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all right Thank You Brett and thank you

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to the AB grad Con organizers this has

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been rfg was a lot of fun and I'm

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looking forward to the rest of AB grad

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con so I'd like to really talk to you

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about complex molecule formation and

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terahertz spectroscopy and really this

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is all about Astra chemistry so Brett

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gave a really great warm up talk so I

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think you guys actually have a lot of

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the basics actually he stoled a lot of

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my thunder so what I'm going to really

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tell you about is the importance of

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molecules really we think in how life

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came to exist on this planet so we've

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just heard a bit about protoplanetary

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disks so this is a artists cartoon of

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one when you go from say a

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protoplanetary disc to a solar system we

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understand pretty well the role that

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molecules play but what was less clear

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is if you have a solar system and a

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solar system like ours we know we have

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life right so really one of the

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important questions in Astro chemistry

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is how do you go from a solar system to

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a solar system with life and really

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we're encouraged that we can learn

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something from the chemistry of space

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that will tell us about life on say a

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planet like Earth because of the

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Stardust mission and when we you know we

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know that now that we've seen glycine in

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the cometary tail of the comet that

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Stardust sampled and this gives us

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really a thought that well okay complex

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molecules are forming in space so maybe

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one of the important ways that we

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actually wind up with the precursors of

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life the prebiotic species that we need

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are some complex molecule formation in

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space that is then subsequently

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delivered to a planet and so if we

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really want to then understand complex

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chemistry in space the place that we

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have to think about our icy death

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screens if you remember something about

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chemistry at some point you might have

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or even physics to have three three

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different species come together and all

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hit each other at the same time it's not

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a straightforward process and in the

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case of having them hitting each other

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and then react that's going to be a very

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rare event but if you have say a third

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body like a dust grain that's just

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floating around you can have some

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molecule come down and stick to its

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surface now it's there first

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amount of time if another molecule comes

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down it can diffuse around find it on

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this guy who is sitting there first and

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react over the course of time you and by

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time we're talking about millions of

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years in you know a star-forming system

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you can build up a layer of ice on the

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surface of this dust grain and the

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molecules that are on this surface will

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affect the the subsequent chemistry and

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this is really what we're thinking about

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in our lab so we want to investigate

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Isis and we're going to take we're not

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going to try to actually say we are

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gonna make what's in space no we're

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gonna go simpler we're going to try and

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look at simple things and slowly build

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up into a bigger and bigger picture so

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that we can understand and try to

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disentangle the complex picture that's

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happening in space from laboratory

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experiments and again this is important

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because if you want to make anything

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more complicated than as Brett was

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saying methyl formate or methanol there

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is no way that you can do this in the

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gas phase so we really need to look at

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Isis so in order for me to take you

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there I do have to take you through a

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quick diversion to the electromagnetic

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spectrum and the region that I'm gonna

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be focusing on here is what I call the

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terahertz region or it's often known as

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the far infrared and the reason is the

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far infrared is because you come down

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from the visible and the near IR mid IR

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you hit the far infrared and it's a

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region that really corresponds to low

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energy vibrations and solids long range

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interactions you need lots of molecules

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participating in in order to actually

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see these vibrational modes and it's

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kind of an interesting region because

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historically it's been a difficult place

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to actually make making detect photons

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and so we're excited to be working here

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because there's a lot of new stuff to

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learn the reason why it's important for

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a stroke a mystery however is that

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fundamentally there are things that we

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can learn from terahertz spectroscopy

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that we'll never be able to learn from

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the near infrared so if you take this

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nice picture of an edge on disk as taken

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by the Hubble Space Telescope you can

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see in the middle here it's black and

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that's because even though there is a

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star at the center of this disk that's

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giving off lots of light there's so much

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material it's so dense through that

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section that we don't see any light

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making it to our tell us

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so if we actually have all this stuff

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there and we want to learn something

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about say maybe the colder part of the

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disk

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we'd like there to be some thermal

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excitation of molecules that would then

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emit photons we can detect if we want to

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look at Isis those need to be cold

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temperatures and if you just take a look

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at my math here at the bottom if we're

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looking or at somewhere in the mid

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infrared around you know a thousand wave

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numbers in order to have thermal

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excitation and actually see emission

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from the outer region of the disk the

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disk would have to be around 1400 Kelvin

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there's not going to be any ice at 1400

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Kelvin so we have to go to the terahertz

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and that's why there are things we can

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learn there that we can't learn anywhere

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else so what do I actually do so I have

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a vacuum chamber in my laboratory and

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inside I have a substrate and I can cool

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that substrate all the way down to 10

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Kelvin I can control the temperature

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between 10 Kelvin at about 300 Kelvin

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and I have this little pipe here that is

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connected to a dosing line where I'd

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have a cylinder or some sample of a

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liquid that I'll get in the gas phase

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and I can leak a few molecules into the

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chamber and those molecules will stick

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to the cold surface they'll stick

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everywhere but you know as long as they

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stick to the surface here which is

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actually a silicon substrate I can then

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take spectroscopy of them so so I have

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terahertz pall source that Brandon is

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actually gonna describe in a little more

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detail but it's pretty cool because we

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actually ionize the air in the

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laboratory and make plasma and that's

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actually our terahertz source and so the

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pulse comes in it interacts with the

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sample it gets absorbed by the sample

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sample reom it's a pulse that then we

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detect in our spectrometer so let me

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show you then just some of the spectra

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that we've collected and you can see

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here this is kind of a almost butterfly

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collecting slide but the the purpose of

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it is to show you that different

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molecules really have distinct spectral

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fingerprints in the terahertz region so

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we've got more simple molecules like

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water water and co2

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we've got more complex molecules here

