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second talk of the day so creech who

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will be talking about some hot Jupiter

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atmospheres all right everyone thank you

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for having me here to talk to you my

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name is sue Kurt and I'm going to

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discuss with you a project I've been

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leading over the last few years to study

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the atmospheres of five hot Jupiter

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exoplanets using the Hubble Space

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Telescope so hmm how do I make this go

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ah like that wonderful so just as an

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outline of my talk I'm going to start

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off by first giving a little bit of an

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overview of the field of transit

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spectroscopy what it is and why we care

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about it since I know this is a meeting

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for a very multidisciplinary meeting

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from there I'll move on to what

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specifically we were trying to do with

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our project I'll move on to the data we

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collected and how we analyzed it what we

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found and then I'll wrap up and

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summarize okay so just as a quick

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overview the last few years have really

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been a golden age for exoplanets our

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discovery rate has been increasing at an

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exponential rate particularly these last

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few years we have almost a thousand

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confirmed exoplanets today and about

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3,000 work candidates to go ahead and

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validate and vet so that's really

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awesome the problem is for most of these

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objects we only have radius or mass

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estimates so we know nothing beyond

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vaguely how big they are and that's a

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problem from an astrobiology perspective

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because if we're trying to characterize

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their habitability or look for evidence

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of life we really need to know a lot

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more but these observations it's very

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hard to do that kind of observations

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first because the planet is a dim

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relative to its star and second because

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it's really hard to separate them out so

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it's hard to differentiate the planets

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emission from the stars emission so for

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most of these plants are kind of stuck

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but for one particular subset of planets

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the transiting planets we can do a lot

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more so just as a reminder these are the

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planets that pass in front of their

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stars from our point of view and for

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these objects we can actually extract

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low resolution spectra so how do we do

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that well there's two phases first in

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primary eclipse or transit where the

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planet passes in front of its hosts

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hosts are thus implanted starlight

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filters through the terminator region of

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the atmosphere imprinting a very subtle

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absorption spectrum when the planet

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passes behind its star you go from

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seeing the light of the planet and the

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star to seeing just a light of the star

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so if you difference that out you see

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the dayside hemisphere integrated

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emission spectrum of the planet

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taken together this lets us understand

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parameters such as the composition of

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the atmosphere its thermal structure and

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its dynamics including the presence and

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absence of clouds as well as any

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atmospheric escape that's going on so

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that's really awesome for for these

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these measurements are still rather

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challenging so the instruments and the

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techniques we have today we've mostly

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been focusing on planets in the hot

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Jupiter class so these are gas giants

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like Jupiter that orbit an extremely

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Coast and close to their host star so

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I'm talking periods of a few days

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temperatures of thousands of Kelvin

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we're refining our oh so these objects

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are interesting in of themselves for

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their planetary science from an

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astrobiology perspective kind of the

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goal is to refine our techniques on

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these easy objects and eventually push

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down to smaller earth-like planets and

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look for bio signatures on that

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metabolic bio signatures such as oxygen

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and methane and so on and so forth so

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that's kind of the kind of the big

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picture where we're going from

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astrobiology perspective so what exactly

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were we doing well what we're really

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trying to do is bring the field of

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transit spectroscopy upon Jupiter's into

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its technological maturity and so what

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we're doing there is transitioning from

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doing one-off studies of aw objects to

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really doing a systematic comparative

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study the first one really done for a

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for hot Jupiters in the near-ir and

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towards us and we were allocated a

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hundred and fifteen orbits of Hubble

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time to study 16 different hot Jupiters

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using the new wide field camera 3

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instron and hubble that was installing

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the last servicing mission we're looking

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with the g1 41 grizzin which spans oh

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I'm just excuse me which spans 1.1 to

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1.7 microns and this has two features

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that are a huge interest to us first you

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have this kind of water absorption band

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at one point 4 microns so measurements

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there can constrain the composition of

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the planet second you have this kind of

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a window into the planets photosphere at

