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[Music]

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how about now okay okay so thanks

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everyone for staying for the last few

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talks of the session I'm Bea I'll be

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talking to you guys today about

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polarimetry it's one cool trick that has

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moms everywhere mad and it's really not

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used as much as it should be it's

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probably something that you heard about

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while you were an undergraduate and have

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since completely forgotten about because

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most of us aren't using it in our

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research

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the idea with polarimetry is really just

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that instead of thinking of life as just

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a scalar with intensity and wavelength

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information that you think of it as a

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vector so you still have that scalar

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information but you also have

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information about your electric field

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oscillation so it's your electromagnetic

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wave having an electric field on

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oscillates up and down side aside in a

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corkscrew Plus polarimetry in terms of

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observing a planet in terms of observing

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a planet what we are going to have at

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least in an ideal case with a nice calm

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main-sequence star it's unpolarized

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incident light coming from my star and

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that's going to be scattering off a

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surface or off of an atmosphere and that

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scattering or reflection is going to

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impart a trend in the way that the

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electric field oscillates and so it's

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going to give us great contrast with our

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stars in those cases I'm talking mostly

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about habitability today but I wanted to

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touch on these other things that

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polarimetry has contributed to

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polarimetry has allowed us to constrain

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albedo of ht1 8-9 7:33 be the original

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claim detection of polarized light from

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that planet is disputed but those non

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detection that dispute that have given

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us some physical constraints on the

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nature of the planet more recently

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observations in polarized light of the

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other ha Jupiter I have up there wasp

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18b have allowed us to exclude certain

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scenarios Venus of course was famously

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observed and polarized like many times

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and that allowed us to determine what

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the cloud species was dominant in that

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atmosphere that that was not a nice

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jungle planet right next door to us in

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the case of Titan polarimetry was used

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to give us the first indication that

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this was a cloudy hazy world and that

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unusual photometry that we saw from that

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was not because we had snow all over the

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surface that's a really interesting

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paper by the way if you look it up

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Illinois 1973 very recently we've had

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observations of solar oblate notes from

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rapidly rotating stars even seeing stars

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reflecting each other's light in

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polarized light and we've had a lot of

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characterization of the interstellar

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medium which is a really vital component

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to studies of exoplanets the polarized

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light that's something that we need to

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take into account

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oh is it thanks okay that sounds better

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yeah all right so as we have a planet

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that's moving through its phases around

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its star we're going to see these key

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features come up in polarized light

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coming from glint off an ocean if it has

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a rainbow from other optical effects

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from clouds and from Rayleigh scattering

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and depending out what wavelengths are

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looking at different features we'll be

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dominant so that allows us to

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characterize the exoplanets around their

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star there's also some stuff that you

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can do as far as bio signatures looking

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for chiral molecules so I'm not really

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going to talk about that today but I

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just wanted to leave it up to remind

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people to look it up so one of the

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strengths of this as I have touched on

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before is that you can naturally know

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that star if it's a calm star you're

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going to create natural contrast with it

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so you don't necessarily need to use

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something like a coronagraph you don't

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necessarily need your planet to be

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transiting the star for you to be able

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to characterize it

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another benefit is that you can derive

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orbital parameters even for planets that

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do not transit there start your

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inclination is going to change the shape

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of your polarized light curve not just

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the intensity but the shape of your

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polarized light curve so that can be

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figured out using this method polarized

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light really lends itself to confirming

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the presence of clouds as well and

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possibly to characterizing them if you

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can get enough data for that so I'm

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going to show you a few models most of

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these models are going to be based on

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chemically evolved models from and

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ruling house keys 2018 papers so he was

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looking at the Trappist one system and

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the kind of archetype planets that we

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might find there so in these graphs that

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I'm going to show you in a little bit

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we're going to be taking a few of these

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archetypes and comparing them to each

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other

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maybe including things like varying

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types of clouds and adding cloud cases

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we're not going to talk about services

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in too much detail but the question was

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if we have this information from the

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scalar components things like the albedo

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of these different surfaces and the

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behavior in scalar light of atmospheres

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and of different types of clouds what

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more can we know by looking at this in

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polarized light so we have that for

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comparison in scalar light we also have

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very different behavior of surfaces in

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polarized light different surfaces

