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 back today. We are strapping in for quite a journey.

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<v Speaker 2>We're diving into a universe that doesn't actually exist in

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<v Speaker 2>the sky, but inside a supercomputer.

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<v Speaker 3>That's right, we're talking about the Flagship two Galaxy Mocks simulation.

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<v Speaker 3>It's genuinely the largest, most detailed synthetic simulation of the

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<v Speaker 3>Cosmos ever put.

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<v Speaker 2>Together, an unprecedented scientific achievement, really, and it's absolutely foundational

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<v Speaker 2>for what's coming next in astronomy.

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<v Speaker 3>Absolutely, So our mission today is to unpack this thing,

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<v Speaker 3>Flagship two. If you're say, prepping for a big meeting

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<v Speaker 3>on where cosmology is headed, or maybe you just want

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<v Speaker 3>to grasp how scientists are actually going to handle the

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<v Speaker 3>insane amount of data coming.

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<v Speaker 2>Our way, then this is the place to be. This simulation.

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<v Speaker 2>It's not just some cool tech demo.

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<v Speaker 3>No, not at all. It's the essential blueprint, the roadmap

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<v Speaker 3>for discovery.

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<v Speaker 2>And the scale of this blueprint, that's what really jumps

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<v Speaker 2>out first. When we say largest, we mean well, utterly

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<v Speaker 2>staggering numbers. We're talking about a digital universe with three

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<v Speaker 2>point four billion simulated galaxies inside it. Just try to

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<v Speaker 2>wrap your head around that amount of information.

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<v Speaker 3>It's almost impossible. And scientists build this this simulated reality

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<v Speaker 3>very deliberately to get ready for and then you know,

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<v Speaker 3>ultimately interpret the flood of data that's coming from ESA's

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<v Speaker 3>EUCLID mission.

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<v Speaker 2>The European Space Agency's big eye in the sky exactly.

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<v Speaker 3>And what's really critical here, you see, is that this

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<v Speaker 3>simulation does two key jobs. It there's two masters if

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<v Speaker 3>you like. Okay, On one hand, preparation, it lets the

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<v Speaker 3>EUCLID team build and crucially test their analysis methods, their

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<v Speaker 3>software pipelines.

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<v Speaker 2>Right ironing out the bugs before the real data hits precisely.

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<v Speaker 3>But on the other hand, there's a kind of prophecy aspect.

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<v Speaker 3>Because the simulation is built on our current best understanding

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<v Speaker 3>of the universe, the standard model of cosmology, it creates

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<v Speaker 3>this perfect theoretical prediction.

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<v Speaker 2>Ah, So it's like here's what the universe should look

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<v Speaker 2>like according to our theories.

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<v Speaker 3>See exactly, it builds the target that reality. The actual

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<v Speaker 3>data from EUCLID has the other hit or miss.

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<v Speaker 2>And as we dig into the sources talking about this work,

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<v Speaker 2>you know, stuff from the EUCHID Consortium and especially these

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<v Speaker 2>amazing algorithms from USh professor Yokenstatal in his team, we

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<v Speaker 2>start to see the whole point is actually designed to

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<v Speaker 2>find the flaws. They're actively looking for where reality might

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<v Speaker 2>just shatter the theory. They call it searching for cracks

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<v Speaker 2>in the standard model.

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<v Speaker 3>It's a really sophisticated strategy. We're going to explore how

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<v Speaker 3>they built this computational colossus, why it's basically the only

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<v Speaker 3>way forward when you're facing this data avalanche, and maybe

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<v Speaker 3>most excitingly, what kind of potential scientific revolution it could

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<v Speaker 3>actually trigger.

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<v Speaker 2>Okay, let's unpack this journey then, starting with just the

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<v Speaker 2>mind bending scale and the cleverness needed to build this

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<v Speaker 2>digital cosmos in the first place. You really have to

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<v Speaker 2>start with the architect, don't we Behind this massive scale

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<v Speaker 2>flagship two you mentioned Youakim Statle, the astrophysicist at UZH.

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<v Speaker 2>He developed the algorithms that really underpin the whole simulation.

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<v Speaker 3>That's the key, because when you're trying to model three

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<v Speaker 3>point four billion objects, the complexity it just explodes. It's

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<v Speaker 3>not linear, it's exponential.

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<v Speaker 2>So it wasn't just about getting a bigger computer, not

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<v Speaker 2>at all.

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<v Speaker 3>It was about having the mathematical insight, the genius really

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<v Speaker 3>to handle the gravitational interactions between all those objects efficiently.

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<v Speaker 2>The famous n body problem, right, calculating how everything pulls

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<v Speaker 2>on everything else exactly.

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<v Speaker 3>And that's the core challenge in any cosmology simulation. Billions

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<v Speaker 3>or in this case, trillions of particles.

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<v Speaker 2>Wow.

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<v Speaker 3>Previous singulations always had to compromise. Either you simulated a

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<v Speaker 3>big volume with low detail or a small volume with

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<v Speaker 3>high detail.

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<v Speaker 2>You couldn't have both, right.

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<v Speaker 3>Statle's work was about optimizing the calculation, finding clever ways

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<v Speaker 3>to group particles and calculate forces so they could manage

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<v Speaker 3>both scale and resolution. The raw computing power is kind

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<v Speaker 3>of useless without the smart algorithms to distribute the work

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<v Speaker 3>and calculate those dynamic interactions across huge cosmic distances effectively.

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<v Speaker 2>And the result of that optimization is just wow. Let's

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<v Speaker 2>say that number again, three point four billion galaxies. That

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<v Speaker 2>gives you the size of the simulated patch of universey

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<v Speaker 2>and the volume. But you pointed out the real complexity

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<v Speaker 2>comes from the depths of the data for each one.

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<v Speaker 2>What kind of details are we talking about for each galaxy?

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<v Speaker 3>Oh, it's incredibly detailed. We're walking high resolution data design

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<v Speaker 3>to mimic what the real EUCLID telescope will actually capture.

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<v Speaker 3>Each of those three point four billion galaxies isn't just

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<v Speaker 3>a point of light. Each one has four hundred modeled properties, four.

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<v Speaker 2>Hundred four hundred properties.

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<v Speaker 3>Per gal like what, well, the basics you'd expect brightness,

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<v Speaker 3>it's position in three D space, it's velocity, how fast

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<v Speaker 3>it's moving. But then crucial details like its metallicity, how

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<v Speaker 3>many heavy elements it has. Okay, it's star formation history,

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<v Speaker 3>when its stars were born, and critically for one of

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<v Speaker 3>euclid's main goals, it's precise shape and orientation. It's ellipticity.