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one point six microns so there are no

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mature observers there and that lets us

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contained the energy budget of the

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planet so those are kind of and this

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work can only really be done from space

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this and that this figure here

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illustrates out the black curve here is

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with c3 sensitivity the red curve is

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telluric absorption so absorption from

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the Earth's atmosphere and you can see

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the very same water feature we hope to

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observe on exoplanets is also present in

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our atmosphere obfuscating observations

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so we unfortunately have to go to space

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for this kind of work

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this slide here has just meant too ill

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to introduce you to our targets so each

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of these black diamonds is a transiting

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exoplanet these are the known transiting

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hot Jupiters as of this past September

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the on the targets an hour an hour study

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are circled in either circled in blue or

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boxed in red depending on whether we

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observe them in transition or eclipse

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some we observe in both the planets that

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we specifically that I specifically I'm

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going to present to you are in green ah

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the our sample includes includes a very

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broad range of diversity it includes

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planets with and without a thermal

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inversion and we and planets that are

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bloated and planets that are non bloated

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so we have a pretty broad range of the

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hot Jupiters in our sample so the

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planets I'm going to discuss today we

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have three of them in transmission one

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of them in emission and one of them was

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four in both oh dear laser pointers

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dying how sad okay so those are objects

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what did we do to them well the what we

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basically did is we use Hubble to image

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to take a time series of spectra during

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the course of an event so as the planet

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transited or went through an eclipse we

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continually image the star and to expect

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drove it we converted these two

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dimensional spectra and 21 them into a

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one dimensional extracted spectrum we

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did background subtraction do and to

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correct out for the effects of residual

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starlight or whatever and that's all we

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did to the data so that's what you get

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with very minimal processing we've been

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down the data if so we'd agree to this

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the spectral resolution in order to

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improve the precision per wavelength

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element so that's what these vertical

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lines here are they do market the

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wavelength ins we broke down our spectra

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into so what do you get if you do that

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well you get something that looks like

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this so this is the transit light curve

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for the planet wasp for an integrated

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white light so if integrated across the

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entire band pass and so right off the

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bat you see our transit you see the dip

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in starlight due to the passage of the

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planet in front of the star and without

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any post-processing that's already

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evident so this is already a huge

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improvement from Nick MOS and other

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instruments in space so this is a very

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good sign for with c3 there's a

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systematic that's evident that's that's

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this kind of ramp effect which are

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rapidly rises and levels off but that's

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the only one and what's good about

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what's good news about that is that it's

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highly periodic

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means we can remove it without reference

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to an instrument model so we to remove

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this effect we follow the divide method

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pioneered by Berta at all the bit is

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deliberate our advisors Canadian and

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Zach when I'd have a little bit of fun

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with them and so the way that works is

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you take the two out of transit orbits

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you average them together and divide

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them into the in transit orbits and

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voila you end up with the photon noise

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limited light curve and so that's really

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great we're able to decorah late without

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reference to an instrument model we care

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about this because the predecessor to

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with c3 Nick most required an instrument

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model to D correlate systemic effects

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and that and that introduced a lot of a

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kind of discussion that people weren't

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really sure whether the features you are

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getting out of those spectra would you

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do the instrument or we're due to

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something that was actually asked you're

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physically there so we sidestepped that

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debate entirely with this with our work

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once you have those d correlated d

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correlated light curves you fit a

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transit model in each channel so you the

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only free parameter allows depth

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everything else is locked down to either

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the literature values or what you

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compute from theoretical stellar models

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and you estimate the errors in two

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different ways Markov chain Monte Carlo

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and residual permutations and you choose

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whichever gives you the larger error

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since you're looking at different

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sources of error so we're trying to be

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as conservative as we can in estimating

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a precision so what do you find well you

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find something that looks like this

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these four plots here are the

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transmission spectrum we extracted for

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the 444 of the planets in our survey so

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that's trace to trace for core 01 and

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wasp or three of these are pretty

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similar trace to trace for and Kuro one