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polarized light in different ways and

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even different types of ices can

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polarize light in slightly different

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ways which could be vital in the far

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future for characterizing some types of

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exoplanets but is immediately useful for

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characterizing the icy moons in our own

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solar system for the plots I'm about to

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show you this is just a dummy plot I

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just wanted to point out that the x-axis

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it's typically going to be just half of

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an orbit so we're going from full phase

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to new phase the y-axis is polarization

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and parts per million so that's telling

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us the size of the signal current

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polarimeters are sensitive to about one

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part per million and then at the top

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I've merged some small end with the

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dashed lines I've merged some key

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features to look for I just want to

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point out that the

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maximum polarization is not necessarily

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the same as where we find the maximum

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signal we need to combine the

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polarization in some cases with the

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amount of light that we're getting

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reflected off the planet and if we're

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looking at a rainbow that that might

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shift depending on the species producing

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the rainbow and the wavelength that

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we're looking at so our first point to

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examine here with one of the tracklist

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cases is that polarizing features have

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distinct shapes and of course their

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dominance varies with wavelength as you

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might expect the Rayleigh scattering

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will be very strong if you're looking at

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blue wavelengths and if you can start

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moving towards redder wavelengths if you

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had a planet that had ocean glint that

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would be a strong polarizing feature and

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that would start to pop out as you look

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towards redder and redder wavelengths if

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we have a planet that has a cloud

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present we get these a very distinct

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rainbow features these are very clear

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features to see in polarized light the

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strength of the rainbow compared to the

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other features like the Rayleigh

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scattering will depend on the cloud

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height if you're very interested in how

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to determine your cloud height and kind

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of disentangle that from molecular

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abundances I would highly recommend

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looking at the paper from Thomas Boucher

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Oh tomorrow she I'm sorry from 2017 it's

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a really brilliant paper but I can't get

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into that right now right and so even in

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cases like this where we have an

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atmosphere that is maybe very strongly

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really scattering and we're masking that

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a weaker rainbow signal from a different

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species in the cloud if we're moving

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towards red wavelengths we're starting

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to be able to pick out the difference in

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those curves the one that has the cloud

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present the one that does not so

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different scenarios of cloudy

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atmospheres do you seem to be

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distinguishable just looking at these

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different Trappist archetypes you can

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tell them apart from one another and of

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course they're going to change in

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wavelength in particular and predictable

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ways so this is suggesting that this

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might be

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useful technique to tell different kind

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of basic anticipated planet archetypes

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apart and I should point out that I'm

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kind of simplifying things here I'm

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showing you the total polarization in

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reality we're normally looking at Stokes

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parameters we have a little bit more

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information than the last few plots that

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I've shown you so we're looking at

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Stokes Q and U and we're getting

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positive and negative values that also

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behave in particular ways depending on

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your rainbow behavior and your

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scattering surface if you're looking at

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a surface if the values on the y-axis

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have been wearing you after I told you

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we can currently detect on to around one

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part per million you might consider

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looking at sub Neptune's mini Neptune's

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so GJ 1214b depending on its cub specie

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is dominant in the upper atmosphere and

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the size of the particles can produce

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optical effects that would be near

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current detection limits with

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contemporary polarimeters so we're

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getting very close to that one part per

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so with a part per million precision

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polarimeter which is what we currently

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have and several hours of observation

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which is pretty typical of an aperture

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polarimeter observing these days if we

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were looking for one of these one

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designed part per million signals from a

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planet we could do that currently just

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with what we have right now with a

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4-metre class telescopes if we're

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looking at a star like HD one eight nine

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if we're looking at a star like Proxima

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Sun and our band we would want to use an

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eight meter telescope Proxima Sun and B

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band if we want to get some comparison

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in the different wavelengths and start

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to tell these features more clearly

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apart we would need to use a thirty

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meter telescope so basically right now

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if there was a hot mini Neptune in

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Proximus then or something larger and

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hotter than that we should be able to

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detect it or almost be able to detect it

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with a dedicated program if we wanted to

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observe a dimmer star of course we just

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need to stare longer use them even

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bigger telescope if we want to be

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looking for planets in polarized light

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that are in the habitable zone this

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would improve or this would require that

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we improve our polarimeter design to

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some degree so I tend to kind of

