WEBVTT - Do we know where dark matter is?

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<v Speaker 1>Hey, or hey, I think I may have lost something.

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<v Speaker 1>Oh did you lose your mind again? I happened a

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<v Speaker 1>long time ago. This is something new? Is it important?

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<v Speaker 1>It's actually kind of a big deal. Is it like

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<v Speaker 1>really small and easy to lose, like your keys or

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<v Speaker 1>your wedding band. No, it's much more embarrassing because it's

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<v Speaker 1>really enormous, like cosmically large, like most of the stuff

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<v Speaker 1>in the universe, and you can't find it. I've been

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<v Speaker 1>looking everywhere for it. Well, I guess you know what

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<v Speaker 1>to do. Oh yeah, what's that? You know? Give it

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<v Speaker 1>a cool sounding name, and then ask the federal government

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<v Speaker 1>to help you find it. Do you think anybody would

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<v Speaker 1>actually fall for that? I think they already have. Hi

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<v Speaker 1>am jorhammy cartoonists and the creator of PhD comics. Hi.

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<v Speaker 1>I'm Daniel. I'm a particle physicist and a professor you

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<v Speaker 1>see Irvine, and I am actually paid to hunt for

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<v Speaker 1>missing things. M interesting, You're like the Lost and Found

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<v Speaker 1>of the universe department. That sounds very unglamorous. I like

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<v Speaker 1>to think of myself more of the Sherlock Holmes of

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<v Speaker 1>the universe. I see you're not in like in the

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<v Speaker 1>basement office with a little window that people go there

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<v Speaker 1>and claim lost things. That's right. I'm not sitting here

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<v Speaker 1>surrounded by people's lost purses or socks. Where do all

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<v Speaker 1>the socks and the dryers go? That's what I want

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<v Speaker 1>to know. We should have a whole episode about that.

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<v Speaker 1>They're orbiting the Earth in the hose zone layer. Well,

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<v Speaker 1>that socks made. They're all connected by wormholes. You think dryers, Well,

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<v Speaker 1>that's spinning and that he could that create a warmhole.

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<v Speaker 1>Keep running your dryer let us know. But welcome to

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<v Speaker 1>our podcast Daniel and Jorge Explain the Universe, a production

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<v Speaker 1>of I Heart Radio, which we operated as a sort

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<v Speaker 1>of lost and found of ideas about the universe. Everything

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<v Speaker 1>we have found about the universe and all the ideas

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<v Speaker 1>we have lost. Everything we do know about what's going

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<v Speaker 1>on out there, the size of the universe, the number

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<v Speaker 1>of dimensions of space, whether or not they're alien creators

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<v Speaker 1>on other planets looking through their telescopes at us. Every

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<v Speaker 1>deep and enormous question about the universe you might consider

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<v Speaker 1>we talk about here on the podcast. Yeah, because it

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<v Speaker 1>is a huge universe full of amazing and wonderful things

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<v Speaker 1>that seem to be screaming at us for us to

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<v Speaker 1>find them. We get light from distant stars all the

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<v Speaker 1>time at all times, radiation, cosmic rays, and it's all

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<v Speaker 1>coming to us sort of one thing for us to

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<v Speaker 1>find out and what's out there and to discover and

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<v Speaker 1>learn about how it all works. You make the universe

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<v Speaker 1>sounds sort of cooperative, like it wants to play a

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<v Speaker 1>role in our science and be helpful. Universe, right, I mean,

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<v Speaker 1>it's constantly shouting at us, isn't it. It is? But

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<v Speaker 1>sometimes these clues are very, very subtle and frustratingly difficult

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<v Speaker 1>to grasp. I feel like the universe is sort of

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<v Speaker 1>playing cat and mouse with us, sometimes hiding all the

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<v Speaker 1>best bits. It's like coy universe, mean, like it wants

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<v Speaker 1>us to find it, but it's not telling us everything

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<v Speaker 1>that it can about itself. Yeah, it doesn't just come

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<v Speaker 1>right out and tell us it's deep nature. It sometimes

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<v Speaker 1>seems to make sense, and then you dig deeper and

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<v Speaker 1>discover oh my gosh, it's bonkers underneath. But there is

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<v Speaker 1>a lot of fascinating information in those little hints that

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<v Speaker 1>do arrive here on Earth. Yeah, and it's pretty amazing that,

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<v Speaker 1>you know, if you think about it, that we're sitting

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<v Speaker 1>on this little rock floating through space in a corner

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<v Speaker 1>of the galaxy, in a little corner of the universe.

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<v Speaker 1>And somehow, from this light that we're getting from distant stars,

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<v Speaker 1>we can somehow piece together the whole structure almost of

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<v Speaker 1>the universe. I like how you just say somehow, you know,

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<v Speaker 1>It's like the information comes and dot dot dot, we

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<v Speaker 1>know these things. You just like, somehow my entire career

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<v Speaker 1>right there. Yeah, somehow it goes to the lost and

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<v Speaker 1>found department in the basement and we get a little

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<v Speaker 1>memo about what happened. That's right. Somehow, because the government

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<v Speaker 1>decides to fund basic science research, we have uncovered some

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<v Speaker 1>truths about the universe. I guess what I mean by

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<v Speaker 1>somehow thought dot dot is you know, mostly engineering and

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<v Speaker 1>then some science, some happy collaboration between scientists and engineers.

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<v Speaker 1>But yeah, we are learning more and more about the universe.

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<v Speaker 1>And there's a big question, especially a big question about

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<v Speaker 1>the universe, about what it's made out of and how

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<v Speaker 1>it's what structured it has out there in the galaxies

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<v Speaker 1>and also in between galaxies. What does it all look like,

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<v Speaker 1>how's it all put together? It's really one of the

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<v Speaker 1>biggest questions in the universe, and one of the first

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<v Speaker 1>questions you might ask, which is what is in the universe?

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<v Speaker 1>What's the universe made out of? Where is all the

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<v Speaker 1>stuff out there? And what kind of stuff is it? Really,

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<v Speaker 1>it's sort of shocking and amazing that we don't know

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<v Speaker 1>the answer to that very basic question about the nature

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<v Speaker 1>of our own reality. Yeah, because the universe sort of

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<v Speaker 1>pulled a fast one on us, right Like it did

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<v Speaker 1>this big reveal twist somewhere a few decades ago where

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<v Speaker 1>we thought we knew what the universe was made out of.

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<v Speaker 1>It was stars and matter and atoms and things like that,

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<v Speaker 1>But suddenly we learned that that was only like five

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<v Speaker 1>percent of it. You know. It's kind of like when

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<v Speaker 1>you're watching a show and Sony you realize that you

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<v Speaker 1>still have like ninety five episodes ago. It's sort of

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<v Speaker 1>like the universe was wearing a mask and then somebody

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<v Speaker 1>pulled it off and we discovered, oh my gosh, there's

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<v Speaker 1>a lot more to it. So much for the universe

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<v Speaker 1>being helpful and revealing, right, well, I think it just

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<v Speaker 1>wants you to keep watching, I guess, trying to parse

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<v Speaker 1>out the information, trying to keep it interesting. Maybe the

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<v Speaker 1>show runners of the Universe are just trying to dole

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<v Speaker 1>out the reveals a little bit at a time. Show runners, Huh,

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<v Speaker 1>so you're a multitheist. I think it's got to be

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<v Speaker 1>a committee. I mean, who, there's so much to do.

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<v Speaker 1>That's not a flattering I guess description of it looks

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<v Speaker 1>like it was made by a committee. The universe looks

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<v Speaker 1>like it had too many writers. Well, it does sometimes

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<v Speaker 1>seem inconsistent, you know. Well, it is sort of a

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<v Speaker 1>mysterious question. What is the universe made out of? And

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<v Speaker 1>as we've learned in the last few decades, it's not

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<v Speaker 1>made out of just stars and atoms and elements. It's

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<v Speaker 1>mostly made out of other things, namely dark matter and

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<v Speaker 1>dark energy. The kind of stuff that makes up you

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<v Speaker 1>and me and hamsters and ice cream and bologna sandwiches

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<v Speaker 1>is actually quite unusual in the universe. Most of the

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<v Speaker 1>stuff that's out there is not stars and gas and

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<v Speaker 1>dust and all the visible stuff. It's something else, something dark,

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<v Speaker 1>something we've only recently discovered exists out there. Yeah, and

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<v Speaker 1>so dark energy is this sort of the phenomenon where

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<v Speaker 1>the universe's expanding faster and faster every second, but dark

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<v Speaker 1>matter is especially sort of weird and concerning because it's matter,

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<v Speaker 1>it's stuff. It's like exerting gravity. You can feel it,

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<v Speaker 1>but we can't see it, which means we don't know

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<v Speaker 1>where it is exactly. We know that dark matter is

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<v Speaker 1>some kind of stuff. There's something out there exerting gravity

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<v Speaker 1>on the rest of the universe, and we can sort

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<v Speaker 1>of tell that it exists, but we don't know what

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<v Speaker 1>it is. And we've done a lot of podcasts digging

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<v Speaker 1>into what it might be. Is it axons? Is it

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<v Speaker 1>black holes? Is it whimps? Is this something else? Something

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<v Speaker 1>weird in there? Even more crazy ideas we haven't yet covered.

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<v Speaker 1>It's sort of like we know there's an elephant in

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<v Speaker 1>the room or in the in the galaxy or the universe,

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<v Speaker 1>but we don't know what it's. What this elephant is doing,

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<v Speaker 1>or you know, what is it like striking a post?

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<v Speaker 1>Is it jogging? Is it sleeping. It's kind of a

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<v Speaker 1>big mystery, like we know it's there, but we sort

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<v Speaker 1>of don't know what it's doing or what structure it has. Yeah,

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<v Speaker 1>you can ask so many fascinating questions. So far, we've

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<v Speaker 1>mostly focused on what is dark matter? Is it this

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<v Speaker 1>kind of particle. Is it that kind of particle but

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<v Speaker 1>equally interesting without even knowing what it's made out of,

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<v Speaker 1>is just wondering, like where is the dark matter? Is

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<v Speaker 1>it here with us in this room? Is it out

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<v Speaker 1>there in deep space? Does it form planets and other

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<v Speaker 1>kinds of structure? Is it smoothly spread out throughout the universe?

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<v Speaker 1>Where in the universe is all of this stuff? So

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<v Speaker 1>today on the podcast, we'll be asking the question, how

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<v Speaker 1>do we know where dark matter is? It sounds like

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<v Speaker 1>he lost you lost it again? Then I feel like

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<v Speaker 1>we said a new word. It was, but now we

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<v Speaker 1>don't know where it is. It is a really important

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<v Speaker 1>question because knowing where the dark matter is can help

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<v Speaker 1>us get clues about what it might be, because certain

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<v Speaker 1>kinds of dark matter might clump up in different ways,

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<v Speaker 1>and other kinds of dark matter might not. Yeah, is

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<v Speaker 1>it is it chunky or smooth? I guess it's a

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<v Speaker 1>big question about the peanut butter dark matter of the universe. Well,

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<v Speaker 1>I hope the showrunners don't disagree about that, because then

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<v Speaker 1>you might get chunky parts of the universe and creamy

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<v Speaker 1>parts of the universe. You're not a creamy peanut butter fan.

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<v Speaker 1>It's all about the chunks, man, It's all about the chunks. Well,

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<v Speaker 1>to each their own may there's a different flavor of

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<v Speaker 1>dark matter for every tape. New Tella there you go,

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<v Speaker 1>New Tella is the best flavor of dark rutter and

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<v Speaker 1>everyone gets a heart attack from being surrounded by all

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<v Speaker 1>this saturated fat. But yeah, it's a big question. Where

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<v Speaker 1>is dark matter and sort of like what structure it

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<v Speaker 1>has in the universe. Is it sort of smoothed out

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<v Speaker 1>there like a big cloud or is it is it chunky?

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<v Speaker 1>Is it in like strands? Is it in clumps? What's

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<v Speaker 1>it doing out there? And this is something that scientists

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<v Speaker 1>are eager to figure out because they just want to

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<v Speaker 1>know where all of this stuff is. They're trying to

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<v Speaker 1>develop a picture of the universe both visible and invisible,

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<v Speaker 1>and of course the invisible stuff much harder to see,

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<v Speaker 1>but since there's much more of it than there is

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<v Speaker 1>the visible stuff, it's a very important question. So, as usual,

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<v Speaker 1>we were wondering how many people out there had thought

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<v Speaker 1>about this question of the location and structure of dark matter.

