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ASTROPARTICLE PHYSICS in SWEDEN experiments

ECFA meeting, May 9, 2008. Olga Botner, Uppsala. ASTROPARTICLE PHYSICS in SWEDEN experiments. Stockholm univ., Royal Inst. of Technology (KTH), Uppsala univ., Kalmar univ. 15 post-PhD researchers + 12 PhD students + 2 engineers externally financed by

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ASTROPARTICLE PHYSICS in SWEDEN experiments

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  1. ECFA meeting, May 9, 2008 Olga Botner, Uppsala ASTROPARTICLE PHYSICS in SWEDENexperiments • Stockholm univ., Royal Inst. of Technology (KTH), Uppsala univ., Kalmar univ. • 15 post-PhD researchers + 12 PhD students + 2 engineers • externally financed by • Swedish Research Council (SRC/VR) investments, salaries, run. costs • Knut and Alice Wallenberg Foundation (KAW) investments • Swedish National Space Board (SNSB)  investments, salaries, run. costs • Swedish Polar Research Secretariat  drillers at the South Pole • large international collaborations • started in ~1990

  2. ScientificScope • knowledge of the Universe from • - studying photons • - charged particles (CRs) GLAST, PoGoLite PAMELA, IceCube+IceTop • what are the sources of the CRs • at the highest energies ? • how are these particles accelerated ? • violent processes in the vicinity of • black holes? • can we learn more from ’s? IceCube COMMON SCIENTIFIC THEME I Understandingprocesses generatingimmenseenergy outflows in the Universe. Active Galactic Nuclei Gamma Ray Bursts

  3. Scientificscope COMMON SCIENTIFIC THEME II Investigation of the possible particlecomposition of DM. • WIMPs in extensions of the SM • - masses order of GeV – TeV • - couplings on the EW scale • could have been thermally produced in the early Universe • give the required relic density without fine-tuning • candidates • - the neutralino  a favourite • - the lightest Kaluza-Klein state • - the inert Higgs IceCube, PAMELA, GLAST

  4. Neutrino Observations with IceCube Atmospheric muons come from above Atmospheric neutrinos • we believe • that sources producing • CRs also produce n’s • n’s propagate through • space with little • hindrance and point • back to their sources p CMB g g g g g g g g g n g Atmospheric neutrinos are isotropic cosmic accelerator

  5. 2007-2008: 18 strings 2006-2007: 13 Strings 2005-2006: 8 Strings 2004-2005 : 1 String IceTop air shower detector threshold ~ 300 TeV • 80 stations with • 320 digital OMs ICECUBE InIce AMANDA • 19 strings • 677 OMs Science menu • UHE ’s • cosmogenic’s • supernova ’s • dark matter • exotica • ex. monopoles, • Q-balls … • 80 strings • 4800 digital OMs • 17 m between DOMs • 125 m between strings complete 2011

  6. Detection principle Digital Optical Module • 10” Hamamatsu PMT • self-contained, reconfigurable • digital DAQ system • timing resolution < 2 ns • robust, low failure rate (1 %) • about 20% of all DOMs are • assembled and quality tested • in Stockholm and Uppsala

  7. Status of AMANDA/IceCube • AMANDA proof of concept • final configuration 2000 taking data, now integral part of IceCube • almost all relevant limits on cosmicfluxesbelow 1018 eV are from AMANDA • IceCubedeployedsuccessfullynow 50% complete • - 1 string (2005)+8 strings (2006) + 13 strings (2007) + 18 strings (2008) • installed strings are immediately operational • mainlyfundedthrough an MRE grant from the NSF  242.1 MUSD • - and Sweden, Belgium, Germany  34.5 MUSD • int’lcollaboration: USA (12 inst)+Europe (15 inst)+Japan+NewZealand • from Sweden: Stockholm univ., Uppsala univ. • first analyses already published • analysis techniques are continually refined as we • gain operational knowledge improved analysis sensitivity

  8. rc c sscatt nint. nm Gcapture Gannihilation m AMANDA – examples Point source searches 2000 - 2004 WIMP search On-Source Off-Source nmap of Northern sky 4282 n’s predominantlyatmospheric • use the Earth as a filter • to removeatmosphericm’s

  9. Swedish groups in AMANDA/IceCube • 8 post-PhD researchers + 5 PhD students • thanks to early support from SRC, KAW and the Swedish Polar Research • substantial contribution to the investment costs and development • large impact and influence • 1st spokesperson for the IceCube collaboration • seat on the executive committee (1/9) • leading role in analysis coord., simulation coord., WIMP wg • speakers committee, publication committee • h/w development for AMANDA – trigger, amplifiers, OMs • assembly and quality tests of DOMs for IceCube (~ 900) • drillers, one winter-over • physics analysis : WIMPs, UHE n’s, ntsearch, (GRB) • ice model, geometry calibration with downgoing m’s