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are all very similar essentially flat I

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present here a schematic I presenter and

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the example of trace to to kind of zoom

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in and discuss the black points are the

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transmission spectra that we derived the

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red point is just a simple flat line fit

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the blue points are conventional solar

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composition oxygen-rich atmospheric

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model and the green points are a more

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exotic carbon-rich atmospheric model

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models courtesy of nickel mother's to

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them the basic the what we basically say

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out of this is that all the models for

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the data equally well our precision is

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not high enough to differentiate between

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them however what we can do is rule out

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atmosphere creations on the scale of 10

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scale heights or more

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and this is significant because there

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have been atmospheric models published

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which called for variations of this size

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so we can at least show that such models

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are not typical the case of wasp or is a

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little more exotic and for this we

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actually do see a source of absorption I

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should clarify here that since so the

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y-axis here is the effective

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planet-sized so absorption shows up as a

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larger effective planet so in case

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you're wondering by an absorption

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feature goes up so we have an absorption

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feature at one point three microns this

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is super weird because we don't expect

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there to be absorption at one point

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three microns so we expected to see same

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thing here but we don't and so so this

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is actually fairly significant

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traditional cloud-free atmospheric

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models are ruled out at ten sigma or

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greater so this is for so there's

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something here on the first thing we did

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is we went back and put this through a

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whole battery of tests to see if you

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could explain this effect from ah from

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stellar activity or from instrumental

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effects we can't so far we want to be

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very conservative of this whole thing so

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we're not claiming the detection of a

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new feature we are saying that there is

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grounds for further follow-up studies

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including follow-up observations as well

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as reanalysis using independent

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techniques of this data set we also

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derived thermal emission spectra for two

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planets so one of those was lost for so

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we have wasp porn transmission and in

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the mission ah so this is a little bit

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of a busy diagram so I'm going to try to

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explicate it a little bit so we what we

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have or down over here is our data but

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we also have a little bit of other data

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other folks if found so this is a

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broadband point from Casares at all and

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this is from the Spitzer Space Telescope

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you have a three different model shown

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here one of them in red is an

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oxygen-rich model with an atmospheric

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inversion so that's a TP profile over

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here and you also have two non-inverted

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atmospheres one oxygen rich in blue and

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one carbon rich in green our data

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specifically is shown zoomed in here in

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this inset and the bottom line is that

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we we strongly disfavor water-rich

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models we seem to we seem to be much

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more consistent with water poor models

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and in particular non-inverted

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atmospheres and by not inverted I don't

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mean strongly non-inverted which would

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look something like that but we clean on

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adverted isothermal atmospheres and

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non-inverting as fears are ruled out

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particularly by the spitzer data so the

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kind of food data we have right now is a

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carbon-rich non-inverted model we have

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we derive similar results or trace three

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to explicate data data here our data is

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shown over here and zoomed in on this

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inset spitzer measurements are here and

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ground-based measurements are here the

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green curve is a solar composition

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atmosphere the brown curve is a depleted

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volatile atmosphere so depleted by by a

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factor of 10 relative to solar and water

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and carbon dioxide and we also show a

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black body which corresponds to an

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isothermal atmosphere and the lot of the

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upshot is between the our data and the

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Spitzer data we're able to constrain out

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the isothermal atmospheres as well as

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the solar composition atmosphere the

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best competent the best fit seems to be

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from a depleted volatile atmosphere so

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what's the upshot of all of this well

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the first in perhaps the most important

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result as this is that we demonstrate

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that with c3 is a very suitable

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instrument for these kind of broad based

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studies of exoplanet atmospheres so you

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can get strong good reliable

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transmission spectra from this and this

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instrument is great for exoplanets

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science for our target specifically we

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derive for transmission spectra and two

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emission spectra from our emission

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spectra we show that larger that

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atmospheric models with large scale

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variations are not common so things that

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happen so if you have an atmospheric

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model that has variations of more than

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10 scale heights that's probably not

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going to be very common in the hot

