Detection of Antimatter in our Galaxy

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1 Impossibile visualizzare l'immagine. La memoria del computer potrebbe essere insu!ciente per aprire l'immagine oppure l'immagine potrebbe essere danneggiata. Riavviare il computer e aprire di nuovo il file. Se viene visualizzata di nuovo la x rossa, potrebbe essere necessario eliminare l'immagine e inserirla di nuovo. Detection of Antimatter in our Galaxy Piergiorgio Picozza INFN and University of Rome Tor Vergata TAUP 2009 Rome, Italy July 1-5, 2009

2 ANTIMATTER Collision of High Energy Cosmic Rays with the Interstellar Gas Annihilation of Exotic Particles Cosmic Rays Leaking Out of Antimatter Galaxies e + p e + p p e + p Evaporation of Primordial Black Holes e - e + Antimatter Lumps In the Milky Way He e + e - e + Pulsar s magnetospheres

3 AMS The Big Bang origin of the Universe requires matter and antimatter to be equally abundant at the very hot beginning

4 Robert L. Golden

5

6 We must regard it rather an accident that the Earth and presumably the whole Solar System contains a preponderance of negative electrons and positive protons. It is quite possible that for some of the stars it is the other way about P. Dirac, Nobel lecture (1933)!

7 Rotation curves of galaxies CMB Large Scale Structure Galaxy clusters Lensing SN Ia Bertone, Hooper & Silk, hep-ph/ Bergstrom, hep-ph/ Jungman et al, hep-ph/

8 THE UNIVERSE ENERGY BUDGET

9

10 Signal (supersymmetry) and background (GLAST-FERMI AMS-02)!

11 Another possible scenario: KK Dark Matter Lightest Kaluza-Klein Particle (LKP): B (1) As in the neutralino case there are 1-loop processes that produces monoenergetic!! in the final state. Bosonic Dark Matter: fermionic final states no longer helicity suppressed. e+e - final states directly produced.

12 Charge-dependent solar modulation Asaoka Y. Et al Present status Solar polarity reversal 1999/2000 " Antiprotons Positrons Moskalenko & Strong 1998 Positron excess? + CR + ISM! p-bar + kinematic threshold: 5.6 GeV for the reaction CR + ISM! " ± + x! µ ± + x! e ± + x CR + ISM! " 0 + x! ##! e ±

13 PAMELA ATIC BESS AMS GLAST/Fermi GAPS 2013 PEBS 2013

14

15 Italy: Bari Florence Frascati Naples Rome Trieste CNR, Florence Russia: Moscow St. Petersburg Germany: Siegen Sweden: KTH, Stockholm

16

17 Flight data: 84 GeV/c interacting antiproton

18 Flight data: 84 GeV/c interacting antiproton

19 Flight data: 92 GeV/c positron

20 Energy range!! Antiprotons 80 MeV GeV!! Positrons 50 MeV 300 GeV!! Electrons up to 500 GeV!! Protons up to 1 TeV!! Electrons+positrons up to 2 TeV (from calorimeter)!! Light Nuclei (He/Be/C) up to 200 GeV/n!! AntiNuclei search sensitivity of 3x10-8 in He/He "!!"#$%&'()*$+,#)'+$-)#)(&,*.,#'(/,0*+#"01-'/,+2)0")+,, "! 3)4,)()-5/,-'(5),, "! 6(2-)0)7)(&)7,+&'&"+&"0+,,

21 #! Main task: multi-spectral remote sensing of earth s surface #! Built by TsSKB Progress in Samara, Russia #! Lifetime >3 years (assisted) #! Data transmitted to ground via high-speed radio downlink #! PAMELA mounted inside a pressurized container Mass: 6.7 tonnes Height: 7.4 m Solar array area: 36 m 2

22

23 SAA 350 km 70 $ % 610 km

24

25

26 preliminary

27 !"#$"#!$$%&!'&

28 Secondary production Moskalenko & Strong 98

29

30 Pulsar Component Yüksel et al. 08 KKDM (mass 300 GeV) Hooper & Profumo 07 Pulsar Component Atoyan et al. 95 Pulsar Component Zhang & Cheng 01 Secondary production Moskalenko & Strong 98

31 DM particles are stable. They can annihilate in pairs. Primary annihilation channels Decay Final states

32 Which DM spectra can fit the data? Boost required by PAMELA

33

34 Wino Dark Matter in a non-thermal Universe G. Kane, R. Lu, and S. Watson arxiv: v3 [astro-ph.he)

35

36

37 All three ATIC flights are consistent Preliminary Preliminary ATIC ATIC 1 ATIC 2 ATIC 4 Source on/source off significance of bump for ATIC1+2 is about 3.8 sigma J Chang et al. Nature 456, 362 (2008) ATIC-4 with 10 BGO layers has improved e, p separation. (~4x lower background) Bump is seen in all three flights. Significance for ATIC1+2+4 is 5.1 sigma

