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Constraints to Dark Matter and cosmic ray propagation by the PAMELA space experiment

Constraints to Dark Matter and cosmic ray propagation by the PAMELA space experiment. Roberta Sparvoli University of Rome ”Tor Vergata” and INFN. Everything starts with …. Evaporation of primordial black holes. Anti-nucleosyntesis. WIMP dark-matter annihilation in the galactic halo.

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Constraints to Dark Matter and cosmic ray propagation by the PAMELA space experiment

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  1. Constraints to Dark Matter and cosmic ray propagation by the PAMELA space experiment Roberta Sparvoli University of Rome ”Tor Vergata” and INFN

  2. Everything starts with …  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  3. Evaporation of primordial black holes Anti-nucleosyntesis WIMP dark-matter annihilation in the galactic halo Background: CR interaction with ISM CR + ISM  p-bar + … and various ideas of theoretical interpretations  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  4.  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  5.  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  6. Charge-dependent solar modulation Solar polarity reversal 1999/2000 Asaoka Y. Et al. 2002 Positron excess? ? ? ¯ + • CR + ISM  p-bar + … • Propagation dominated by nuclear interactions • Kinematical threshold: Eth~5.6 for the reaction CR antimatter Experimental scenario before PAMELA WHAT DO WE NEED TO BETTER UNDERSTAND ? Measurements at higher energies Better knowledge of background High statistics Continuous monitoring of solar modulation Long Duration Flights Positrons Antiprotons ___ Moskalenko & Strong 1998 • CR + ISM  p± + x m± + x  e± + x • CR + ISM  p0 + x gg e± • Propagation dominated by energy losses • (inverse Compton & synchrotron radiation) • Local origin (@100GeV 90% from <2kpc)  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  7. PAMELA pre-history  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  8. Italy CNR, Florence Bari Florence Frascati Naples Rome Trieste Russia Moscow St. Petersburg Germany Sweden Siegen KTH, Stockholm The PAMELA collaboration  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  9. PAMELA Scientific goals Halo p-bar, e+  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  10. PAMELA design performance Maximum detectable rigidity (MDR) energy rangeparticles in 3 years Antiprotons80 MeV ÷190 GeV O(104) Positrons50 MeV ÷ 270 GeV O(105) Electrons up to 400 GeV O(106) Protonsup to 700 GeV O(108) Electrons+positronsup to 2 TeV (from calorimeter) LightNuclei up to 200 GeV/n He/Be/C: O(107/4/5) Anti-Nuclei searchsensitivity of 3x10-8 in anti-He/He Magnetic curvature & trigger spillover shower containment  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  11. PAMELA detectors Main requirements  high-sensitivity antiparticle identification and precise momentum measure + - • Time-Of-Flight • plastic scintillators + PMT: • Trigger • Albedo rejection; • Mass identification up to 1 GeV; • - Charge identification from dE/dX. • Electromagnetic calorimeter • W/Si sampling (16.3 X0, 0.6 λI) • Discrimination e+ / p, anti-p / e- • (shower topology) • Direct E measurement for e- • Neutron detector • 36 He3 counters • High-energy e/h discrimination GF: 21.5 cm2 sr Mass: 470 kg Size: 130x70x70 cm3 Power Budget: 360W • Spectrometer • microstrip silicon tracking system+ permanent magnet • It provides: • - Magnetic rigidity R = pc/Ze • Charge sign • Charge value from dE/dx  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  12. The Resurs DK-1 spacecraft  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  13.  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  14.  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  15. Launch from Baikonur June 15th 2006, 0800 UTC. ‘First light’ June 21st 2006, 0300 UTC. • Detectors operated as expected after launch • Different trigger and hardware configurations evaluated  PAMELA in continuous data-taking mode since commissioning phase ended on July 11th 2006 PAMELA milestones Main antenna in NTsOMZ Trigger rate* ~ 25 Hz Fraction of live time* ~ 75% Event size (compressed mode) ~ 5kB 25 Hz x 5 kB/ev ~ 10 GB/day (*outside radiation belts) • Today 1212 days in flight • >14 TBytes of raw data downlinked • >109 triggers recorded and under analysis  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  16. Antiproton/positron discrimination energy measurement  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  17. e- e+ ‘Electron’ ‘Hadron’ p, d p Antiparticle selection  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  18. Antiprotons  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  19. High-energy antiproton analysis • Analyzed data July 2006 – February 2008 (~500 days) • Collected triggers ~108 • Identified ~ 10 106 protons and ~ 1 103 antiprotons between 1.5 and 100 GeV ( 100 p-bar above 20 GeV ) • Antiproton/proton identification: • rigidity (R)  SPE • |Z|=1 (dE/dx vs R)  SPE&ToF • b vs R consistent with MpToF • p-bar/p separation (charge sign)  SPE • p-bar/e- (and p/e+ ) separation CALO • Dominant background spillover protons: • finite deflection resolution of the SPE  wrong assignment of charge-sign @ high energy • proton spectrum harder than antiproton  p/p-bar increase for increasing energy (103 @1GV 104 @100GV) •  Required strong SPE selection  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  20. Proton-spillover background • Electrons: efficiently removed by CALO • Pions (from interactions in dome) : about 3% in the pbar sample  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  21. PAMELA: Antiproton-to-proton ratio PRL 102, 051101 (2009)  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  22. PAMELA: Antiproton-to-proton ratio PRL 102, 051101 (2009)  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  23. PAMELA: Antiproton-to-proton ratioNew (preliminary) data ! Full statistics  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  24. PAMELA: Antiproton flux preliminary • PAMELA  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  25. Positrons  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  26. S1 CARD CAT S2 TOF SPE CAS S3 CALO S4 ND High-energy positron analysis • Analyzed data July 2006 – February 2008 (~500 days) • Collected