  10. Extensions of IceCube Lowenergy Deep Coreext. • radio • acoustics UHE: • 6 densely instrumented strings • funds granted by KAW 2007 • an active volume of IceCube x 100 • Sweden takes part in the acoustics R&D • in the center of IceCube • below 1750 m (excellent ice) - assess South Pole ice properties - develop hardware • full year observation of the Sun • sources in the direction of the • galactic center • lowenergythreshold

  11. 350 km 70.0o 610 km • a satellitebasedpowerfulchargedparticleidentifier • launched June 15, 2006 from Baikonur, Kazakhstan • ellipticalorbit: altitude 350 – 610 km, inclination 70 • continuousdata-taking > 600 days • >109 triggers recorded and under analysis • int’lcollaboration: Italy (7 inst) + Russia (3 inst) • + Germany + Sweden • from Sweden: KTH (3 post-PhD researchers + 3 PhD students)

  12. Scientific goals • search for dark matter annihilation • search for anti-helium (primordial antimatter) • study of cosmic-ray propagation • - light nuclei and isotopes • study of electron spectrum (local sources?) • study solar physics and solar modulation • study terrestrial magnetosphere

  13. e+ p (He,...) e- _ p Sweden’s contribution 21.5 cm2sr Trigger, ToF, dE/dx Anticoincidence reduces out of acceptance background ~1.3 m 0.45 T magnet + silicon tracker + - Sign of charge, rigidity, dE/dx ~470 kg ~360 W Si-W Electron energy, dE/dx, lepton-hadron separation

  14. Design performance Energy rangeParticles/3 years Antiproton flux 80 MeV - 190 GeV O(104) Positron flux 50 MeV – 270 GeV O(105) Electron/positron flux up to 2 TeV (from calorimeter) Electron flux up to 400 GeV O(106) Proton flux up to 700 GeV O(108) Light nuclei (up to Z=6) up to 200 GeV/n He/Be/C: O(107/4/5) Antinuclei search Sensitivity of O(10-8) in He-bar/He • unprecedented statistics and new energy rangefor CR physics • e.g. contemporary antiproton & positron energy, Emax 50 GeV • simultaneous measurements of many species • constrain secondary production models 1 HEAT-PBAR flight ~ 22.4 days PAMELA data 1 CAPRICE98 flight ~ 3.9 days PAMELA data

  15. Secondary production ‘M+S model’ + primarycc distortion Secondary production Moskalenko&Strong Secondary production ‘C94 model’ + primarycc distortion Secondary production Secondary production Primary production cc annihilation m(c) = 964 GeV positrons Secondary production (CAPRICE94-based) Primary production cc annihilation m(c) = 336 GeV anti-protons backgrounds: 1. Simon et al., ApJ 499 (1998) 250 2. Ullio , astro-ph/9904086 3. Bergström et al., ApJ 526 (1999) 215 4. Moskalenko &Strong, ApJ 493 (1998) 694 5. Protheroe, ApJ 254 (1982) 391 6. Baltz&Edsjö, Phys Rev D59 (1999) 023511

  16. Antiproton / proton flux ratio Preliminary • order of magnitude more data that all previous measurements • significant new data at high energies

  17. PAMELA summary • PAMELAhas been in orbit and studying charged cosmic rays for • almost 2 years (3 year nominal mission) • Sweden participates in the governingbodies of Pamela • PAMELA is routinely collecting data, ~109 triggers have been • registered to date, and ~15 GB of data is down-linked per day • results on antiproton to proton flux ratio (2 – ~80 GeV) are being • prepared for PRL; future publications will cover lower and higher • energies (>~ 50 MeV and <~200 GeV ) • results on positron fraction to follow shortly • many other results also in preparation (cosmic ray electrons, • nuclei, search for antihelium, solar flares, radiation belts, …) • A new era in space-based cosmic-ray physics!

  18. The Gamma-rayLarge Area Space Telescope GLAST • satellite based -ray detector • low Earth circular orbit: altitude 550 km, inclination 26 • operational goal: > 5 years • 2 instruments • Large Area Telescope (LAT)  sensitivity range 20 MeV – 300 GeV • Gamma-ray Burst Monitor (GBM) • main science goals: • search for evidence of DM annihilation • high energy behaviour of GRBs and transients • int’l collaboration: USA (8 inst)+France (4 inst)+Italy (6 inst) • +Japan (2inst)+Sweden (3 inst) • Sweden: Stockholm u., KTH, Kalmar (4 post-PhD researchers • + 2 PhD-students)

  19. Overview of Large Area Telescope Precision Si-strip Tracker measure the g direction gamma ID Segmented Anticoincidence detector reject background of charged cosmic rays HodoscopicCsI(Tl) calorimeter measure the g energy image the shower  TKR High aspect ratio = Small FOV CAL e– ~180 cm 3000 kg ~120 cm e+ • Swedish contributions • the full set (>1500) CsIcrystals for the • calorimeter (1999) • testing and qualification of the crystals Low aspect ratio = Large FOV TKR CAL

