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um so i know a lot of you were at

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abradcon last year and a lot of you

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weren't anyone who wasn't um my name's

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alyssa i work with ralph padres who's

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the director of the origins institute at

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mcmaster university

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and he started this institute

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specifically to look at the origins of

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life um on planets and origins of stars

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on the universe and origins of stellar

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systems

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all things sorry thank you

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they're gonna go away okay

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um so it's a really big deal just in

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terms of origins of life so my work

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specifically has to do with seeding life

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on exoplanets so i look um mostly at

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amino acid

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concentrations on meteorites and how

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those might be produced within

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meteoritic parent bodies and then

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transferred to exoplanets by these

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meteoritic impacts

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i did not include

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a plot of what i did last year

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i will just describe it in just a second

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just for for background knowledge so

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anyway the point of what i do

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um i'm looking at the synthesis of the

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amino acids in the parent bodies

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meteoritic parent bodies um i look at

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the concentrations and study the theory

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behind how those amino acids got there

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and the whole point of why we even

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started doing this research is because

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we know that there are biomolecules

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present in meteorites and that you know

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when we go to antarctica or wherever and

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pick up those meteorites we have all the

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biomolecules in them but there are also

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i mean there's evidence for some of

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those amino acids being extraterrestrial

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in origin so it's not that their

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terrestrial contamination they really

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were created in space and brought to

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earth by these meteorites

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and again this is just the theory for

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how life

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starts on planets

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so the big picture of what i'm trying to

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do

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um is actually model the synthesis so

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i'm using some theoretical amino acid

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synthesis equations and being like look

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let's use the computer and if we put in

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this amino acid equation let's see if we

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can match the amino acid concentrations

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that we see in observed meteorites that

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we pick up off the ground

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so the first part of my project which is

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what i was doing last year was just

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trying to find all of the meteoritic

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abundance data because there's a lot of

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it out there i mean we've known for ages

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there are amino acids in these

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meteorites but there's a lot of data to

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collate to be able to to verify that

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when i'm modeling my amino acid

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abundances i'm actually matching what

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we're really seeing so the second second

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part which is what i've started just

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recently is actually doing the modeling

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so now i have something to aim for i

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have my concentrations that i know and

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now i'm changing the dials on my model

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to try to recreate those abundances that

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we get out

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i wish i had brought it yeah i didn't

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bring it um

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so last year what i was doing was

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looking at how the concentrations of

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these amino acids change with gibbs free

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energy so gibbs free energy is just a

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measure of

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how how spontaneous a reaction is it's

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how much the reaction wants to occur and

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what happened last year pretend on this

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screen that i have a

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um just like an exponential decrease on

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a graph and this side is concentration

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of amino acid and this side is gibbs

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free energy increasing gibbs free energy

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and the relationship that i got out of

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my data last year was that you have

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more amino acids being created with an

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increase in gibbs free energy which is

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exactly the pattern that we would expect

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to see

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but now given that relationship

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i've come back through all my data

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um

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oh i was going to talk about meteorites

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i kind of just skipped a slide let's

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pretend that didn't happen meteorites

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which have been mentioned um there's a

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whole lot of meteorites i don't look at

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most of them about four percent of

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meteorite falls or something called um

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these carbonaceous chondrites that i

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look at that's this green column here on

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the left and these the cmci cr cvs also

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the cos

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and

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working on new data the the cbs

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um have an extremely high content of for

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all meteorites they have an extremely

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high content of biomolecules and of

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water so these are really the meteorite

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classes that we want to look at when

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we're looking for amino acids

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and in addition to these letters which

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describe the different meteorite types

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they also fall into a petrologic class

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and this this the chart down here on the

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bottom just tells you roughly how

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altered these meteorites are so in the

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temperature range which i look at is

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between about 150 and 200 degrees c

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which is right in here and that

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corresponds to the meteorite classes

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mostly cm and c2 so i tend to stay

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within the cmc2 class of meteorites

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this goes back to the data so this is

