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you

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[Music]

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thank you for being here I'm speaking on

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behalf of my collaborators Maggie

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Turnbull Eric Mamo check Ella Osby a

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ginger Skolnick and the rest of the ASU

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Nexus team what we've done is we've put

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together multiple different sorts of

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stellar properties and we smash them

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together in order to form ketchup

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catalogue Estella unified properties

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yeah I made that pun all right so this

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is based off of EXO cat which is the

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catalogue that Maggie Turnbull put

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together about a year or two ago and

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this is created in order to support

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imaging mission such as W first what

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she's done is she's combined looked

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through all the literature and she's put

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together a stellar information for stars

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within 30 parsec so right now EXO cat

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has 2351 stars in it now one of the

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hardest things that maggie has done is

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she's actually tried to understand

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exactly how some of these stars are

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identified you'd think it'd be a simple

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one-to-one correlation but it's not so

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there are some stars for example that

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have a Hipparchus name but really they

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are two stars in there and one of them

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doesn't have a name or there are other

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cases where one star has two names or

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suddenly we see that there's unresolved

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stars at all sharing the same thing so

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this is actually fairly complicated when

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you're trying to very pointedly look at

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one specific object so Maggie has done

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the very time-consuming they're very

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painful task of going through and trying

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to identify when I say Hipparcos number

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what am I actually referring to so she's

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put together all of this information for

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the different components within the

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catalog

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she's also include the basic

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observational data and derive stellar

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parameters and as I said she's gone

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through and done the binary and multiple

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system breakdowns

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so all of ketchup is based on EXO cat

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but additionally we've added into that

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the Hypatia catalog so this is my own

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baby it isn't it is a stellar abundance

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catalog that's an amalgam it from 200

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different literature sources so what

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I've done is I've combined stellar

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abundance data for stars that are all

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within 150 parsecs of the Sun ftk type

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of 11 m/s and and combined all the stars

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that have both iron and a different

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element so what you're seeing on the

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x-axis are all the elements in the

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different species that are thin Hypatia

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but also the number of stars for which

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these elements have been measured so you

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see on right here is iron and that is

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going to be the most so it's five

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thousand nine hundred and eighty but we

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also have quite a number of elements

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that are sort of like the lower

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refractories and just as a little plug

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especially because I'm talking about a

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database the head patient catalog will

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soon be an online autonomous database

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such that anybody can go and look at

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this data and you can look at the

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multi-dimensional aspect of the data

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because I have stellar properties of

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abundances for stars as done by

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different groups so you don't just need

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to email me anymore you can go online

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yourself and look at the data and plot

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it in real time so that's going to be

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high patient catalog calm it should be

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available in the fall and there's going

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to be a special session at the double-a

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s winter and a booth so if you like swag

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I'll have swag alright so what we did

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was we combined then EXO cat and Hypatia

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and the overlap on that with about 800

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stars so x''k added about 2300 Hypatia

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as has 800 stellar abundances in

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addition to that Ella Osby and of Janish

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Skolnick once there ended a cross

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matching of all of these stars with

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Galax so as i mentioned by Adam earlier

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galaxy's is looking at UV photometry I

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have listed here the wavelengths of the

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different bands so what you're seeing in

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a blue are the far UV so what they're

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you can see like at a temperature

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greater than 5500 Kelvin which is where

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the photosphere is dominating so you're

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getting a rather tight correlation with

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temperature but then as temperature

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decreases below 5500 you're seeing a

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scatter because now the chromosphere

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sort of taken over being the dominant

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source and now we're seeing some stellar

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activity activity which is fairly

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interesting overlaid on top is in the

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red is the NIR UV and you see that we

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have far less stars that have near view

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measurements and that's because about

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5,200

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the we get is sort of the nonlinear

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response regime of Galax so what we're

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looking at with respect to this data is

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the incident UV flux that might happen

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that might occur on a planet's surface

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and how that would affect ultimately