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<v Speaker 1>So Daniel went out there to ask people on the internet,

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<v Speaker 1>how do we know where dark matter is? So if

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<v Speaker 1>you'd like to put your brain in the test and

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<v Speaker 1>answer questions that leading physicists don't know the answer to,

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<v Speaker 1>please write to me two questions at Daniel and Jorge

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<v Speaker 1>dot com. Here's what people had to say. Well, doc

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<v Speaker 1>matter reacts with gravity, so by looking out into the universe, Um,

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<v Speaker 1>we can sort of detect where the doc matter is

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<v Speaker 1>because of its effect on gravity. I know that it's

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<v Speaker 1>by gravity. Is the gravitational lensing that makes it possible

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<v Speaker 1>to have like some kind of ideas where it could

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<v Speaker 1>be dark matter in the universe. The distortion of light

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<v Speaker 1>suggests that there are more matter out there that we

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<v Speaker 1>can actually say whenever it's like bands. Well, once again,

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<v Speaker 1>I assume this has to do with the pot with

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<v Speaker 1>the examples and instance, as you were talking of these

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<v Speaker 1>massive tubs of argone if I'm not mistaken, that are

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<v Speaker 1>deep underground. We cannot see what dark matter itself is.

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<v Speaker 1>Light travels straight through it, but we can see other

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<v Speaker 1>planets and we can see light being distorted by the

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<v Speaker 1>gravitational effects of what dark matter is itself. I'd say

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<v Speaker 1>we know where the dark matter is because we can

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<v Speaker 1>see the gravitational force it exerts on the visible matter

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<v Speaker 1>around it. Next to that, it also bends light from

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<v Speaker 1>distant galaxies when it comes towards us. So I'd say

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<v Speaker 1>gravity is the usual suspect for us knowing where dark

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<v Speaker 1>matter is. Who is d M? I think I've heard

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<v Speaker 1>that dark matter is everywhere, that it just kind of

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<v Speaker 1>permeates the universe, so all over the place. So my

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<v Speaker 1>guess is for what we know dark matter is, or

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<v Speaker 1>how we know it is, if it gives off gravitational

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<v Speaker 1>waves because it interacts with stuff through gravity, then we

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<v Speaker 1>would use something that detects gravitational waves to see either

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<v Speaker 1>how far away it is or where it is in

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<v Speaker 1>respect to something else. I think we know where dark

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<v Speaker 1>matter is by looking for localized gravitational effects like lensing

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<v Speaker 1>or relative velocities that aren't completely explained by matter we

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<v Speaker 1>can observe in other ways. Right, A pretty interesting answer

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<v Speaker 1>is a lot of people went with gravity, which is true, right, Like,

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<v Speaker 1>like that's how we initially discovered dark matter is through gravity. Yeah,

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<v Speaker 1>that's basically the only way we can sense dark matter,

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<v Speaker 1>and so gravity is basically the answered. Gravity is the

0:12:05.120 --> 0:12:07.880
<v Speaker 1>reason we know dark matter exists, and dark matter is

0:12:07.920 --> 0:12:13.360
<v Speaker 1>basically an explanation for otherwise unexplainable gravity. So yeah, gravity

0:12:13.440 --> 0:12:16.600
<v Speaker 1>is basically our portal into the dark universe. And I

0:12:16.640 --> 0:12:20.760
<v Speaker 1>like this person who said who is dark matter? It's

0:12:20.800 --> 0:12:23.920
<v Speaker 1>like who it this new phone? I think that's because

0:12:24.000 --> 0:12:26.520
<v Speaker 1>in the question I wrote d M instead of dark matter,

0:12:26.760 --> 0:12:31.040
<v Speaker 1>assuming that everybody would know what DM meant, right, who

0:12:31.120 --> 0:12:34.559
<v Speaker 1>doesn't know what DM is? I was sliding into some

0:12:34.640 --> 0:12:36.160
<v Speaker 1>of these d M s with that one. I guess

0:12:37.120 --> 0:12:40.959
<v Speaker 1>you're being a physicism using acronyms on people who had

0:12:40.960 --> 0:12:43.720
<v Speaker 1>no idea what those acronyms are. But yeah, a lot

0:12:43.760 --> 0:12:46.080
<v Speaker 1>of people seem to set and have a basic idea

0:12:46.120 --> 0:12:48.440
<v Speaker 1>that it's through gravity. But the picture is a little

0:12:48.480 --> 0:12:50.880
<v Speaker 1>bit more complicated than that, right, I mean, we sort

0:12:50.880 --> 0:12:54.120
<v Speaker 1>of know that it's there because of gravity, but sort

0:12:54.160 --> 0:12:56.719
<v Speaker 1>of finding out exactly where it is or whether it

0:12:56.840 --> 0:13:00.440
<v Speaker 1>clumps or strands or smooth, that's much harder because we

0:13:00.480 --> 0:13:02.840
<v Speaker 1>can't see it right exactly. We can't see it in

0:13:02.880 --> 0:13:05.000
<v Speaker 1>the way that we can see the other kinds of matter.

0:13:05.280 --> 0:13:08.080
<v Speaker 1>It doesn't give off light, it doesn't reflect light. Remember

0:13:08.080 --> 0:13:10.240
<v Speaker 1>that dark matter is a bit of a confusing name

0:13:10.600 --> 0:13:14.920
<v Speaker 1>because dark matter is not actually dark. It's transparent, it's invisible.

0:13:15.040 --> 0:13:17.360
<v Speaker 1>It's not like a cloud of dark matter between you

0:13:17.440 --> 0:13:20.680
<v Speaker 1>and another star would block your view of that star.

0:13:21.160 --> 0:13:23.080
<v Speaker 1>If that were tue would be much easier to see

0:13:23.160 --> 0:13:26.440
<v Speaker 1>dark batter than it is today. Instead, light passes right

0:13:26.480 --> 0:13:29.040
<v Speaker 1>through dark matter. So give us, maybe start us off

0:13:29.040 --> 0:13:32.040
<v Speaker 1>with a refresher of dark matter or d M as

0:13:32.080 --> 0:13:34.080
<v Speaker 1>the physicist call it. You know, what do we know

0:13:34.120 --> 0:13:36.520
<v Speaker 1>about it? Well, we know that dark matter is about

0:13:36.600 --> 0:13:40.280
<v Speaker 1>twenty five of the energy budget of the universe. That

0:13:40.360 --> 0:13:42.839
<v Speaker 1>means if you take like a cubic light year of space,

0:13:42.920 --> 0:13:46.560
<v Speaker 1>or any volume of space, then of the energy in

0:13:46.640 --> 0:13:50.000
<v Speaker 1>that space is devoted to the mass of dark matter,

0:13:50.240 --> 0:13:53.840
<v Speaker 1>whereas five percent of the energy budget of any chunk

0:13:53.880 --> 0:13:57.280
<v Speaker 1>of space on average, you know, averaging over big distances,

0:13:57.600 --> 0:14:00.400
<v Speaker 1>is devoted to making things like stars and gala seas

0:14:00.440 --> 0:14:02.600
<v Speaker 1>and dust and giraffes and all of that kind of

0:14:02.800 --> 0:14:05.400
<v Speaker 1>normal matter made out of atoms. And that means that

0:14:05.440 --> 0:14:08.480
<v Speaker 1>there's a huge amount of dark matter. That a galaxy,

0:14:08.520 --> 0:14:11.959
<v Speaker 1>for example, is mostly dark matter. That the universe, the

0:14:12.080 --> 0:14:15.040
<v Speaker 1>stuff in the universe, the matter, you know, the physical

0:14:15.080 --> 0:14:18.360
<v Speaker 1>form of the universe is mostly dark matter. So we've

0:14:18.400 --> 0:14:20.960
<v Speaker 1>been studying the universe for thousands of years looking up

0:14:20.960 --> 0:14:24.080
<v Speaker 1>at the sky wondering how things work, and only recently

0:14:24.120 --> 0:14:26.880
<v Speaker 1>have we discovered that we've been missing most of it.

0:14:27.080 --> 0:14:29.800
<v Speaker 1>So that's pretty exciting. And we know that dark matter

0:14:29.960 --> 0:14:32.640
<v Speaker 1>is not made out of atoms, not made out of

0:14:32.640 --> 0:14:34.600
<v Speaker 1>the kind of stuff that you and I are made

0:14:34.600 --> 0:14:36.960
<v Speaker 1>out of. If it were, then it would probably interact

0:14:37.040 --> 0:14:39.600
<v Speaker 1>with light. And we can also do some careful accounting

0:14:39.600 --> 0:14:41.920
<v Speaker 1>from the very beginning of the universe, where we know

0:14:42.040 --> 0:14:44.840
<v Speaker 1>something about how much material there was to make atoms,

0:14:45.040 --> 0:14:47.080
<v Speaker 1>we can kind of account for where all of that went.

0:14:47.280 --> 0:14:49.920
<v Speaker 1>So we're pretty sure. We're almost certain that dark matter

0:14:49.960 --> 0:14:52.600
<v Speaker 1>is some kind of matter that doesn't give off light

0:14:52.680 --> 0:14:55.480
<v Speaker 1>or reflect light. It must be made out of something else.

0:14:55.720 --> 0:14:57.800
<v Speaker 1>And we know that it doesn't move very fast. We

0:14:57.880 --> 0:15:00.480
<v Speaker 1>call it cold dark matter, the as if it did,

0:15:00.520 --> 0:15:03.600
<v Speaker 1>it would spread out much more throughout the universe. Yeah,

0:15:03.600 --> 0:15:05.720
<v Speaker 1>and it's kind of interesting because I think I almost

0:15:05.720 --> 0:15:08.320
<v Speaker 1>feel like like, in a way, physicists called this thing

0:15:08.560 --> 0:15:10.760
<v Speaker 1>or named it a little bit too early, you know

0:15:10.840 --> 0:15:12.360
<v Speaker 1>what I mean, Like we gave it a name like

0:15:12.400 --> 0:15:14.400
<v Speaker 1>a dark matter, maybe a little too early, Like maybe

0:15:14.400 --> 0:15:16.280
<v Speaker 1>you should have kept going and say that you know

0:15:17.120 --> 0:15:20.040
<v Speaker 1>of the universe is just something that we don't understand

0:15:20.200 --> 0:15:22.560
<v Speaker 1>or something that is not like the rest of the

0:15:22.640 --> 0:15:25.000
<v Speaker 1>stuff in the universe. Well, that doesn't work as well

0:15:25.000 --> 0:15:28.800
<v Speaker 1>in grand proposals as a nice zingy phrase like dark matter.

0:15:31.280 --> 0:15:33.880
<v Speaker 1>But yeah, but I know what, I guess the point

0:15:33.920 --> 0:15:35.640
<v Speaker 1>is it really we don't know that much about it.

0:15:35.680 --> 0:15:37.680
<v Speaker 1>I mean, we sort of know it's presence, or at

0:15:37.760 --> 0:15:39.480
<v Speaker 1>least we know it's the effect on the rest of

0:15:39.480 --> 0:15:41.720
<v Speaker 1>the universe, but we don't even know if it's matter. Right, Well,

0:15:41.760 --> 0:15:44.720
<v Speaker 1>we know that it generates gravity, which suggests that it's

0:15:44.800 --> 0:15:49.320
<v Speaker 1>curves space according to general relativity. And so either our

0:15:49.440 --> 0:15:53.320
<v Speaker 1>understanding of how space curves is wrong, or it's some

0:15:53.440 --> 0:15:56.520
<v Speaker 1>new kind of energy and matter that does curve space.

0:15:57.000 --> 0:16:00.600
<v Speaker 1>And it's possible that we don't understand gravity. It's certain

0:16:00.800 --> 0:16:03.840
<v Speaker 1>that we don't have complete understanding of gravity. There are

0:16:03.960 --> 0:16:08.480
<v Speaker 1>alternative ideas to explain dark matter using variations on gravitational theory,

0:16:08.600 --> 0:16:11.520
<v Speaker 1>but none of them can really explain everything that we see.

0:16:12.000 --> 0:16:15.160
<v Speaker 1>And so you're right that we're not certain that it's matter.

0:16:15.360 --> 0:16:18.200
<v Speaker 1>But it's the simplest explanation that fits all of the data.