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summarize polarimetry by saying that

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although the nature of polarimetry

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reduces the throughput of your photons

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it improves contrast and certainty so we

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really need to be thinking about the

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scenarios in which this is a useful

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technique and whether or not we want to

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be building our telescopes and our

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instruments for this sort of thing and

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if so what particular things we want to

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be looking for because it is certainly

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useful in some cases particularly

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dealing with clouds and things that are

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not transiting we need to continue to

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characterize noise particularly from

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stellar activity and cool stars

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especially if we want to keep looking at

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M dwarfs to overcome issues with food

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put to some degree we can use things

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like dedicated stairs and thoughtful

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observations being a little more

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particular than maybe we've been in the

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past about which planets we're looking

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at and to overcome noise we can consider

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things like simultaneous observations

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that will help us characterize things

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like stellar activity to help us

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characterize that noise and also

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improving technology which sounds like a

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you know kind of ask a really easy thing

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to say an hard thing to do but I just

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want to point out that hippy the most

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sensitive polarimeter in the world right

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now for visible wavelengths is built

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from the 3d printed components and

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optical and lab materials that you can

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get out of a lab catalog is a very

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inexpensive it's very reproducible and

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there are great ideas out there about

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how to improve the the noise the the

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throughput and the abilities of

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polarimeters that people have but

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couldn't maybe be funded I don't have a

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particular it is just to be clear so I

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just want to end on this note of

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pointing out that many upcoming space

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telescopes and ground-based telescopes

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have or considering having or definitely

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planning to have polarimeters we

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voir origins Space Telescope the TMT the

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e-elt w first all have plans for

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polarimeters or considering fans for

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polarimeters we need to think really

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hard over what wavelengths those

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polarimeters will cover for example

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leVoir will only be in the UV and

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origins would Chris be in infrared and

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the kind of science that we would be

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able to do with that we also need to

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think about architecture and whether

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it's useful for the kind of science that

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we want to do for us to have our

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polarimeters in front of our own master

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after them because that's going to also

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determine obviously the type of science

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that we could be doing and without all

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open it to questions yes so are you

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assuming like it covers the entire

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planet like a disk integrated right so

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then you're really combining yeah yeah

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so so these are disk integrated the

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signals for planets that have a uniform

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coverage of whatever it is that I've

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done there so they can have a different

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grounds and a different you know

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different layers of clouds but it's over

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the entire planet the output from these

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star which is modeling code that I use

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actually does produce a pretty outfit so

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it's in the works I guess I don't know

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how fast it'll come up but it's in the

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works to be able to produce or be able

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to use a 3d input to like improve the

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swath of things that we could be

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exploring with B star yeah RJ hi RJ from

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Oxford at the beginning you mentioned

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chiral molecules and then you said you

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were going to talk about it anymore but

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I wanted to ask if so do chiral

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molecules produce like a noticeable

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polar

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signal in mmm spectroscopy yeah so

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chiral molecules can impart circularly

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polarized light that's really too weak

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of a signal for anytime in the near

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future to be doing that with exoplanets

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most likely but it's something that's

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really useful and interesting for

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astrobiology studies in our own solar

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system you could potentially be doing

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this just with like a Europa Lander or

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something like that yes that was a

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really interesting talk Ted camasta q

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Chicago so it seemed like you needed

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like phase resolved observations to get

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information about say like clouds or

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something in the atmosphere do you

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always need like a full half orbit phase

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curve or is there like shorter term

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observations that can tell you something

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similar you could if you have some idea

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of what you want to look for or what you

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could anticipate from a planet which I

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mean you can just sometimes do from

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physics knowing the size of it and what

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sort of you know Cubs you might expect

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where you can just kind of sample around

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where you might expect say a rainbow and

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see if you do see the peak in the

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rainbow exactly where you predict if you

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think that there's water clouds at the

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top of the atmosphere does that arise at

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the right spot for the cloud height that

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you expect you can you can really narrow

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this down so you can just do a lot of

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sampling at a particular point if that's

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something that you're looking for if

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you're trying to do something like

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constraint orbital parameters or

400
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something like that that's depending a

401
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lot more on like the general shape up

402
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the curves and you would want really

403
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good sampling throughout if there are no

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additional

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questions thank Kim