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alright great well I'm really excited to

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be following these talks because last

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few have concentrated on prebiotic

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chemistry in the early Earth and I want

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to go even earlier about this early in

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the formation of the earth so when I

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think about the life cycle I think on a

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more cosmic scale where we start with a

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protoplanetary nebula here which

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eventually as a star turns on collapses

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down to form a protoplanetary disk thin

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that disk you get condensation of dust

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grains and Isis into larger bodies

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comets asteroids planetesimals and

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eventually planets and then on those

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planets you eventually get the impact of

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a lot of the leftover comets and

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asteroids and at some point in this life

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cycle life is formed and then is

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destroyed in a fiery explosion and

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returned back into the cosmic lifecycle

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so we've heard a lot about getting life

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from say amino acids as a starting

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material and we all know that amino

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acids are found in comets from the start

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up mission or meteoritic samples but

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what we don't know in my field

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astrochemistry is how the heck those

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things got there in the first place

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there's been a lot of theories but

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there's no proof definitive proof of how

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those amino acids glycine being that the

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simplest and most abundant one we found

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got their start with so I'm interested

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in exactly where in this cycle from the

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protoplanetary nebula to even impact on

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the planet did glycine form that it

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formed the gas phase one of these two

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phases did it form in the icy surfaces

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of dust grains anywhere along this path

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or did you have to wait until you're in

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the bulk ice on comets or even there's

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been some theoretical papers that say if

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you smash a comment into the earth the

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heat of that impact can drive the

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formation of a whole bunch of organic

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molecules so last year I presented on

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the search for a molecule called

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hydroxylamine here n h 2o h and this was

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kind of the last gasp for trying to form

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glycine in the gas phase

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this reaction with acetic acid which is

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very abundant in the interstellar medium

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directly forms glycine and NH 2 H was

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predicted by us for chemical models to

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be quite abundant but as it turned out

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we couldn't find it at all in fact our

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upper limits were about a million times

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less than what was predicted by the

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theories and then some very recent

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theoretical work has said this reaction

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has a reaction berry and won't go in the

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gas phase in the is M anyways so that

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kind of Nyx's the formation of glycine

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in the gas phase as long as as far as

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we're concerned so that leaves us with

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the solid phase and just about four

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months ago a very talented astro

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chemical modeller Rob Garrard use a

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complex gas grain reaction Network to

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see if he could form glycine in the icy

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mantels of dust grains and in fact he

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finds yeah we can form it and then we

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can actually pop it off from those dust

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grains into the gas phase and use Alma

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our most sensitive radio telescope to

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detect it there's the signal the

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strongest signal from glycine towards a

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nearby star forming region that's really

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cool but the accuracy of these gas grain

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chemical networks relies necessarily on

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how well we know the starting parameters

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what's available to work within these

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Isis how much is there there of it and

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what's the temperature of these

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molecules and the problem is in Isis we

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know very little about what's actually

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there we think we know a lot but we have

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very little proof this is a list of

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detected molecules in Isis we know about

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a hundred and seventy or so molecules in

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the interstellar medium the ones that

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aren't in brackets are the only ones

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that are confirmed to be a nice as the

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ones in brackets we think we see what

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we're not certain and these are the

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major ice constituents you see here are

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actually quite simple molecules and the

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reason we're having so much trouble is

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because these observations are being

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done in the infrared the infrared is

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great for getting simple abundant

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molecules but it suffers a bit for a few

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reasons you have to do all of your

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observations in absorption for the most

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part which means that the ice that

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you're looking at behind it on a direct

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line of sight to us has to be a really

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bright source to absorb against that's

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usually a star and that really limits

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the number of places we can go looking

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for so our sample size is low too

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art with and the features in the

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infrared are usually broad and they

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blend together in these Isis and you

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really have to have an abundant molecule

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with distinct features to pick them out

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if you want to look in a mission that

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would be cool you wouldn't have to have

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a background star but the problem is if

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you want to fall on the part of the

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blackbody radiation curve where you can

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actually get light out of the grains in

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a detectable amount the grains have to

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be so hot that you can't have ice on

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them in the first place the other

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problem is the clouds that you're

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emitting from have such a high optical

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depth those photons just can't escape

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first part so you're kind of screwed for

