3>and distributed in the right shape. When you line all

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<v Speaker 3>three of those up, the odds of it being some

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<v Speaker 3>random astronomical objects start to drop very very quickly.

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<v Speaker 2>The observational data is lining up with the theoretical profile

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<v Speaker 2>of a wimpiss. So let's talk about that profile. What

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<v Speaker 2>does a twenty GF gamma ray tell us about the

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<v Speaker 2>wink that made it?

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<v Speaker 3>Well, this is where it gets really exciting for the

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<v Speaker 3>particle physicists. You can work the map backwards. A gamma

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<v Speaker 3>ray with twenty gv of energy would be produced by

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<v Speaker 3>the annihilation of WIMPs that each have a mass of

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<v Speaker 3>roughly five hundred times the mass of a.

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<v Speaker 2>Proton proton masses. Now is that significant in the grand

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00:14:04.399 --> 00:14:07.399
<v Speaker 2>scheme of all the theories out there? Where does a

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<v Speaker 2>five hundred proton mass particle fit?

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<v Speaker 3>It's extremely significant because it starts to narrow things down.

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<v Speaker 3>For a long time, many of the most popular theories,

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<v Speaker 3>especially those connected to supersymmetry, were predicting much heavier WIMPs,

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<v Speaker 3>maybe thousands of times the mass of a proton.

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<v Speaker 2>So this is actually on the lighter side of what

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00:14:24.639 --> 00:14:25.519
<v Speaker 2>people were expecting.

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00:14:25.639 --> 00:14:28.360
<v Speaker 3>It is. A wimp with about five hundred times of

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00:14:28.399 --> 00:14:31.519
<v Speaker 3>proton's mass is still very heavy, but it falls into

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00:14:31.559 --> 00:14:34.639
<v Speaker 3>a specific window that a lot of previous searches might

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00:14:34.679 --> 00:14:38.000
<v Speaker 3>have overlooked. It immediately forces theorists to look at a

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00:14:38.000 --> 00:14:41.120
<v Speaker 3>different set of models. Any new theory of dark matter

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00:14:41.240 --> 00:14:43.159
<v Speaker 3>now has to be able to produce a particle with

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00:14:43.240 --> 00:14:45.799
<v Speaker 3>this specific mass. It's a hard data point.

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<v Speaker 2>So you had the energy peak at twenty gv, but

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<v Speaker 2>not just a single spike, right, The annihilation should produce

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<v Speaker 2>a whole spectrum of energies.

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<v Speaker 3>Yes, and that's another crucial piece of the puzzle. The

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00:14:56.039 --> 00:14:59.039
<v Speaker 3>overall shape of the energy signal they found, not just

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00:14:59.120 --> 00:15:02.799
<v Speaker 3>the peak, also aligns incredibly well with the spectrum you'd

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<v Speaker 3>expect from whimps of this mass annihilating into other particles

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00:15:07.159 --> 00:15:08.720
<v Speaker 3>like bottom quarks for example.

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<v Speaker 2>It's the whole package. Yeah, the energy, the shape, the spectrum,

319
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<v Speaker 2>it all fits.

320
00:15:13.080 --> 00:15:15.399
<v Speaker 3>It's a remarkably coherent picture.

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00:15:15.840 --> 00:15:19.720
<v Speaker 2>But as we said, the galactic center is chaos. How

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00:15:19.720 --> 00:15:22.360
<v Speaker 2>did they convince themselves and how do they convince the

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00:15:22.399 --> 00:15:24.879
<v Speaker 2>rest of the world that this isn't just some other

324
00:15:24.960 --> 00:15:28.320
<v Speaker 2>weird thing that also happens to produce twenty jv gamma

325
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<v Speaker 2>rays is.

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<v Speaker 3>The most difficult part of the analysis, and it's what

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00:15:31.279 --> 00:15:33.960
<v Speaker 3>makes this claim so credible. They had to systematically rule

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<v Speaker 3>out everything else pulsars have the wrong energy spectrum. Cosmic rays.

329
00:15:38.320 --> 00:15:41.279
<v Speaker 3>Hanging gas clouds produce gamma rays, but again the shape

330
00:15:41.279 --> 00:15:43.240
<v Speaker 3>in the spectrum don't match this halo.

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<v Speaker 2>And their main strategy was to look just outside the

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<v Speaker 2>very center right to avoid the worst of the noise.

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<v Speaker 3>Exactly, they deliberately cut out the data from the central

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00:15:53.120 --> 00:15:56.960
<v Speaker 3>galactic plane itself, because it's just saturated with radiation from

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<v Speaker 3>known sources. They focused on the extended diffuse glow around

336
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<v Speaker 3>that noisy core.