0:16:18.360 --> 0:16:21.800
<v Speaker 1>A new kind of particle that only interacts gravitationally, explains

0:16:21.880 --> 0:16:24.840
<v Speaker 1>basically everything that we see out there in the universe,

0:16:25.120 --> 0:16:28.280
<v Speaker 1>from the ripples in the earliest light to the structure

0:16:28.280 --> 0:16:31.480
<v Speaker 1>of the universe today to the rotations of galaxies. So

0:16:31.520 --> 0:16:34.800
<v Speaker 1>we're not certain, but it's the best candidate. Maybe should

0:16:34.840 --> 0:16:38.760
<v Speaker 1>have called it dark probably matter or dark most likely

0:16:38.760 --> 0:16:42.760
<v Speaker 1>matter d M M L D d M l M.

0:16:43.160 --> 0:16:45.160
<v Speaker 1>But we, as you said, so far, we only know

0:16:45.200 --> 0:16:48.080
<v Speaker 1>about it because of its gravitational effects, right, But we

0:16:48.120 --> 0:16:50.640
<v Speaker 1>sort of know quite a few things about sort of

0:16:50.840 --> 0:16:53.160
<v Speaker 1>generally where it is. We do have a good idea

0:16:53.320 --> 0:16:57.280
<v Speaker 1>of where it might be because of its gravitational effects. Right,

0:16:57.360 --> 0:17:00.440
<v Speaker 1>it is invisible. It doesn't give off light or interact

0:17:00.480 --> 0:17:03.280
<v Speaker 1>with any other kind of force. But gravity is local. Right,

0:17:03.320 --> 0:17:05.920
<v Speaker 1>if you are close to something, it tugs on you

0:17:06.119 --> 0:17:08.720
<v Speaker 1>more strongly than if you're far from something. So if

0:17:08.760 --> 0:17:10.840
<v Speaker 1>you're measuring the gravity of an object, if you can

0:17:10.920 --> 0:17:13.640
<v Speaker 1>only tell if something is there because of its gravity,

0:17:13.920 --> 0:17:16.240
<v Speaker 1>you can get an idea for where it is based

0:17:16.240 --> 0:17:18.880
<v Speaker 1>on what it tugs on. For example, we can see

0:17:18.880 --> 0:17:21.080
<v Speaker 1>the black holes are there because of the way the

0:17:21.119 --> 0:17:25.600
<v Speaker 1>stars move around them without actually directly seeing black holes,

0:17:25.800 --> 0:17:28.320
<v Speaker 1>and so gravity definitely can give you a picture as

0:17:28.320 --> 0:17:30.840
<v Speaker 1>to where things are in the universe, and we have

0:17:30.880 --> 0:17:33.480
<v Speaker 1>a rough idea for where dark matter is. We think

0:17:33.520 --> 0:17:37.280
<v Speaker 1>that dark matter is mostly lined up with the normal matter.

0:17:37.440 --> 0:17:40.000
<v Speaker 1>That where you see a galaxy is where there's a

0:17:40.080 --> 0:17:43.520
<v Speaker 1>huge clump of dark matter. So every galaxy, we think,

0:17:43.560 --> 0:17:46.600
<v Speaker 1>for example, is embedded in a huge cloud. We call

0:17:46.640 --> 0:17:50.400
<v Speaker 1>it a dark matter halo for every galaxy. Yeah, it's

0:17:50.400 --> 0:17:53.880
<v Speaker 1>like where you see regular stars and planets, you see

0:17:54.000 --> 0:17:56.840
<v Speaker 1>dark matter. Or it's almost like the opposite, right, it's

0:17:56.880 --> 0:17:59.119
<v Speaker 1>like where you see dark matter is where all the

0:17:59.160 --> 0:18:01.880
<v Speaker 1>stars and planets formed. In a way, yes, stars are

0:18:01.880 --> 0:18:04.479
<v Speaker 1>more like the tracers for the rest of stuff, right,

0:18:04.560 --> 0:18:07.200
<v Speaker 1>dark matter leads the way. There's more dark matter than

0:18:07.240 --> 0:18:10.160
<v Speaker 1>everything else. And so it's actually like where the dark

0:18:10.200 --> 0:18:13.920
<v Speaker 1>matter started clumping is where the normal matter fell into

0:18:14.000 --> 0:18:17.320
<v Speaker 1>it because of its gravity and then formed galaxies and

0:18:17.440 --> 0:18:19.840
<v Speaker 1>stars and all kinds of stuff that we can see.

0:18:20.040 --> 0:18:22.320
<v Speaker 1>So you know how when the military is fighting at night,

0:18:22.359 --> 0:18:24.280
<v Speaker 1>they shoot bullets and then occasionally, like one out of

0:18:24.320 --> 0:18:27.320
<v Speaker 1>every thousand bullets is a tracer. It's like glows, so

0:18:27.359 --> 0:18:29.840
<v Speaker 1>they can see where they're shooting. Stars are sort of

0:18:29.880 --> 0:18:32.000
<v Speaker 1>like that. They follow the dark matter, and they give

0:18:32.040 --> 0:18:34.960
<v Speaker 1>us a clue as to where that dark matter is.

0:18:35.520 --> 0:18:38.640
<v Speaker 1>And that's why we think that most galaxies are embedded

0:18:38.640 --> 0:18:42.639
<v Speaker 1>in this cloud, this halo of sort of spherical, sort

0:18:42.680 --> 0:18:46.040
<v Speaker 1>of a little bit elliptical dark matter that goes well

0:18:46.119 --> 0:18:49.080
<v Speaker 1>beyond actually where the stars are. Yeah, I've heard this

0:18:49.240 --> 0:18:52.359
<v Speaker 1>sort of analogy that regular matter like planets and stars.

0:18:52.400 --> 0:18:54.760
<v Speaker 1>It's sort of like the sprinkling on the icing of

0:18:54.800 --> 0:18:57.720
<v Speaker 1>a cupcake. Like, not just like in terms of our

0:18:57.800 --> 0:19:00.840
<v Speaker 1>relative importance to that and this the eye of the universe,

0:19:00.880 --> 0:19:02.760
<v Speaker 1>but also kind of like you know, sprinkles stick to

0:19:02.800 --> 0:19:05.120
<v Speaker 1>the icing in a cupcake. You know, you can't sort

0:19:05.160 --> 0:19:08.159
<v Speaker 1>of have sprinkles anywhere else. They're like, you know, the

0:19:08.200 --> 0:19:12.640
<v Speaker 1>sprinkles sort of tell you where the icing is. Yeah,

0:19:12.640 --> 0:19:15.240
<v Speaker 1>the sprinkles are sort of the stars, and the icing

0:19:15.280 --> 0:19:17.600
<v Speaker 1>is sort of dark matter, and the cupcake itself is

0:19:17.680 --> 0:19:20.359
<v Speaker 1>dark energy. That gives you sort of a sense of

0:19:20.400 --> 0:19:24.080
<v Speaker 1>the relative fractions of the energy budget of the universe. Yeah,

0:19:24.240 --> 0:19:26.439
<v Speaker 1>so I guess we are just the hangar ons of

0:19:26.480 --> 0:19:29.879
<v Speaker 1>the universe. We're just hanging onto dark matter. And so

0:19:30.000 --> 0:19:32.239
<v Speaker 1>let's get into a little bit more detail about what

0:19:32.320 --> 0:19:35.600
<v Speaker 1>we know about this halo around galaxies and also how

0:19:35.680 --> 0:19:38.399
<v Speaker 1>we know where it is, but first let's take a

0:19:38.480 --> 0:19:53.760
<v Speaker 1>quick break. All right, we're talking about dark matter and

0:19:54.119 --> 0:19:57.359
<v Speaker 1>where exactly it is, because I guess we know it's there,

0:19:57.359 --> 0:20:00.520
<v Speaker 1>but physicists can't find it. It's pretty tricky to nail

0:20:00.560 --> 0:20:04.159
<v Speaker 1>down an individual piece of dark matter, for example, because

0:20:04.160 --> 0:20:07.719
<v Speaker 1>it only interacts gravitationally, imagine trying to find like an

0:20:07.760 --> 0:20:10.840
<v Speaker 1>invisible piece of sand in your room. How would you

0:20:10.880 --> 0:20:14.440
<v Speaker 1>detect it? It's gravity is essentially nothing because gravity is

0:20:14.440 --> 0:20:17.359
<v Speaker 1>a really really weak force. All of the other forces

0:20:17.400 --> 0:20:21.760
<v Speaker 1>of electromagnetism, even the weak force, is much stronger than gravity.

0:20:22.119 --> 0:20:24.800
<v Speaker 1>So in order to detect something through gravity, you need

0:20:24.840 --> 0:20:26.760
<v Speaker 1>to have a huge force. You need to have like

0:20:26.920 --> 0:20:30.160
<v Speaker 1>a planet sized force or a solar system sized force

0:20:30.520 --> 0:20:33.680
<v Speaker 1>because gravity is so weak. So when we use gravity

0:20:33.720 --> 0:20:36.040
<v Speaker 1>to look for dark matter, we can only sort of

0:20:36.080 --> 0:20:39.360
<v Speaker 1>tell the large scale structure. It's very difficult to get

0:20:39.359 --> 0:20:42.480
<v Speaker 1>a fine grained picture of where things are. But even

0:20:42.520 --> 0:20:45.119
<v Speaker 1>though it's very weak gravitation, and we do have a

0:20:45.200 --> 0:20:47.600
<v Speaker 1>kind of a pretty good idea of what shape it

0:20:47.680 --> 0:20:50.280
<v Speaker 1>has in the galaxy, right like this halo, it's not

0:20:50.440 --> 0:20:53.240
<v Speaker 1>just like a blob. It has some sort of shaped

0:20:53.280 --> 0:20:55.720
<v Speaker 1>to it. That's right. It tends to be denser at

0:20:55.720 --> 0:20:59.040
<v Speaker 1>the core and thinner further out, much like the visible

0:20:59.080 --> 0:21:01.320
<v Speaker 1>matter in the galaxy. See, and we can tell where

0:21:01.320 --> 0:21:03.760
<v Speaker 1>it is because it has an effect on how the

0:21:03.800 --> 0:21:07.040
<v Speaker 1>stars spin. Right, Like, the old familiar story is that

0:21:07.080 --> 0:21:09.840
<v Speaker 1>we know that dark matter is there because we see

0:21:09.840 --> 0:21:12.960
<v Speaker 1>the speed of stars is way too high. If dark

0:21:13.000 --> 0:21:16.119
<v Speaker 1>matter wasn't there, then if the galaxy was spinning this quickly,

0:21:16.119 --> 0:21:19.280
<v Speaker 1>you should be throwing its stars out into interstellar space.

0:21:19.640 --> 0:21:23.240
<v Speaker 1>It needs more gravity, something out there to hold those

0:21:23.280 --> 0:21:26.439
<v Speaker 1>stars in place for the galaxy to spin this fast.

0:21:26.800 --> 0:21:28.680
<v Speaker 1>That's the old story that just tells us that dark

0:21:28.760 --> 0:21:31.280
<v Speaker 1>matter is there. But we can get much more fine

0:21:31.400 --> 0:21:35.000
<v Speaker 1>grained information. We can tell where in the galaxy that

0:21:35.119 --> 0:21:38.080
<v Speaker 1>dark matter is by measuring the velocity of stars at

0:21:38.119 --> 0:21:41.320
<v Speaker 1>different points as you move closer in or further out

0:21:41.440 --> 0:21:44.119
<v Speaker 1>from the center of the galaxy. Right, Because I guess

0:21:44.160 --> 0:21:46.240
<v Speaker 1>what you're saying is that if the dark matter was

0:21:46.320 --> 0:21:49.879
<v Speaker 1>all clumped together in the very very center of the galaxy,

0:21:50.119 --> 0:21:52.200
<v Speaker 1>the stars will move differently than if it was more

0:21:52.200 --> 0:21:54.920
<v Speaker 1>spread out throughout the whole galaxy. Right. Yeah, If you

0:21:55.000 --> 0:21:57.840
<v Speaker 1>are a star moving through the galaxy, then the thing

0:21:57.880 --> 0:22:01.000
<v Speaker 1>that determines your speed is how much stuff there is

0:22:01.560 --> 0:22:04.080
<v Speaker 1>closer to the center of the galaxy than you are.

0:22:04.320 --> 0:22:06.719
<v Speaker 1>You're not sensitive to anything that's further out than you.