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a mission and in the laboratory you're

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in directly measuring the optical

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constants that's n the index of

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refraction k the amount of absorption

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you get through here and these are

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really important for modelers who are

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looking at radiative transfer so how

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light gets through different layers of

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Isis say and unfortunately in directly

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measuring these in the infrared produces

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errors and those errors propagate

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through and make these calculations a

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little wishy-washy so what I want to do

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is see if we can get a little bit better

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by looking in the terahertz region of

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the spectrum so my background is in

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laboratory microwave spectroscopy and

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submillimetre spectroscopy and in space

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astronomical observations in absorption

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you don't need a background star to

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absorb in the terahertz the black and

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grey body radiation coming off of dust

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is sufficiently you can just absorb

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against the background continuum so we

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can look at a whole lot more place as a

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wider sample set and there might

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actually be some narrower features here

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and the terahertz features tend to be a

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little more distinct spectrally we can

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also look at a mission because the

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blackbody curve allows us to have colder

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ice grains that are emitting photons

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that we can see especially since there's

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a lower optical depth in the terahertz

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so they have a better chance of reaching

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us so we can look at their signals and

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we can also directly measure the optical

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constants so we get are so much higher

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accuracy and the terahertz so what's our

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experimental tech what's been done in

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the terahertz so far experimentally well

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some people have tried to cheat they

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take a Fourier transform infrared

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spectrometer and push it out of spec and

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then get all the way down to about three

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terahertz which is pretty good

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and they have fairly decent resolution

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about one wave number but you're still

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in directly measuring the optical

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constants and the work done so far has

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been largely on these known interstellar

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molecules so water methanol ammonia

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simple things that we already know are

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there so what we want to do is see if we

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can look at some more interesting

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molecules that we think have to be in

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these Isis to form glycine but we're not

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certain so we take a silicon substrate

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ins few millimeters thick and cool it

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down to between 10 and 150 Kelvin and an

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evacuated healing cryostat we spray gas

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phase molecules at it and they freeze

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into a layer of ice so this is a really

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simple technique and then we can shoot

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radiation through it so we have our own

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ftir here for diagnostic purposes and

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then we can shoot terahertz through the

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other way and we detect these signals

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and transfer them to absorption spectra

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so here's a layout of the actual

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spectrometer we have our silicon

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substrate here in our cryo set our ftir

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gets bounced in the way we generate our

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terahertz is actually really cool we

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take a really high-powered laser

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operating at 800 nanometers we frequency

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double some of the light so we have two

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colors of light going into our nitrogen

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purge box and then we focus it down if

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you focus it right it turns into a

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plasma in air it looks like a little

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miniature Sun and it's the oscillation

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of electrons back and forth in this

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plasma that emits a very broad very

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intense burst of terahertz radiation so

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we take that focus it through the sample

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and then detect it on the other side

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using what's called electro-optical

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rectification which is a really cool

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technique that I don't have time to talk

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about suffice it to say what it does is

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it directly measures the electric field

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of our pulse that's how we can get these

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optical constants out directly we don't

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have to do any Kramer's chromate kroenig

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analyses or other assumptions get these

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optical constants out right now we can

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cover from about 300 gigahertz to 7.5

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terahertz at modest resolution within

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the next few months we know we can get

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ourselves probably up to about 20

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terahertz in broadband but

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and down to about a factor of 10 better

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and resolution so this is what we've

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looked at so far we've had our

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instrument operating for about a little

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over a month at this level of efficiency

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we've done the simple Isis so far as

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well as methyl formate here which is a

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very well-known interstellar weed in a

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more complex molecule and we've also

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started to do some mixtures and I think

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my labmates back home have actually run

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a few more mixtures while I've been here

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so I'm just going to show you results

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from to hear the simplest and the most

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complex pure species we've run because

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their spectra they're cool to look at

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but they're all going to look kind of

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the same if I show you everything we've

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done so here's water the most abundant

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interstellar ice and what we have here

253
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are just three different thicknesses so

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we started putting down ice and we

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gradually increase the thickness and

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kept taking absorption spectra from

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about 300 gigahertz up to seven and a

258
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half terahertz and you can see here

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these nice distinct absorption features

260
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are growing in right out in the

