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hello everyone my name is alexander

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thielen

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i'm an astrobiology npp postdoc at

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assets goddard space flight center

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and thank you for joining me today at

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april icon where i'll be talking about

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the exploration of titan's atmospheric

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chemistry and dynamical state

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with alma titan herbert is a substantial

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atmosphere which is primarily composed

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of molecular nitrogen

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there's also a small percentage of

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methane molecular hydrogen and all of

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these species are dissociated and

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recombined

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into a wealth of organic compounds today

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we'll be talking about mostly

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hydrocarbon and nitrile species but

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there are also some oxygen burying

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species such as carbon monoxide and a

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wealth of yet to be identified

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heavy ionospheric species in the upper

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atmosphere

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over on the right we have a temperature

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profile of

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the earth and these are remarkably

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similar in shape although titan's

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profile is much more extended

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and much colder the study of titan and

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the sub millimeter which we'll be

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discussing today

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between about a 1070 kilometers

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is comparable to previous observations

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by the cassini spacecraft and those from

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the ground

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in the uv and in the infrared the

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combination of all of these studies

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allows us to characterize titan's

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atmosphere

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chemically and dynamically and allows us

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to answer some questions

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such as how extensive is the atmospheric

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chemistry and the molecular inventory

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of titan and how are these trace

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constituents distributed spatially and

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temporally

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for interest to astrobiology we also

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wonder how are these species able to

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interact with the surface and possibly

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tighten the subsurface ocean

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to try to answer some of these questions

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we use the atacama large millimeters

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submillimeter array or alma which is

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located high in the chilean desert

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close to 5000 meters in altitude almost

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comprised of 66 antenna dishes

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in multiple different arrays and these

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are movable

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which allows for baselines between 150

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meters and 16 kilometers

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this enables fairly high spatial

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resolution

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at these long wavelengths and you can

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see that titan is a fairly

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bright and compact continuum source at

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these frequencies

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and as such alma used titan for a number

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of different flux calibration

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observations since its inception in 2011

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all the way until 2017

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so there's a wealth of titan

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observations that are available on the

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alma science archive for us to use

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when looking through the alma flux

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calibration archive

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of titan observations we quickly found

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that alma has a variety of capabilities

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that are

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suitable for planetary atmosphere

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studies in addition to those of

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astrophysical and extra galactic sources

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this includes the coverage of numerous

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molecular species which may appear in

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planetary atmospheres

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for chemistry and isotopic ratio studies

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the high

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spectral resolution of alma heterodyne

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spectra allow for

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wind speed measurements through doppler

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shift and also to resolve

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atmospheric emission lines which allow

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you to measure the temperature

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the abundance of gas with altitude

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the spatial resolution as mentioned

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before allows us to map

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these things instantaneously to look at

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abundance or brightness temperature maps

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and the sensitivity of the array as a

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whole allows for

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new molecular detections in the

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atmosphere of titan and other solar

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system targets

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here's a representative spectrum of

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titan which is actually obtained from

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flux calibration observations so roughly

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two and a half minutes

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on source during 2014 but even in this

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short integration

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we can see the richness of these

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submillimeter spectra

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over on the left we have a band of

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acetonitrile we have these two

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relatively strong lines

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of hydrogen cyanide isotopes the carbon

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and nitrogen

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isotopes and then we even have some low

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signal

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acrylonitrile or ethyl cyanide

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transitions here

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so analyzing these spectra in a number

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of different ways will

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allow us to complete some of the

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projects that i'll describe

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here after and even just integrating

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over

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these spectral lines you can obtain

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these nice

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emission maps which will show you a

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snapshot view

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of the distribution of a given molecular

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species

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at a certain time when the observation

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was taken so

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on the top row we have hc3n or

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cyanoacetylene which we can see

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very rapidly transitions from the north

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pole to the south pole during

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2012 to 2015 and this is because of the

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relatively

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short photochemical lifetime of this

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species whereas

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in contrast the bottom row we can see

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ch3cn

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or pseudonitrile which we showed

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previously which stays at the north pole

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much longer than saturn acetylene

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because of its long photochemical

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lifetime which

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makes it a good tracer of the dynamics

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of titan's atmosphere

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there's a few ways that we can assess