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Jupiter class at least if it stays free

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we identify a potential new feature in

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the wasp for atmosphere that reserves

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follow-up and bass are an emission

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spectra we find that our exoplanets are

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a little bit more water port than we

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expected them to be and if you really

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want to nail down the water composition

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we also show that since we're spectively

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photon noise limited what you really

379
00:12:54,130 --> 00:12:52,220
want is more photon so you need to do a

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00:12:55,960 --> 00:12:54,140
multi visit observing campaign if you

381
00:12:58,540 --> 00:12:55,970
want to really try to characterize the

382
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abundance of water because this seems to

383
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be more water poor than expected so

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that's roughly where so that's roughly

385
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where we're at I'd love to take

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certainly so I'm not an expert on this I

387
00:13:26,720 --> 00:13:25,110
would really absolutely so the question

388
00:13:29,059 --> 00:13:26,730
was could I elaborate more on what i

389
00:13:30,800 --> 00:13:29,069
mean by carbon-rich atmospheres um so

390
00:13:32,240 --> 00:13:30,810
I'm not an expert on this the seminal

391
00:13:35,179 --> 00:13:32,250
paper certain my new COO mother's to

392
00:13:36,470 --> 00:13:35,189
them but basically so so so

393
00:13:38,749 --> 00:13:36,480
traditionally in exoplanets we always

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00:13:39,650 --> 00:13:38,759
assume that okay a hot Jupiters

395
00:13:42,410 --> 00:13:39,660
atmosphere is probably going to be

396
00:13:43,759 --> 00:13:42,420
similar to its star and and generally

397
00:13:45,769 --> 00:13:43,769
that means you have a carbon to oxygen

398
00:13:46,699 --> 00:13:45,779
ratio that's less than one if on the

399
00:13:49,189 --> 00:13:46,709
other hand you have a carbon to oxygen

400
00:13:50,269 --> 00:13:49,199
ratio that's greater than one on the

401
00:13:51,350 --> 00:13:50,279
what all the water is going to go away

402
00:13:52,819 --> 00:13:51,360
and all you're going to be left with is

403
00:13:53,960 --> 00:13:52,829
a bunch of carbon compounds so the

404
00:13:56,480 --> 00:13:53,970
atmospheric spectrum will be really

405
00:13:58,639 --> 00:13:56,490
different a carbon-rich a rat mysterious

406
00:14:01,009 --> 00:13:58,649
claim for the exoplanet lost 12 it was

407
00:14:03,110 --> 00:14:01,019
later disfavored based on based on re

408
00:14:04,670 --> 00:14:03,120
analysis of the data however it still

409
00:14:13,730 --> 00:14:04,680
remains a valid possibility that we need

410
00:14:15,079 --> 00:14:13,740
to consider go ahead so the question was

411
00:14:16,759 --> 00:14:15,089
if we had to speculate on what the wasp

412
00:14:19,249 --> 00:14:16,769
or feature was what would he expect it

413
00:14:20,689 --> 00:14:19,259
be the answers we have no idea we spent

414
00:14:23,509 --> 00:14:20,699
literally about a year trying to follow

415
00:14:24,499 --> 00:14:23,519
up and figure out ways the to explain

416
00:14:26,300 --> 00:14:24,509
what was going wrong because we were

417
00:14:28,009 --> 00:14:26,310
pretty sure we were wrong the only

418
00:14:29,150 --> 00:14:28,019
reason I'm presenting it to you now is

419
00:14:30,439 --> 00:14:29,160
that we couldn't figure out why we were

420
00:14:32,240 --> 00:14:30,449
wrong so we have to conclude that maybe

421
00:14:33,530 --> 00:14:32,250
it's real the reason we were so

422
00:14:35,689 --> 00:14:33,540
conservative is that there exists

423
00:14:37,639 --> 00:14:35,699
nothing in conventional hot Jupiter line

424
00:14:40,519 --> 00:14:37,649
lists that absorbs there in any