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you

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[Music]

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all right thank you very much I'm a

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member of the GPI instrument team as

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well as the X plan of survey team I'm a

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co-lead for the debris disc science and

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today I'll give you a update on the

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progress of our survey now that is

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great so the purpose of our survey is to

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explore this region between 5 and 50 au

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for young jupiter-mass planets let's see

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roughly some kind of work right here all

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right good all right in this region

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right here this is a plot of semi-major

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axis versus planet mass previous direct

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imaging surveys were sensitive to wider

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separation planets and now we're

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extending to this region here which is

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beginning to overlap with the radio

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velocity detected planets between 5 and

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10 and you we've been awarded 890 hours

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of Gemini South time making this one the

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largest and most Ematic surveys for

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extrasolar planets the other large

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survey is being conducted by sphere on

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the VLT we have 600 targets that we plan

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to observe so far we've observed 340 G

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pi is specifically designed for high

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contrast imaging it's a facility

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instrument though so there are many

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users and principal investigators

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outside of the G PI's team who are

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interested in for example imaging pre

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main sequence stars or some targets

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which are not on our reserve catalogue

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you need a star that's brighter than

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ninth magnitude to serve as a natural

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guide star has a relatively small field

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of view of 2.8 arc seconds by 2.8 arc

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seconds and it achieves a relatively low

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spectral resolution in that

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the survey started in December of 2014

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it's strictly conducted in the H band

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and we also have a dual channel

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polarimetry mode where we search for

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polarization signatures from scattering

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from dust grains around stars the the

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sample of stars was developed in a

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period of three years preceding the

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survey by Jenny patients and in Suk song

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and we've selected stars that are all

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roughly younger than 300 million years

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and within 150 parsec these are the

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directly image planets so far with cheap

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I three of these have three of these

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systems are previously known HR 8799 9

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508 6b and beta pick B and our new

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detection is 51 Airy p51 Airy is

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actually part of the beta pick moving

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group so it's age is 20 million years it

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is a hierarchical triple system so

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there's a 2,000 a you to the south or

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roughly an arc minute to the south

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there's a close pair of binary M dwarfs

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the mass of 51 a DB is roughly 2 to 3

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Jupiter masses and because it's such a

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young system it was imaged many times

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before by the previous generation of

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instrumentation so this really

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highlights the fact that this improved

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contrast provided by G PI really makes a

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difference in our exploration parameter

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space the spectrum shows deep methane

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absorption so much like here's the

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methane band here and H band we see this

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absorption so it's very much like our

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own Jupiter Eric Nielsen one of our

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postdocs is developing our sensitivity

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assessing the sensitivity of our survey

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after 300 stars and this is our

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sensitivity plot our current sensitivity

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plot as function of planet mass

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whose 10 Jupiter masses at semi-major

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axis previous surveys would not have

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been sensitive to planets in this regime

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and this is in fact what GPI is

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accomplishing and this point shows the

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detection of 51 re B it's very

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interesting now now this is a plot of

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our entire sample so far but you can

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split the sample up into the different

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spectra the stellar masses and this is

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quite interesting if you look at our our

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sensitivity limits as function of

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spectral type or stellar mass all the

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extrasolar planets are detected around

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higher mass stars so we were sensitive

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indeed to jupiter-mass planets at this

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range of semi-major axis around lower

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mass stars but they have not been

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detected they're not there so there

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seems to be a strong correlation of the

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frequency of giant planets in the 5 to

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58 you read semi-major axis region with

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stellar mass we still want to finish our

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survey to see if this is confirmed this

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is real and in fact as we image the

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remainder of our sample and other 260

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here's an image gallery of the debris

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disks we've imaged the structure and

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morphology of these debris disks can

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indicate the presence of sub

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jupiter-mass planets that aren't

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directly detected but modified through

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gravitational perturbations the

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structure of the debris disks so for the

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remainder of the talk I wanted to

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highlight sort of the wider impact of G

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pie and I'll discuss two systems which

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both have debris disks and directly

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image planets one is HD 106 906 where

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the central star is actually a binary

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pair of f5 stars age 30 million years

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and ska sin and I'll also talk about

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beta pick which is a more massive star

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at 19.3 parsec in age 20 million years

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so first with 106 906 the

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extrasolar planet 106 906 be has 11

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Jupiter masses but it's at a very wide

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separation it's at 700 au from the star

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and this was in fact detected previous

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to the start of the G PI survey by

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Vanessa Bailey at all here in Arizona

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and with G PI what we accomplished is

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the detection of scattered light from

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the the debris disc surrounding the

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primary and the new result and it's

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quite surprising is that the debris disc

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detected with G PI it's position angle