0:22:06.920 --> 0:22:09.080
<v Speaker 1>It's sort of like if you dig into the Earth,

0:22:09.280 --> 0:22:12.080
<v Speaker 1>then everything that's further out from you, that's above you

0:22:12.640 --> 0:22:15.560
<v Speaker 1>doesn't affect your gravity at all because it all cancels out.

0:22:15.600 --> 0:22:17.639
<v Speaker 1>It's only stuff that's closer to the center of the

0:22:17.640 --> 0:22:20.240
<v Speaker 1>Earth than you are. So it's the same for a star.

0:22:20.520 --> 0:22:23.600
<v Speaker 1>The star is speed basically tells you how much stuff

0:22:23.640 --> 0:22:26.560
<v Speaker 1>there is between it and the center of the galaxy.

0:22:26.680 --> 0:22:28.520
<v Speaker 1>So as you look at the velocity of the star

0:22:28.760 --> 0:22:30.960
<v Speaker 1>as you move further out from the center, it gives

0:22:31.000 --> 0:22:33.159
<v Speaker 1>you a picture for where that dark matter has to

0:22:33.160 --> 0:22:36.720
<v Speaker 1>be to explain that velocity. The dark matter was all

0:22:36.720 --> 0:22:39.560
<v Speaker 1>clumped together at the very center of the galaxy, then stars,

0:22:39.560 --> 0:22:41.840
<v Speaker 1>you know, halfway out from the disk would be moving

0:22:41.920 --> 0:22:44.600
<v Speaker 1>faster because it would be a stronger force from all

0:22:44.640 --> 0:22:48.000
<v Speaker 1>of that gravity. Instead, if it's spread out really, really far,

0:22:48.320 --> 0:22:50.600
<v Speaker 1>then some of that stuff is outside those stars and

0:22:50.640 --> 0:22:53.280
<v Speaker 1>it doesn't affect them. It doesn't pull them towards the center,

0:22:53.280 --> 0:22:55.960
<v Speaker 1>it doesn't speed them up as much. Yeah, I guess

0:22:56.000 --> 0:22:58.080
<v Speaker 1>it's sort of like, if you're in the middle of

0:22:58.440 --> 0:23:00.800
<v Speaker 1>a cloud of dark matter, you're not to feel its

0:23:00.840 --> 0:23:03.919
<v Speaker 1>gravitation effects a much because it's pulling you in all directions,

0:23:04.119 --> 0:23:06.919
<v Speaker 1>Whereas if you're really really far away from it, the

0:23:06.920 --> 0:23:08.840
<v Speaker 1>whole blob, then you are going to feel sort of

0:23:08.880 --> 0:23:11.439
<v Speaker 1>its entire gravity. Yeah, and so that's how we know

0:23:11.520 --> 0:23:13.640
<v Speaker 1>that it's more dense in the middle. And that's kind

0:23:13.640 --> 0:23:16.160
<v Speaker 1>of important, right, It is important, and it's not something

0:23:16.160 --> 0:23:19.760
<v Speaker 1>that we really fully understand. Like if you do simulations

0:23:19.760 --> 0:23:22.240
<v Speaker 1>and you say we think we understand how galaxies might

0:23:22.240 --> 0:23:24.600
<v Speaker 1>have formed, and how this halo formed and all the

0:23:24.640 --> 0:23:27.680
<v Speaker 1>dark matter swirls together to make this well that forms

0:23:27.680 --> 0:23:30.399
<v Speaker 1>the galaxy, then we predict a certain shape for that

0:23:30.480 --> 0:23:32.840
<v Speaker 1>dark matter density. We predicted to be sort of like

0:23:32.960 --> 0:23:35.880
<v Speaker 1>peaky near the center, that like most of the dark

0:23:35.880 --> 0:23:38.280
<v Speaker 1>matter should be right at the center and then should

0:23:38.320 --> 0:23:40.520
<v Speaker 1>fall off kind of quickly. But what we observe when

0:23:40.520 --> 0:23:42.160
<v Speaker 1>we go out there and we look at the dark

0:23:42.200 --> 0:23:45.560
<v Speaker 1>matter see where it actually is based on these rotation curves,

0:23:46.080 --> 0:23:48.720
<v Speaker 1>is that it's not as peaky near the center. It's

0:23:48.720 --> 0:23:51.879
<v Speaker 1>more like a broad, flat core, like a big blob

0:23:52.000 --> 0:23:54.919
<v Speaker 1>of dark matter, it's not as like pointed at the center.

0:23:55.240 --> 0:23:58.640
<v Speaker 1>So that's a current mystery we don't really understand. Dark

0:23:58.680 --> 0:24:01.600
<v Speaker 1>matter doesn't seem to be as clumped towards the center

0:24:01.720 --> 0:24:03.639
<v Speaker 1>as we thought. And I guess part of it is that,

0:24:03.720 --> 0:24:05.119
<v Speaker 1>you know, a lot of people sort of wonder like,

0:24:05.160 --> 0:24:07.280
<v Speaker 1>if there is that much dark matter out there, why

0:24:07.320 --> 0:24:10.040
<v Speaker 1>doesn't it just collapse into a dark matter black hole?

0:24:10.160 --> 0:24:13.160
<v Speaker 1>But we we've talked about before how dark matter basically

0:24:13.359 --> 0:24:17.360
<v Speaker 1>is not sticky with itself, like it doesn't feel besides gravity,

0:24:17.440 --> 0:24:19.600
<v Speaker 1>It doesn't feel any other force that would make it

0:24:19.680 --> 0:24:23.359
<v Speaker 1>stick together, Like our adoms have the electromagnetic force to

0:24:23.480 --> 0:24:25.879
<v Speaker 1>make them stick, but dark matter doesn't appear to have

0:24:26.040 --> 0:24:28.479
<v Speaker 1>something like that. And that force is important if you're

0:24:28.480 --> 0:24:30.359
<v Speaker 1>going to fall into the black hole, because you have

0:24:30.400 --> 0:24:33.400
<v Speaker 1>to have some way to lose your angular momentum. Dark matter,

0:24:33.480 --> 0:24:36.520
<v Speaker 1>like everything else, is spinning and swirling, and the reason

0:24:36.560 --> 0:24:38.920
<v Speaker 1>that things don't fall into a black hole is because

0:24:38.960 --> 0:24:41.480
<v Speaker 1>they are swirling around it, the way the Earth is

0:24:41.560 --> 0:24:44.280
<v Speaker 1>orbiting the Sun and not falling into it. For the

0:24:44.280 --> 0:24:46.320
<v Speaker 1>Earth to fall into the Sun, it would have to

0:24:46.400 --> 0:24:49.679
<v Speaker 1>somehow lose its velocity. It would have to bump into

0:24:49.760 --> 0:24:52.919
<v Speaker 1>something we have to get slowed down. That only happens

0:24:52.960 --> 0:24:55.240
<v Speaker 1>if there's some sort of like sticky force that can

0:24:55.320 --> 0:24:58.000
<v Speaker 1>do that. So for a dark matter, that's really hard

0:24:58.080 --> 0:25:00.960
<v Speaker 1>because it passes right through itself, it passes right through

0:25:01.080 --> 0:25:03.720
<v Speaker 1>normal matter. It's very hard for it to lose its

0:25:03.720 --> 0:25:06.439
<v Speaker 1>speed or its angular momentum. So that's why this halo

0:25:06.520 --> 0:25:10.000
<v Speaker 1>of dark matter is bigger than the visible galaxy because

0:25:10.040 --> 0:25:13.040
<v Speaker 1>dark matter actually finds it harder to collapse, harder to

0:25:13.160 --> 0:25:16.080
<v Speaker 1>fall into black holes, right, you know, And so it's

0:25:16.160 --> 0:25:18.840
<v Speaker 1>been this big diffusion. It has this interesting shape. So

0:25:18.880 --> 0:25:20.640
<v Speaker 1>then how else can we sort of know about its

0:25:20.640 --> 0:25:23.800
<v Speaker 1>structure besides it's sort of general blobby shape. Well, one

0:25:23.840 --> 0:25:26.520
<v Speaker 1>of the listeners got it right thinking about how dark

0:25:26.560 --> 0:25:29.600
<v Speaker 1>matter distorts the path of light. We can tell when

0:25:29.600 --> 0:25:32.439
<v Speaker 1>there's a big blob of dark matter between us and

0:25:32.560 --> 0:25:35.920
<v Speaker 1>something else because it acts like a lens in the sky.

0:25:36.119 --> 0:25:39.320
<v Speaker 1>Remember that dark matter, even though it's invisible and light

0:25:39.359 --> 0:25:42.760
<v Speaker 1>can pass through it, it does change the shape of space.

0:25:43.280 --> 0:25:45.200
<v Speaker 1>And that means the space can act like a lens,

0:25:45.320 --> 0:25:47.360
<v Speaker 1>and so light will pass through it, but it will

0:25:47.400 --> 0:25:49.639
<v Speaker 1>get bent on the way. And so if there's a

0:25:49.680 --> 0:25:52.720
<v Speaker 1>big blob of dark matter between us and a distant galaxy,

0:25:52.760 --> 0:25:56.080
<v Speaker 1>for example, it will change the shape of that galaxy distorted,

0:25:56.359 --> 0:25:58.000
<v Speaker 1>just as if there was a lens there. So we

0:25:58.040 --> 0:26:00.399
<v Speaker 1>can use that to try to get idea is for

0:26:00.480 --> 0:26:03.959
<v Speaker 1>where dark matter might be interesting. So dark matter does

0:26:04.000 --> 0:26:07.399
<v Speaker 1>seem to clump within our galaxy? Is that what you're saying? Like,

0:26:07.440 --> 0:26:10.680
<v Speaker 1>maybe within our galaxy there are spots where dark matter

0:26:10.760 --> 0:26:13.960
<v Speaker 1>seems to be denser than others. That's hard to tell

0:26:14.040 --> 0:26:17.040
<v Speaker 1>because this kind of gravitational effect is kind of rare,

0:26:17.280 --> 0:26:20.359
<v Speaker 1>Like you need a clear background galaxy and then you

0:26:20.400 --> 0:26:22.639
<v Speaker 1>need a blob of dark matter right in front of

0:26:22.640 --> 0:26:25.280
<v Speaker 1>it has to be like perfectly lined up, so it's

0:26:25.320 --> 0:26:28.760
<v Speaker 1>tough to use this. They call this strong gravitational lensing

0:26:29.119 --> 0:26:31.439
<v Speaker 1>to get a clear picture for where the dark matter is,

0:26:31.480 --> 0:26:34.359
<v Speaker 1>because we don't have really enough examples, so it's not

0:26:34.400 --> 0:26:36.800
<v Speaker 1>a great way to tell where the dark matter is.

0:26:36.960 --> 0:26:39.520
<v Speaker 1>A better way to tell if dark matter clumps up

0:26:39.880 --> 0:26:43.000
<v Speaker 1>is to look for its effect on stars. So not

0:26:43.080 --> 0:26:45.920
<v Speaker 1>just like the velocity of stars as they weave around

0:26:45.960 --> 0:26:48.919
<v Speaker 1>the center of the galaxy, but their motion in other directions,

0:26:48.960 --> 0:26:51.680
<v Speaker 1>like if there is a big clump of dark matter

0:26:51.720 --> 0:26:54.840
<v Speaker 1>and especially dense blob of dark matter. It will affect

0:26:54.840 --> 0:26:57.840
<v Speaker 1>how stars are moving around it. It will change the

0:26:57.880 --> 0:27:01.520
<v Speaker 1>motion of those stars. It will attract them, it'll reflect them.

0:27:01.520 --> 0:27:03.439
<v Speaker 1>I see. So if you look sort of look at

0:27:03.480 --> 0:27:05.680
<v Speaker 1>the overall motion of all the stars in the galaxy,

0:27:05.760 --> 0:27:07.359
<v Speaker 1>if you see that there are you know, sort of

0:27:07.359 --> 0:27:10.320
<v Speaker 1>wiggles here and there or little you know, eddies or

0:27:10.400 --> 0:27:13.240
<v Speaker 1>little clumps of stars forming, then you know that there's

0:27:13.240 --> 0:27:15.840
<v Speaker 1>something else there and that it's not the dark matter

0:27:15.960 --> 0:27:18.959
<v Speaker 1>is not perfectly smooth. Yes, And we recently launched a

0:27:19.000 --> 0:27:23.000
<v Speaker 1>satellite called Gaya which is mapping the galaxy in four dimensions.