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<v Speaker 2>Why is the shape the ellipticity so important that they'd

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<v Speaker 2>spend all that computational effort modeling at three point four billion.

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<v Speaker 3>Times ah because that's the bedrock of the dark matter

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<v Speaker 3>mapping effort. We'll get more into this, but basically, EUCLID

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<v Speaker 3>finds dark matter by looking for tiny distortions in the

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<v Speaker 3>shapes of background galaxies caused by gravitational.

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<v Speaker 2>Lenses right the like it's bent by unseen mass exactly.

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<v Speaker 3>So, if your synthetic universe, your simulation doesn't have accurately

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<v Speaker 3>modeled galaxy shapes to begin with, you can't properly train

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<v Speaker 3>the software that's supposed to detect those lensing distortions in

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<v Speaker 3>the real data, So.

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<v Speaker 2>You wouldn't know if your software was working correctly.

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<v Speaker 3>Precisely, you couldn't accurately and interpret the real observations. Those

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<v Speaker 3>four hundred properties are what tie the simulation directly to

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<v Speaker 3>the specific physics and the specific measurements EUCLID is designed to.

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<v Speaker 2>Make okay and tracing back even further before they even

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<v Speaker 2>put the galaxies in the underlying structure, the cosmic web,

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<v Speaker 2>that came from an even bigger calculation, didn't it.

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<v Speaker 3>Oh yes, before populating it with galaxies, the simulation first

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<v Speaker 3>built the large scale structure, the scaffolding of the universe,

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<v Speaker 3>you could say, the dark matter halos and the filaments.

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<v Speaker 2>Connecting them, the cosmic web.

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<v Speaker 3>That's it, and that structure was built by tracking the

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<v Speaker 3>gravitational interactions. Wait for it, four trillion particles, four trillion trillon,

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<v Speaker 3>four trillion individual points, each representing a chunk of mass

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<v Speaker 3>pulling on every other chunk over billions of years of

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<v Speaker 3>simulated cosmic time.

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<v Speaker 2>That number just defines the sheer massive scope of that

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<v Speaker 2>initial n body calculation. You're modeling every significant lump and

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<v Speaker 2>bump in matter density across this huge volume of space,

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<v Speaker 2>simulating gravity's effect over cosmic history.

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<v Speaker 3>Think about the memory needed just to store the position

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<v Speaker 3>and velocity of four trillion points at any given moment, let.

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<v Speaker 2>Alone calculate all the forces between them constantly exactly.

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<v Speaker 3>It's a staggering computational.

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<v Speaker 2>Feat and managing that four trillion interacting particles in one

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<v Speaker 2>giant calculation that's almost beyond imagining. It needed serious computing power,

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<v Speaker 2>right institutional scale. Where did they actually do this?

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<v Speaker 3>Yeah, this monster calculation was run back in twenty nineteen.

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<v Speaker 3>They used the piz Dint supercomputer at the Swiss National

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<v Speaker 3>Supercomputing Center CSCs and Lugano, Switzerland.

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<v Speaker 2>PiZZ Date wasn't that one of the fastest in the

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<v Speaker 2>world at the time It was.

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<v Speaker 3>Indeed, in twenty nineteen, PiZZ Date was ranked the third

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<v Speaker 3>most powerful supercomputer on the planet.

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<v Speaker 2>Okay, and to give people context on what that means

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<v Speaker 2>in terms of resources, the sources really highlight the commitment involved.

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<v Speaker 2>This wasn't just like a big job they ran overnight.

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<v Speaker 3>No far from it. Get this, more than eighty percent

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<v Speaker 3>of PiZZ Dant's entire capacity was dedicated solely to this

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<v Speaker 3>one calculation.

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<v Speaker 2>Eighty percent. Imagine basically shutting down almost everything else happening

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<v Speaker 2>at a major national supercomputing center just to run one simulation.

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<v Speaker 3>It shows you how important this was and just how

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<v Speaker 3>challenging it was computationally. Statle himself said, and I'm quoting here,

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<v Speaker 3>it was a huge challenge to simulate such a large

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<v Speaker 3>portion of the universe at this resolution in a single calculation.

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<v Speaker 2>Because it had never been done before. They needed that massive,

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<v Speaker 2>sustained dedication of resources.

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<v Speaker 3>Absolutely, it pushed the limits.

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<v Speaker 2>So it's important for people listening to understand this two

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<v Speaker 2>step process. Right First, the pure physics track, those four

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<v Speaker 2>trillion particles, let gravity shape the cosmic web over billions

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<v Speaker 2>of years. That builds the underlying framework.

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<v Speaker 3>Yes, the scaffolding, the dark matter distribution. That's step one.

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<v Speaker 3>Step two is then more astrophysical and arguably more complex

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<v Speaker 3>in some ways. Once you have those structures, the dark

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<v Speaker 3>matter halos where galaxy should form the connecting filaments, you

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<v Speaker 3>then have to populate them with synthetic galaxies. And these

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<v Speaker 3>aren't just random points. They have to obey the known

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<v Speaker 3>physical laws of how galaxies actually form and evolve, and critically,

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<v Speaker 3>they have to mimic exactly what the EUCLID instruments will observe.

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<v Speaker 2>So they look like real galaxies to the telescopes, cameras

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<v Speaker 2>and spectrographs.

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<v Speaker 3>Exactly complete with those four hundred properties for each of

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<v Speaker 3>the three point four billion galaxies. This is what produces

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<v Speaker 3>that realistic blueprint Statle talks about a simulation of what

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<v Speaker 3>yuclind will actually see when it looks to the sky.

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<v Speaker 2>So the gravitational physics creates the container, the large scale structure,

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<v Speaker 2>and then the astrophysics fills that container with the right

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<v Speaker 2>kinds of objects, the things EUCLID is actually looking for,

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<v Speaker 2>the light sources. That interplay between modeling the invisible dark

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<v Speaker 2>matter structures and the visible galaxies is really the genius

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<v Speaker 2>of Flagship two.

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<v Speaker 3>It bridges the gap between fundamental theory and actual observation,

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<v Speaker 3>which brings us neatly to the crucial why why go

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<v Speaker 3>to all this trouble? Why dedicate eighty percent of one

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<v Speaker 3>of the world's fastest supercomputers to building a fake universe?

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<v Speaker 2>And the answer really comes down to the sheer amount

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<v Speaker 2>of data that the real EUCLID mission is generating.

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<v Speaker 3>Exactly, let's quickly ground ourselves in what EUCLID is doing.

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<v Speaker 3>It's an ESA space telescope launched in June twenty twenty

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<v Speaker 3>three started its survey, and it's designed to look at

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<v Speaker 3>a huge chunk of the sky over a third of

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<v Speaker 3>the entire celestial sphere, with unprecedented resolution both in imaging

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<v Speaker 3>and spectroscopy.