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titan's dynamical state using

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alma observations the first is through

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the retrieval of temperature

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from carbon monoxide from roughly the

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tropopause

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around 60 kilometers to the lower

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mesosphere above

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500 kilometers and this is because co is

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well mixed in the atmosphere titan at

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roughly 50 parts per million

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so here is a composition of different

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radio transfer

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retrieval results of titan's temperature

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at different latitudes which i've made

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into a temperature map

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during 2017 in titan's northern summer

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solstice

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so we can see a large warming that

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occurs at the

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subsolar latitudes around 26 north but

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there's also

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warming that's occurring in the

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stratopause

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at the north polar region and the mid

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southern latitudes

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and this is indicative of titan's global

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pole the pole circulation cell

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which is currently lofting air from the

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northern or

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summer pole down into the southern

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winter pole we can measure titan's

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atmospheric temperature further up in

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the atmosphere using emission lines of

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hcn

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as you can see over here on the left

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these really broad features

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allow us to sound temperatures into the

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800 and 900 kilometer range and in

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particular

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this absorption core in the hdm spectra

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allows us to infer the mesopause

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temperature of titan which hasn't really

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been

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studied in depth with latitude or with

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time

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before these analyses so this is a

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preliminary result but we're seeing

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already from

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observations that the mesopause likely

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varies

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significantly in both its altitude and

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its temperature measurement

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so this is you know largely due to wave

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motion and changes in the atmospheric

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composition which can have effects on

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the radiative energy budget

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of titan's atmosphere we've previously

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seen that this portion of the atmosphere

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is really variable with time from

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alma's high spectral resolution

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capabilities allow us to

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observe doppler shifts in emission lines

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of rotational spectra

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which we can directly map to wind

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speed magnitudes in the atmosphere of

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titan depending on what chemical species

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you're observing you can look between

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300 and 1000 kilometers in the

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atmosphere depending on where the

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species

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line core is sensitive to emission so

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in martin coroner's paper from last year

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we were looking at

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ch3cn hc3n and hnc

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wind maps from 2017 and comparing those

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to

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the published ones in 2016 from luciano

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where they found a thermospheric jet in

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titan's upper atmosphere around the

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equator

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our wind speed measurements showed a

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dramatic decrease

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over this nine-month period of about 47

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which is due to a dynamical instability

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or variable wave activity

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between the middle and the upper

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atmosphere of titan which is really cool

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now moving on to some chemistry and

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composition studies which

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are possible from these alma

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observations we can take the

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temperatures that we retrieved earlier

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from co and acn

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and use them to do radio transfer

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analysis in multiple occasions on

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titan's disk to make these abundance

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maps with latitude and altitude or

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pressure

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so on the left we have a map of

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cytoacetylene

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with altitude and on the right we have a

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pseudo nitrile

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and again similar to the maps that i

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showed

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a few slides ago both of these molecules

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have an abundance

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enhancement towards the pole and in

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particular the enhancement of the south

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pole compared to the equator

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for these species varies by an order of

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magnitude which is

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really interesting and the global

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circulation of titan's pole the pole

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cell is also evident

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here in the enhancement above the south

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pole and

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the relative dearth of each of these

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molecular species towards the equator or

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and maybe more exciting is the detection

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of a new molecular species

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in titan's atmosphere which has a lot of

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applications for both

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its overall chemistry feedback into its

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atmospheric dynamics and for

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perspectives on astrobiology

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previous detections from our group early

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on included

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c2h5cn or just ethyl cyanide on the top

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and c2h3cn which is vinyl side on the

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bottom which had a lot of interest

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from the astrobiology community and

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last year we made two new molecular

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detections in the atmosphere of titan

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using dedicated alma observations from

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2016-2019

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on the top i'm showing the detection of

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methyl cyanoacetylene in this

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purple spectrum inset from our 2019 data

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and this molecule ch3c3n is

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the largest nitrogen bearing species

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00:09:36,070 --> 00:09:34,880
that we've found thus far also has a

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00:09:39,389 --> 00:09:36,080
really long name

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00:09:41,509 --> 00:09:39,399
and in contrast to this molecule is

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cyclopropanilidine which also has a long

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name and is the smallest

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cyclic molecule that we found thus far