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what i have spent an entire year doing

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no one likes looking at tables i have a

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table that takes 12 pages to print just

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full of amino acid abundance data didn't

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want to show you that so instead here's

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at least a graph with colors on it

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these are just the cm meteorites

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everything along the x-axis is a

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different sample of meteorites and along

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the y-axis is just concentration so

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that's parts per billion of amino acid

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in whatever meteorite and then all the

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different lines are the different amino

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acid types

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so generically glycine is one of the

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most common and easiest to form amino

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acids that we see

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so it's this dark blue line that's

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mostly towards the top and then you get

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some variation but in general kind of

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the the pattern to see from the cms is

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that you have fairly high concentrations

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in here you know you have 10 to the 3

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and 10 to the four concentrations of all

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these amino acids

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as opposed to something like this we

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have fewer fewer ci meteorites but you

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know now we're down you know 10 to the 3

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10 to the two range for the ci type

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meteorites

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cos again

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crs are interesting classically cms are

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supposed to be the meteorites that have

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the the greatest biomolecule

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concentrations in there but there are a

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couple of exceptions and those

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exceptions all are within the cr class

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of meteorites you see these guys

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these guys here have up into the 10 to

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the 5 10 to the 6 parts per billion

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concentrations of amino acids

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and that doesn't mean anything well i'm

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sorry that's not what i meant it means

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stuff on its own not to me it's

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important to me because that means when

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i try to do my modeling i can't just

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match something according to an order of

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magnitude now i have it gets into

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variation you know over multiple orders

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of magnitude which is just hard to do

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computationally

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oh and cvs more meteorites lots of

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meteorites

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this is

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probably um

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this is my baby this is a year's worth

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of work in one plot

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i don't get pretty pictures like a lot

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of

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total average amino acid concentration

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so each different color each column is a

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different amino acid and they've been

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averaged and totaled over the different

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meteorite classes and petrologic types

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so this is very broken down according to

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the pressure and the temperature

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involved in making these meteorites and

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what you see is exactly what we saw in

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the earlier pattern you have the cm2 and

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the cr2s that have orders of magnitude

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more concentration of amino acids than

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something like the ci's you know the

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petrologic type ones and the cvs and the

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cos

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so that's just reassuring

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um after we have that data what we need

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to do is convert it because parts per

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billion is useful to the observers

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um but when it comes out of my computer

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it doesn't happen in parts per billion i

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get data that um

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doesn't look like that so this graph is

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just showing you

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specifically i'm relating all of the

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concentrations in this graph i'm now

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just dividing them by the concentration

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of glycine so that we have a plot

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relative to glycine in this image

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this is specifically for the cm type

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meteorites and this for the crs

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and again the takeaway message for here

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is that

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with some exceptions you classically

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have like six or so amino acids that

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really are the amino acids that stand

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out for being present in uh in

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meteorites so we have a lot of a lot of

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glycine a lot of alanine usually we have

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more serine aspartic acid glutamic acid

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and valine are kind of the main

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things

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um

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it doesn't look like it i know they're

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not really exciting pictures but that

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was a lot of work it was a lot of work

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so the point is now i have

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concentrations and i know what i'm

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looking for um so now we come back and

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do this which is what i'm working on

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just now

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um

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this is done with a program called chem

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app chem app

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is

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gibbs free energy of a system that you

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input so i can take chemap and i say hey

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i want you to consider all of these

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reactants so we use something called

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strecker synthesis to model the reaction

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of or the the synthesis amino acid so we

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input hcn and ammonia and water and some

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aldehydes and what we hope to get out

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are

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relative concentrations of these six

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amino acids uh relative to the glycine

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that match the observed abundances

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and you can see that's actually working

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pretty well

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yay um

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so sorry observed is in the red on the

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the left side of each of these bars

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the red is observed abundances of some

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amino acid and the green on the right

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side is simulated so that's what's

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coming out of my of my model and you can

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see that easily to within

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roughly an order of magnitude i'm