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habitability so in that case we can look

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at the ratio of the flux densities and

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the far UV and near UV band passes so

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this is what we're looking at here on

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the X around the y axis with respect to

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them to the text effective temperature

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now Ella has gone through and she's

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removed all of the binaries from this

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sample to make sure that what we're

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seeing is really what we think we're

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seeing so for the stars that I have

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circled what we have are incidences of

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very high stellar activity which is very

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interesting and important to know with

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respect to this huge catalog now we have

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eric banachek who went through and did

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actually he did two things I didn't put

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up a slide but he went through and redid

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all of our spectral types he is the Guru

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as far as I'm concerned of all spectral

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type things so he redid all the spectral

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types for a source but he also did

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x-rays and so he went through and

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determined the x-ray fluxes luminosities

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and the fractional luminosities for

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stars within ketchup but he did so in a

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way that has never been done before he

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used three different missions so he

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looked at chandra which has a peak

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energy range of 0.5 to 7k UV and i had a

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total of 37 ketchup stars and he did x

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mm which is 0.15 to 15 ke v and had a

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total of 137 ketchup stars and I'm

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finally rosette which had a peak energy

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range of 0.12 to 4k TV and had had a lot

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so 907 ketchup stars so now these all

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these different missions have sort of

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different baselines and so he went

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through and and reconverted them to the

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same baseline in this case it was the

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rosette soft x-ray flux system such that

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apples could be compared to apples and

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we could look at these across the fan so

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this was brand new nobody's ever gone

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through and redoes all of these x-ray

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luminosities and from there we're able

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to infer the ages of these stars so

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altogether when you have ketchup you

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will have a lot of data so

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these I tried lifting it all of it just

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so you can understand the really like

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breath of what we're working with here

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so not only do have X ra Dec and XYZ

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coordinates but we have those component

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analyses that determined by Maggie and

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the different Hut part goes number Xin

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the system if that's the case where

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we're looking at overlaps we have a

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kinematic thin vs. thick disk

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determination BVB - the determinations

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and then we have this spectral type as

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we're done by Erik because he's awesome

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and this effective temperature that I've

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pulled from the pastel dataset I've

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included iron carbon oxygen magnesium

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silicon calcium and aluminum and as was

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mentioned by Patrick because I look I

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have an amalgam at data set of stellar

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abundances what that means is I have

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multiple groups who have measured the

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same element in the same star so when I

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go through and try to determine what and

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overall abundances I take not just the

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error that people gave me but I look at

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this difference or like what I call the

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spread between these groups because that

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in my mind is the most important

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understanding of how well do we know the

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abundance in a star and more often than

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not the spread between different groups

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is greater than their respective error

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that they tend to give so this is an

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overall a good indicator of how well do

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we understand these abundances so that

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will be included so the spread for the

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abundances then we have the new UV

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magnitude fluxes in there errors and the

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far UV for the ultraviolet and then

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we'll have all of this great information

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I'm not even going to read all of it off

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from the x-ray difference all the

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different x-ray sources so this will be

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coming soon we are almost finished with

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it in fact the goal especially since all

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my collaborators are in the room is to

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submit at the end of May we're doing

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this and that it will be available

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online because of course the whole point

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of doing this especially as as part of

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the ASU Nexus team is to put all the

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stages together such that people can use

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it and find out as much about these

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nearby stars as possible and use it in

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their own research thank you very much

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why not 35 parsecs Maggie why not 35

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parsecs

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why not 25 but just weird that number

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Maggie could you come up to the mic you

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know this is based on the Hipparcos

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catalog which is our most complete

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source of parallax information and you

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know beyond 30 parsecs ish hey you're

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not really complete with g-type stars

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anymore and be the I mean you're just

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including more and more junk in the

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sample basically I mean not that those

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aren't great stars but we just don't

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yeah

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would ya this is also true for the

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stellar abundances after about 30

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parsecs we the the sample just drops off

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pretty hard all right no more questions