triggers ~108 • Identified ~ 150 103 electrons and ~ 9 103 positrons between 1.5 and 100 GeV (180 positrons above 20 GeV) • Electron/positron identification: • rigidity (R)  SPE • |Z|=1 (dE/dx=MIP)  SPE&ToF • b=1 ToF • e-/e+ separation (charge sign)  SPE • e+/p (and e-/p-bar) separation CALO • Dominant background interacting protons: • fluctuations in hadronic shower development  p0 ggmight mimic pure em showers • proton spectrum harder than positron  p/e+ increase for increasing energy (103 @1GV 104 @100GV) •  Required strong CALO selection  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  27. Positron identification with CALO 51 GV positron • Identification based on: • Shower topology (lateral and longitudinal profile, shower starting point) • Total detected energy (energy-rigidity match) • Analysis key points: • Tuning/check of selection criteria with: • test-beam data • simulation • flight data  dE/dx from SPE & neutron yield from ND • Selection of pure proton sample from flight data (“pre-sampler” method): • Background-suppression method • Background-estimation method 80 GV proton Final results make NO USE of test-beam and/or simulation calibrations. The measurement is based only on flight data with the background-estimation method  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  28. Particle selection after total energy cut and starting point of the shower e+ e - (anti p) p + -  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  29. PAMELA: Positron fraction NATURE 458, 697, 2009 • (Moskalenko & Strong 1998) • GALPROP code • Plain diffusion model • Interstellar spectra Solar modulation effects Anomalous increasing ?  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  30. PAMELA: Positron fraction wrt other exp’s NATURE 458, 697, 2009  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  31. Different statistical approaches for the bkg Data: July 2006  December 2008  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  32. New data + systematic error In publication on APP ! Data: July 2006  December 2008  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  33. PAMELA antimatter data: Do we have any antimatter excess in CRs?  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  34. ~20% • NB! • Solar modulation • Nuclear cross-section • … Antiproton-to-proton ratioSecondary Production Models CR + ISM  p-bar + …  Uncertainty band related to propagation parameters (~10% @10 GeV)  Additional uncertainty of ~25% due to production cs should be considered !! No evidence for any antiproton excess  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  35. Positron fractionSecondary Production Models CR + ISM  p± + … m± + …  e± + … CR + ISM  p0 + … gg e± • Increasing positron fraction only if • ge- gp > 0.6 • unlikely (Serpico 2008) Quite robust evidence for a positron excess  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  36. Primary positron sources Dark Matter • e+ yield depend on the dominant decay channel • LSPs (SUSY) seem disfavored due to suppression of e+e- final states • low yield (relative to p-bar) • soft spectrum from cascade decays • LKPs seem favored because can annihilate directly in e+e- • high yield (relative to p-bar) • hard spectrum with pronounced cutoff @ MLKP (>300 GeV) • Boost factor required to have a sizable e+ signal • NB: constraints from p-bar data!! • Other hypothesys possible and under study (i.e. Minimal DM Model, decaying DM, new gauge bosons, …) LKP -- M= 300 GeV (Hooper & Profumo 2007) More than 150 articles claim DM is discovered !  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  37. Example: dark matter  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  38. Primary positron sources Astrophysical processes • Local pulsars are well-known sites of e+e- pair production (the spinning B of the pulsars strips e- that emit gammas then converting to pairs trapped in the cloud, accelerated and then escaping at the Poles) :  they can individually and/or coherently contribute to the e+e- galactic flux and explain the PAMELA e+ excess (both spectral feature and intensity) • No fine tuning required • if one or few nearby pulsars dominate, anisotropy could be detected in the angular distribution • possibility to discriminate between pulsar and DM origin of e+ excess All pulsars (rate = 3.3 / 100 years) (Hooper, Blasi, Seprico 2008)  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  39. Example: pulsars  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  40. Explanation with supernovae remnantsShaviz and al. astro-ph.HE0902.0376  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  41. Positrons from old SNR’sP. Blasi 0903.2794  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  42. Standard Positron Fraction Theoretical Uncertainties γ = 3.54 γ = 3.34 Need for high statistics CR measurements T. Delahaye et al., arXiv: 0809.5268v3  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  43. Electrons Any positron source is an electron source too …  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  44. Recent claims of (e++e-) excess g = 3.0 FERMI does not confirm the ATIC bump but finds an excess wrt conventional diffusive models  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  45. PAMELA electron flux measurements Key points wrt other experiments (ATIC, HESS, FERMI) : • Combination of CALO and SPECTROMETER allow energy self- calibration in flight no dependence on ground calibrations or MC simulations • Very deep CALO (16 X0)  containment of the shower maximum beyond 1 TeV • Neutron detector help proton rejection, especially at high energy • No atmospheric contamination • Possibility to disentangle electrons from positrons But .. • Smaller acceptance  lower statistics  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  46. PAMELA electron flux preliminary  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  47. PAMELA electron flux wrt other exp’s preliminary  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  48. PAMELA electron flux preliminary Data ready by the end of the year Primary source ???  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  49. Protons, nuclei, …  Roberta Sparvoli  October 8th, 2009  Como (Italy)

  50. Galactic protons and Helium fluxes preliminary p He  Roberta Sparvoli  October 8th, 2009  Como (Italy)

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