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the Cana Tory transport vehicle carrying

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supplies to the International Space

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Station is carrying a lot of supplies

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for science onboard including a large

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astrophysics mission coming up

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unpressurized on the exposed pallet the

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colorimetric electron telescope known as

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colette is destined for the outboard end

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of Kibo out on the exposed facility for

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a study of high-energy cosmic rays and

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today we learn more about that from dr.

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John waffle he's a professor emeritus at

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Louisiana State University's Department

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of physics and astronomy and a

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co-investigator on the Colet team that's

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led by dr. Shoji Torre of Waseda

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University in Japan explained to us how

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this telescope works I mean how does it

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go about searching for cosmic rays

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okay well cosmic rays come at you from

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all directions and all the time because

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they may originate outside our solar

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system elsewhere in the galaxy so what

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we basically do is sit there and just

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look so it's a long exposure every time

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one of these high-energy cosmic rays

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comes at us and it starts triggering the

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instrument and we were then we record it

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add it to the data set and eventually we

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will build up enough statistics to

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analyze for all the things that were

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that were interested in I guess that's

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the question then what is it are you

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interested in then astrophysicists

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what's the value of knowing about cosmic

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rays okay well cosmic rays are the

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highest energy particles known in the

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universe nature somehow accelerates

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cosmic rays to vast energies far higher

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than we can do that at the biggest

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accelerator for example the LHC at CERN

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and what we're interested in is is a how

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they do that and be what material is

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being accelerated what where did this

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stuff come from and so to do that what

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we want to do is we want to measure the

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composition we want to know how many

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electrons are there how many protons I'm

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a helium carbon nitrogen oxygen iron etc

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to try to piece together this whole

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question of how nature does this massive

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acceleration how it ejects these

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particles that have been with us in our

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solar system for billions of years based

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on the old meteorite measurements oh and

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they're a standard part of our of our

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environment you're taking a census of

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what's out there we're taiking to take a

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census evolve it but we're trying to

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take it at at higher energies and it's

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ever been taken before and that's that's

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the key as you move to the higher and

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higher energy that's where they we're

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beginning to see now that's where the

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action is starting to show up well one

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of the the stated goals here is that

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you're using this to address the

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existence of dark matter

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how does measuring cosmic rays help you

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do that well the whole idea here is that

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if there are dark matter particles out

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there of one sort or another and they

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they're their own antiparticle so they

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annihilate with with each other when

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they do that they turn into normal

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particles ie they turn into electron

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positron pairs or they turn into proton

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any protons or they turn into various

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kinds of W bosons things like that but

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when they do that they're their mass

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energy the rest mass becomes their

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kinetic energy so they suddenly appear

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at these very very high energies as a

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particle zipping around just like the

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cosmic rays so the idea is you may be

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able to find them within the cosmic ray

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beam now to do that we have to look and

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see if we can find some kind of anomaly

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and the electron plus positron spectrum

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or we also have a capability to measure

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very high-energy gamma rays see if we

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can find a signature in in the gamma ray

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region at these ultra high energies I

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also read that your

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interested in finding what it says are

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nearby sources of high-energy cosmic

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rays I mean how close are you looking ok

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well nearby is is a has to be viewed and

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astronomers terms and I will what were

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basically looking for is sources that

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are within about one thousand parsecs of

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the solar system and are less than about

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10 to the fifth years old

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that's one about a hundred thousand

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years old why is that

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well the reason is that at the electrons

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unlike protons and other particles they

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lose energy via inverse Thompson and

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synchrotron processes as they move

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through the galaxy interacting with

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matter photons and magnetic fields and

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they lose energy at a phenomenal rate

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what that means is that these very high

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energies they can't travel very far

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before they're totally degraded thus

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anything we see has to be coming from

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somewhat relatively nearby otherwise it

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would just never get here from there so

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in that sense what you do is then you

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sit around and say well what's out there

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within within a kiloparsec from us and

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you find things like supernova remnants

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mono gems of burnover reminisce

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Cygnus loop the Velo supernova remnant

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and you say well could these be

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producing high-energy electrons and so

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you go back to some of the theories and

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do some more calculations and you come

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out with yes they could be maybe not but

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they could be so the idea being if we

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can see one of these sources sticking up

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beyond above the normal background of

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all the other electron positrons that

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are matter that we're seeing we would be

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able to actually pinpoint a for the

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first time a source of charged particle

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acceleration that was in our relatively

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nearby or close solar neighborhood you

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might you might say that would give us

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something phenomenal to study because

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then we

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go out looking to see what these

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particular objects if we can pin it down

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are actually doing in detail and learn a

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whole lot about what makes them tick

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well dr. Zweifel good luck the interest

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to do to see it fly and and see it go to

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work and we are equally as well

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interested in the successful launch and

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starting to get some data after all

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these years so thank you very much thank

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you dr. John Wavell is professor

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emeritus at Louisiana State University