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you

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[Music]

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well first I'd like to thank my

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conference organizers for giving me the

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opportunity to speak with you today

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about some of my thesis research and

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low-mass stars and containing this trend

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of basically learning more about the

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m-dwarf population and this is doing and

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I'd also like to take a moment to

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acknowledge my collaborators on this

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project as well okay so first off as

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we've heard M Norris are really forming

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the dominant constituent of the sellout

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of population and this is visualized

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here on the right and a snapshot from a

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graphic from a drew Cordell and the

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recons team of the solar neighborhood so

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looking at the 25 parsecs with our Sun

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here at the center showing the over 20

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over 75 percent of the stars in our

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solar neighborhood are these low mass M

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dwarf stars and that we and as we've

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heard already this week there's great

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intrinsic interest in understanding the

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planet properties of these stars as well

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as investigating and assessing their

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however will zones and intrinsic

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properties so one of the things that

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despite the the great abundance

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preponderance of these low mass stars

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there's still a lot that we haven't

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learned yet about their binary

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properties the properties of their pro

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planetary discs and the platforming

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potential of these systems and so of

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course all of these three key aspects

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play into what we can understand about

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the habitable zones when these systems

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the disk truncation that might be

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altered by the presence of a binary

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companion the content of the disks

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youselves and a dynamical history and

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evolution and interplay between the star

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the disk and planet and so to

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investigate this today I'm going to be

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talking about two main results so there

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we go one field m-dwarf multiplicity so

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we're looking at just this interior 15

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parsec region of the closest brightest m

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dwarf to measure their binary properties

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and then we're going to move outward to

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the tourist star forming region one

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hundred and forty parts like distant

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which is about one to two million years

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old to understand the protoplanetary

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disk properties of much younger analog

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systems so starting off of the binaries

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the first thing that I talk about is our

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M dwarfs in multiples or mm survey so

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this is a volume limited survey of 245

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stars within fifteen parsecs and we can

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see that plotted here on this these are

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all about 500 stars

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within 15 parsecs of the Sun from the

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Hipparchus satellite we're looking at

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the brightness and V magnitude versus

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the color and we're focusing on this

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region here of the early M dwarf stars

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and the early to mid M dwarfs also have

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a nice match with the target selection

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that will be upcoming for for example

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the test mission which will look at the

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nearest brightest M stars with this

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population we're searching for stellar

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and sub speller companions so looking

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for binaries with orbital separations

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from about one of you all the way up to

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10,000 au and we're doing this with a

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combination of multi epoch imaging

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approaches so we have high-resolution

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archival high-resolution new and

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archival adaptive optics imaging and

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this lets us look very close in from

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about 1 to 100 au for close binary

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companions and we complement this with

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our tribal wide field plate imaging from

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a historic digitized surveys that really

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give us about more than 50 years of

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baseline to find comoving wide objects

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out to ten thousand eight so shown here

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we can see some of the example companion

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systems with a variety of architectures

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mass ratios between the primary and

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companion star and of this 245 stars we

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find about 65 of them have comoving

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stellar companions ranging from as close

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as about point Q all the way out to

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about 2500 au and on the right we're

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looking at our survey sensitivity so

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this is the mass in solar masses of a

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companion that we could detect in our

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imaging survey you can see that we get

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all the way down to the bottom of the

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main sequence so the transition between

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hydrogen burning stars to brown dwarfs

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and planets and then we are sensitive to

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about 3 au with a by 106 there's an

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almost hundred percent completeness to

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finding companions in this range so we

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can take these binary detection and we

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can start to look at kind of aggregate

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population properties of our nearest m

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dwarf neighbors and so what we're

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looking at here is the separation

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distribution so this is just a histogram

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of the fraction of systems as a function

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of the separation of the systems in the

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AU and what I want to take it like the

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take away home take a waypoint here to

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be is that the closer orbital

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separations are found with these lower

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mass primary stars so if we start with a

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type stars in about 300 au is where we

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find the typical binary separation if we

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move inward to solar-type fgk stars then

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it's about 30 au and

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you can see in our read mr. Graham here

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we actually don't see the population

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turnover but we see the bulk of the

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binaries are at this sort of six to ten

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au separation range so very very close

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tight binary systems we can then take

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our population and look at just a

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fraction of systems that have binary as

