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CREAM: at The High Energy at The High Energy Cosmic Ray Frontier Cosmic Ray Frontier Theresa Brandt COSMO 08 Madison, Wi. The Ohio State University Columbus, OH, USA 25 Aug 08 Bunerd The CREAM C ollaboration: University of Maryland H.

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SLIDE 1

at The High Energy at The High Energy Cosmic Ray Frontier Cosmic Ray Frontier

CREAM:

Theresa Brandt The Ohio State University Columbus, OH, USA COSMO 08 Madison, Wi. 25 Aug 08

Buénerd

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SLIDE 2

University of Maryland

  • H. S. Ahn, P. Bhoyer, O. Ganel, J.H. Han, K.C. Kim, M. H. Lee, L. Lutz, A. Malinine,
  • E. S. Seo, R. Sina, P. Walpole, J. Wu, J. H. Yoo, Y. S. Yoon, S. Y. Zinn

Ehwa Womans University, S. Korea

  • H. J. Hyun, J. A. Jeon, J. K. Lee, G. Na, S. W. Nam, I. H. Park, N. H. Park, J. Yang

University of Sienna & INFN, Italy

  • M. G. Bagliesi, G. Bigongiari, P. Maestro, P. S. Marrocchesi, R. Zei

University of Chicago

  • P. Boyle, S. Swordy, S. Wakely

Goddard Space Flight Center

  • L. Barbier, J. Link, J. Mitchell

Ohio State University

  • P. Allison, J. J. Beatty, T. J. Brandt

University of Minnesota

  • J. T. Childers, M. A. DuVernois

Northern Kentucky University

  • S. Nutter

Kent State University

  • S. Minnick

Penn State University

  • T. Anderson, N. Conklin, S. Coutu, M. Geske, S. I. Mognet

Kyungpook National University, S. Korea

  • H. Park

Laboratoire de Physique Subatomique et de Cosmologie,Grenoble, France

  • A. Barrau, O. Bourrion, J. Bouvier, B. B
  • yer, M. Buenerd, L. Derome, L. Eraud,
  • R. Foglio, L. Gallin-Martel, M. Mangin-Brinet, A. Putze, Y. Sallaz-Damaz, J. P. Scordilis

Centre d’Etude Spatiale des Rayonnements, Toulouse, France

  • R. Bazer-Bach, J.N. Perie

Universitad Nacional Autónoma de Mexico, Mexico

  • A. Menchaca-Rocha

The CREAM Collaboration:

and WFF

Also thanks to: NSF, INFN, KICOS, and MOST

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SLIDE 3

Tevatron LHC

  • S. Swordy, et. al.

All-particle CR Spectrum

25 Aug 08 3

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SLIDE 4

Abundance

Hörandel

C O N B Be Li F Sc Ti V

Cosmic ray abundances

➢

trace solar system values

➢

implying stellar origin.

Even-odd effect:

➢

Even-charge elements more abundant due to stability in stellar nucleosynthesis.

➢

Over-abundance of unstable elements in CRs implies spallation of primaries during propagation.

Fe

4

  • T. Brandt, Ohio State

25 Aug 08

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SLIDE 5

Cosmic Ray Energetics and Mass

CREAM III launch, Buénerd

Particle Detector

Charge and Energy:

➢ +1 ≤ Z ≤ 26 ➢ 1012 eV <~ E <~1015 eV

from 4 main subsystems:

➢ TCD (Z), TRD (E), SCD (Z), Cal (E)

Timing Charge Detector, Transition Radiation Detector, Silicon Charge Detector, and Calorimeter

Flown on a Long-Duration Balloon over Antarctica

➢ CREAM I: 42 days

(16 Dec 04 - 27 Jan 05)

➢ CREAM II: 28 days

(16 Dec 05 - 13 Jan 06)

➢ CREAM III: 28 days

(19 Dec 07 - 16 Jan 08)

  • T. Brandt, Ohio State

5 25 Aug 08

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SLIDE 6

Transition Radiation Det. (+Cherenkov):

➢ Ionization & TR ⇒ γ, Z ➢ Tracking (mm) and E ➢ Threshold: Z>3 ➢ Cher → γ → E

CREAM I

Timing Charge Det.:

➢ Scintillation ⇒ Z, β ➢ σZ ~ 0.2-0.35e

➢ High Z trigger

➢ PMTs read out with

  • v. fast electronics

Silicon Charge Det:

➢ Si ⇒ Z, E ➢ σZ ~ 0.2e ➢ smaller (area ~

half) acceptance than TCD Calorimeter:

➢ Inelastic interactions

in Carbon target

➢ Track secondaries ➢ W & Scin. fibers

measure Edep

➢ Hi E trigger

How CREAM (I) does all that.

6

  • T. Brandt, Ohio State

25 Aug 08

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SLIDE 7

Carbon: σ = 0.16 e

Charge

CREAM I 7

Oxygen: σ = 0.17 e from TCD and SCD

  • T. Brandt, Ohio State

25 Aug 08

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Energy

8

Cross-calibration of TRD and Calorimeter energy measurements

Maestro et al. 30th ICRC, Merida, 2007

Oxygen, Cal Carbon, Cal Oxygen, Cher Monte Carlo

  • T. Brandt, Ohio State

25 Aug 08

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SLIDE 9

Preliminary Results

9

  • T. Brandt, Ohio State

25 Aug 08

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SLIDE 10

(GeV/nucleus)

Carbon and Oxygen Spectra

CREAM Collaboration

10

Preliminary Preliminary

  • T. Brandt, Ohio State

25 Aug 08

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SLIDE 11

Boron:Carbon

11

CREAM I HEAO-3-C2 δ = 0.6 δ = 0.7 δ = 0.333

CREAM I, arXiv:080817.18

Lines:

  • Simple Leaky-box

model with range of propagation index δ

Error Bars: (Vertical)

  • Line: Statistical
  • Shaded: Systematic,

dominated by uncertainties in atmospheric secondary production at E > 300GeV/n

  • T. Brandt, Ohio State

25 Aug 08

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SLIDE 12

Nitrogen:Oxygen

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Lines:

  • Simple Leaky-box

model assuming δ = 0.6 with range of N/O in source

Error Bars: (Vertical)

  • Line: Statistical
  • Shaded: Systematic,

dominated by uncertainties in atmospheric secondary production at E > 300GeV/n CREAM I HEAO-3-C2 N/O = 10% N/O = 15% N/O = 5%

  • T. Brandt, Ohio State

25 Aug 08 CREAM I, arXiv:080817.18

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➢

CREAM data agrees with previous measurements and has extended the Carbon and Oxygen spectra in energy.

➢

CREAM has extended the Boron to Carbon and Nitrogen to Oxygen ratios with good statistics 2 orders of magnitude higher in energy.

➢

The galactic propagation index from B:C corresponds to a high energy propagation pathlength of ~1 g/cm2 and, in conjunction with the N:O ratio, suggests a source N abundance at high energies of ~10%.

➢

CREAM II and III have increased our statistics; further analysis is

  • forthcoming. Systematic errors can be reduced by improving our

understanding of nuclei interactions.

➢

CREAM IV is being prepared to fly again this winter.

Conclusions

13

  • T. Brandt, Ohio State

25 Aug 08