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<v Speaker 2>That combination of vast area and sharp detail that's the

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<v Speaker 2>source of the problem, isn't it the data logistics problem?

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<v Speaker 3>It is. Julian Adamik, one of the key collaborators on

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<v Speaker 3>Flagship two, puts it very clearly. He explains that EUCLID

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<v Speaker 3>produces data in such sheer volume and speed that having

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<v Speaker 3>humans analyze it manually is just completely impossible.

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<v Speaker 2>Give us a sense of that impossibility. You mentioned three

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<v Speaker 2>point four billion galaxies in the simulation right now.

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<v Speaker 3>Imagine trying to process the real data for billions of

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<v Speaker 3>galaxies and they have Hypothetically, a highly trained astrophysicist could

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<v Speaker 3>analyze everything about one galaxy in just one.

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<v Speaker 2>Second, which is ridiculously fast, totally unrealistic.

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<v Speaker 3>Yeah, but even then it would take centuries of NonStop

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<v Speaker 3>work just to get through the catalog once. And EUCLID

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<v Speaker 3>is delivering this data continuously day after day.

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<v Speaker 2>Wow, that's yeah, that's a staggering bottleneck. It almost feels

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<v Speaker 2>a bit demoralizing. Scientists build this incredible instrument that produces

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<v Speaker 2>data they know they can't possibly look at themselves.

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<v Speaker 3>Well, it's just the focus. The human element moves away

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<v Speaker 3>from clicking on individual galaxies towards designing the algorithms the

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<v Speaker 3>automated systems that can handle the load. And this is

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<v Speaker 3>why the mock data, the Flagship two simulation is absolutely crucial.

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<v Speaker 2>Because you need something to test those algorithms on before

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<v Speaker 2>the real, precious unique data arived.

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<v Speaker 3>Exactly, you have to develop and rigorously test the methodology

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<v Speaker 3>for interpreting these massive, complex data sets in advance. You

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<v Speaker 3>get afford to wait for the real data stream to

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<v Speaker 3>start and then begin figuring out how to process.

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<v Speaker 2>We just fall hopelessly behind.

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<v Speaker 3>Hopelessly you need to be ready to process it almost instantly,

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<v Speaker 3>often within hours or days of it coming down from

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<v Speaker 3>the telescope because the data pipelines have to run continuously

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<v Speaker 3>to keep up.

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<v Speaker 2>So the simulation Flagship two becomes the ultimate training ground.

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<v Speaker 2>It's the perfect controlled environment for the AI and machine

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<v Speaker 2>learning algorithms that have to do the heavy lifting.

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<v Speaker 3>That's a great way to put it. If the simulation

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<v Speaker 3>is this perfect theoretical universe based on known physics, scientists

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<v Speaker 3>can feed that simulated data into their algorithms.

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<v Speaker 2>And see if the algorithms correctly identify all three point

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<v Speaker 2>four billion fake galaxies and measure their four hundred properties accurately.

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<v Speaker 3>Yes, And just as importantly, see if the algorithms correctly

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<v Speaker 3>identify and handle the errors and complexities they'll encounter in real.

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<v Speaker 2>Data, like what kind of errors.

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<v Speaker 3>Things like instrumental effects, noise cosmic rays hitting the detector,

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<v Speaker 3>but also tricky astrophysical things like accurate measuring the shapes

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<v Speaker 3>for lensing, or dealing with deeplending objects. Yeah, where two

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<v Speaker 3>or more galaxies overlap in the image on the sky

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<v Speaker 3>and the software has to figure out that they're separate

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<v Speaker 3>objects and measure their properties individually.

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<v Speaker 2>That's really hard, I can imagine. So if your mock

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<v Speaker 2>data Flagship two is this perfect high resolution replica where

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<v Speaker 2>you know the ground truth, you know exactly where every

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<v Speaker 2>galaxy is and what its property should be, you know

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<v Speaker 2>the right then you can run your software on it,

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<v Speaker 2>see where it makes mistakes, and fine tune it until

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<v Speaker 2>it reaches the accuracy and reliability needed for the real mission.

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<v Speaker 3>Exactly, you calibrate your tools on the simulator before you

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<v Speaker 3>use them on the real sky.

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<v Speaker 2>And this also helps tackle that huge problem in astronomy

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<v Speaker 2>systematic errors. When you look at the real universe and

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<v Speaker 2>find something weird, how do you know if it's genuinely

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<v Speaker 2>new physics or just some subtle bias in your telescope

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<v Speaker 2>or your analysis software.

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<v Speaker 3>Flagship two helps isolate that if your algorithm process is

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<v Speaker 3>the perfect synthetic universe and consistently finds, say that it

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<v Speaker 3>underestimates the distances to small, faint galaxies, then you know

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<v Speaker 3>that bias comes from the algorithm itself or how it

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<v Speaker 3>interacts with simulated instrument effects, not from some strange new

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<v Speaker 3>property of the actual universe. You can then fix the

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<v Speaker 3>code before you let it loose on the real euclid data.

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<v Speaker 2>It really underscores how modern astronomy isn't just about pointing

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<v Speaker 2>telescopes anymore. It's deeply intertwined with sophisticated data science, computer science,

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<v Speaker 2>preemptive coding.

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<v Speaker 3>Absolutely, the modern astronomer, especially on these big survey projects,

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<v Speaker 3>is often as much a data pipeline manager and algorithm

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<v Speaker 3>developer as they are a traditional observer. That simulation isn't illuxiery,

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<v Speaker 3>it's a necessity. It's like a massive digital dress rehearsal,

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<v Speaker 3>or maybe a digital safety net.

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<v Speaker 2>Okay, now we get to what, for many people is

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<v Speaker 2>the really exciting part, the potential scientific drama, because while

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<v Speaker 2>Flagship two is fundamentally this incredible technical exercise in preparation.

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<v Speaker 3>Data handling, algorithm testing, its.

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<v Speaker 2>Ultimate scientific purpose is actually to challenge our current understanding

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<v Speaker 2>of the universe, to actively seek out the flaws in

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<v Speaker 2>our best theories.

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<v Speaker 3>It really is a high stakes test, and it's essential

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<v Speaker 3>for listeners to remember, as we discussed that Flagship two,

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<v Speaker 3>the mock universe is built entirely on the foundation of

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<v Speaker 3>the standard cosmological model, which.

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<v Speaker 2>Is called Lambda CDM. Right, can we just quickly recap

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<v Speaker 2>what that model actually assumes?

