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PDQ BACH Fort Sumner 1998

MP BACH M ulti P ixel B alloon-borne A ir CH erenkov Detection of Iron Cosmic Rays Using Direct Cherenkov Radiation Imaged with a High Resolution Camera. PDQ BACH Fort Sumner 1998. POD. Current knowledge of the iron spectrum.

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PDQ BACH Fort Sumner 1998

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  1. MP BACHMultiPixelBalloon-borne Air CHerenkovDetection of Iron Cosmic Rays Using Direct Cherenkov Radiation Imaged with a High Resolution Camera

  2. PDQ BACH Fort Sumner 1998 POD

  3. Current knowledge of the iron spectrum Energy spectrum of Iron cosmic rays multiplied by E2.5 from different observations. JACEE and RUNJOB, emulsion instruments, are a compilation of many balloon flights. CRN was conducted on the space shuttle. CREAM, ATTC and TRACER are balloon payloads flown from Antarctica and Sweden. BACH payload was flown from Ft Sumner. Soodpioneered the BACH technique. KASKADE (two different interaction models) and EAS-TOP (upper and lower limits) are air shower data. HESS data (two different interaction models) are ground level observations of Cerenkov light imaging.

  4. As the particle penetrates into denser air, the Cherenkov angle and intensity increase. First photons are emitted just on the axis defined by the particle path, but subsequent photons lie further and further from the axis when they reach any given depth in the atmosphere forming a circular spot or “pool” of light . This trend continues until the particle is roughly two scale heights (15 km) above an observer, when proximity finally wins out.

  5. CORSIKA Simulation • Simulates detailed particle propagation and generates CK photons in the atmosphere

  6. Light Pool at 35 km Altitude

  7. Idealized Detector Images, 500TeV Fe Camera locations in light pool Non- Interacting Interacting

  8. Cartoon Illustration ofMPBACH Event

  9. Deflection in the Earth’s Magnetic Field * Energy & Charge dependence *

  10. Extra slides

  11. Pixilated Camera Image

  12. With only the DCs, reconstruct trajectory εc is the CK emission vector as viewed from Camera 1 and 2 θcH Directional cosine observations from the camera and camera location on the gondola z S θcL Pathlength to emission point εca εcb y x θ φ (x2,0) (x1,0) (xo,yo) Camera 1 event plane Camera 2 event plane Intersection of Plane C1 and C2 forms a line that lies along the particle trajectory cross product of these two normal C1 and C2 vectors gives a vector which is perpendicular to both of them and which is therefore parallel to the line of intersection of the two planes. So this cross product will give a direction vector for the line of intersection. Set z=0 and solve for x and y

  13. Particle trajectory passes through the x,y plane at location xo,yo The particle incident angle with respect to z is θ and φ is the polar θc= Cerenkov angle which is a function of z (air density) Sis the trajectory straight path-length from the x-y plane intersection to the CK emission point as viewed by camera 1 No Magnetic Field z S θc Pathlength to emission point εc y x θ φ (x2,0) (x1,0) (xo,yo) It can be shown that S is related to the other quantities as εc is the CK emission vector as viewed from Camera 1 y Camera 2 Camera 1 x x1 z

  14. If the steepening at the cosmic ray knee is caused by a magnetic rigidity dependent mechanism, as a result of an acceleration process limited in a rigidity dependent manner or rigidity dependent propagation, there should be systematic changes in the cosmic ray composition through this region. It is difficult to see how SN could accelerate protons to energies much beyond ~1015eV/particle. Heavier cosmic rays, for example iron nuclei, could reach energies over an order of magnitude higher than this via the same mechanism. The objective of this project is to improve our knowledge of the Iron Flux from 5x103 to 3x106GeV

  15. Explicitly determine the relationship for the x,y crossing point at z=0 θcH z S θcL Pathlength to emission point εca εcb y x θ φ (x2,0) (x1,0) (xo,yo)

  16. Directional cosine observations from the camera and camera location on the gondola θca z S θcb Pathlength to emission point The trajectory vector S has been determine and is then used to calculate the Cerenkov angle at each intersection point εca εcb y x θ φ (x2,0) (x1,0) (xo,yo) The index of refraction at each intersection altitude point must be determined to calculate the energy

  17. Altitude (km) Altitude (km) ThetaC (degrees) Altitude (km)

  18. Results The calculated energy uses only the directional cosines, camera location and atmospheric model

  19. Camera 1 Image Camera 2 Image z degrees degrees y degrees degrees x θ φ (x2,0) (x1,0) (xo,yo) Example MPBACH Simulated Event Cartoon

  20. Cherenkov Light Distribution from Interacting and Non-Interacting Primaries Non-interacting Vertical Iron, 1PeV Cherenkov Total Light Output, 1PeV H He Fe Si O Peaks indicate the non-interaction events

  21. As the particle penetrates into denser air, the Cherenkov angle and intensity increase. First photons are emitted just on the axis defined by the particle path, but subsequent photons lie further and further from the axis when they reach any given depth in the atmosphere forming a circular spot or “pool” of light . This trend continues until the particle is roughly two scale heights (15 km) above an observer, when proximity finally wins out. 75km Altitude (km) 35km -8 0 8 Distance from Axis (m)

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