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[Music]

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[Applause]

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I'm gonna tell you about these detection

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that we reported in the paper about year

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and a half ago of methyl chloride in

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particular and the co materia regions

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and also about the ongoing lab work that

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we're doing at JPL to support this

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detection and maybe guide future

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observation to observe more of these

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pieces so first of all why methyl

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halides well these pieces are abundant

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in the atmosphere of the earth so a

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couple of decades ago they were mainly

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found because of industrial processes

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but these days they're actually the the

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main production source is actually for

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biological processes so for example

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metabolizing allergens into the oceans

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by allergies and they will reject our

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gano allergens into the atmosphere and

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due to this connection between biology

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and for these pieces they were proposed

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as potential biomarkers if observed in

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the atmosphere of exoplanets this was

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further supported by the fact that in

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the interstellar medium

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well we actually detect allergens pieces

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but very small ones so HCl HCl plus and

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so on and most of the halogens

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especially for chlorine here is actually

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found in the diffuse interstellar medium

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and noting two molecular clouds were

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star formations happening so the

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question we have is there is there an

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actual disconnect between the allergen

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chemistry and the organic chemistry that

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we see in star forming and plant forming

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environments so to figure this out we

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search for them into purchased of our

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environments and specifically within the

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framework of the pills program but is an

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Alma program so Alma looked at the

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rotation lines towards a low mass

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produced are here for this pills program

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led by yes or Genson so this producer RS

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16 to 9 3 24 22 is actually thought to

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be an analogue of water sun looked like

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when it was forming so we looked at

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rotational lines nearby one of

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sources source be around 16 to 9 free

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and within this large program we

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actually covered a large frequency range

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at a very nice pectoral resolution that

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allowed us to to look at this lines and

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also at a very high angular resolution

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point five our second which for this

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sources correspond to about sixty you

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it's actually very small for pretty

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stuff so this is what the data look like

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it's lots and lots of lines it's

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actually a spectrum that is taking at

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one special like expected at one

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position towards the star we actually

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have a whole map of these and all of

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these are rotational lines from

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molecules and myths of them are like

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molecules that we know that we have been

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observed that have been observed before

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like methanol dimethyl ether and so on

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deteriorated version of these but some

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of these lines are actually due to

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molecules that haven't been identified

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before and this was the case for methyl

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chloride so this is what we found this

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is the detection that we got so for the

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35 chlorine and the 37 chlorine as you

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can see the lines are like very intense

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we can actually detect them up to k

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equal four into is 13 to 12 transition

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for this symmetric top molecule so nice

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we can fit them we can derive a benign

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we can direct column density for these

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two species and by doing the ratio of 35

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chlorine over 37 we actually find 2.1 in

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this star forming region so for those of

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you who are familiar with the value of

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isotopic ratio for chlorine and the

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solar system it's going to be a bit of a

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surprise in the solar system we expect

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the value at 3.1 but it's actually not

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surprising to find 2.1 because detection

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previous detection of HC else of it

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found this ratio to be 2.1 and it's

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actually now accepted that this ratio

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changes in different molecular clouds

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nearby our solar system so this is what

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also combining these two abundances and

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comparing them to that of methanol one

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of very big

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this organic molecule in this region we

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found a ratio about 10 to the minus 4 so

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it's Medicare ID is not in abundance

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pieces in these environments but it's

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not negligible either and we see it here

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I'm showing you here the emission of

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methyl chloride around this protostars

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eschews be here and I was actually the

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spectrum that I show you here was

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extracted at this position to here so so

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we detected this methyl chloride around

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illumise protostar and some of the

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members of the pills team we're actually

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also members of the Rosina team that

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looked at the outgassing a comet 67p and

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so we like them to look in the spectra

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of Rosina and especially the DFM s to

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see if a that we would find this methyl

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tried and it was actually there have a

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small shoulder here around my 50s so

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that the the resolution of this mass

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spectrometer is such that you can

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disentangle different isomer at one

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specific amu we can disentangle for

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different atomic composition and that's

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how we could like get this methyl

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chloride detection we see the 35

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chlorine we don't see the 37 but it's

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not surprising if you accept this free

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point one isotopic ratio for chlorine in

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the solar system what is interesting is

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to look at the abundance at which we

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observed ethyl chloride versus methanol

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around 67 P and we found 10 to the minus

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4 which is similar to what we've seen

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for the protostar and this supports the

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possible scenario of an inheritance of

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chemistry form in the pretty little

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regions that would be inherited down to

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come at from ingredients or at least a

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scenario what the chemistry is similar

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in these two environments so the

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question is how do we form methyl

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chlorine how does it got here and while

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we don't know yet but other chemical

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models actually took a crack headed

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after this detection was published and

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they actually found that you could form