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<v Speaker 3>Sure, land to CDM basically says the universe is made

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<v Speaker 3>up of a few key ingredients governed by Einstein's general relativity.

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<v Speaker 3>There's ordinary matter like us, stars, gas, but much more importantly,

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<v Speaker 3>there's cold dark matter.

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<v Speaker 2>CDM, invisible slow moving.

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<v Speaker 3>Stuff exactly invisible, doesn't interact with light, moves relatively slowly,

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<v Speaker 3>and its gravity dictates where structures like galaxies and galaxy

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<v Speaker 3>clusters form. That's the CDM part, okay, and the lambda

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<v Speaker 3>landis represents the cosmological constant. This is the simplest mathematical

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<v Speaker 3>form of dark energy, an intrinsic energy of space itself

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<v Speaker 3>that causes the expansion of the universe to accelerate.

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<v Speaker 2>So dark mata pulls things together, dark energy pushes things apart,

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<v Speaker 2>basically in simple terms.

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<v Speaker 3>Yes, and this LAMB to CDM model, despite its weird ingredients,

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<v Speaker 3>has been incredibly successful. It explains a vast range of

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<v Speaker 3>observations from the cosmic microwave background radiation left over from

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<v Speaker 3>the Big Bang right up to the large scale distribution

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<v Speaker 3>of galaxies we see today.

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<v Speaker 2>So Flagship two simulates a perfect LAMB to CDM universe,

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<v Speaker 2>and the expectation as both statal and atomic mention is

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<v Speaker 2>that euclid's actual observations will broadly speak and confirm the

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<v Speaker 2>matter distribution predicted by Flagship two. That's the baseline, hope

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<v Speaker 2>or expectation.

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<v Speaker 3>That's the baseline. But science rarely progresses just by confirming

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<v Speaker 3>what we already think we know. The real excitement lies

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<v Speaker 3>in the potential for disagreement. Scientists are actively hoping to

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<v Speaker 3>find places where the model breaks down.

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<v Speaker 2>They explicitly anticipate surprises and on a expected discoveries. As

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<v Speaker 2>the sources say, they seem quite convinced the model isn't

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<v Speaker 2>the final word.

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<v Speaker 3>Well, yes, because there are already hints tensions in existing data.

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<v Speaker 3>Statle uses that striking phrase, we already see indications of

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<v Speaker 3>cracks in the standard model.

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<v Speaker 2>That sounds significant. What sort of cracks is he likely

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<v Speaker 2>referring to? Where are these tensions showing up already?

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<v Speaker 3>There are a few areas. Probably the most famous is

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<v Speaker 3>the Hubble tension. Different methods of measuring the current expansion

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<v Speaker 3>rate of the universe the Hubble constant are giving slightly

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<v Speaker 3>but persistently different answers.

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<v Speaker 2>Measuring it locally using supernovae gives one value. Measuring it

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<v Speaker 2>based on the early universe light gives another.

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<v Speaker 3>Exactly and they don't quite agree within their error bars.

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<v Speaker 3>That's a crack.

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<v Speaker 2>Yeah.

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<v Speaker 3>There are also potential issues, though perhaps less statistically strong,

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<v Speaker 3>with how dark matter seems to clump on smaller scales

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<v Speaker 3>compared to LAMB to CDM predictions, or maybe slight inconsistencies

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<v Speaker 3>in gravitational lensing measurements.

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<v Speaker 2>So these are subtle discrepancies found by cobbling together data

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<v Speaker 2>from different telescopes different methods.

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<v Speaker 3>Right, And the hope or expectation is that EUCLID, with

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<v Speaker 3>its huge uniform high precision survey covering billions of years

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<v Speaker 3>of cosmic time in one.

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<v Speaker 2>Go, might finally provide data clear enough and statistically powerful

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<v Speaker 2>enough to show definitively whether these cracks are real and

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<v Speaker 2>maybe reveal new phenomena that LAMB to CDM just cannot explain,

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<v Speaker 2>things about the cosmic web structure or galaxy evolution that

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<v Speaker 2>don't fit the simple.

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<v Speaker 3>Rules that tension really defines the scientific knife edge. Here

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<v Speaker 3>Atomic sums it up perfectly. It will be exciting to

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<v Speaker 3>see whether the model holds up against euclid's high precision data,

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<v Speaker 3>or whether we uncover signs of new shortcomings.

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<v Speaker 2>So Flagship two acts as the perfect theoretical benchmark. It's

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<v Speaker 2>the idealized prediction. EUCLID delivers the messy, complicated.

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<v Speaker 3>Reality, and of that reality, the EUCLID data deviates significantly

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<v Speaker 3>and systematically from the flagship two prediction.

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<v Speaker 2>You can't just blame the simulation because you know exactly

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<v Speaker 2>what physics went into it standard Lambda CDM precisely.

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<v Speaker 3>The blame has to fall on the input physics. The

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<v Speaker 3>assumptions of land to CDM must be wrong or at

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<v Speaker 3>least incomplete.

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<v Speaker 2>And that deviation that confirmed crack. That's where the scientific

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<v Speaker 2>revolution would have to start.

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<v Speaker 3>Absolutely. It would force cosmologists back to the drawing board.

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<v Speaker 3>Do we need more complex form of dark energy? Does

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<v Speaker 3>dark matter have some unexpected properties? Does gravity itself behave

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<v Speaker 3>differently on cosmic scales than Einstein predicted?

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<v Speaker 2>Maybe considering alternative theories like mond, modified Newtonian dynamics or

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<v Speaker 2>other modified gravity ideas.

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<v Speaker 3>Potentially Yes, the simulation, by providing that precise baseline, clarifies

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<v Speaker 3>exactly where and by how much the standard model is failing.

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<v Speaker 3>It points the way for the next generation of theories.

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<v Speaker 2>Okay, let's zoom in on one of those potentially revolutionary areas,

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<v Speaker 2>dark energy it's arguably the best mystery in cosmology. And

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<v Speaker 2>within that standard LAMB to CDM model that Flagship two

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<v Speaker 2>is built on, dark energy is represented in the simplest

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<v Speaker 2>possible way.

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<v Speaker 3>Right exactly as Statle puts it quite bluntly. In the model,

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<v Speaker 3>dark energy is just a constant. It's the cosmological constant Lambda,

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<v Speaker 3>meaning it's unchanging, unchanging in space, unchanging in time. It's

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<v Speaker 3>treated as an intrinsic property of space itself, a constant

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<v Speaker 3>energy density everywhere that doesn't dilute as the universe expands.

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<v Speaker 3>It's the simplest mathematical term you can add to Einstein's

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<v Speaker 3>equations to get accelerated expansion.