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all and so what we're looking at here is

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the companion star fraction as a

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function of primary mass so the most

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massive stars here solar-type stars are

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new I'm dwarf points and then the brown

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dwarf population and what we see is that

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we have decreasing multiplicities with

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decreasing primary mess well me about

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23% of M dwarfs have binary companions

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but what we're really looking at here is

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that we have fewer binary systems the

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ones that we do have are much much

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closer and this is of course going to

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have really important dynamical

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interactions with the extent of the

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habitable zone dynamical interaction

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between the disk and planets

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okay so we're going to move outward now

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140 parsecs distant to the torah' star

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forming region shown in the background

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here and what we wanted to do here was

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really understand the dust inventory

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within disks of these analog systems

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that are much younger around low-mass

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stars and what we wanted to be able to

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do with these measurements of the disk

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mass within the planetary disc is kind

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of get a handle on the planet forming

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potential of M dwarfs and how that might

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compare to that of higher mass stars

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then we can take those properties and we

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can try to understand how they might

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vary with the mass of the central star

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the region age and environment and so

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this is part of an ongoing survey the

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torus boundary is substellar or T Buster

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race and was started in 2014 we took far

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infrared detection of the lowest mass

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stars the latest M dwarfs and brown

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dwarfs in this young star forming region

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with known for our detections we know

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that they have protoplanetary disks and

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we followed them up with Alma 885 micron

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continuum observations and these really

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give us a handle on the submillimetre

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emission from the dust grains in the

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propietary disk systems and show here is

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that the population that we're looking

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at this time spans the breadth of the

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okay so what we found from the survey of

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24 targets which include 10-round or

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systems and twelve very low mass star

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systems is that we have 22 detections

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which is really quite a surprise these

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objects are so faint and young and the

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disks where the properties are pretty

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uncertain before we were able to use the

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sensitivity of allness to measure the

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disk the disk dust masses in these

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systems and so what we're looking at

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here is an example detection this is

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just the spectral energy distribution so

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the flux at different wavelengths in

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microns and so we see the contribution

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from the star here the tell-tale

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signature of a disk around the system

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and the new alma measurement here and

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something else you can see is that this

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is our beam size the resolving capacity

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of the all mobster patient's to

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understand the extent of the emission in

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the disk and you can see that we're

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actually starting to resolve these

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systems and get a handle on what the

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disk sizes are actually and so what we

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can do with these submillimetre

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continuum flexes is we hear a little bit

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before is we can use these to estimate

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the mass of dust and submillimetre

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grains for these lowest mass systems we

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find that they range from about 0.3 to

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22 earth masses in total of some

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millimetre greens so we can visualize

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this and I'll step through kind of

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everything that's going on this plot one

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step at a time

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right here we're looking at the disk

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dust mass in Earth masses so 110 100 as

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a function of the disco stellar mass in

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solar masses so we have the solar type

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FG k stars here we've got the M dwarfs

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that really span a broad range of

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stellar masses and the brown dwarf

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regime demarcate adhere the red points

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are our new observations from Alma and

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the background points are the what was

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previously known for the rest of torus

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for the higher mass population can see

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that we're extending this well into the

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brown dwarf regime with these detection

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also plotted here for reference

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comparison in high Smulders talkie

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tooter are the heavy element masses that

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are metric from the capillarity km stars

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and what we've shown up here to kind of

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guide the eye is an estimate of what the

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minimum a solar nebula

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should be so we're saying that from what

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we know about the solar system what's

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required to form Jupiter and the planets

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in our solar system if you estimate that

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to be about 30 earth masses were suggest

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then you can demarcate this regime as

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whether or not your disks actually have

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enough solid material to kind of make it

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into this into this region and what we

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see is that the early under worse and of

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course the fgk stars are making into

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this region but due to this decline in

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dust masses we go to the lowest mass Co

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stars the lower mass M dwarfs and brown

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dwarfs really aren't making it up into

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this regime and this is providing some

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signature potentially explaining why

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direct imaging surveys have looked have

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really focused on the lowest mass M

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dwarfs to find directly imaged Jupiter

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analogues but it's been very very

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difficult to find movies directly image

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giant planets around the lowest mass

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stars and for reference because we're

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all very keen on understanding where

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Trappist 1 and similar systems these