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is misaligned

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with that of the star we looked at

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archival HST images and saw features in

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the outer region which suggested a

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highly perturbed debris disc and what

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I'm showing you here is our latest data

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using HST States this is unpublished to

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data the observations were made just six

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weeks ago confirming that the morphology

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of the outer disk is highly perturbed

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this is not instrumental this is the

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actual structure of the debris disk

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showing a long and flat westward

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extension and a radially truncated this

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is roughly 300 au and vertically

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distended eastern side as if the whole

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system is in the state of dynamical

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upheaval may be analogous to our own

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solar system's period of late heavy

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bombardment this work has already

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inspired two Theory papers that have

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come out investigating how the planet or

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a passing star could invoke these

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asymmetries we also have looked at the

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Alma cycle one data which is a non

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detection in the sense that the

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signal-to-noise of the cycle one data is

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two and a half or two sigma but the

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orientation of these contours is exactly

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aligned with the position angle of the

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disc and we've applied for cycle five

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Alma time to discover the spatial

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we'll be on to beta pick beta pick has

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always been known to be an edge-on

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system since it was first discovered in

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1984 so when the planet was discovered

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beta pick be an actual question was you

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have a directly image planet the system

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is edge on is this a unique case in

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nature where we would be able to

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characterize an extrasolar planet not

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only because it's directly imaged but

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because it will also transit the star so

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we've been monitoring beta picked B over

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the last three years using G PI we've

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published three papers on this and in

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our last paper we've determined the

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orbital elements very precisely here you

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can see that you can see the time here

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and that beta pick B is now about to

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transit in front of the star

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unfortunately our analysis indicates

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through this work by graduate student

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Jason Wang at Berkeley that the the

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orbital elements aren't a show that the

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inclination is not exactly a John

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unfortunately the planet will not pass

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in front of the star it's just missing

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it by 0.2 au or 10 mili arcseconds the

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good news is the hill sphere of the

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planet is transiting so this is an

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opportunity to search for planetary

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rings the what G PI has provided is this

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ephemeris for the transit which is now

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being used by many groups all around the

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world to monitor beta pick for planetary

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rings the hill sphere has already oops

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the hill sphere has already started

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passing in front of the star in early

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April by June 20th half a hill sphere

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will be in front of the star and closed

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approaches August 31st problem is that

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beta pick is at right ascension six

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hours so you can observe it from most

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observatories in the summer so we have

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two solutions we have a Hubble program

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to monitor beta pick using whiskey three

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uva's in spatial scanning mode we've

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already obtained data at two epochs

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or the ingress and we will re observe

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beta pick in July in August to see if

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there's been any extinction of life due

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to foreground dust surrounding the

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planet we also have collaborated with

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teams in Antarctica it turns out that

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Antarctica is a great place for

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astronomy in July and August because

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it's always dark there the the Chinese

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and French have transit monitoring

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telescopes there the Chinese at dome a

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and the French at dome C and the French

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in particular will be monitoring beta

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pick 24 hours a day seven days a week

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through all of July and August searching

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for ring signatures what do we expect to

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find well what about moons the transit

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depths of a moon of moons is roughly a

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micro max so we don't have that

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precision our precision is roughly a

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millimes so that is very very good for

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detecting rings and if the structure of

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rings shows gaps maybe we could also

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infer the presence of circum planetary

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moons okay so that was a brief summary

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of what we've accomplished with with g

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pi to date loud covered one new

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extrasolar planet we've determined the

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orbital elements of the other extra

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planets we can characterize their

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atmospheres through the spectra that we

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obtain with G PI and there's a much

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broader impact with follow-up HST and

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Alma imaging as well as hopefully with

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JWST in the future and this transit

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monitoring campaign of beta pick is

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ongoing with the potential of

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discovering planetary rings around

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another planet thank

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[Applause]

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excellent thank you we have about three

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minutes for questions so if you have a

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question please come up to the mic

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okay well I think we'll thank you very

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much on to our next speaker oh we have a

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question Oh perfect thanks Paul

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it's great to see the results coming

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along and I want to ask about the

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sensitivity plot you showed earlier in

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your talk we had the contours yeah

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and was there an assumption in those

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sensitivity calculations of if each star

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had one planet then we should have seen

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seen it - this many stars or was it

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driven by a current rates of it was

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really rare occurence rates yeah so we

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were in fact using some of the

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occurrence rates in terms of the the

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distribution of orbital elements is that

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from RV surveys is that what you're

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asking right yeah I know the activity of

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obvious stops Peter out once you get to

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know yeah we were all but although some

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of the assumptions have to do with the

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RV statistics from from coming at Al and