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<v Speaker 2>But the whole point of EUCLID, one of its primary

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<v Speaker 2>missions is to rigorously test whether that assumption holds true.

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<v Speaker 2>Is it really just a constant? Why is finding that

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<v Speaker 2>out so critical?

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<v Speaker 3>Because if it's not a constant, if its strength or

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<v Speaker 3>density has changed over cosmic history, then it's not just

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<v Speaker 3>some background property of space time. It must be something dynamic,

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<v Speaker 3>something physical that evolves.

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<v Speaker 2>Which would completely change our picture of the universe's past

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<v Speaker 2>and presumably its future fate.

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<v Speaker 3>Absolutely, if it's a true constant Lambda, the acceleration continues relentlessly,

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<v Speaker 3>leading eventually to a big freeze or maybe even a

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<v Speaker 3>big rip where everything gets torn apart. But if dark

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<v Speaker 3>energy is dynamic, if its strength changes, well, all bets

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<v Speaker 3>are off. It could fade away, could strengthen, It could oscillate.

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<v Speaker 2>And isn't this where theoretical ideas like quintessence come in?

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<v Speaker 3>Yes, exactly. Quintessence is the general name physicists give to

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<v Speaker 3>hypothetical dynamic forms of dark energy, usually pictured to some

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<v Speaker 3>kind of slowly evolving scalar field spread throughout space, a

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<v Speaker 3>bit like the field that might have driven inflation in

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<v Speaker 3>the very early universe, but operating now.

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<v Speaker 2>So finding evidence that lambda isn't constant would be huge.

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<v Speaker 2>It would mean moving from this simple placeholder to needing

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<v Speaker 2>a whole new physical theory of this dynamic field.

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<v Speaker 3>Precisely, it opens up a whole new realm of fundamental physics.

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<v Speaker 2>So how does EUCLID actually test this? How can it

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<v Speaker 2>tell if dark energy was the same strength billions of

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<v Speaker 2>years ago as it is today.

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<v Speaker 3>It comes back to the sheer scale and depth of

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<v Speaker 3>its survey. EUCLID is mapping the positions and distances of

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<v Speaker 3>billions of galaxies across a huge volume of space looking

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<v Speaker 3>back up to ten billion years in cosmic time.

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<v Speaker 2>So it's effectively creating snapshots of the universe at different ages.

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<v Speaker 3>That's a good way to think of it. By measuring

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<v Speaker 3>galaxies at different look back times, astronomers can reconstruct the

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<v Speaker 3>history of cosmic expansion.

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<v Speaker 2>How do they measure the expansion rate at those past times?

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<v Speaker 2>Is it just about how clustered the galaxies are.

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<v Speaker 3>It's primarily done through measuring distances and redshifts very precisely. Redshift,

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<v Speaker 3>as you know, is the stretching of light's wavelength as

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<v Speaker 3>it travels through the expanding universe.

427
00:22:28.440 --> 00:22:31.160
<v Speaker 2>The farther away something is, the more its light is stretched,

428
00:22:31.160 --> 00:22:32.359
<v Speaker 2>the higher it's red shift.

429
00:22:32.480 --> 00:22:36.200
<v Speaker 3>Correct, and the relationship between distance and redshift isn't constant.

430
00:22:36.440 --> 00:22:38.759
<v Speaker 3>It depends on how fast the universe was expanding at

431
00:22:38.759 --> 00:22:42.680
<v Speaker 3>different times in the past. Euclid uses techniques like measuring

432
00:22:42.759 --> 00:22:48.039
<v Speaker 3>baryon acoustic oscillations characteristic patterns in how galaxies cluster as

433
00:22:48.039 --> 00:22:51.200
<v Speaker 3>a sort of standard ruler to get precise distances at

434
00:22:51.200 --> 00:22:52.000
<v Speaker 3>different redshifts.

435
00:22:52.160 --> 00:22:55.920
<v Speaker 2>Ah okay, So by measuring these standard rulers at various

436
00:22:55.960 --> 00:22:59.519
<v Speaker 2>distances and thus various past times. They can chart the

437
00:22:59.559 --> 00:23:00.920
<v Speaker 2>expansion history.

438
00:23:00.799 --> 00:23:04.880
<v Speaker 3>Precisely ademic frames the core question they're asking. We can

439
00:23:04.880 --> 00:23:07.079
<v Speaker 3>see how the universe expanded at that time, looking back

440
00:23:07.119 --> 00:23:11.279
<v Speaker 3>billions of years, and measure whether this constant really remained constant.

441
00:23:11.519 --> 00:23:14.880
<v Speaker 3>They're literally mapping the acceleration rate over cosmic time.

442
00:23:15.000 --> 00:23:18.200
<v Speaker 2>And if that acceleration rate was different, say five billion

443
00:23:18.240 --> 00:23:21.000
<v Speaker 2>years ago compared to ten billion years ago, or compared

444
00:23:21.000 --> 00:23:21.839
<v Speaker 2>to it today.

445
00:23:21.640 --> 00:23:24.799
<v Speaker 3>Then LAMB is not a constant. Game over for the

446
00:23:24.839 --> 00:23:27.599
<v Speaker 3>simplest model, that would be the smoking gun evidence that

447
00:23:27.680 --> 00:23:30.440
<v Speaker 3>we need new physics beyond standard LAMB to CDM to

448
00:23:30.519 --> 00:23:31.839
<v Speaker 3>explain dark energy.

449
00:23:32.039 --> 00:23:34.880
<v Speaker 2>Now, Statle does add a note of caution rate. He

450
00:23:35.000 --> 00:23:38.400
<v Speaker 2>suggests you could might not deliver the final definitive answer

451
00:23:38.440 --> 00:23:39.680
<v Speaker 2>on dark energy overnight.

452
00:23:40.200 --> 00:23:43.400
<v Speaker 3>Yeah, he manages expectations a bit. It's unlikely to be

453
00:23:43.440 --> 00:23:47.839
<v Speaker 3>a single Eureka moment from one data release. Understanding dark

454
00:23:47.960 --> 00:23:51.759
<v Speaker 3>energy is incredibly challenging, but he expresses strong confidence that

455
00:23:52.000 --> 00:23:54.440
<v Speaker 3>you could will bring us a step closer to understanding

456
00:23:54.440 --> 00:23:56.279
<v Speaker 3>the mysterious realm of dark energy.

457
00:23:56.480 --> 00:24:00.720
<v Speaker 2>It's about gathering that unprecedentedly precise day data and needed

458
00:24:00.759 --> 00:24:03.839
<v Speaker 2>to really start ruling out possibilities. Can we rule out

459
00:24:03.880 --> 00:24:06.960
<v Speaker 2>the simple constant. If so, what kind of dynamic behavior

460
00:24:07.039 --> 00:24:08.960
<v Speaker 2>does the data favor exactly?

