A likelihood method for measuring the ultrahigh energy cosmic ray composition

被引：3

作者：

Abbasi, R. U.

Abu-Zayyad, T.

Amman, J. F.

Archbold, G. C.

Belov, K.

Blake, S. A.

Belz, J. W.

BenZvi, S.

Bergman, D. R.

Boyer, J. H.

Burt, G. W.

Cao, Z.

Connolly, B. M. ^{[1
]}

Deng, W.

Fedorova, Y.

Findlay, J.

Finley, C. B.

Hanlon, W. F.

Hoffman, C. M.

Holzscheiter, M. H.

Hughes, G. A.

Huntemeyer, P.

Jui, C. C. H.

Kim, K.

Kirn, M. A.

Knapp, B. C.

Loh, E. C.

Maestas, M. M.

Manago, N.

Mannel, E. J.

Marek, L. J.

Martens, K.

Matthews, J. A. J.

Matthews, J. N.

O'Neill, A.

Painter, C. A.

Perera, L.

Reil, K.

Riehle, R.

Roberts, M.

Rodriguez, D.

Sasaki, M.

Schnetzer, S.

Seman, M.

Sinnis, G.

Smith, J. D.

Snow, R.

Sokolsky, P.

Springer, R. W.

Stokes, B. T.

机构：

[1] Univ Utah, Dept Phys, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA

[2] Los Alamos Natl Lab, Los Alamos, NM USA

[3] Univ Montana, Dept Phys & Astron, Missoula, MT 59812 USA

[4] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ USA

[5] Columbia Univ, Dept Phys, Nevis Lab, New York, NY 10027 USA

[6] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA

[7] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba, Japan

来源：

ASTROPARTICLE PHYSICS | 2006年 / 26卷 / 01期

基金：

美国国家科学基金会;

关键词：

cosmic rays; acceleration of particles; composition;

D O I：

10.1016/j.astropartphys.2006.04.007

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Air fluorescence detectors traditionally determine the dominant chemical composition of the ultrahigh energy cosmic ray flux by comparing the averaged slant depth of the shower maximum, X-max, as a function of energy to the slant depths expected for various hypothesized primaries. In this paper, we present a method to make a direct measurement of the expected mean number of protons and iron by comparing the shapes of the expected X-max distributions to the distribution for data. The advantages of this method includes the use of information of the full distribution and its ability to calculate a flux for various cosmic ray compositions. The same method can be expanded to marginalize uncertainties due to choice of spectra, hadronic models and atmospheric parameters. We demonstrate the technique with independent simulated data samples from a parent sample of protons and iron. We accurately predict the number of protons and iron in the parent sample and show that the uncertainties are meaningful. (c) 2006 Published by Elsevier B.V.

引用

页码：28 / 40

页数：13

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