Multimessenger PerspectivesMultimessenger PerspectivesTeV Particle Astrophysics 2009, Menlo Park, CA, July 15, 2009

Eun-Suk Seo

IPST and Dept. of Phys.University of Maryland

SOURCESInterstellar

medium ChandraSNRs, shocksSuperbubbles

photon emission

X, γe-

P e-γ

Synchrotron

Inverse ComptonBr

acceleration PHe

C, N, O etc.Z = 1- 92

γ

gas

P

Inverse Compton

Bremstrahlung

+

CGROEnergy lossesReacceleration

DiffusionConvection

PHe

C, N, O etc. gasHalo

Disk: sources, gas B

oπ+π −πe+e-

Voyagerγ

Exotic Sources:Antimatter

pescape

BBe

10Be ACE

ATIC

AntimatterDark matter etc..

AMSBESS

ATIC

CREAM

Cosmic Ray Propagation

Consider propagation of CR in the interstellar medium with random hydromagnetic waves.

Steady State Transport Eq.:⎤⎡

∑<

+=⎥⎥⎦

⎤

⎢⎢⎣

⎡⎟⎠⎞

⎜⎝⎛

∂∂

+∂

∂

∂∂

++∂

∂

∂∂

∂jk

jkjjionj

jjj

jj Sqf

dtdpp

pppf

Kppp

fvmz

fD

z ,

22

22

11σρ

The momentum distribution function f is normalized as where N is CR number density, D: spatial diffusion coefficient, σ: cross

section…

fpdpN ∫= 2

{ } kjk

jkjj

ionjj

j

e

j Im

QI

dxdE

dEdI

mXI

∑<

+=⎥⎥⎦

⎤

⎢⎢⎣

⎡⎟⎠⎞

⎜⎝⎛+++

σρ

ασ

0

...

Cosmic ray intensityEscape length XeReacceleration parameter α

jkionje <⎥⎦⎢⎣ ⎠⎝ ρ0,

)()( 02 pfpAEI jjj =

CREAM Eun-Suk Seo 3

Reacceleration parameter αE. S. Seo and V. S. Ptuskin, Astrophys. J., 431, 705-714, 1994.

Cosmic Ray Energetics And Mass (CREAM)

TCDTCDTCD

Upper TRD

Lower TRD

Cherenkov

Upper TRD

Lower TRD

Cherenkov

Upper TRD

Lower TRD

Cherenkov

Calorimeter

Lower TRD

SCD S0/S1Target 1Target 2

Calorimeter

Lower TRD

SCD S0/S1Target 1

Calorimeter

Lower TRD

SCD S0/S1Target 1Target 2

CommandDataM d l

CommandDataM d l

CommandDataM d lModuleModuleModule

H. S. Ahn et al., NIM A, 579, 1034-1053, 2007; Seo et al, Adv. Space Res. 42, 1656-1663, 2008

CREAM 4Eun-Suk Seo

Four successful flights: ~119 days cumulative exposure

CREAM-I12/16/04 – 1/27/05

Record breaking 42 days

CREAM-II12/16/05-1/13/06

28 d

CREAM-III12/19/07-1/17/08

29 d

CREAM-IV12/19/08 – 1/7/09

19 days 13 hrsRecord breaking 42 days 28 days 29 days 19 days 13 hrs

Many thanks to CSBF, WFF, NSF & RPSC for a great campaign!

CREAM 5Eun-Suk Seo

Charge MeasurementsAhn et al, Nucl. Instr. and Meth. A , 602, 525, 2009; Park et al., Nucl. Instr. Meth. A, 581, 133-135, 2007

TCD

SCD

Si

Fe

σ ~ 0 2e p HeC

ONNe

MgSi

CREAM Eun-Suk Seo 6

σz 0.2e p

Calorimeter data for > 3 decades in energySeo et al., Nucl. Phys. B Proc. Suppl. 176, 155, 2008; Seo et al, J. Phys. Soc. Japan, Suppl. A. 78, 63, 2009

• Consistent power law for all particle data from 4 flights• Lower Energy Threshold for CREAM-III & IV

1014 eV

1015 eV

CREAM 7Eun-Suk Seo

What is the history of cosmic rays in the Galaxy?Ahn et al. Astropart. Phys., 30/3, 133-141, 2008

• Measurements of the relative abundances of secondary cosmic rays (e g secondary cosmic rays (e.g., B/C) in addition to the energy spectra of primary nuclei will allow determination of cosmic-ray determination of cosmic ray source spectra at energies where measurements are not currently available

• First B/C ratio at these high energies to distinguish among the propagation

d lmodelsδ−∝RXe

CREAM Eun-Suk Seo 8

Elemental e e aSpectra

CREAM Eun-Suk Seo 9

P & He: prior to CREAM

γ−∝EI ∝EIj

JACEE J CγP = 2.80 ± 0.04γHe = 2.68+0.04-0.06

ATIC2γ = 2 63 ± 0 01AMS

RUNJOBγP = 2.78 ± 0.05

(2.74 ± 0.08) γ = 2 81 ± 0 06γP = 2.63 ± 0.01

γHe = 2.58 ± 0.01γP = 2.78 ± 0.009γHe = 2.74 ± 0.01

γHe = 2.81 ± 0.06(2.78 ± 0.2)