0:27:23.400 --> 0:27:26.480
<v Speaker 1>It measures the position, the location of all these stars

0:27:26.560 --> 0:27:30.000
<v Speaker 1>and their velocity. So we're getting this incredible map. It

0:27:30.080 --> 0:27:33.320
<v Speaker 1>has like a billion stars with their position and their

0:27:33.359 --> 0:27:36.560
<v Speaker 1>velocity map. Then we can use this to look for deviations.

0:27:36.560 --> 0:27:39.360
<v Speaker 1>Were like, well, if dark matter was perfectly smooth, what

0:27:39.359 --> 0:27:42.040
<v Speaker 1>would we expect all these stars to be doing. And

0:27:42.280 --> 0:27:45.080
<v Speaker 1>are any stars doing anything weird? And if they are,

0:27:45.160 --> 0:27:47.240
<v Speaker 1>we can sort of back that out and figure out

0:27:47.400 --> 0:27:50.440
<v Speaker 1>where dark matter has to be to explain any weird

0:27:50.480 --> 0:27:52.960
<v Speaker 1>patterns of the star motion. Right, Because I guess if

0:27:53.040 --> 0:27:56.320
<v Speaker 1>dark matter was perfectly smooth, Peanut butter like this kind

0:27:56.320 --> 0:28:00.000
<v Speaker 1>of smooth cloud. Then you would expect all the stars

0:28:00.040 --> 0:28:03.040
<v Speaker 1>us to be basically moving along as if it was

0:28:03.080 --> 0:28:05.400
<v Speaker 1>in a lazy river, right, like everyone sort of moving

0:28:05.440 --> 0:28:08.200
<v Speaker 1>at the same You know, nobody would be going much

0:28:08.240 --> 0:28:10.840
<v Speaker 1>faster than or slower than any of the other stars. Yeah,

0:28:10.840 --> 0:28:13.440
<v Speaker 1>at the same radius, right, we expect as you go out,

0:28:13.520 --> 0:28:15.679
<v Speaker 1>as you change your radius relative to the center of

0:28:15.680 --> 0:28:18.239
<v Speaker 1>the galaxy, these things will change, just like they do

0:28:18.240 --> 0:28:21.040
<v Speaker 1>in our solar system. Pluto's not moving around the Sun

0:28:21.080 --> 0:28:23.680
<v Speaker 1>as fast as Jupiter, which is not moving as fast

0:28:23.720 --> 0:28:26.640
<v Speaker 1>as Mercury, because as you go further out the gravitational

0:28:26.680 --> 0:28:29.120
<v Speaker 1>force is weaker. But you'd expect things at the same

0:28:29.240 --> 0:28:32.240
<v Speaker 1>radius to basically be having the same motion. And so

0:28:32.280 --> 0:28:35.280
<v Speaker 1>if you see deviations, then you know dark matter is there,

0:28:35.440 --> 0:28:37.920
<v Speaker 1>and we do sort of expect there to be clumps.

0:28:38.000 --> 0:28:40.719
<v Speaker 1>We expect that the galaxy, for example, has lots of

0:28:40.760 --> 0:28:44.080
<v Speaker 1>other galaxies inside of it that it has absorbed. We

0:28:44.120 --> 0:28:46.800
<v Speaker 1>think that the history of our galaxy includes lots of

0:28:46.840 --> 0:28:50.160
<v Speaker 1>collisions to form the Milky Way, and you would suspect

0:28:50.160 --> 0:28:53.120
<v Speaker 1>that those galaxies might still have like their dark matter

0:28:53.200 --> 0:28:57.360
<v Speaker 1>halos embedded within hours because I guess you would expect

0:28:57.400 --> 0:29:00.960
<v Speaker 1>our matter to be clumpy because regg or matter is clumpy,

0:29:01.040 --> 0:29:04.120
<v Speaker 1>so in a way, like wouldn't our regular matter also

0:29:04.200 --> 0:29:07.960
<v Speaker 1>sort of catalyze or trigger dark matter to clump. Our

0:29:08.000 --> 0:29:10.600
<v Speaker 1>matter is clumpy, But that's because it's sticky, right, It

0:29:10.720 --> 0:29:14.160
<v Speaker 1>can form these blobs, so when gravity pulls it together,

0:29:14.520 --> 0:29:18.160
<v Speaker 1>it sticks together and then that accumulates forms this runaway effect,

0:29:18.360 --> 0:29:21.160
<v Speaker 1>whereas dark matter is not sticky, and so dark matter

0:29:21.200 --> 0:29:24.800
<v Speaker 1>halos can pass right through each other without very much distortion.

0:29:24.920 --> 0:29:27.480
<v Speaker 1>The other question is a cool one, like do stars

0:29:27.640 --> 0:29:30.560
<v Speaker 1>form clumps of dark matter? And this is something people

0:29:30.560 --> 0:29:32.440
<v Speaker 1>have studied. They've tried to look to see if there's

0:29:32.480 --> 0:29:35.520
<v Speaker 1>like an intense blob of dark matter inside the sun,

0:29:35.640 --> 0:29:38.440
<v Speaker 1>for example. But remember that there's much more dark matter

0:29:38.560 --> 0:29:40.640
<v Speaker 1>than there is normal matter, and so dark matter sort

0:29:40.640 --> 0:29:43.720
<v Speaker 1>of wins the gravitational battles. You would expect it to

0:29:43.800 --> 0:29:46.520
<v Speaker 1>mostly go the other direction, that dark matter would influence

0:29:46.760 --> 0:29:49.920
<v Speaker 1>the pattern of normal matter rather than vice versa. But yeah,

0:29:50.000 --> 0:29:52.400
<v Speaker 1>it is a tug of war. Interesting you're saying dark

0:29:52.440 --> 0:29:56.400
<v Speaker 1>matter is ignoring us. Basically it's ghosting us. It mostly can.

0:29:56.640 --> 0:29:59.240
<v Speaker 1>But back to this question of like following the stars.

0:29:59.440 --> 0:30:02.080
<v Speaker 1>There are some really cool things that we do see

0:30:02.160 --> 0:30:05.480
<v Speaker 1>inside our galaxy. We can see the remnants of other

0:30:05.520 --> 0:30:09.320
<v Speaker 1>galaxies that the Milky Way has eaten, little mini galaxies

0:30:09.320 --> 0:30:12.680
<v Speaker 1>we call these dwarf galaxies, and some of these are

0:30:12.800 --> 0:30:16.120
<v Speaker 1>really really interesting because they're super high in dark matter.

0:30:16.640 --> 0:30:19.120
<v Speaker 1>Like our galaxy has a lot of dark matter, but

0:30:19.200 --> 0:30:22.680
<v Speaker 1>some of these dwarf galaxies are almost entirely dark matter,

0:30:23.040 --> 0:30:25.120
<v Speaker 1>and we can tell that they're there because we see

0:30:25.240 --> 0:30:29.560
<v Speaker 1>stars orbiting these invisible dark matter halos. So there's sort

0:30:29.600 --> 0:30:33.160
<v Speaker 1>of like many clumps of dark matter within our dark

0:30:33.160 --> 0:30:36.800
<v Speaker 1>matter halo. Interesting, so it is clumpy, but maybe because

0:30:36.920 --> 0:30:39.840
<v Speaker 1>we've we've added the clumps kind of yeah, because we've

0:30:39.960 --> 0:30:43.479
<v Speaker 1>formed our big halo from a bunch of clumps. So

0:30:43.520 --> 0:30:46.040
<v Speaker 1>we think these clumps formed initially each one of these

0:30:46.120 --> 0:30:49.280
<v Speaker 1>its own galaxy, and then galaxies eventually do merge and

0:30:49.320 --> 0:30:53.320
<v Speaker 1>collide and form bigger galaxies. And sometimes those dark matter

0:30:53.360 --> 0:30:57.080
<v Speaker 1>halos don't necessarily spread out and just join like the

0:30:57.120 --> 0:30:59.600
<v Speaker 1>original creamy blob of the Milky Way. They sort of

0:30:59.640 --> 0:31:02.080
<v Speaker 1>stay there as chunks, and you can tell of they're

0:31:02.200 --> 0:31:06.760
<v Speaker 1>because the stars swirling around those little dwarf galaxies. Well,

0:31:06.800 --> 0:31:08.760
<v Speaker 1>here's the question. Do you think the dark matter in

0:31:08.760 --> 0:31:11.280
<v Speaker 1>our galaxy is spinning also with the rest of the

0:31:11.400 --> 0:31:14.160
<v Speaker 1>stars and galaxies, or is it just standing still. It's

0:31:14.160 --> 0:31:17.640
<v Speaker 1>almost certainly spinning. That's the reason that it doesn't collapse

0:31:17.720 --> 0:31:19.840
<v Speaker 1>into the black hole in the center. If it was

0:31:19.880 --> 0:31:22.320
<v Speaker 1>standing still, then that gravity from that black hole would

0:31:22.320 --> 0:31:25.240
<v Speaker 1>just suck it up. So it's almost certain that it's rotating.

0:31:25.440 --> 0:31:28.480
<v Speaker 1>That we can't measure that directly, right, we haven't seen that,

0:31:28.880 --> 0:31:31.120
<v Speaker 1>but we're fairly certain that it has to be otherwise

0:31:31.120 --> 0:31:34.920
<v Speaker 1>it would have collapsed. So through strong gravitational lensing we

0:31:34.960 --> 0:31:38.120
<v Speaker 1>can tell that there are some clumps out there, and

0:31:38.200 --> 0:31:40.680
<v Speaker 1>through some of these absorbed galaxies we know there are

0:31:40.680 --> 0:31:42.520
<v Speaker 1>clumps out there, but what else do we know about

0:31:42.520 --> 0:31:45.200
<v Speaker 1>this clumpiness. We can also try to measure the clumpiness

0:31:45.280 --> 0:31:48.360
<v Speaker 1>by looking at the effect of our gravity on things

0:31:48.680 --> 0:31:52.200
<v Speaker 1>near the galaxy. So sometimes these mini galaxies or these

0:31:52.200 --> 0:31:55.680
<v Speaker 1>globular clusters get sucked inside the galaxy. Sometimes they're in

0:31:55.840 --> 0:31:59.240
<v Speaker 1>orbit around the galaxy. So for example, the large Magellanic

0:31:59.280 --> 0:32:01.479
<v Speaker 1>Cloud is a ab of stuff that's sort of like

0:32:01.520 --> 0:32:04.600
<v Speaker 1>a satellite galaxy of the Milky Way, and often these

0:32:04.600 --> 0:32:08.240
<v Speaker 1>galaxies get torn apart, they don't hold themselves together. They

0:32:08.240 --> 0:32:11.640
<v Speaker 1>turn into these streams. So around the galaxy there are

0:32:11.640 --> 0:32:15.000
<v Speaker 1>these things called stellar streams, which are these like lines

0:32:15.240 --> 0:32:18.880
<v Speaker 1>of stars moving in a loop sort of around the galaxies.

0:32:19.040 --> 0:32:21.640
<v Speaker 1>It's sort of like the galaxy has rings of stars

0:32:22.840 --> 0:32:28.640
<v Speaker 1>interesting like accidents almost, yeah, and they're sort of swooping

0:32:28.760 --> 0:32:31.560
<v Speaker 1>around the galaxy. And those are very sensitive to the

0:32:31.600 --> 0:32:35.160
<v Speaker 1>distribution of dark matter. So if, for example, the dark

0:32:35.200 --> 0:32:38.200
<v Speaker 1>matter halo is clumpy, it will affect how those stars

0:32:38.240 --> 0:32:41.760
<v Speaker 1>get pulled apart and whether they're like gaps in those streams.

0:32:42.040 --> 0:32:44.640
<v Speaker 1>So there are people right now studying these stellar streams.