461
00:24:09.279 --> 00:24:12.119
<v Speaker 3>And again, having flagship two, which was built assuming lambda

462
00:24:12.200 --> 00:24:15.839
<v Speaker 3>as a constant, provides that perfect reference point. Any deviation

463
00:24:15.960 --> 00:24:18.599
<v Speaker 3>UCLI finds in the actual expansion history will stand out

464
00:24:18.640 --> 00:24:21.880
<v Speaker 3>starkly when compared to the simulation's prediction. It sharpens the search.

465
00:24:22.119 --> 00:24:26.240
<v Speaker 2>So to achieve these really ambitious goals testing the constancy

466
00:24:26.240 --> 00:24:30.359
<v Speaker 2>of dark energy, mapping dark matter, looking for cracks in

467
00:24:30.400 --> 00:24:35.319
<v Speaker 2>the standard model, EUCLID relies on some pretty sophisticated observational techniques.

468
00:24:35.480 --> 00:24:37.440
<v Speaker 2>We should probably touch on those. It's not just taking

469
00:24:37.480 --> 00:24:38.759
<v Speaker 2>pretty pictures.

470
00:24:38.319 --> 00:24:43.160
<v Speaker 3>Definitely not. It's about precision and scale combined. It really

471
00:24:43.240 --> 00:24:46.359
<v Speaker 3>is the most comprehensive survey ever attempted in terms of

472
00:24:46.400 --> 00:24:49.839
<v Speaker 3>both the volume covered and the detail captured within that volume.

473
00:24:49.960 --> 00:24:53.119
<v Speaker 2>Okay, let's start with mapping the invisible stuff dark matter.

474
00:24:53.680 --> 00:24:57.640
<v Speaker 2>You mentioned gravitational lensing earlier. How does EUCLID actually use that?

475
00:24:57.920 --> 00:25:01.880
<v Speaker 3>Right? So, EUCLID has incredibly high spatial resolution, meaning it

476
00:25:01.880 --> 00:25:05.359
<v Speaker 3>can take really sharp images. This allows its researchers to

477
00:25:05.359 --> 00:25:09.200
<v Speaker 3>detect very subtle distortions in the shapes of literally billions

478
00:25:09.200 --> 00:25:10.599
<v Speaker 3>of distant background galaxies.

479
00:25:10.680 --> 00:25:13.240
<v Speaker 2>These aren't the dramatic arcs and multiple images you see

480
00:25:13.279 --> 00:25:15.519
<v Speaker 2>from strong lensing around massive galaxy cluster.

481
00:25:15.680 --> 00:25:19.039
<v Speaker 3>No, this is weak lensing. The effect is tiny, just

482
00:25:19.079 --> 00:25:22.599
<v Speaker 3>a slight statistical preference for galaxies behind a massive structure

483
00:25:22.880 --> 00:25:26.319
<v Speaker 3>to appear slightly stretched or sheared in a particular direction.

484
00:25:26.240 --> 00:25:28.680
<v Speaker 2>Like looking through a very subtly warped window pane.

485
00:25:28.680 --> 00:25:32.559
<v Speaker 3>As you say, exactly, and the warping the distortion is

486
00:25:32.599 --> 00:25:35.480
<v Speaker 3>caused by the gravitational pull of all the mass lying

487
00:25:35.519 --> 00:25:39.039
<v Speaker 3>between us and those background galaxies, primarily the invisible clumps

488
00:25:39.039 --> 00:25:41.599
<v Speaker 3>and filaments of dark matter that make up the cosmic web.

489
00:25:41.799 --> 00:25:46.359
<v Speaker 2>So by measuring these tiny systematic distortions across billions of

490
00:25:46.440 --> 00:25:48.480
<v Speaker 2>galaxies spread over the sky.

491
00:25:48.640 --> 00:25:51.400
<v Speaker 3>Scientists can essentially reverse engineer a map of where the

492
00:25:51.440 --> 00:25:54.200
<v Speaker 3>intervening mass must be. They can figure out the distribution

493
00:25:54.240 --> 00:25:55.960
<v Speaker 3>of the stuff doing the bending, even.

494
00:25:55.839 --> 00:25:57.599
<v Speaker 2>Though they can't see the dark matter directly.

495
00:25:57.720 --> 00:26:01.680
<v Speaker 3>Correct The result is a massive three dimensional map of

496
00:26:01.759 --> 00:26:05.440
<v Speaker 3>the dark matter distribution across a huge portion of the universe.

497
00:26:06.079 --> 00:26:09.279
<v Speaker 3>This map is crucial for testing the predictions of Flagship two,

498
00:26:09.799 --> 00:26:13.759
<v Speaker 3>which remember simulated precisely how dark matters should be distributed

499
00:26:13.920 --> 00:26:15.960
<v Speaker 3>according to lambda CDM physics.

500
00:26:16.119 --> 00:26:18.480
<v Speaker 2>Okay, so weak lensing gives you the map of the

501
00:26:18.519 --> 00:26:21.240
<v Speaker 2>mass distribution, but you need to know where things are

502
00:26:21.240 --> 00:26:24.279
<v Speaker 2>in three D space, especially their distances, to make sense

503
00:26:24.279 --> 00:26:27.960
<v Speaker 2>of cosmic evolution and expansion history. How does EUCLID get

504
00:26:27.960 --> 00:26:28.599
<v Speaker 2>the distances.

505
00:26:28.960 --> 00:26:33.480
<v Speaker 3>That's where the complementary technique comes in spectroscopy. EUCLID has

506
00:26:33.519 --> 00:26:37.920
<v Speaker 3>an instrument called NISP near ineferred spectrometer and photometer that

507
00:26:37.960 --> 00:26:41.440
<v Speaker 3>can measure the spectrum of light from millions upon millions.

508
00:26:41.079 --> 00:26:44.079
<v Speaker 2>Of galaxies, breaking the light down into its constituent colors

509
00:26:44.160 --> 00:26:45.160
<v Speaker 2>like a prism does.

510
00:26:45.160 --> 00:26:49.200
<v Speaker 3>Exactly, and by doing that, scientists can measure the galaxy's

511
00:26:49.240 --> 00:26:53.880
<v Speaker 3>redshift with very high accuracy. They look for characteristic features

512
00:26:53.880 --> 00:26:57.519
<v Speaker 3>in the spectrum absorption or emission lines from specific chemical

513
00:26:57.519 --> 00:27:01.400
<v Speaker 3>elements and see how much they've been shifted towards words, longer,

514
00:27:01.519 --> 00:27:03.759
<v Speaker 3>redder wavelengths due to cosmic expansion.