CREAM Eun-Suk Seo 10

CREAM: p & He spectra are not the sameOur fluxes are significantly higher than the extrapolation of a single-power law fit to the l

Unpublished Data low energy spectra

Different types of

Not shownDifferent types of sources or acceleration mechanisms? (e g mechanisms? (e.g., Biermann, P. L. A&A 271, 649,1993)

CREAM Eun-Suk Seo 11

TeV spectra are harder than spectra <100 GeV/n Departure from a single power law caused by cosmic ray interactions

ith th sh ck?with the shock?(e.g., Ellison et al. ApJ540, 292, 2000)Unpublished Data The reported flattening of the synchrotron spectrum of SN1006 indicated spectral curvature which

Not shownspectral curvature, which provides evidence that cosmic rays are dynamically important (Allen et al. ApJ683/2,773, 2008).

CREAM Eun-Suk Seo 12

Heavies look like He

Unpublished Data Not shown

CREAM Eun-Suk Seo 13

Electrons: the same valley?

Chang et al. Nature, 456. 362, 2008

Abdo et al. PRL, 102, 181101, 2009

If so is a single mechanism responsible for all the If so, is a single mechanism responsible for all the elements, as well as electrons?

CREAM Eun-Suk Seo 14

Results & Implications

• Spectral difference between p and He– Are there different types of sources or acceleration mechanisms? Are there different types of sources or acceleration mechanisms?

(Biermann, P. L. A&A 271, 649,1993)• Flattening of elemental spectra at high energies

– Evidence for concavity due to cosmic ray interactions with the shock? Evidence for concavity due to cosmic ray interactions with the shock? (Ellison et al. ApJ 540, 292,2000; Allen et al. ApJ 683/2,773, 2008).

– Indicate source spectra that are harder than previously thought, based on the low energy data?

Some propagation effect, such as reacceleration, boosts low energy spectra? – Contributions from multi sources (Zatsepin & Sokolskaya, A&A 458, 1,

2006)f ff f l d f h l – If not an effect of acceleration or propagation, and if the conventional

model is valid, are we seeing a local source of hadrons? Related to 10 TeV anisotropy reported by Milagro (Abdo et al. PRL, 101, 221101, 2008)?221101, 2008)?Related to the electron excess reported by ATIC?

CREAM Eun-Suk Seo 15

Refurbish CREAM-III (IV) for CREAM-V (VI) integrationCREAM-V Launch is planned for December 2009

CREAM Eun-Suk Seo 16

A step closer to ULDB

Successful SPB Test Flight

7 MCF At FloatThe super pressure balloon’s altitude stability

CREAM-IV

ANITA-II

SPB

CREAM Eun-Suk Seo 17

54 days (12/28/08 – 2/20/09)

http://cosmicray.umd.edu/creamCREAM Collaboration

http //cosm cray.um . u/cr am

E. S. Seoa,b, H. S. Ahn a, P. Allisonc, T. Andersond, M.G. Bagliesie, L. Barbierf, A. Barraug, R. Bazer-Bachig, J. J. Beatty c, G. Bigongiarie, P. Bhoyar a, P. Boyleh, T. T Brandt c M Buénerdg N B Conklind S Coutud L Deromeg M A DuVernois j T. Brandt , M. Buénerdg, N. B. Conklin , S. Coutu , L. Deromeg, M. A. DuVernois j, O. Ganela, M. Gesked, J. H. Hana, J. A. Jeonk, K. C. Kima, M. H. Leea, J. Linkf, L. Lutza, A. Malinina, M. Mangin-Brinet g, P. S. Marrocchesie, P. Maestroe, A. Menchaca-Rochal, J. W. Mitchellf, S. I. Mognet e, G. Nak, S. Namk, S. Nutterm, I. H. Parkk, N. H. Parkk, J. N. Périég , A. Putzg, Y. Sallaz-Damazg, S. Swordyh, S.

h k by

Wakelyh, P. Walpolea, J. Wua, J. Yangk, Y. S. Yoonb, R. Zeie, and S. Y. Zinna

aInst. for Phys. Sci. and Tech., University of Maryland, College Park, MD 20742, USAbDept. of Physics, University of Maryland, College Park, MD 20742, USA

cDept of Physics Ohio State University Columbus Ohio 43210 USADept. of Physics, Ohio State University, Columbus, Ohio 43210, USAdDept. of Physics, Penn State University, University Park, PA 16802, USA

eDept. of Physics, University of Siena and INFN, Via Roma 56, 53100 Siena, ItalyfNASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

gLaboratorire de Physique Subatomique et de Cosmologie, Grenoble, FrancehE i F i I i d D f Ph i U i i f Chi Chi IL 60637 USAhEnrico Fermi Institute and Dept. of Physics, University of Chicago, Chicago, IL 60637, USAiCentre d’Etude Spatiale des Rayonnements, UFR PCA - CNRS - UPR 8002, Toulouse, France

jSchool of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USAkDept. of Physics, Ewha Womans University, Seoul, 120-750, Republic of Korea

lInstituto de Fisica, Universidad Nacional Autonoma de Mexico, Mexico

CREAM Eun-Suk Seo 18

Instituto de Fisica, Universidad Nacional Autonoma de Mexico, MexicomDept. of Physics and Geology, Northern Kentucky University, Highland Heights, KY 41099,

USA