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like acetone and methanol and you can

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see again these features are very

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distinct from

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spectrum to the next which gives us hope

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that we'll be able to actually identify

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different species if they're in a more

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complicated ice now what are some of the

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useful things that we can learn from

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these spectra it's actually oh it would

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be great if we could look at a

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protoplanetary disc and learn something

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about and know with certainty the local

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temperature so if you look at our

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terahertz spectra this is this is carbon

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dioxide ice and I've I've taken spectra

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with the ice health at three different

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temperatures and you can see in the

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inset as I wore as I saw as a cool the

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ice down to colder and colder

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temperatures the the peak of a spectral

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feature actually shifts and this is

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great so this means that now if I if I

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were to actually see something you know

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here versus here I can actually tell you

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what the temperature is and you can do

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this in the laboratory obviously it'll

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be more difficult in space but this is a

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potentially and interesting result so

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what are these vibrations and I just

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really you know have to show you some

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some cartoons from some DFT calculations

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where we've simulated the spectra of

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these of these features and you can see

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here that they really are collective

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motions these are entire planes of of

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co2 molecules in this solid that are

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sliding against each other or in the

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case of the second mode that you saw in

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the spectrum kind of moving with respect

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to one another so really think of these

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as as phonon modes as large long range

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interactions that really require very

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little energy to tweak but and as a

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result they're very very sensitive to

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the structure of the material which

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means they're sensitive to the structure

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that we're going to see really

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interesting differences when we talk

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about mixtures and that's what I have on

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this slide you can see we start off with

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water and I'm going with increasing the

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methanol concentration as I go down the

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slide until I have pure methanol and you

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can see I start with with features

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either the very characteristic features

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here of water this feature really

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actually corresponds to the sort of

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bilayer of a water ice stretching like

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this and and as I as I add methanol this

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feature slowly goes away when I have a

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sort of one-to-one mixture I really have

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this big almost amorphous blob

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as I add more methanol we start to see

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maybe these aren't maybe these are the

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methanol features growing in here and

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then pure methanol is very clear and and

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this is the same spectrum like I had on

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the first light so so one of the really

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bringing this to one more thing that we

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really think is interesting about the

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chemistry of say a place like a

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protoplanetary disk terahertz

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spectroscopy really seems to give us the

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chance to say something maybe about the

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thermal history of an ice and so what do

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I mean by that well everything I've

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shown you so far as a crystalline solid

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so that means when I when I showed you I

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was depositing my ice and I had that

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substrate that I could change the

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temperature I actually kept that

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substrate warmer and the idea is when

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when the substrate is warmer when the

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molecules leak into the chamber and they

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hit the substrate they have enough

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energy to relax and find sort of their

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lowest energy position and in that case

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we're actually going to wind up with a

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nice ordered crystal structure if I

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actually instead of doing that I

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actually kept my substrate colder

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I would actually wind up with an

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amorphous solid because when the

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molecules come in and stick they don't

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have enough energy to reorient they

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can't actually find their lowest energy

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equilibrium position relative to all of

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the other molecules in the solid so we

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wind up with this big amorphous blob and

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if you look again you know this this is

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water and there's this feature here that

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kind of you know maybe if you squint I

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mean it looks like this but it's bigger

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and broader and doesn't have as clean of

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features so we compare you know this

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spectrum taking at 10 Kelvin here with

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this spectrum take it at 10 Kelvin here

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there's an obvious there's an obvious

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difference okay but that's not a thermal

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history effect because I've just these

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are two separate ices but if I take this

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ice and I warm it up so you think if I

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warm something up all the way up to this

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say that the state same temperature at

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which I deposited the first ice it would

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have enough energy to reorient and

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become a crystalline solid in my

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spectrum should look just like this but

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as you can see from this top spectrum

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that's not the case so there is a

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feature that that looks

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like this but it's actually shifted

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relative to this peak and you know

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there's a lot more structure here than

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there is here so one of the things you

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can imagine happening is hey you are in

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a protoplanetary disk and some dust

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grain with some ice on it goes from you

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know colder spot to a warmer spot back

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to a colder spot you might actually be

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able to learn something about the

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history of that dust grain and thus the

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chemistry of what's going on in the disk

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and so with that the take home thoughts

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are really that you know terahertz

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spectroscopy is really sensitive to both

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the structure and a temperature of Isis

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we can just distinguish them with their

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thermal history and when we think that

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this is a this is going to be a useful

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tool to understanding complex molecule

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formation and to bring it all back to

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astrobiology if we can understand

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complex molecule formation

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maybe we can understand how we wind up

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with life on this planet and with that

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I'd like to say my lab mates and my

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advisor at all the people for funding

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and everybody for their attention thank

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questions for Marco Marco thanks for the

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talk so in one slice you show the ratio

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different ratio of the water and the

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methyl whatever the two organics so I'm

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just wondering if you can predict that

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when you get spectrum together I don't

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know if it is proportional four and if

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you can predict the ratio of the water

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to the organics are you saying could I

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could I predict what the spectrum looks

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like I would say that we we could maybe

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try although I think the theory these

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are kind of hard theoretical problems

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because they they do really require a

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picture that involves say what the what

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the unit cell structure looks like of

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say a crystalline material and if it's

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not crystalline it gets even harder so I

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would say it's possible but it's it's

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definitely a hard fioretto problem it's

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it's not one that we've looked at oh oh

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I see what you're saying okay sure the

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answer is yes and but what you'd have to

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do is you we'd have to do you know we'd

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have to have built up a library of

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spectra so they're taking spectra at

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different ratios and then we we would be

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able to figure out then say if we had a

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blank spectrum we didn't know what the

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ratio was we could compare it to our

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laboratory database and go from there