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exciting new transiting m dwarf

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exoplanet systems live chopped this one

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is right here at the brown dwarf brown

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dwarfs regime and if you take the

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estimated masses and the planets from

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the most recent papers you can see it

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kind of fits here sort of at the top of

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that envelope so this is giving us some

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idea of maybe starting to look into

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things like planet formation if this

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efficiency of the dust masses into

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planetary bodies and one more thing that

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we can do with these data is we can look

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at comparison between the very young 1

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million year old tourists are from your

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region and that of upper Scorpius which

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is in the 510 million range and so we're

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looking at here again is the same axis

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Deaf's mass and Earth's mass earth

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masses versus the mass of the star the

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red points are all of the young Taurus

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populations and then these older

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population is shown here in teal points

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for older for schoo population and what

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we can see is there's about a factor of

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3 decrease in the dust mask content from

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1 million years to about 10 million

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years and so this is giving us some idea

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about potential time skills for planet

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formation as these submillimetre grains

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are converted into potentially larger

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bodies and also on I suggest that you

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look forward to Ilario stock where she's

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going to be doing more of these

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comparisons with other types of star

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forming regions okay so in summary from

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these two investigations into low mass

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stars we have the binary occurrence is

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lower for M dwarfs but they're closer

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and this is going to have important

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impact on our understanding of the

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properties of these systems if we go to

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the younger population and do some

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investigations in the submillimetre we

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see that there's not only the stuff

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depletion but we see significant

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we've decreased dust masses for the

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lowest mass stars and brown dwarfs and

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maybe this is helping us understand

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what's happening in terms of the giant

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planet population as well as what's

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going on for the younger analog

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environments for systems like Trappist

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thank you for your time all right we

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three minutes in fact please come to the

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Maggie toka Alera Pascucci I wanted to

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know when you say that to resolve the

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Browns of disks with Alma what was the

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00:11:59,630 --> 00:11:55,709
beam that you had a beam was about point

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three 2.4 arc seconds and you always

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resolve the disc where you see origamis

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some are resolving some are unresolved

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and a quite a fear in this kind of

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marginal regime where they're only just

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resolved in the uv-plane okay all right

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so you can give a percentage erina Amish

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oh the fraction of systems um let's see

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00:12:19,010 --> 00:12:17,160
it was actually a bit surprising that

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both the brown dwarfs and M dwarfs had

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kind of equal fractions of resolved

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00:12:25,460 --> 00:12:23,220
disks which then again may say something

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00:12:26,780 --> 00:12:25,470
about the formation processes that are

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undergoing in this different stellar

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masses of systems but kind of close to

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the 50 G's ffth percent range tadka

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masak university of arizona so when you

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showed that the M dwarf companion

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fraction was increasing towards closer

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separations

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that's from direct imaging of course so

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what about RV oh yeah yeah that's great

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so there's a section that mysterious gap

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within three au where we're not actually

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sensitive to companions is a perfect

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place to do the radial velocity and

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spectroscopic binary population and

355
00:13:01,610 --> 00:13:00,060
there hasn't been a comprehensive survey

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00:13:03,560 --> 00:13:01,620
to look at like a volume limited sample

357
00:13:05,780 --> 00:13:03,570
in the same way but some preliminary

358
00:13:07,699 --> 00:13:05,790
estimates and some actually estimates

359
00:13:10,010 --> 00:13:07,709
from the kepler eclipsing binary sample

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place that even higher so maybe kind of

361
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closer to the like the 16% range at max

362
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but it's desperate for like a

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combination of all the techniques to

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00:13:23,689 --> 00:13:21,680
absolutely thank you wait I had one

365
00:13:26,150 --> 00:13:23,699
Chris yeah I just wanted to know those

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deaths masses in the indoors are there

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any correlations with ages of the system

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00:13:33,030 --> 00:13:31,180
yeah so we we looked at that and the

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ages are difficult the tourist is

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thought to have some spread in age not

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just to be one to two million years but

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also to have some intrinsic spread but

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from the values that were reported for

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the ages of the systems that we looked

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00:13:47,280 --> 00:13:44,530
out there was no correlation between

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seeing the slightly older tourists have

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a lower desk population but the agents

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00:13:53,280 --> 00:13:51,670
right knees are pretty big yeah okay

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thank you all right let's thank our