515
00:27:04.160 --> 00:27:07.160
<v Speaker 2>And as we establish, redshift is the key indicator of

516
00:27:07.240 --> 00:27:11.559
<v Speaker 2>distance in an expanding universe. More redshift means farther away

517
00:27:11.799 --> 00:27:12.759
<v Speaker 2>and further back in.

518
00:27:12.759 --> 00:27:16.720
<v Speaker 3>Time, precisely so, by getting these accurate spectroscopic redshifts for

519
00:27:16.759 --> 00:27:20.599
<v Speaker 3>a huge number of galaxies euclib can pinpoint their distances

520
00:27:20.640 --> 00:27:24.119
<v Speaker 3>with unprecedented accuracy. This is what allows them to slice

521
00:27:24.160 --> 00:27:26.759
<v Speaker 3>the universe up into those different timebins we talked about

522
00:27:26.960 --> 00:27:29.359
<v Speaker 3>to map the expansion rate over ten billion years.

523
00:27:29.480 --> 00:27:32.000
<v Speaker 2>So it's the combination the two techniques that's really powerful.

524
00:27:32.160 --> 00:27:34.599
<v Speaker 2>The sharp imaging gives you the galaxy shapes for weak

525
00:27:34.720 --> 00:27:37.279
<v Speaker 2>lensing mapping mass, and.

526
00:27:37.240 --> 00:27:40.559
<v Speaker 3>The sectrocity gives you the precise red shifts for distances

527
00:27:40.920 --> 00:27:43.279
<v Speaker 3>mapping expansion history and three D position.

528
00:27:43.480 --> 00:27:46.400
<v Speaker 2>That's the synergy. You put them together and you build

529
00:27:46.480 --> 00:27:49.880
<v Speaker 2>up this incredibly detailed three dimensional map of both the

530
00:27:49.960 --> 00:27:54.079
<v Speaker 2>visible galaxies and the invisible dark matter structures spanning this

531
00:27:54.400 --> 00:28:00.000
<v Speaker 2>enormous cosmic sphere with a radius of ten billion light years,

532
00:27:59.799 --> 00:28:02.839
<v Speaker 2>a survey of cosmic structure and evolution covering more than

533
00:28:02.880 --> 00:28:04.960
<v Speaker 2>two thirds of the universe's entire history.

534
00:28:05.400 --> 00:28:08.319
<v Speaker 3>Just staggering. And there's one more benefit of casting such

535
00:28:08.319 --> 00:28:11.559
<v Speaker 3>a wide net, isn't there The possibility of finding things

536
00:28:11.559 --> 00:28:12.519
<v Speaker 3>you aren't even looking for.

537
00:28:12.640 --> 00:28:12.880
<v Speaker 1>Ah.

538
00:28:13.039 --> 00:28:16.400
<v Speaker 2>Yes, the element of serendipity. Because euclid is surveying such

539
00:28:16.400 --> 00:28:19.960
<v Speaker 2>a truly vast volume of space, the chances of stumbling

540
00:28:20.039 --> 00:28:23.519
<v Speaker 2>upon extremely rare or unexpected objects or phenomena are actually

541
00:28:23.559 --> 00:28:24.160
<v Speaker 2>quite high.

542
00:28:24.400 --> 00:28:26.880
<v Speaker 3>A Domic mentions this right, that some things are just

543
00:28:27.319 --> 00:28:32.839
<v Speaker 3>intrinsically extremely uncommon. Maybe a specific type of superluminous supernova,

544
00:28:32.960 --> 00:28:35.319
<v Speaker 3>or a weird kind of quasar, or a particular stage

545
00:28:35.319 --> 00:28:38.319
<v Speaker 3>of galaxy merging that only happens fleetingly.

546
00:28:37.960 --> 00:28:40.559
<v Speaker 2>Exactly in any small patch of sky. You might never

547
00:28:40.599 --> 00:28:43.599
<v Speaker 2>see one. But when your survey volume encompasses billions of

548
00:28:43.680 --> 00:28:46.079
<v Speaker 2>light years, you're bound to catch some of these rare

549
00:28:46.119 --> 00:28:48.359
<v Speaker 2>events just by sheer statistical luck.

550
00:28:48.640 --> 00:28:52.480
<v Speaker 3>That's the idea. Adamic says. The chances of finding unexpected

551
00:28:52.599 --> 00:28:56.640
<v Speaker 3>or rare objects are high. This is pure discovery space.

552
00:28:57.160 --> 00:29:00.519
<v Speaker 3>You might find objects or phenomena that challenge existing theories

553
00:29:00.720 --> 00:29:04.279
<v Speaker 3>in ways nobody even anticipated, simply because nobody had looked

554
00:29:04.279 --> 00:29:07.480
<v Speaker 3>wide enough and deep enough before. Hashtag tag tag outro

555
00:29:08.200 --> 00:29:10.680
<v Speaker 3>so to kind of wrap this all up. This incredible

556
00:29:10.720 --> 00:29:15.240
<v Speaker 3>Flagship two simulation, this universe built inside PiZZ dain. It's

557
00:29:15.240 --> 00:29:19.319
<v Speaker 3>playing these three really critical intertwined roles right now at

558
00:29:19.319 --> 00:29:20.799
<v Speaker 3>this pivotal moment in astronomy.

559
00:29:20.799 --> 00:29:22.079
<v Speaker 2>Okay, let's recap them first.

560
00:29:22.240 --> 00:29:25.880
<v Speaker 3>First, it's the essential data preparation engine. It allowed scientists

561
00:29:25.920 --> 00:29:28.799
<v Speaker 3>to develop and test the automated software pipelines needed to

562
00:29:28.839 --> 00:29:32.799
<v Speaker 3>actually handle euclid's massive data volume. Without it, they'd be drowning.

563
00:29:32.920 --> 00:29:33.839
<v Speaker 2>Got it. Second.

564
00:29:34.079 --> 00:29:36.880
<v Speaker 3>Second, it's the highest precision test bed ever created for

565
00:29:36.920 --> 00:29:39.839
<v Speaker 3>the standard LANDB to CDM model of cosmology. It's the

566
00:29:39.880 --> 00:29:42.839
<v Speaker 3>perfect theoretical prediction against which the real universe will be.

567
00:29:42.839 --> 00:29:44.400
<v Speaker 2>Measured looking for those cracks.

