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Laboratory Astrophysics in Taiwan-studying properties of cosmic ray showers using NSRRC
1.5 GeV electron beam
G.-L. Lin
National Chiao-Tung U.
Taiwan
KAW4 2006
Outline
• General Features of Laboratory Astrophysics
• Fluorescence Measurements Using SLAC 28.5 GeV e- beam
• Cherenkov Measurements Using NSRRC 1.5 GeV e- beam
• Concluding remarks
1. Calibration of observations - Precision measurements to calibrate observation processes - Development of novel approaches to astro-experimentation - Though non-exotic, value to astrophysics most certain
2. Investigation of dynamics - Astro-conditions hard to recreate in the lab - Many MHD or plasma processes scalable by extrapolation
3. Probing fundamental physics - Underlying physical principles in nature still to be discovered - Extreme limits render signatures faint – a challenging task - Though challenging, potential returns in science most significant
General Features of LabAstro-Using Lasers and Particle Beams as Tools -
P. Chen, Workshop on laboratory astrophysics using high intensity particle and photon beams.
Fluorescence from Air in Showers(FLASH)
J. Belz1, D. Bergman5, Z. Cao2, F.Y. Chang4, P. Chen3*, C.C. Chen4, C.W. Chen4, C. Field3, P. Huentemeyer2, W-Y. P. Hwang4, R. Iverson3, C.C.H. Jui2,
G.-L. Lin4, E.C. Loh2, K. Martens2, J.N. Matthews2, J.S.T. Ng3, A. Odian3, K. Reil3, J.D. Smith2, P. Sokolsky2*, R.W. Springer2,
S.B. Thomas2, G.B. Thomson5, D. Walz3, A. Zech5
1University of Montana, Missoula, Montana2University of Utah, Salt Lake City, Utah
3Stanford Linear Accelerator Center, Stanford University, CA4Center for Cosmology and Particle Astrophysics (CosPA), Taiwan
5Rutgers University, Piscataway, New Jersey
* Collaboration Spokespersons
The Motivation For FLASH
• The ultra-high energy cosmic ray (UHECR) spectra measured by HiRes (fluorescence) and AGASA (scintillation counter ground array) differ significantly in slope for E~1020 eV.
• This discrepancy can be possibly accounted for by a systematic difference in the energy scale (~25%)
The Energy Reconstruction of UHECR
in the Fluorescence Technique
L. R. :
0
00
dX
dE
X
E
eXdXXNX
EE
ionc
ec
em
Fitted from the atmospheric scintillation process—model independent!
D. J. Bird et al., APJ 424,491-502,(1994)
How well do we know the fluorescence efficiency?Can the fluorescence yield accurately reconstruct the longitudinal profile Ne(X)?
Integrating the energy deposition alongthe path and correcting for missing energy
Beam spot monitor
Main fluorescence chamber
Grating spectrograph
Beam dump
Toroid
The thin target Experiment Layout
PMT
Filter wheel
LEDs
Fluorescence vessel
bafflers
The Existing Air Fluorescence Yield Measurements—without Showers
• Kakimoto et al., NIM A372 (1996)
• Nagano et al., Astroparticle Physics 20, 293-309 (2003)
• Belz et al., to appear in Astroparticle Physics; astro-ph/0506741
• Huentemeyer et al., presented at ICRC 05
Universal electron energy distribution in different shower ages
F. Nerling et al., astro-ph/0506729
•The shower age S=3X/(X+2Xmax) determines the electron-positron spectrum. •Mean electron (positron) energies near the shower maximum are very similar for primary 30 GeV electrons and primary 1019 eV protons —superposition at works! SLAC is a right place as 31010 eV5 108/bunch~1019 eV.
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The Fluorescence Technique Validated
• Comparison of fluorescence yields and ionization longitudinal profiles. The sum of points in each profile is independently normalized to unity.
• The ion chamber data points correspond to slightly larger radiation lengths.
• Both fluorescence and ionization longitudinal profiles agree well with simulations(Geant3 and EGS4).
astro-ph/0510375, to appear in Astroparticle Physics
Studying Cherenkov light from air showers with NSRRC 1.5 GeV e- beam
T.C. Liua, F.Y. Changa, C.C. Chenb,C.W. Chenb, Y. T. Yangd, K.T Hsu.d,M.A. Huangc, P.W.Y. Hwangb, G.L. Lina
(a) Institute of Physics, National Chiao-Tung University, 1001 Ta Hsueh Rd., Hsin-chu, 300, TAIWAN, ROC.(b) Institute of Astrophysics, National Taiwan University, 1, Sec. 4, Roosevelt Rd. Taipei, 106, TAIWAN, ROC.(c) Department of Physics, National United University, 1, Lien-da, Kung-ching Li, Miao-Li, 36003, TAIWAN, ROC (d) National Synchrotron Radiation Research Center
Motivation• Cherenkov light is an important background in the fluorescence me
asurement. A correct estimation of this contribution is needed. F. Nerling et al. for Auger Collaboration, ICRC 05
• Previous estimation of Cherenkov contribution were based upon simulations. It is desirable to have a direct measurement.
Page 12
Page 30
NSRRC (National Synchrotron Radiation Research Center)
1993 Apr. First beam stored in the storage ring Oct. Taiwan Light Source Dedication Ceremony2000 Feb. 1.5 GeV full energy injection
The 1.5 GeV electron beamNational Synchrotron Radiation Research Center
Each bunch carries 109 electrons
Total energy ~ 1 EeVThe electrons are injected from booster ring with 10 Hz frequency
Experimental Platform
1.5 GeV electron beam
Removable radiator system
Light path
Thin Foil
Lateral Profile
Each block contains 1/3 R.L.
10cm2.9cm
10cm
1 r.l.=8.9 cm
The CCD quantum efficiency is not uniform
Fluorescence contributions arise between 300 nm and 400 nm.
The Cherenkov photon yield verse particle energy
The simulated longitudinal profile has to be folded with Cherenkov photon yield.
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The fluorescence contribution has to be subtracted from the data—using simulations tested by FLASH thick target experiment.Angular distributions of Cherenkov photons will be studied as well.
Concluding Remarks
• A brief history of laboratory astrophysics program in Taiwan was reviewed.
• We have shown the results of FLASH thin and thick target runs.
• The rationale of FLASH thick target run is applied to measure the Cherenkov light from particle showers using NSRRC 1.5 GeV electron beams. Work in progress!