0:32:44.640 --> 0:32:47.800
<v Speaker 1>They're like probes of that dark matter halo to look

0:32:47.840 --> 0:32:49.720
<v Speaker 1>to see if there are clumps in the dark matter

0:32:49.720 --> 0:32:52.880
<v Speaker 1>halo or to see if it's like perfectly spherical or

0:32:52.960 --> 0:32:55.440
<v Speaker 1>kind of elliptical. So these are very nice ways to

0:32:55.480 --> 0:32:58.200
<v Speaker 1>tell how much dark matter they're passing through and how

0:32:58.240 --> 0:33:01.920
<v Speaker 1>clumpy it is. Interesting, and so that's one way to

0:33:01.960 --> 0:33:04.680
<v Speaker 1>sort of know the clumpiness of dark matter. And what

0:33:04.800 --> 0:33:06.920
<v Speaker 1>have we learned from all of these different ways. We

0:33:06.920 --> 0:33:09.160
<v Speaker 1>don't have a great picture of where dark matter is

0:33:09.160 --> 0:33:11.720
<v Speaker 1>in the galaxy. People often write in and ask like

0:33:12.000 --> 0:33:14.760
<v Speaker 1>where is the dark matter? Can we see like planets

0:33:14.760 --> 0:33:17.240
<v Speaker 1>of dark matter or that's kind of stuff. Really, we're

0:33:17.280 --> 0:33:19.920
<v Speaker 1>not very sensitive to the details. We know that the

0:33:19.960 --> 0:33:22.920
<v Speaker 1>Milky Way has a big blob of dark matter that

0:33:23.000 --> 0:33:26.800
<v Speaker 1>it's probably elliptical, you know, it's not totally spherical. We

0:33:26.800 --> 0:33:30.920
<v Speaker 1>can see some clumps where these faint dwarf galaxies were absorbed,

0:33:31.040 --> 0:33:33.400
<v Speaker 1>but we don't have a great sense for the structure

0:33:33.480 --> 0:33:36.800
<v Speaker 1>of the dark matter. It's mostly smooth, but we can't

0:33:36.800 --> 0:33:39.200
<v Speaker 1>see things smaller than like, you know, tend to the

0:33:39.280 --> 0:33:42.640
<v Speaker 1>six stars. I see, like the smallest clump we can

0:33:42.720 --> 0:33:45.360
<v Speaker 1>sort of tell right now is is tend to the

0:33:45.440 --> 0:33:48.880
<v Speaker 1>six billions of kilometers maybe tend to the six solar

0:33:48.920 --> 0:33:52.520
<v Speaker 1>masses equivalents of dark matter? Is like the smallest chunk

0:33:52.520 --> 0:33:55.760
<v Speaker 1>of things we can tell. Well, that's like our our

0:33:55.800 --> 0:33:58.720
<v Speaker 1>best resolution of our picture of dark matter in the galaxy.

0:33:58.760 --> 0:34:02.480
<v Speaker 1>It's like a pixel this side a million sons. So

0:34:02.520 --> 0:34:05.560
<v Speaker 1>we're not very sensitive and that's just because it's mostly smooth.

0:34:05.800 --> 0:34:08.160
<v Speaker 1>There aren't a lot of features to see, who we think,

0:34:08.440 --> 0:34:11.240
<v Speaker 1>and because we're not very sensitive to it. Again, gravity

0:34:11.320 --> 0:34:13.759
<v Speaker 1>is very weak and it's our only way of interacting

0:34:13.760 --> 0:34:16.239
<v Speaker 1>with it. Which makes it kind of frustrating. All right, well,

0:34:16.360 --> 0:34:19.080
<v Speaker 1>it sounds like it's still yet to be discovered. Who knows,

0:34:19.120 --> 0:34:23.160
<v Speaker 1>Maybe it's forming giant dark matter squirrels or bananas or

0:34:23.200 --> 0:34:25.360
<v Speaker 1>grass out there, but we just can't see it with

0:34:25.480 --> 0:34:28.040
<v Speaker 1>our current resolution. And so let's get a little bit

0:34:28.040 --> 0:34:30.799
<v Speaker 1>into what the overall picture of dark matter then is

0:34:30.880 --> 0:34:34.279
<v Speaker 1>in the universe, and also what's happening between galaxies. But

0:34:34.360 --> 0:34:49.520
<v Speaker 1>first let's take another quick break. All right, Daniel has

0:34:49.600 --> 0:34:53.080
<v Speaker 1>lost his dark matter and his mind apparently. Did you

0:34:53.120 --> 0:34:55.080
<v Speaker 1>lose your mind looking for the dark matter? I did.

0:34:55.080 --> 0:34:59.719
<v Speaker 1>It's driving me crazy. Where are you? It's avoiding you,

0:34:59.760 --> 0:35:02.000
<v Speaker 1>It's else see you. It is a little bit ghosting

0:35:02.160 --> 0:35:05.040
<v Speaker 1>us as humanity because we know it's there, but it

0:35:05.080 --> 0:35:08.040
<v Speaker 1>doesn't seem to want to make expressence known to us.

0:35:08.080 --> 0:35:10.680
<v Speaker 1>In detail, we sort of have a big picture of

0:35:10.719 --> 0:35:12.960
<v Speaker 1>it that it's in a big clump around the galaxy,

0:35:13.120 --> 0:35:15.839
<v Speaker 1>mostly concentrated in the middle. We see some clumps out there,

0:35:15.920 --> 0:35:18.279
<v Speaker 1>but we don't know the exact structure of dark matter.

0:35:18.440 --> 0:35:20.799
<v Speaker 1>But we do sort of know it's density out there, right,

0:35:20.800 --> 0:35:23.279
<v Speaker 1>We have some figures for its general density. Yeah, And

0:35:23.280 --> 0:35:26.600
<v Speaker 1>it's quite interesting because we think that on average over

0:35:26.680 --> 0:35:30.280
<v Speaker 1>the universe, dark matters like eight percent of the matter

0:35:30.480 --> 0:35:33.000
<v Speaker 1>of the universe, but in our neighborhood it is actually

0:35:33.000 --> 0:35:35.440
<v Speaker 1>a little bit different. The Milky Way, for example, we

0:35:35.480 --> 0:35:39.720
<v Speaker 1>think is nine five dark matter. So our whole galaxy

0:35:39.840 --> 0:35:41.879
<v Speaker 1>is kind of badly named. It should be called like

0:35:42.120 --> 0:35:45.400
<v Speaker 1>the Dark Way or something, the Chocolate Milk Galaxy, the

0:35:45.520 --> 0:35:49.120
<v Speaker 1>darklan Milky Way, the Dark Chocolate Way or something. So

0:35:49.160 --> 0:35:52.120
<v Speaker 1>we're like nine percent dark matter, which means if we

0:35:52.160 --> 0:35:56.240
<v Speaker 1>have like you know, the equivalent of ninety billion times

0:35:56.320 --> 0:35:58.920
<v Speaker 1>the mass of the Sun in terms of stars and

0:35:59.040 --> 0:36:01.000
<v Speaker 1>gas and all that kind of stuff, that means that

0:36:01.000 --> 0:36:03.919
<v Speaker 1>there's like two trillion times the mass of the Sun

0:36:04.120 --> 0:36:06.960
<v Speaker 1>in dark matter. It's just so much more. And it's

0:36:07.000 --> 0:36:10.880
<v Speaker 1>like twenty times as much dark matter in our galaxy

0:36:11.080 --> 0:36:13.920
<v Speaker 1>as normal matter, which is a bigger ratio than the

0:36:13.960 --> 0:36:16.479
<v Speaker 1>rest of the universe. Well, that's true for regular matter.

0:36:16.560 --> 0:36:19.640
<v Speaker 1>To write like our Milky Way has a higher density

0:36:19.640 --> 0:36:22.000
<v Speaker 1>of regular matter than the rest of the universe or

0:36:22.080 --> 0:36:24.280
<v Speaker 1>some other parts of the universe. Right, Yeah, that's true.

0:36:24.600 --> 0:36:28.439
<v Speaker 1>But on average galaxies have about eighty percent dark matter,

0:36:28.520 --> 0:36:32.840
<v Speaker 1>and our galaxy is so there's a big variation. Galaxy

0:36:32.880 --> 0:36:35.560
<v Speaker 1>the galaxy and how much dark matter there is. Oh,

0:36:35.600 --> 0:36:39.319
<v Speaker 1>I mean our galaxy has more than other galaxies. Absolutely, Yeah,

0:36:39.360 --> 0:36:42.920
<v Speaker 1>we are a darker galaxy than most interesting we're more mysterious,

0:36:42.920 --> 0:36:45.000
<v Speaker 1>I guess. Yeah. And there's some galaxies out there that

0:36:45.040 --> 0:36:48.480
<v Speaker 1>are overwhelmingly dark matter, like nine points something per cent.

0:36:48.640 --> 0:36:50.680
<v Speaker 1>And then there are some galaxies that have very little

0:36:50.760 --> 0:36:52.920
<v Speaker 1>dark matter. We think that might be evidence of collisions

0:36:52.960 --> 0:36:55.799
<v Speaker 1>where dark matter gets separated from the normal matter. All

0:36:55.840 --> 0:36:58.560
<v Speaker 1>sorts of crazy stuff. These things tell you the crazy

0:36:58.640 --> 0:37:01.800
<v Speaker 1>cosmic history of all of these objects. Interesting. And again

0:37:01.840 --> 0:37:03.880
<v Speaker 1>you can tell by when you look at these galaxies

0:37:03.880 --> 0:37:06.760
<v Speaker 1>out there. You can tell that they're holding on together

0:37:07.080 --> 0:37:09.200
<v Speaker 1>more than they should by the number of stars or

0:37:09.239 --> 0:37:11.239
<v Speaker 1>the brightness of them. Right. Yeah, you can tell when

0:37:11.239 --> 0:37:14.239
<v Speaker 1>a galaxy is overwhelmingly dark matter because it's stars are

0:37:14.320 --> 0:37:17.279
<v Speaker 1>moving super duper fast compared to how bright they are,

0:37:17.520 --> 0:37:20.480
<v Speaker 1>And so we can see these faint dwarf galaxies, for example,

0:37:20.680 --> 0:37:23.400
<v Speaker 1>just have a handful of stars, but they're whizzing around

0:37:23.400 --> 0:37:26.040
<v Speaker 1>in a circle and there's not nearly enough gravity to

0:37:26.080 --> 0:37:28.319
<v Speaker 1>hold them in place. Just from the stuff that we

0:37:28.400 --> 0:37:30.799
<v Speaker 1>can see, so it's pretty cool, but it's so far away.

0:37:30.800 --> 0:37:32.279
<v Speaker 1>How do you know it's not just like filled with

0:37:32.600 --> 0:37:36.080
<v Speaker 1>the black holes or something or rocks dark rocks, because

0:37:36.080 --> 0:37:38.239
<v Speaker 1>we can see light passing through it, right, we can

0:37:38.239 --> 0:37:41.040
<v Speaker 1>see through it to something else behind it. If there

0:37:41.080 --> 0:37:42.880
<v Speaker 1>was a black hole there, it would absorb the light.

0:37:43.000 --> 0:37:45.480
<v Speaker 1>If it was just like a huge death star or

0:37:45.520 --> 0:37:48.719
<v Speaker 1>something cloaked, then it would absorb that light. So we

0:37:48.800 --> 0:37:52.120
<v Speaker 1>see it as invisible, not as dark all right, So then, um,

0:37:52.160 --> 0:37:54.719
<v Speaker 1>it's sort of danser in our galaxy. What about in

0:37:55.000 --> 0:37:57.640
<v Speaker 1>in our more immediate neighborhood or like a star solar

0:37:57.680 --> 0:38:01.080
<v Speaker 1>system also extra dark mattery, it's and in our neighborhood.

0:38:01.080 --> 0:38:04.920
<v Speaker 1>Remember that while the Milky Way is dark matter that

0:38:05.080 --> 0:38:08.200
<v Speaker 1>is spread out throughout the stars, we think, so normal

0:38:08.239 --> 0:38:11.399
<v Speaker 1>matter clumps up a lot more than dark matter, which

0:38:11.400 --> 0:38:14.239
<v Speaker 1>means that there isn't that much dark matter in any

0:38:14.320 --> 0:38:17.720
<v Speaker 1>like cubic light year of space. So in a cubic

0:38:17.800 --> 0:38:20.520
<v Speaker 1>light year of space, there's less than a one quarter

0:38:20.760 --> 0:38:23.479
<v Speaker 1>of one one thousands of the mass of the Sun.

0:38:23.880 --> 0:38:25.920
<v Speaker 1>In a cubic light year of space, that's like a

0:38:26.000 --> 0:38:28.960
<v Speaker 1>quarter of the mass of Jupiter in a cubic light

0:38:29.040 --> 0:38:31.080
<v Speaker 1>year of space. That's how much dark matter there is.