568
00:29:44.480 --> 00:29:48.359
<v Speaker 3>And third and third, building on that, it serves as

569
00:29:48.359 --> 00:29:52.160
<v Speaker 3>the indispensable guide for interpreting the complex cosmic history that

570
00:29:52.240 --> 00:29:55.720
<v Speaker 3>EUCLID is now observing. By comparing the real data to

571
00:29:55.759 --> 00:29:59.359
<v Speaker 3>the simulation, scientists can better understand the growth of structure,

572
00:29:59.559 --> 00:30:03.079
<v Speaker 3>thetion of galaxies, and the nature of dark energy over time.

573
00:30:03.400 --> 00:30:06.000
<v Speaker 2>And this isn't just theoretical anymore. Things are happening. You

574
00:30:06.079 --> 00:30:08.680
<v Speaker 2>mentioned the first data release, the quick data release that

575
00:30:08.680 --> 00:30:10.400
<v Speaker 2>came out in March twenty twenty five.

576
00:30:10.559 --> 00:30:13.160
<v Speaker 3>That's right. Even that was just a small taste relatively

577
00:30:13.200 --> 00:30:16.920
<v Speaker 3>speaking of a full survey, but it already provided new insights,

578
00:30:16.960 --> 00:30:20.279
<v Speaker 3>particularly into galaxy clusters and the structure of the nearby

579
00:30:20.319 --> 00:30:23.799
<v Speaker 3>cosmic web, and papers based on that and related simulation

580
00:30:23.920 --> 00:30:27.799
<v Speaker 3>work are already being published in journals like Astronomy and Astrophysics.

581
00:30:27.920 --> 00:30:29.799
<v Speaker 2>And there's a plan for more data coming soon.

582
00:30:30.039 --> 00:30:33.079
<v Speaker 3>Yes, the next major planned data release, which will be

583
00:30:33.160 --> 00:30:37.200
<v Speaker 3>significantly larger, is expected sometime in spring twenty twenty six.

584
00:30:37.400 --> 00:30:38.880
<v Speaker 3>So the pace is really picking up.

585
00:30:39.160 --> 00:30:42.440
<v Speaker 2>It's a rapid unfolding of discovery where every step relies

586
00:30:42.480 --> 00:30:45.920
<v Speaker 2>heavily on that groundwork laid by the simulation. Those processing

587
00:30:45.960 --> 00:30:49.240
<v Speaker 2>pipelines tested on Flagship two, they're running now on the

588
00:30:49.240 --> 00:30:49.960
<v Speaker 2>real data.

589
00:30:50.039 --> 00:30:52.079
<v Speaker 3>Absolutely, the preparation is paying off.

590
00:30:52.279 --> 00:30:54.240
<v Speaker 2>What really stands out to me thinking about the whole

591
00:30:54.240 --> 00:31:00.240
<v Speaker 2>project is the almost philosophical intent behind Flagship two. Here

592
00:31:00.240 --> 00:31:03.960
<v Speaker 2>we have the most sophisticated, detailed digital model of reality

593
00:31:03.960 --> 00:31:08.160
<v Speaker 2>ever created, built explicitly not just to confirm what we

594
00:31:08.200 --> 00:31:10.960
<v Speaker 2>think we know, but specifically to find the errors in

595
00:31:11.000 --> 00:31:14.559
<v Speaker 2>our understanding. It's like building a perfect machine designed to

596
00:31:14.720 --> 00:31:18.000
<v Speaker 2>highlight its own potential flaws when compared to the real thing.

597
00:31:18.240 --> 00:31:20.279
<v Speaker 3>That's a great way to put it. It's a theoretical

598
00:31:20.319 --> 00:31:23.480
<v Speaker 3>construct designed in a sense to be proven wrong or

599
00:31:23.480 --> 00:31:26.759
<v Speaker 3>at least incomplete, in the most informative way possible.

600
00:31:26.519 --> 00:31:30.319
<v Speaker 2>And that sets up this fascinating tension that you listening

601
00:31:30.319 --> 00:31:33.279
<v Speaker 2>should really keep in mind. As the euclid results continue

602
00:31:33.319 --> 00:31:35.680
<v Speaker 2>to roll in over the next few years exactly.

603
00:31:35.880 --> 00:31:39.759
<v Speaker 3>You've got this perfect, pristine, synthetic universe inside Flagship two,

604
00:31:39.880 --> 00:31:43.160
<v Speaker 3>totally controlled high resolution built strictly on the rules of

605
00:31:43.240 --> 00:31:45.880
<v Speaker 3>LAMB to CDM physics. And then you have the messy,

606
00:31:45.920 --> 00:31:49.680
<v Speaker 3>noisy complex real data arriving from the EUCLID telescope, full

607
00:31:49.720 --> 00:31:54.519
<v Speaker 3>of unexpected glitches, statistical fluctuations, and potentially truly baffling outliers.

608
00:31:54.920 --> 00:31:58.839
<v Speaker 2>So the big question becomes if the broad strokes match.

609
00:31:59.240 --> 00:32:02.359
<v Speaker 2>If the for all map of the cosmos looks roughly

610
00:32:02.400 --> 00:32:05.839
<v Speaker 2>like the simulation predicts, but there are these nagging discrepancies,

611
00:32:06.279 --> 00:32:09.680
<v Speaker 2>maybe dark matter clumps slightly differently in nearby voice and expected,

612
00:32:09.839 --> 00:32:12.960
<v Speaker 2>or maybe a few of those super rare unpredicted objects

613
00:32:13.079 --> 00:32:15.799
<v Speaker 2>keep popping up. Which do you trust more?

614
00:32:16.079 --> 00:32:20.359
<v Speaker 3>Do you emphasize the broad confirmation that seems to reinforce

615
00:32:20.519 --> 00:32:24.079
<v Speaker 3>decades of established physics, or do you focus on those

616
00:32:24.119 --> 00:32:27.319
<v Speaker 3>unexpected outliers, the cracks, the things that don't fit the

617
00:32:27.359 --> 00:32:29.279
<v Speaker 3>model and seem to demand entirely new.

618
00:32:29.160 --> 00:32:33.240
<v Speaker 2>Theories that tension right there between the expected pattern and

619
00:32:33.279 --> 00:32:36.640
<v Speaker 2>the surprising detail. That's where the future of cosmology is

620
00:32:36.640 --> 00:32:39.079
<v Speaker 2>being forged. That's where the discoveries will likely lie.

621
00:32:39.160 --> 00:32:41.400
<v Speaker 3>Absolutely it's an exciting time to be watching. Thanks for

622
00:32:41.440 --> 00:32:42.559
<v Speaker 3>joining us for this exploration.

623
00:32:42.640 --> 00:32:43.559
<v Speaker 2>We'll see you next time.

624
00:33:01.000 --> 00:33:03.000
<v Speaker 3>The school

625
00:33:05.559 --> 00:33:21.559
<v Speaker 2>Last