38 I. Cholis et al. arxiv: v1 See Neal Weiner s talk

39 All electrons

40

41

42 Where do positrons come from? Mostly locally within 1 Kpc, due to the energy losses by Synchrotron Radiation and Inverse Compton Typical lifetime Antiprotons within 10 Kpc

43 H. Yüksak et al., arxiv: v2 Contributions of e- & e+ from Geminga assuming different distance, age and energetic of the pulsar diffuse mature &nearby young pulsars Hooper, Blasi, and Serpico arxiv:

44 Pulsars: Most significant contribution to high-energy CRE: Nearby (d < 1 kpc) and Mature (104 < T/yr < 106) Pulsars S. Profumo

45 Interaction of high energy gamma-rays with star-light F A Aharonian and A M Atoyan J. Phys. G: Nucl. Pan. Phys. 17 (1991)

46 ! = 3.54! = 3.34 T. Delahaye et al., arxiv: v3

47 Proton and Helium spectra, July 2006 Pamela preliminary

48 Li/C Be/C B/C

49 BESS-Polar II Launch - December 22, 2007 J.W.Mitchell and A. Yamamoto - Antimatter and Dark Matter from Space: BESS-Polar, PAMELA Physics Workshop 2009,Rome, Italy May 11,

50 BESS Detector!!Rigidity measurement!! SC Solenoid (L=1m, B=1T)!! Min. material (4.7g/cm 2 )!! Uniform field!! Large acceptance!!central tracker!!!(drift chamber!!!& ~200µm!! Z, m measurement! "!!!R,'!--> m = ZeR 1/! 2-1!!!dE/dx --> Z! TOF! ', de/dx! JET/IDC! Rigidity!

51 BESS Polar II Observations/Expectations! Event rate ~2.5 khz; Total events ~4.7 x 10 9! Total data volume 13.5 TB (3.07 kb/event)! Expected antiprotons ~10, times previous Solar minimum dataset Antiproton Antideuteron Antihelium (Search for PBH) (Search for PBH) (Search for Antimatter)! J.W.Mitchell and A. Yamamoto - Antimatter and Dark Matter from Space: BESS-Polar, PAMELA Physics Workshop 2009,Rome, Italy May 11,

52 95% of the $1.5 billion to build AMS has come from international partners. TRD! Vacuum! Case! Tracker! MAGNET! He Vessel! RICH! AMS is a DOE Sponsored International Collaboration

53 Manifested on STS-134 September AMS on ISS Magnet Time of Flight Silicon Tracker Calorimeter RICH

54 Gamma Rays

55 Direct search for antimatter: AMS on ISS He Li Be B C Collect 2 billion nuclei with energies up to 2 trillion ev N O F Ne Na Mg Al Si P S Cl Ar K Ca Sc Ti V Cr Mn Fe Co y06k301 Atomic Number Sensitivity of AMS: If no antimatter is found => there is no antimatter to the edge of the observable universe (~ 1000 Mpc).

56 antiprotons Unique Feature Of AMS positrons Combining searches in different channels could give (much) higher sensitiviy to SUSY DM signals gamma rays anti deuterons

57 ! Pair annihilating WIMPS produce: _ #, ), e + p (% (% q,h,w X _ p _ n _ D Dark Matter Model Hadronization Monte Carlo Coalescence Model F. Donato et al. Antideuterons as a signature of supersymmetric dark matter. Phys. Rev D, 62(4):

58 General Antiparticle Spectrometer (GAPS) _ D Segmented Detector "* TOF Target Degrader 35 kev "* 19 kev "* 75 kev n=2 Atomic Transitions Refilling e - n=3 n=4 n=5 Auger e - n=6 #% #% #% n=n K ~15 n o,l o Ladder Deexcitations *n=1, *l=1 Exotic Atom " +% n=1 "!% "!% " $% " +% Nuclear Annihilation K.Mori et al. APJ

59 Background 60 GeV neutralino

60 PEBS - Positron Electron Balloon Spectrometer

61 PEBS

62

63

64 BESS Collaboration! High Energy Accelerator Research Organization(KEK) The University of Tokyo BESS Collaboration National Aeronautical and Space Administration Goddard Space Flight Center University of Maryland Kobe University University of Denver (Since June 2005) Institute of Space and Astronautical Science/JAXA

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