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00:09:49,829 --> 00:09:48,000
in any solar system object

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both of these molecules have column

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density measurements which are

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00:09:56,310 --> 00:09:53,839
far below everything else that we've

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00:09:59,190 --> 00:09:56,320
found thus far in titan's atmosphere

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00:10:00,870 --> 00:09:59,200
so alma really is one of the best tools

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00:10:04,150 --> 00:10:00,880
that we have in the moment to push

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00:10:05,990 --> 00:10:04,160
the molecular inventory and the you know

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00:10:08,870 --> 00:10:06,000
photochemical products of titan's

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00:10:10,790 --> 00:10:08,880
atmosphere even further

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00:10:12,310 --> 00:10:10,800
finally alma allows us to observe many

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different isotopic species in the

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atmosphere of titan on the top

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row we have ch3d as well as isotopes of

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00:10:22,710 --> 00:10:19,120
hcn and on the bottom right we have

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00:10:25,110 --> 00:10:22,720
co and ch3 cn isotopes

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shown and their respective values are

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00:10:28,949 --> 00:10:26,399
printed below

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00:10:31,030 --> 00:10:28,959
the investigation of isotope ratios

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00:10:32,949 --> 00:10:31,040
gives us insights into the formation and

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evolution of the atmosphere of titan

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00:10:38,150 --> 00:10:36,079
and nitrogen and carbon ratios give us

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00:10:40,710 --> 00:10:38,160
some insights into the selective

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00:10:42,069 --> 00:10:40,720
isotopic fractionation that happens in

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the upper atmosphere

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00:10:46,150 --> 00:10:44,079
the dh ratio of titan is interesting

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because it's an order of magnitude

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00:10:49,269 --> 00:10:48,320
higher than that of saturn or jupiter is

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much more in line

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00:10:53,350 --> 00:10:51,839
with the oceans on earth similarly the

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00:10:57,030 --> 00:10:53,360
oxygen ratios on titan are pretty

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00:10:59,910 --> 00:10:58,949
so in summary this was a collection of

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00:11:00,710 --> 00:10:59,920
different projects that we've been

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00:11:03,509 --> 00:11:00,720
working on

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00:11:04,230 --> 00:11:03,519
and nasa are using alma to observe titan

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00:11:06,150 --> 00:11:04,240
and also

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now to observe other planetary

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00:11:08,790 --> 00:11:08,160
atmospheres but alma is a really great

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00:11:10,550 --> 00:11:08,800
tool

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00:11:12,310 --> 00:11:10,560
to look at the spatial and temporal

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00:11:12,949 --> 00:11:12,320
variations in the temperature the

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00:11:15,350 --> 00:11:12,959
abundance

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00:11:17,509 --> 00:11:15,360
and the wind speeds of different plants

341
00:11:19,509 --> 00:11:17,519
and its high sensitivity allows for

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00:11:21,829 --> 00:11:19,519
the detection of new complex molecular

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00:11:23,829 --> 00:11:21,839
species and also isotopes

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00:11:24,949 --> 00:11:23,839
these things together allow us to

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00:11:27,269 --> 00:11:24,959
examine the

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00:11:28,470 --> 00:11:27,279
chemical complexity and the evolution of

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00:11:30,310 --> 00:11:28,480
planetary atmospheres

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00:11:31,670 --> 00:11:30,320
and for titan in particular allows us to

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00:11:32,630 --> 00:11:31,680
continue the legacy of the cassini

350
00:11:35,110 --> 00:11:32,640
huygens mission

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00:11:36,230 --> 00:11:35,120
after its end in 2017 and observe

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00:11:37,910 --> 00:11:36,240
seasonal changes

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00:11:40,069 --> 00:11:37,920
in titan after its northern summer

354
00:11:41,990 --> 00:11:40,079
solstice these measurements will help us

355
00:11:45,030 --> 00:11:42,000
to constrain photochemical and dynamical

356
00:11:47,350 --> 00:11:45,040
models of titan's atmosphere and

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00:11:49,190 --> 00:11:47,360
we'll hopefully get more observations

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00:11:50,150 --> 00:11:49,200
that are dedicated observations of titan

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00:11:51,430 --> 00:11:50,160
in the future