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00:16:02.679 --> 00:16:04.679
<v Speaker 2>So they looked at the subtle glow in the back range,

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00:16:04.799 --> 00:16:07.080
<v Speaker 2>not the bright fireworks in the foreground.

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00:16:06.919 --> 00:16:10.440
<v Speaker 3>Right, and by doing that, they isolated a signal that is,

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<v Speaker 3>in their words, not easily explained by any of the

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00:16:13.200 --> 00:16:17.000
<v Speaker 3>usual suspects. When you've ruled out every known possibility, the

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00:16:17.000 --> 00:16:20.279
<v Speaker 3>one that remains, no matter how extraordinary, starts to look

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<v Speaker 3>pretty compelling.

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00:16:21.279 --> 00:16:23.960
<v Speaker 2>And the most compelling explanation left on the table is

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00:16:24.000 --> 00:16:28.159
<v Speaker 2>the annihilation of a five hundred proton mass dark matter particle.

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<v Speaker 3>It all points in that direction, the energy, the distribution,

347
00:16:30.639 --> 00:16:33.879
<v Speaker 3>the frequency, it all converges on that one whim model.

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00:16:34.399 --> 00:16:37.200
<v Speaker 2>Okay, so this is the moment everything pivots. If this

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00:16:37.279 --> 00:16:40.480
<v Speaker 2>signal holds up to scrutiny. If this really is wimp annihilation,

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<v Speaker 2>then we're not talking about a theory anymore.

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<v Speaker 3>We're talking about a real physical particle. As Professor Totwani

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<v Speaker 3>himself said, this would mark the first time humanity has

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<v Speaker 3>seen dark matter.

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00:16:50.960 --> 00:16:53.799
<v Speaker 2>And that leads directly to the massive consequences for physics

355
00:16:54.039 --> 00:16:55.000
<v Speaker 2>for the Standard model.

356
00:16:55.240 --> 00:16:59.080
<v Speaker 3>The Standard Model of particle physics has been unbelievably successful,

357
00:17:00.000 --> 00:17:02.720
<v Speaker 3>describes all the known particles, all the forces, but it

358
00:17:02.759 --> 00:17:06.119
<v Speaker 3>has these two huge glaring holes in it. It can't

359
00:17:06.119 --> 00:17:08.839
<v Speaker 3>explain gravity, and it has absolutely nothing to say about

360
00:17:08.920 --> 00:17:09.440
<v Speaker 3>dark matter.

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00:17:09.720 --> 00:17:13.240
<v Speaker 2>So if this WIMP is real, it is by definition

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00:17:13.599 --> 00:17:17.359
<v Speaker 2>a new particle. It's something that exists outside that beautiful

363
00:17:17.759 --> 00:17:18.920
<v Speaker 2>established framework.

364
00:17:19.160 --> 00:17:22.400
<v Speaker 3>It's the first definitive piece of evidence that the Standard

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00:17:22.400 --> 00:17:26.640
<v Speaker 3>Model is incomplete. This wimp. It's massive, it interacts with

366
00:17:26.680 --> 00:17:29.480
<v Speaker 3>the weak force, but it just doesn't fit anywhere on

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00:17:29.480 --> 00:17:32.359
<v Speaker 3>the current chart of quarks and leftones. It's like finding

368
00:17:32.359 --> 00:17:34.759
<v Speaker 3>a new continent on a map you thought was finished.

369
00:17:34.799 --> 00:17:36.039
<v Speaker 2>It means you have to draw a new map.

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00:17:36.119 --> 00:17:37.960
<v Speaker 3>You have to expand the theory. It means there's an

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<v Speaker 3>entire dark sector of particles and forces that we've been

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<v Speaker 3>totally oblivious to it fundamentally changes our definition of what

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<v Speaker 3>matter even is.

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00:17:45.799 --> 00:17:49.039
<v Speaker 2>But a claim that big one that rewrites the textbooks

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<v Speaker 2>requires an unbelievable amount of proof. This is where the

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00:17:52.440 --> 00:17:58.079
<v Speaker 2>scientific community goes from excitement to intense skepticism.

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00:17:57.480 --> 00:18:00.839
<v Speaker 3>And rightly so. The urgeon of proof is an enormous So.

378
00:18:00.839 --> 00:18:04.039
<v Speaker 2>What does that verification process actually look like? It can't

379
00:18:04.079 --> 00:18:06.240
<v Speaker 2>just be one team's analysis.

380
00:18:06.160 --> 00:18:09.519
<v Speaker 3>No, absolutely not. There are two main lines of attack here.

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00:18:10.079 --> 00:18:13.839
<v Speaker 3>First is independent verification. Other teams of physicists around the

382
00:18:13.880 --> 00:18:16.880
<v Speaker 3>world need to take the exact same public data from

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00:18:16.880 --> 00:18:21.960
<v Speaker 3>the Fermi telescope and run their own completely independent analysis, using.