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terahertz region that we're interested

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in it we can also tell the difference in

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the structure of the ice so if you

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00:10:05,369 --> 00:10:03,819
deposit at a higher temperature there's

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energy for these molecules to move

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around and get into a formation that

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they like kristalyn if you deposit at a

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lower temperature say down at 10 Kelvin

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here they just stick in whatever way

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that they actually hit the ice and they

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they form an or morphus solid so you can

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see the difference in sharp distinct

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features versus a just kind of blobby

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thing here and the formation of this ice

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the weather its crystalline or amorphous

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is a big question in an astro chemistry

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right now it has a big impact on the way

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the molecules move around inside the ice

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to react the matrix that they have to

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work with so here's methyl formate it's

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the poster child for grain surface

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chemistry in the is em as far as we know

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we can't form this in the gas phase at

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all there's a whole whopping ton of it

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out there it pollutes our spector all

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the time and it has to be formed on the

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grain surfaces despite that there's no

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definitive detection of it or gneisses

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so if we can do that that would be

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fantastic and it's rather complex

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structure so maybe we can see some

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interesting features from it and the

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terahertz the same kind of plot we're

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just making the ice thicker and thicker

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as it grows in you can see here we got

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actually a lot more structure to the

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spectrum than we had in water and in

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different places which is fantastic for

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distinguishing things we can also look

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at crystal and versus amorphous again

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and you see here we're excited really

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excited about this spectra because these

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seem to be very sharp very distinct

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features even at low resolution so if

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you can imagine ten times better

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resolution on this and a couple months

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we think we're going to get some really

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interesting features here so where are

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we going next with this well we want to

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compare to the Herschel data archive and

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the spectra that are coming off of the

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almost science verification data these

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operate real near are interested

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frequency range these are

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state-of-the-art facilities and the data

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is all publicly available within the

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next year or two which would be

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fantastic ideally we'd like to operate

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with Sofia the Fifi instrument exactly

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mimics our frequency range and about the

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same resolution which would be fantastic

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but it hasn't come online yet science

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testing is just coming up for this new

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proposal cycle and they're offering

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seven and a half hours of which we're

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going to get none so we're going to have

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to wait a year to look at that but we're

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really excited because even these

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preliminary results show that we should

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be able to identify some more complex

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molecules and get a better understanding

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of what we have to work with to make

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glycine and other amino acids not on

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earth but before we got here with that

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sources of funding and acknowledgments

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and thank you for your attention all

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are you planning to propose of your

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observations for the next cycle or do

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you want to wait for working and

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commissioning Oh Fifi yeah we're gonna

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have to wait for the commissioning and

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safety to go online the great instrument

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theoretically covers a good frequency

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range but the windows they're offering

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are so small they cover maybe one or two

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of our resolution elements right now so

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it's just not a broadband enough system

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we'd love to use Fifi but we don't think

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we have a shot at seven and a half hours

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so I realize this is an incredibly long

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shot but what are the prospects if any

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for eventually ever detecting a chiral

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signature in this glycine or anything

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like that ah well I don't I don't know

355
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what how much to give away here there

356
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are there have been reports mumblings

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among my colleagues of some possible

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detection of some tyrol molecules most

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of these are just single line detection

360
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right now so that's just one spectral

361
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feature not enough to definitively

362
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identify anything but i would say

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especially with Alma coming online fully

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within the next year or so and we should

365
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we should see some detection of chiral

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molecules shortly I think awesome thank

367
00:14:28,340 --> 00:14:24,810
you yeah just to follow up can you there

368
00:14:30,530 --> 00:14:28,350
any ice topic ratio so you can go can we

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00:14:34,580 --> 00:14:30,540
get isotopic ratios uh yeah absolutely

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um so I mean we pick up h2d ratios all

371
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the time and that's actually how we're

372
00:14:41,360 --> 00:14:40,080
trying not us but Astra chemical

373
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modelers are trying to understand the

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infall of water to former assoc from the

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different parts of forming

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protoplanetary disks carbon-12 carbon-13

377
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ratios are easy to pick up from carbon

378
00:14:59,480 --> 00:14:54,300
monoxide measurements as well as oxygen

379
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18 17 ratios yeah all right well if

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that's it can we give a hand for all