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a methyl chloride efficiently by

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chlorination or at regeneration of

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carbon of methyl onto the gray

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surface that you find in this in the

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purchaser or envelope so you form ch3cl

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and then the grains in the outer part of

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the particular envelope flow towards the

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central object so when it's forming and

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so the grains warm up and Myka's that

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you would form into the the ice surface

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will dissolve in the gas phase and be

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able thats how we can detect them with

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radio interferometers of course this is

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the theory this is what the models tells

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us but we need to perform laboratory

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experiments to figure out what is the

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actual formation mechanism but before

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doing that what we also need to know is

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how to quantify methyl chloride in this

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in the solid state if we want to test

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this formation scenario and for this so

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we need to do laboratory study and

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specifically looking at a spectroscopic

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studies because spectroscopy is the main

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tool that we have to look at molecule

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formation in the solid state so infrared

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spectroscopy in the mid are so that's

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what we're currently doing so it's

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ongoing work at JPL

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that we're doing cycle looking in the

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spectroscopy of these methyl halides so

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in pure ice films in this case and what

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we would like to know is to derive band

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strength for the different vibration of

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this pure of its molecules in the solid

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States so here I'm showing you the

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spectra that we get by depositing so

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molecule so ch3 FC or a CLC Revere or C

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a tree I on two cold substrates

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interrogating the spectroscopy with

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Fourier transform infrared spectroscopy

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and as you can see well we can attribute

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the emission the vibrations so for the

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CH stretching and the CH free

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deformation here

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there's not a huge change between the

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different types of allergens but of

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course once you go towards here tree

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rocks or CAC X so C F or C CL stretch

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very clear like changes due to the

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presence of the allergen and the nature

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of the allergen to get the bends ranked

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what we're doing is that we're

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integrating the optical depth under

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these bands divided by the column

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density of ice between

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and this is what we report here I warmed

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up the ice at different temperatures and

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as you can see the band strength for a

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difference see extra edge and CHP rock

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doesn't really change with temperature

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I'm inversa decrees here for chri high

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temperature most likely due to the onset

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of this origin but what actually changed

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is the shape of the features that you

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get so this is what we get when we

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deposit this films at low temperature

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and when we increase temperature we have

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like like very different shape my

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Seikaly due to the crystallization of

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these films in water ice we also observe

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the change of temperature here that is

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most likely due to the diffusion of

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molecules so here so water to see a tree

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I attend to one mixture at high

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temperature you can have diffusion these

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molecules likely segregates and that's

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why we can observe signature of

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crystallization so we get this been

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strength

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another characteristic and other

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behavior of this icing that we are

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highly interested in would be to look at

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the thermal desorption of his ices and

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that's what we've been doing this time

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by depositing ice film onto not a window

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band to a currently called

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micro balance so we deposited them

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different ice films of different

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thicknesses and what we did with micro

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balance is to follow the ice loss versus

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temperature and looking at the

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derivative here so ice loss rate versus

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temperature which you can see is that

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for the different thicknesses well the

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rate does not change this is typical of

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zero for the desorption kinetics you can

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fit this rates by music by this equation

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extracting here the doozers and energy

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said adsorption that you need to

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overcome to have desorption occurring

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these are the energy that I gets as you

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can see if there's not a clear

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correlation with the mass here Tracy L

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is a bit out of the way here and this

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miss actually because not just the mass

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is involved into the desorption of this

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species but also other parameters such

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as the polarity or even the size of

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these molecules ch3cl here is really

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standing out

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could he explain this like the dipole

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moment here and could explain why it's

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stickier and it takes more energy to

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dissolve so pushing further towards

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Astrophysical implication we can use

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this sublimation energy that we derived

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in the laboratory to like measure well

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predicts and derive where the desorption

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France of these species are going to be

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in around protostars

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so like derive where the snow lines are

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going to occur and that's what I've been

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doing here with quick calculation so the

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definition of the snow line of the

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desorption front is where the flux of

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adsorption equals the flux of adsorption

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equals the flux of desorption by like

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00:11:53,110 --> 00:11:50,630
equating the impingement rate of the