384
00:18:21.799 --> 00:18:23.960
<v Speaker 2>Their own methods, their own code, to see if they

385
00:18:24.039 --> 00:18:25.599
<v Speaker 2>find the same thing exactly.

386
00:18:26.000 --> 00:18:28.440
<v Speaker 3>Can they filter out the background noise in their own

387
00:18:28.480 --> 00:18:31.720
<v Speaker 3>way and still pull out that same twenty gv halo.

388
00:18:31.839 --> 00:18:33.160
<v Speaker 2>That's step one, and what's step two.

389
00:18:33.440 --> 00:18:36.880
<v Speaker 3>Step two is finding the signal somewhere else. Finding it

390
00:18:36.960 --> 00:18:40.759
<v Speaker 3>once in a very messy place is fantastic, but finding

391
00:18:40.759 --> 00:18:44.160
<v Speaker 3>the exact same signal in a completely different, much cleaner

392
00:18:44.240 --> 00:18:45.960
<v Speaker 3>environment that would be undeniable.

393
00:18:46.079 --> 00:18:48.240
<v Speaker 2>This is the wimprerun you mentioned. Yeah, you need to

394
00:18:48.240 --> 00:18:51.160
<v Speaker 2>find a cosmic clean room, a place that's packed with

395
00:18:51.279 --> 00:18:54.240
<v Speaker 2>dark matter but doesn't have all the other astrophysical fireworks

396
00:18:54.279 --> 00:18:54.960
<v Speaker 2>going off.

397
00:18:54.759 --> 00:18:57.200
<v Speaker 3>And we know exactly what to look for. Those The

398
00:18:57.240 --> 00:19:00.759
<v Speaker 3>perfect targets are the dwarf galaxies that or our own

399
00:19:00.799 --> 00:19:01.359
<v Speaker 3>Milky Way.

400
00:19:01.400 --> 00:19:02.759
<v Speaker 2>Why are they so perfect for this.

401
00:19:02.960 --> 00:19:06.000
<v Speaker 3>Because they are completely dominated by dark matter. They have

402
00:19:06.119 --> 00:19:08.440
<v Speaker 3>very few stars, so they're very dim, but they have

403
00:19:08.480 --> 00:19:11.759
<v Speaker 3>a huge amount of mass for their size. Their mass

404
00:19:11.799 --> 00:19:13.319
<v Speaker 3>to light ratio is off the.

405
00:19:13.319 --> 00:19:15.799
<v Speaker 2>Charts, and crucially, they're quiet.

406
00:19:16.039 --> 00:19:19.319
<v Speaker 3>They're very quiet. They don't have supermassive black holes at

407
00:19:19.319 --> 00:19:22.200
<v Speaker 3>their centers, they're not forming lots of new stars, they

408
00:19:22.200 --> 00:19:25.359
<v Speaker 3>don't have the chaos of the Milky Way's core. They

409
00:19:25.359 --> 00:19:29.559
<v Speaker 3>are almost pure, clean laboratories for studying dark matter.

410
00:19:29.759 --> 00:19:31.640
<v Speaker 2>So if you point the Fermi telescope at one of

411
00:19:31.640 --> 00:19:35.000
<v Speaker 2>these dwarf galaxies and you see that same twenty gv

412
00:19:35.240 --> 00:19:36.559
<v Speaker 2>gamma ray signal.

413
00:19:36.359 --> 00:19:38.519
<v Speaker 3>Then you've got it. That's the nail on the coffin.

414
00:19:38.599 --> 00:19:41.119
<v Speaker 3>Because you've now seen the exact same fingerprint from the

415
00:19:41.160 --> 00:19:44.960
<v Speaker 3>exact same particle in two radically different environments. The odds

416
00:19:45.000 --> 00:19:47.319
<v Speaker 3>of that being a coincidence are practically zero.

417
00:19:47.519 --> 00:19:50.079
<v Speaker 2>That would be the moment you can confidently say you've

418
00:19:50.079 --> 00:19:51.720
<v Speaker 2>discovered the dark matter particle.

419
00:19:52.279 --> 00:19:55.480
<v Speaker 3>That's what would provide the overwhelming evidence. And Professor Totani

420
00:19:55.559 --> 00:19:58.000
<v Speaker 3>himself points this out. He says, detecting the signal from

421
00:19:58.079 --> 00:20:01.720
<v Speaker 3>dwarf galaxies would provide even stronger evidence that the gamma

422
00:20:01.759 --> 00:20:05.000
<v Speaker 3>rays originate from dark matter. We're all basically waiting for

423
00:20:05.039 --> 00:20:05.680
<v Speaker 3>that confirmation.