0:38:31.480 --> 0:38:34.160
<v Speaker 1>M t gives you took Jupiter and spread it over

0:38:34.280 --> 0:38:37.160
<v Speaker 1>billions of miles, right, it wouldn't be very much. And

0:38:37.160 --> 0:38:39.480
<v Speaker 1>you know, if you zoom in, for example, into like

0:38:39.520 --> 0:38:43.760
<v Speaker 1>a cubic meter, that's like ten the minus twenty two

0:38:44.200 --> 0:38:47.520
<v Speaker 1>grams of dark matter in a cubic meter. So you know,

0:38:47.560 --> 0:38:50.200
<v Speaker 1>if you look at the space around you in your office,

0:38:50.239 --> 0:38:53.360
<v Speaker 1>for example, then there's just like a super tiny amount

0:38:53.400 --> 0:38:56.200
<v Speaker 1>of dark matter, almost hard to measure, but some of

0:38:56.239 --> 0:38:58.320
<v Speaker 1>it's there are a few particles. And if you zoom

0:38:58.320 --> 0:39:00.879
<v Speaker 1>out to like the whole volume of the Earth, there's

0:39:00.960 --> 0:39:04.040
<v Speaker 1>less than a kilogram of dark matter in the volume

0:39:04.120 --> 0:39:06.839
<v Speaker 1>of the Earth. Again, these are sort of approximations, right,

0:39:06.840 --> 0:39:09.400
<v Speaker 1>because he told me earlier that our ability to resolve

0:39:09.480 --> 0:39:11.960
<v Speaker 1>or a resolution of dark matter is pretty bad. So

0:39:12.000 --> 0:39:14.239
<v Speaker 1>how do we know like that there isn't the sort

0:39:14.239 --> 0:39:16.640
<v Speaker 1>of clump of dark matter just around us right now?

0:39:16.880 --> 0:39:19.640
<v Speaker 1>We don't know absolutely, We do not know. We are

0:39:19.680 --> 0:39:21.480
<v Speaker 1>not sensitive to these things, so it could be a

0:39:21.520 --> 0:39:24.520
<v Speaker 1>lot clumpier than we think these numbers are, assuming that

0:39:24.600 --> 0:39:28.240
<v Speaker 1>dark matter is mostly smoothly spread out throughout the galaxy

0:39:28.520 --> 0:39:31.360
<v Speaker 1>according to the distribution that we've seen from the radius.

0:39:31.400 --> 0:39:33.880
<v Speaker 1>But we absolutely cannot tell if there's like a huge

0:39:33.960 --> 0:39:36.000
<v Speaker 1>blob of dark matter that we're sitting in, or if

0:39:36.040 --> 0:39:39.120
<v Speaker 1>there's almost no dark matter in our neighborhood. And remember

0:39:39.120 --> 0:39:42.560
<v Speaker 1>that we have experiments underground looking for dark matter particles.

0:39:42.600 --> 0:39:45.520
<v Speaker 1>They're basically trying to measure how the Earth is moving

0:39:45.560 --> 0:39:48.760
<v Speaker 1>through this dark matter wind, and they haven't seen anything.

0:39:49.120 --> 0:39:51.640
<v Speaker 1>And one of my favorite explanations is like, well, maybe

0:39:51.680 --> 0:39:53.840
<v Speaker 1>we're just happy to be sitting in a bubble that

0:39:53.920 --> 0:39:56.560
<v Speaker 1>has almost no dark matter in it, which would make

0:39:56.560 --> 0:39:59.200
<v Speaker 1>it impossible for us to detect that dark matter wind.

0:39:59.480 --> 0:40:02.279
<v Speaker 1>We just don't know it's ghosting us and avoiding is

0:40:02.480 --> 0:40:05.040
<v Speaker 1>physically at the same time. But it's kind of interesting

0:40:05.080 --> 0:40:07.839
<v Speaker 1>because I think what you talked about earlier, how like

0:40:07.880 --> 0:40:11.000
<v Speaker 1>in the volume of the Earth, there's about one squirrels

0:40:11.000 --> 0:40:13.640
<v Speaker 1>worth full of dark matter. Like that's not a lot, right,

0:40:13.640 --> 0:40:15.359
<v Speaker 1>and the whole Earth is pretty big, but you only

0:40:15.360 --> 0:40:18.080
<v Speaker 1>have one squirrel full of dark matter, And that's why

0:40:18.120 --> 0:40:21.880
<v Speaker 1>we can't ever detected gravitationally. You know, we're literally looking

0:40:21.920 --> 0:40:25.520
<v Speaker 1>for a squirrel that's hiding inside the Earth, and that's

0:40:25.520 --> 0:40:27.840
<v Speaker 1>pretty hard to tell the difference. We can't measure the

0:40:27.880 --> 0:40:31.440
<v Speaker 1>number of squirrels on Earth. Using grabic, you'd go nuts.

0:40:33.040 --> 0:40:35.160
<v Speaker 1>But yeah, so let's talk about then, now, sort of

0:40:35.239 --> 0:40:38.120
<v Speaker 1>dark matter between galaxies, because you know, there's a lot

0:40:38.120 --> 0:40:40.520
<v Speaker 1>of space between galaxies and we sort of have a

0:40:40.520 --> 0:40:43.560
<v Speaker 1>pretty good idea of the structure of the universe, you know,

0:40:43.680 --> 0:40:47.240
<v Speaker 1>the galaxy clusters and superclusters. Is does dark matter also

0:40:47.280 --> 0:40:50.080
<v Speaker 1>follow these clusters? We think that mostly does, and again

0:40:50.200 --> 0:40:53.080
<v Speaker 1>we think it's sort of the opposite that normal matter

0:40:53.280 --> 0:40:56.920
<v Speaker 1>follows the path of dark matter. But it's much harder

0:40:56.960 --> 0:41:01.000
<v Speaker 1>to see the things between galaxies because there's much less

0:41:01.040 --> 0:41:04.280
<v Speaker 1>light there and there's much less visible objects. Like mostly

0:41:04.320 --> 0:41:06.800
<v Speaker 1>we have seen where dark matter is within our galaxy

0:41:07.040 --> 0:41:10.440
<v Speaker 1>by following the path of stars, their rotation, their wiggles,

0:41:10.800 --> 0:41:13.480
<v Speaker 1>their distortions, all that kind of stuff where there are

0:41:13.520 --> 0:41:16.480
<v Speaker 1>in stars like tracers to tell us where things are

0:41:16.600 --> 0:41:20.399
<v Speaker 1>between galaxies. So it's much trickier. Yeah, I guess you

0:41:20.400 --> 0:41:22.720
<v Speaker 1>you can sort of extrapolate, right what we can see

0:41:22.760 --> 0:41:24.960
<v Speaker 1>a little bit around this, then you sort of assume

0:41:25.000 --> 0:41:26.960
<v Speaker 1>that that's what's happening maybe in the rest of the

0:41:27.040 --> 0:41:29.680
<v Speaker 1>universe sort of, But we know that the galaxies are

0:41:29.760 --> 0:41:31.840
<v Speaker 1>very different from the rest of the universe. Like, we

0:41:31.880 --> 0:41:35.000
<v Speaker 1>know that there's a huge gravitational well that we are sitting,

0:41:35.000 --> 0:41:37.480
<v Speaker 1>and that's why there's a galaxy right here, there's a

0:41:37.520 --> 0:41:39.960
<v Speaker 1>big blob of dark matter. What does it look like

0:41:40.080 --> 0:41:43.719
<v Speaker 1>between our galaxy and Andromeda? You know, are there strands

0:41:43.800 --> 0:41:46.680
<v Speaker 1>of dark matter? How quickly does it pete route? Are

0:41:46.719 --> 0:41:49.280
<v Speaker 1>there blobs of dark matter out there without any stars

0:41:49.280 --> 0:41:51.480
<v Speaker 1>in them at all? And so one way we can

0:41:51.520 --> 0:41:53.600
<v Speaker 1>try to figure that out is to look at how

0:41:53.719 --> 0:41:57.399
<v Speaker 1>light from distant galaxies is distorted as it passes through

0:41:57.400 --> 0:42:01.520
<v Speaker 1>that space. I see, based can do the gravitational lensing

0:42:01.520 --> 0:42:04.760
<v Speaker 1>but with galaxies and look for blobs in between galaxy.

0:42:04.800 --> 0:42:06.839
<v Speaker 1>But then these blobs we got to be humongous, right,

0:42:06.880 --> 0:42:09.400
<v Speaker 1>those blobs would have to be humongous. And in this

0:42:09.440 --> 0:42:12.239
<v Speaker 1>case we use a slightly different technique than we do

0:42:12.320 --> 0:42:15.279
<v Speaker 1>for looking at like one specific blob before. What we

0:42:15.280 --> 0:42:18.000
<v Speaker 1>were doing is called strong lensing, And that's like, I

0:42:18.040 --> 0:42:20.400
<v Speaker 1>want to have a blob of dark matter right between

0:42:20.400 --> 0:42:22.400
<v Speaker 1>me and another galaxy, so I can see like a

0:42:22.520 --> 0:42:25.920
<v Speaker 1>massive distortion. You can see one galaxy how it's distorted,

0:42:25.920 --> 0:42:28.200
<v Speaker 1>and you can use that to measure the massive stuff

0:42:28.200 --> 0:42:30.680
<v Speaker 1>between you and other galaxies. If instead you think the

0:42:30.719 --> 0:42:33.080
<v Speaker 1>dark matter is sort of spread out, so it doesn't

0:42:33.160 --> 0:42:37.200
<v Speaker 1>really distort any individual photon that much. You can do

0:42:37.239 --> 0:42:41.000
<v Speaker 1>something called weak gravitational lensing where you look at lots

0:42:41.040 --> 0:42:43.920
<v Speaker 1>of galaxies and you look for lots of very small

0:42:44.000 --> 0:42:47.080
<v Speaker 1>distortions and you sort of add them up statistically to

0:42:47.120 --> 0:42:49.440
<v Speaker 1>get a map for where the dark matter might be

0:42:49.520 --> 0:42:52.000
<v Speaker 1>and where it might not be. So you see sort

0:42:52.000 --> 0:42:55.920
<v Speaker 1>of like fewer generalized distortions over here and more generalized

0:42:55.960 --> 0:42:58.720
<v Speaker 1>distortions over there. It can tell you sort of where

0:42:58.760 --> 0:43:02.080
<v Speaker 1>the dark matter is dens or and where it's less dense. Interesting,

0:43:02.120 --> 0:43:05.360
<v Speaker 1>you started looking for sort of wiggles in the overall picture.

0:43:05.560 --> 0:43:07.720
<v Speaker 1>But how would you know that is dark matter? Would

0:43:07.719 --> 0:43:10.040
<v Speaker 1>that be changing? Are you assuming that it changes as

0:43:10.080 --> 0:43:12.360
<v Speaker 1>our view of the universe changes. Well, we think we

0:43:12.440 --> 0:43:15.040
<v Speaker 1>know what galaxies should look like when they're not distorted,

0:43:15.280 --> 0:43:18.960
<v Speaker 1>and so we compare how galaxies look too ideas of

0:43:19.000 --> 0:43:21.120
<v Speaker 1>how a galaxy should look when it's not distorted, and

0:43:21.160 --> 0:43:24.200
<v Speaker 1>how it should look when it's slightly distorted by dark matter.

0:43:24.520 --> 0:43:27.160
<v Speaker 1>And so we can use that to estimate like how

0:43:27.239 --> 0:43:30.719
<v Speaker 1>much distortion galaxies have. But it's very very weak. You know,

0:43:30.760 --> 0:43:32.920
<v Speaker 1>it's hard to tell the difference between a galaxy that's

0:43:32.960 --> 0:43:35.920
<v Speaker 1>undistorted and slightly distorted. And that's why we need like

0:43:36.040 --> 0:43:39.000
<v Speaker 1>thousands of galaxies to add this up statistically to get

0:43:39.000 --> 0:43:41.440
<v Speaker 1>a sense for where the dark matter is interesting. And

0:43:41.480 --> 0:43:43.640
<v Speaker 1>this is like an ongoing thing, right, Like there's people

0:43:44.040 --> 0:43:47.040
<v Speaker 1>looking for these ripples in our view of the universe. Yeah,

0:43:47.120 --> 0:43:49.760
<v Speaker 1>this is recent. Actually there's a program using a huge

0:43:49.800 --> 0:43:53.719
<v Speaker 1>telescope with a massive camera five hundred and seventy megapixels.