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actually getting out concentrations that

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agree with observed values of amino

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acids for um

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for

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yeah

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i totally just lost my train of thought

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sorry where it's working it's working

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yay is the point

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um

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so matching matching amino acid

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abundances yay and i'm done and i'm

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actually on time um ralph my supervisor

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undergraduate help darren yay

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thanks i'm done

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over here sure just a quick one um why

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are you normalizing it to like why

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glycine um i couldn't give you an exact

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answer because classically people who

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have looked at amino acids on meteorites

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normalize everything to glycine it's

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just kind of historical yeah it's just

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people have done that for

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as long as i like standard mean ocean

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water yeah okay that's just what um

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convention is the word that i want it's

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just convention by now

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good question though i wondered the same

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thing i never found out

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uh if i could i'd like to add to that

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comment um

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normalization to glycine occurs because

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it's the simplest amino acid so it makes

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sense to normalize to the one that's

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easiest to make

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i have a question about

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your striker synthesis simulation so

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i want to make sure i didn't

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misinterpret what you said did you say

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that you

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put aldehydes into your

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strecker model synthesis

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that should be formed by the striker

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synthesis yes we are only considering

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striker synthesis that begins with the

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aldehydes we are not doing formation of

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aldehydes in our model because it gets

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too complicated we have too many

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variables if we include everything that

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also is needed to make the aldehydes but

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because we have detected aldehydes in

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comets and meteorites and stuff like

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this we're assuming that they're there

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so in our model it is very much assuming

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an unnecessary amount of

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of aldehydes that are already in the

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system these are the amino acids we

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would produce

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okay so

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you're considering striker synthesis

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starting from the aldehyde yes

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but strecker synthesis makes the

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aldehyde stricter synthesis makes the

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amino acids

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right so the the aldehydes form first

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then that's protonated and you get the

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amino acid

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but the aldehyde is formed with in the

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presence of ammonia and hcn like you

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mentioned yes so that's the precursor

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that's formed during striker synthesis

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yes so are you're simulating the latter

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half of the strike so not the entire

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striker synthesis process no we're not

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doing formation valve heights we're

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saying given aldehydes because once you

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have an aldehyde you react again with

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the hcn and the ammonia and the other

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things and what comes out the far end is

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an amino acid that's it's very no one's

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ever done this before and you i can't

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include all the parameters in this model

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right off the bat it's impossible so

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we're for now looking specifically at

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amino acid concentrations and trying to

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all right so also in your synthetic

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model you're only using like a normal um

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well

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aldehydes and those sort of things do

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you have any of the exotic charge

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species that you see in dusk screen

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formations or the meteorites to take

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into account some of those or is it just

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the basic striker synthesis model it's

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again mostly basic because this research

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is so new we have another summer student

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right now who's looking at ketones and

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carboxylic acids and we're trying to get

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other data outside of just the

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meteorites that we have but from my

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project which because no one's done this

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before it's very much limited to this

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set of meteorites and just like half a

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dozen aldehydes

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all right yeah it's it both of your

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points are very valid and that's future

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work that we would like to do it's just

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because we haven't had

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a chance yet

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hi alyssa thank you that was very nice

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talk um i wanted to comment on the one

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slide that you showed the different

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classes of meteorites it looked like

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two of the classes that were in the

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center that had more the red orangey

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colors oh go back

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whoa back

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sorry you just passed it oh this one yes

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that one so cm2 and cr2 it looks like

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the the orange and reds are more

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hydrophobic amino acids i was wondering

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if you could comment on the significance

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of that compared to the other classes

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is there one

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um i am not a chemist

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um i'm sure there is we've had um some

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other people that are interested in this

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work that want to look more at some

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specific chemical

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behaviors of these amino acids

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i can absolutely not comment on that

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sorry um people are looking at you know

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hydrophobicity and

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electron stuff stuff and how conductive

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they are and all these other things and

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i'm like yeah sure you know

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so they do that i have no idea