278
00:11:55,269 --> 00:11:53,120
item of the molecules equals to

279
00:11:57,519 --> 00:11:55,279
desorption rates you can derive this

280
00:12:00,400 --> 00:11:57,529
temperature here which for a species

281
00:12:02,650 --> 00:12:00,410
using typical abundances gives you the

282
00:12:05,319 --> 00:12:02,660
following temperature around the

283
00:12:09,699 --> 00:12:05,329
protostar and by like using this

284
00:12:11,500 --> 00:12:09,709
temperature and a temperature profile

285
00:12:14,410 --> 00:12:11,510
around Purdue star so here it's actually

286
00:12:15,670 --> 00:12:14,420
the profile for sixty to ninety three we

287
00:12:17,530 --> 00:12:15,680
are observed methyl chloride you can

288
00:12:19,180 --> 00:12:17,540
actually predict that methyl chloride

289
00:12:22,090 --> 00:12:19,190
pure methyl chloride will dissolve

290
00:12:24,220 --> 00:12:22,100
around 130 EU from the central object

291
00:12:28,210 --> 00:12:24,230
it's going to be further out for methyl

292
00:12:30,819 --> 00:12:28,220
fluoride and closer for the other methyl

293
00:12:34,329 --> 00:12:30,829
halide which is interesting to see also

294
00:12:34,720 --> 00:12:34,339
is that another 140 you value better

295
00:12:36,610 --> 00:12:34,730
again

296
00:12:38,470 --> 00:12:36,620
it's actually quite close to where we

297
00:12:40,360 --> 00:12:38,480
detect this methyl chloride here with

298
00:12:42,040 --> 00:12:40,370
our mother beam that I show you here is

299
00:12:44,199 --> 00:12:42,050
about 68 you

300
00:12:46,540 --> 00:12:44,209
and it's actually corresponds to here

301
00:12:48,519 --> 00:12:46,550
where the two beams where here we have

302
00:12:50,680 --> 00:12:48,529
this like onset of this urgent when you

303
00:12:53,860 --> 00:12:50,690
start to see methyl chloride popping up

304
00:12:58,269 --> 00:12:53,870
into the gas phase all right so that

305
00:13:01,210 --> 00:12:58,279
leaves me to my conclusions so I showed

306
00:13:02,980 --> 00:13:01,220
you detections of methyl chloride around

307
00:13:05,829 --> 00:13:02,990
pretty star around pretty star and

308
00:13:09,370 --> 00:13:05,839
around a comet's really showing that

309
00:13:11,439 --> 00:13:09,380
there's a link between the organic and

310
00:13:13,900 --> 00:13:11,449
the allergen chemistry in industrial

311
00:13:16,980 --> 00:13:13,910
environments these molecules are not

312
00:13:19,740 --> 00:13:16,990
direct biomarkers if observed in the

313
00:13:21,750 --> 00:13:19,750
in the atmosphere of exempt annette's

314
00:13:23,220 --> 00:13:21,760
however we need more detection to figure

315
00:13:25,710 --> 00:13:23,230
out what is the standard like the

316
00:13:28,740 --> 00:13:25,720
regular like typical amounts of his

317
00:13:30,240 --> 00:13:28,750
compounds in interest our environment to

318
00:13:36,389 --> 00:13:30,250
see if an exoplanet she would have

319
00:13:38,579 --> 00:13:36,399
differences in in in in abundance for

320
00:13:41,310 --> 00:13:38,589
the spectroscopic experiments we serve

321
00:13:44,550 --> 00:13:41,320
at the CX and the CH works were highly

322
00:13:46,620 --> 00:13:44,560
depending on the type of methyl halides

323
00:13:48,269 --> 00:13:46,630
that you have and the ur like depends

324
00:13:51,180 --> 00:13:48,279
their shape depends on the temperature

325
00:13:52,769 --> 00:13:51,190
of the ice film so they can be used to

326
00:13:55,040 --> 00:13:52,779
probe the ice environment we also derive

327
00:13:58,320 --> 00:13:55,050
Ben's rain that now can be employed to

328
00:14:00,720 --> 00:13:58,330
quantify a cone the formation of these

329
00:14:03,120 --> 00:14:00,730
pieces in ice films the desorption

330
00:14:04,949 --> 00:14:03,130
energy showed us that they're not

331
00:14:06,870 --> 00:14:04,959
circular it is to the mass of these

332
00:14:10,019 --> 00:14:06,880
pieces that other parameters are

333
00:14:13,050 --> 00:14:10,029
involved when predicting when measuring

334
00:14:15,240 --> 00:14:13,060
disturbs in energy of molecules you need

335
00:14:18,660 --> 00:14:15,250
to look at effects like the size of

336
00:14:20,160 --> 00:14:18,670
polarity and the calculation of where

337
00:14:21,420 --> 00:14:20,170
the sublimation front would be showed us

338
00:14:23,579 --> 00:14:21,430
that it's in agreement with what has

339
00:14:25,949 --> 00:14:23,589
been observed by Alma but the search for

340
00:14:28,110 --> 00:14:25,959
CH ret which didn't detect yet is going

341
00:14:30,180 --> 00:14:28,120
to be much more complicated since it is

342
00:14:32,360 --> 00:14:30,190
or further out and the Colombian cities

343
00:14:35,880 --> 00:14:32,370
are expecting dust to be lower than