0:43:53.719 --> 0:43:56.640
<v Speaker 1>It's called the Dark Energy Survey, and this camera is

0:43:56.680 --> 0:43:59.560
<v Speaker 1>basically build just to do this, just to look at

0:43:59.600 --> 0:44:02.440
<v Speaker 1>all the galaxies and build a huge map. And they've

0:44:02.440 --> 0:44:06.200
<v Speaker 1>studied a hundred million galaxies out there, like think about

0:44:06.200 --> 0:44:09.520
<v Speaker 1>all the crazy stars and planets and everything that's out there,

0:44:09.520 --> 0:44:12.359
<v Speaker 1>a hundred million of those. And they have built a

0:44:12.400 --> 0:44:15.520
<v Speaker 1>map of where they think the dark matter is between

0:44:15.719 --> 0:44:19.000
<v Speaker 1>galaxies using this weak lensing idea. Because I guess we

0:44:19.040 --> 0:44:21.359
<v Speaker 1>can tell how old they are the galaxies, right, and

0:44:21.400 --> 0:44:23.279
<v Speaker 1>how far away they are from from us, not just

0:44:23.360 --> 0:44:25.080
<v Speaker 1>in the night sky, and so we can build the

0:44:25.239 --> 0:44:28.080
<v Speaker 1>three D map right exactly. We know where galaxies are

0:44:28.120 --> 0:44:30.520
<v Speaker 1>because we can look at like Type one A supernova

0:44:30.560 --> 0:44:33.040
<v Speaker 1>within them. We can measure their brightness, and we can

0:44:33.040 --> 0:44:35.319
<v Speaker 1>tell how far away they are based on how bright

0:44:35.360 --> 0:44:38.239
<v Speaker 1>they appear to be here on Earth. So we have

0:44:38.360 --> 0:44:41.080
<v Speaker 1>this incredible three D map of all the galaxies and

0:44:41.080 --> 0:44:43.600
<v Speaker 1>then this thing is taking careful pictures of them to

0:44:43.680 --> 0:44:46.640
<v Speaker 1>try to estimate how much each one is distorted, and

0:44:46.640 --> 0:44:49.160
<v Speaker 1>then it's comparing that to our idea for where we

0:44:49.200 --> 0:44:51.800
<v Speaker 1>think the dark matter should be. We have an idea

0:44:51.840 --> 0:44:53.840
<v Speaker 1>for where we think dark matter should be based on

0:44:53.880 --> 0:44:56.759
<v Speaker 1>where all the galaxies are. Sort of back that up

0:44:56.800 --> 0:44:59.759
<v Speaker 1>to the early universe and say where were the dark

0:44:59.800 --> 0:45:02.319
<v Speaker 1>matter are have to have been in order to make

0:45:02.360 --> 0:45:05.080
<v Speaker 1>these galaxies end up here and that galaxy end up

0:45:05.120 --> 0:45:07.880
<v Speaker 1>there to sort of create the large scale structure that

0:45:07.920 --> 0:45:11.440
<v Speaker 1>we see, because we think that mostly where galaxies ended

0:45:11.520 --> 0:45:14.160
<v Speaker 1>up depends on where dark matter was. So we have

0:45:14.280 --> 0:45:16.359
<v Speaker 1>like a simulation for where we think the dark matter

0:45:16.440 --> 0:45:19.240
<v Speaker 1>should be based on our idea of how it all works.

0:45:19.440 --> 0:45:20.960
<v Speaker 1>And then we go out of measure and build a

0:45:21.000 --> 0:45:23.759
<v Speaker 1>real map of where the dark matter is, and then

0:45:23.920 --> 0:45:26.799
<v Speaker 1>we can compare the two and that's when the fund starts. WHOA,

0:45:26.960 --> 0:45:29.120
<v Speaker 1>So what have we found? Do they match or are

0:45:29.160 --> 0:45:32.600
<v Speaker 1>they very different? They mostly match, like it mostly makes sense.

0:45:32.640 --> 0:45:35.000
<v Speaker 1>The dark matter is mostly where we expect, but there

0:45:35.000 --> 0:45:37.640
<v Speaker 1>are some deviations. It looks like dark matter sort of

0:45:37.680 --> 0:45:40.920
<v Speaker 1>more spread out than we expected. Instead of being in

0:45:40.960 --> 0:45:44.560
<v Speaker 1>these like thin strands between galaxies, it tends to be

0:45:44.760 --> 0:45:47.640
<v Speaker 1>sometimes in places where you don't expect. It's like spread

0:45:47.680 --> 0:45:50.880
<v Speaker 1>out and globbed out more than we expected, more than

0:45:50.880 --> 0:45:54.279
<v Speaker 1>our simulations predict. It's just a few percent compared to

0:45:54.320 --> 0:45:57.480
<v Speaker 1>our predictions, but it's an important deviation. It means that

0:45:57.560 --> 0:45:59.920
<v Speaker 1>like maybe something's going on with that dark matter, or

0:46:00.000 --> 0:46:01.920
<v Speaker 1>maybe dark matter is made out of something weird we

0:46:01.920 --> 0:46:04.680
<v Speaker 1>didn't understand, or maybe we've made a mistake in building

0:46:04.680 --> 0:46:06.719
<v Speaker 1>our map of dark matter. But it's sort of like

0:46:06.800 --> 0:46:09.160
<v Speaker 1>at the edge of science. These are very very recent

0:46:09.200 --> 0:46:14.080
<v Speaker 1>results that dark matter just wants to be alone between

0:46:14.080 --> 0:46:16.040
<v Speaker 1>the galaxy or maybe it got timed out. But I

0:46:16.040 --> 0:46:18.760
<v Speaker 1>guess what's surprising is that there is dark matter between

0:46:18.800 --> 0:46:22.399
<v Speaker 1>galaxies because there's not much matter out there, so why

0:46:22.400 --> 0:46:26.360
<v Speaker 1>wouldn't this dark matter also accumulate regular matter. There is

0:46:26.400 --> 0:46:28.640
<v Speaker 1>actually a good bit of regular matter out there is

0:46:28.680 --> 0:46:31.400
<v Speaker 1>it's just not glowing like a huge amount of the

0:46:31.640 --> 0:46:34.880
<v Speaker 1>atoms in the universe are actually between galaxies and this

0:46:35.080 --> 0:46:39.520
<v Speaker 1>intergalactic matter, these streams of stuff, and so there's a

0:46:39.560 --> 0:46:41.640
<v Speaker 1>good bit of stuff out there. There's just not enough

0:46:41.719 --> 0:46:45.759
<v Speaker 1>density to form stars and planets and galaxies and all

0:46:45.840 --> 0:46:47.960
<v Speaker 1>kinds of stuff. And so that's why it's not as

0:46:48.040 --> 0:46:51.600
<v Speaker 1>visible because it doesn't glow interesting. But then what what

0:46:51.760 --> 0:46:54.200
<v Speaker 1>make some dark matter have a lot of bright matter

0:46:54.280 --> 0:46:56.960
<v Speaker 1>in it and some nut the denser blobs of dark

0:46:57.000 --> 0:47:00.600
<v Speaker 1>batter did form enough stuff to create galaxies and stars.

0:47:00.760 --> 0:47:04.120
<v Speaker 1>The kind of strands we're talking about between galaxies is

0:47:04.120 --> 0:47:06.440
<v Speaker 1>a smaller fraction of the amount of dark matter. The

0:47:06.480 --> 0:47:09.560
<v Speaker 1>density is not there in order to create the gravitational Well,

0:47:09.600 --> 0:47:13.080
<v Speaker 1>you need to attract enough hydrogen to get stars to form.

0:47:13.600 --> 0:47:16.360
<v Speaker 1>Pretty cool, so the galaxy still show you where like

0:47:16.400 --> 0:47:19.200
<v Speaker 1>the densest blobs of dark matter are in the universe,

0:47:19.480 --> 0:47:23.600
<v Speaker 1>Like the dark matter also various in density out there. Absolutely, yeah, alright,

0:47:23.600 --> 0:47:25.160
<v Speaker 1>well it sort of sounds like do you sort of

0:47:25.200 --> 0:47:27.759
<v Speaker 1>know where dark matter is but maybe not too super

0:47:27.840 --> 0:47:30.920
<v Speaker 1>high resolution where you can tell if it's super clumpy

0:47:31.040 --> 0:47:34.279
<v Speaker 1>or super smooth. And also we have a pretty good

0:47:34.280 --> 0:47:36.879
<v Speaker 1>picture of where it is in the whole universe. Yeah,

0:47:36.920 --> 0:47:39.560
<v Speaker 1>and scientists are working very hard to build more and

0:47:39.600 --> 0:47:43.240
<v Speaker 1>more sensitive tools to try to use these little gravitational

0:47:43.280 --> 0:47:46.560
<v Speaker 1>clues to build as accurate and as localized a map

0:47:46.600 --> 0:47:49.400
<v Speaker 1>of dark matter as possible, because the better map of

0:47:49.480 --> 0:47:51.759
<v Speaker 1>dark matter we get in our galaxy, the more we

0:47:51.800 --> 0:47:54.279
<v Speaker 1>can study what it might be and how it came

0:47:54.320 --> 0:47:56.960
<v Speaker 1>to be where it is. Yeah. I guess the big

0:47:57.040 --> 0:47:58.560
<v Speaker 1>question now is what are you gonna do when you

0:47:58.560 --> 0:48:03.600
<v Speaker 1>find it? Daniel retire. Yeah, like the dog that finally

0:48:03.600 --> 0:48:05.400
<v Speaker 1>catches up the car and doesn't know what to do

0:48:05.440 --> 0:48:07.879
<v Speaker 1>with it. Oh, we'll find some other mystery to focus on.

0:48:08.080 --> 0:48:11.080
<v Speaker 1>You'll come up with another cool name darkest. We always

0:48:11.120 --> 0:48:13.960
<v Speaker 1>have the seventy of the universe called dark energy that

0:48:14.000 --> 0:48:17.640
<v Speaker 1>we haven't even gotten started on. Yeah, that's another huge mystery,

0:48:17.760 --> 0:48:20.279
<v Speaker 1>huge hole in our view of the universe and them.

0:48:20.320 --> 0:48:22.319
<v Speaker 1>Hopefully you won't lose your mind trying to find them.

0:48:22.520 --> 0:48:27.000
<v Speaker 1>I lost eight years ago. All right, Well, another awesome

0:48:27.000 --> 0:48:29.000
<v Speaker 1>reminder that there's still a lot of universe out there

0:48:29.000 --> 0:48:31.759
<v Speaker 1>to be discoverned. You know, anyone listening to this could

0:48:31.800 --> 0:48:33.880
<v Speaker 1>be the person that comes up with the next great

0:48:33.920 --> 0:48:37.440
<v Speaker 1>idea or the next grade concept that makes sense of

0:48:37.480 --> 0:48:39.719
<v Speaker 1>all this and helps us find these big mysteries in

0:48:39.760 --> 0:48:42.279
<v Speaker 1>the universe. If you're in trance by the concept of

0:48:42.360 --> 0:48:45.319
<v Speaker 1>building maps and discovering the way the world is and

0:48:45.360 --> 0:48:48.760
<v Speaker 1>how everything looks. Remember, the biggest map of the most

0:48:48.800 --> 0:48:51.799
<v Speaker 1>important stuff in the universe is still being drawn. You

0:48:51.800 --> 0:48:54.600
<v Speaker 1>can really lose yourself in that search for lost things.

0:48:54.800 --> 0:48:57.839
<v Speaker 1>Come join me in the asylum or the basement Lost

0:48:57.840 --> 0:49:00.759
<v Speaker 1>and Found department. Well, if they for joining us, we

0:49:00.800 --> 0:49:11.880
<v Speaker 1>hope you enjoyed that. See you next time. Thanks for listening,

0:49:11.880 --> 0:49:14.600
<v Speaker 1>and remember that Daniel and Jorge explained. The Universe is

0:49:14.640 --> 0:49:18.160
<v Speaker 1>a production of I Heart Radio. Or more podcast from

0:49:18.160 --> 0:49:21.920
<v Speaker 1>my Heart Radio visit the I Heart Radio app, Apple Podcasts,

0:49:22.040 --> 0:49:24.400
<v Speaker 1>or wherever you listen to your favorite shows.