424
00:20:05.839 --> 00:20:08.480
<v Speaker 2>Now. It's just an incredible journey. You go from Fritz

425
00:20:08.519 --> 00:20:12.480
<v Speaker 2>Wicki nearly a century ago, just looking at fuzzy smudges

426
00:20:12.519 --> 00:20:15.960
<v Speaker 2>of light moving too fast, to today where we're pinpointing

427
00:20:16.000 --> 00:20:18.720
<v Speaker 2>the energy signature of their invisible components colliding.

428
00:20:19.000 --> 00:20:22.240
<v Speaker 3>It's a beautiful example of how theory and observation work

429
00:20:22.359 --> 00:20:26.240
<v Speaker 3>together over decades. It shows that sometimes the biggest discoveries

430
00:20:26.279 --> 00:20:30.160
<v Speaker 3>aren't about seeing something totally unexpected, but about finally building

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<v Speaker 3>the tools to see something we knew deep down had

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<v Speaker 3>to be there all along.

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<v Speaker 2>All right, So let's wrap up this deep dive and

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<v Speaker 2>boil it down to the key takeaways, the things you

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<v Speaker 2>should remember from this whole incredible story.

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<v Speaker 3>First, it all started with gravity. Zwiki in the nineteen

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00:20:45.720 --> 00:20:48.559
<v Speaker 3>thirties saw that galaxies were moving too fast, which meant

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<v Speaker 3>there had to be a huge amount of invisible or

439
00:20:51.720 --> 00:20:55.200
<v Speaker 3>dark matter, providing the extra gravitational glue.

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00:20:55.319 --> 00:20:57.680
<v Speaker 2>Second, the main theory to explain this was the WIMP,

441
00:20:57.960 --> 00:21:01.160
<v Speaker 2>the weekly interacting massive particle, and the key idea is

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<v Speaker 2>that when two whimps collide, they annihilate and produce a

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<v Speaker 2>detectable flash of high energy gamma rays.

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<v Speaker 3>Third, that's the breakthrough. Professor Totani's team, using data from

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<v Speaker 3>the Fermi telescope, found a signal that fits that description perfectly,

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00:21:16.079 --> 00:21:19.039
<v Speaker 3>a diffuse halo of gamma rays right at twenty gv

447
00:21:19.519 --> 00:21:20.680
<v Speaker 3>near the galactic center.

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00:21:20.839 --> 00:21:23.839
<v Speaker 2>And that signal is consistent with a WIMP that has

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<v Speaker 2>a mass about five hundred times that of a proton,

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00:21:26.960 --> 00:21:29.400
<v Speaker 2>a signal that can't be easily explained away by any

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00:21:29.480 --> 00:21:31.039
<v Speaker 2>other known astronomical source.

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<v Speaker 3>And if this gets confirmed, it's the first time we've

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<v Speaker 3>ever seen dark matter, and it proves the existence of

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<v Speaker 3>a new particle beyond the standard model. It literally changes physics.

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<v Speaker 2>And finally, the next crucial step is verification. Scientists are

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<v Speaker 2>now looking for that exact same twenty gv signature in

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<v Speaker 2>the clean, quiet environments of dwarf galaxies. If they find

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<v Speaker 2>it there, it's case closed.

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<v Speaker 3>So for you, the listener, You're now completely up to

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<v Speaker 3>speed on what could be one of the biggest scientific

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<v Speaker 3>revolutions of our lifetime. This isn't just an actandemic paper.

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<v Speaker 3>It is fundamentally redrawing the map of our universe.

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<v Speaker 2>Which brings us to our final provocative thought. If we

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<v Speaker 2>are just now, after one hundred years, finally confirming the

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<v Speaker 2>existence of the stuff that makes up eighty five percent

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<v Speaker 2>of all matter, It makes you wonder, doesn't it.

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<v Speaker 3>It really does.

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<v Speaker 2>If that much of the universe was completely invisible to

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<v Speaker 2>us until now, what else is out there? What other particles,

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<v Speaker 2>what other forces might be lurking just beyond the reach

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<v Speaker 2>of our current technology, just waiting for the next Zwiki

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<v Speaker 2>or the next Fermi telescope to bring them into the light.

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<v Speaker 3>The invisible universe might be far stranger and more complex

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<v Speaker 3>than we can even begin to imagine.

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<v Speaker 2>A truly mind bending thought. Thank you so much for

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<v Speaker 2>joining us on this deep dive into one of the

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<v Speaker 2>Cosmos' greatest mysteries. Keep asking questions and we'll see you

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<v Speaker 2>next time.

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<v Speaker 1>The Steam.

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<v Speaker 3>School stas SA