  20. Sweden in GLAST • leadingrole in Dark Matterworking group • activerole in GRB working group • multi-wavelength observations of AGN • participation in instrument analysis and beam test • participation in governingbodies of GLAST • physics interest focuses on DM searches • prime candidates SUSY c, UED, inert Higgs • sources • galactic centre • galactic halo • galactic satellites/ dwarf galaxies • extra-galactic diffuse • ”smoking gun”  DM annihilation into gg or gZ MC 5s signal at 200 GeV • backgrounds • CR induced diffuse galactic g-rays • extra-galactic diffuse g-rays (superposed AGN) • charged particles

  21. GLAST Status • integration and environmental tests • complete (no failures, no performance • changes) • flight software updates and • thermal-vacuum tests completed • The LAT is at Cape Canaveral, Florida. • COMPARISON WITH EGRET • Field of View factor ~ 4 • Point Spread function factor > 3 • Effective area factor > 5 • A factor > 30 improvement in sensitivity below < 10 GeV, and >100 at higher energies. expected launch: 2008

  22. g SLAC / KIPAC, Hawaii KTH, Stockholm University Tokyo Institute of Technology, Hiroshima University, ISAS. [25 – ~80 keV] g • photons can be characterised by their energy, direction, time of detection andpolarisation • polarisation never exploited at these energies • measuring the polarisation of gamma-rays provides a powerful diagnostic for source emission mechanisms • polarisationcan occur through scattering / synchrotron processes, interactions with a strong magnetic field •  sensitive to the ‘history’ of the photon e.g. G L A S T [10 keV – 300 GeV]

  23. PoGOLite payload

  24. PoGOLite Summary • PoGOLite stands to open a new observation window on sources such as rotation-powered pulsars and accreting black holes through a measurement of the polarisation of soft gamma rays (25 - ~80 keV). • KTH chairs the collaboration • Sweden (KTH Physics and SU Astronomy) contribute with the anticoincidence system, polarimeter construction, attitude control system and lead the pathfinder flight campaign. • A prototype detector has been tested with polarisedphoton, proton, and neutron beams and the design and simulation validated. • Construction of flight hardware is currently in progress in Stockholm • Pathfinder balloon flight from Esrange, northern Sweden, 2010.

  25. Extra material

  26. Drill tower 5 MW Hot water generator Hose reel IceTop tanks Hot-water drilling

  27. Detector medium: ice to meet you Scattering Absorption bubbles ice dust dust Measurements: ►in-situ light sources ►atmospheric muons Average optical ice parameters: abs ~ 110 m @ 400 nm lsca ~ 20 m @ 400 nm

  28. to catch n’s at the highest energies … listen sudden energy deposit of ~109 GeV acoustic particle shower heating  sudden thermal expansion  acoustic pulse note the scale! radio particle shower  moving charge excess  radio pulse both methods in exploratory phase: - assess South Pole ice properties - develop hardware Proposed : 91 holes, 1 km spacing 5 radio+3 acoustic sensors/hole

  29. Diffuse • GZK: 1/year? • Diffuse GRB: 20/year (Waxman) • Diffuse AGN: few  >100/year (Mannheim) • Point like: • GRB (030329): 1-10/burst (Waxman) • AGN (3C279): few/year (Dermer) • Galactic SNR (Crab): few/year? (Protheroe) • Galactic microquasars: 1-100/year (Distefano) Expected rates from astrophysical sources per square km

  30. Antiprotons PAMELA Secondary production‘C94 model’ + primarycc distortion Secondary production (upper and lower limits) Simon et al. ApJ 499 (1998) 250. Primary production from cc annihilation (m(c) = 964 GeV) Secondary production(CAPRICE94-based) Bergström et al. ApJ 526 (1999) 215 Ullio : astro-ph/9904086

  31. Secondary production‘Moskalenko + Strong model’ without reacceleration. ApJ 493 (1998) 694. Positrons PAMELA Secondary production‘M+S model’ + primarycc distortion Secondary production‘Leaky box model’ R. Protheroe, ApJ 254 (1982) 391. Primary production from cc annihilation (m(c) = 336 GeV) Baltz + Edsjö, Phys Rev D59 (1999) 023511.

  32. 84 GV interacting antiprotoncandidate

  33. 92 GV positron candidate

  34. GLAST Sweden Sweden provided the full set of CsI crystals for the calorimeter (1999), subsequently testing and qualification of the crystals. (Wallenberg foundation: 20 MSEK) Today: Leading role in Dark Matter working group Active role in GRB working group Multi-wavelength observations of AGN Partipation in instrument analysis and beam test Participation in governing bodies of GLAST Funding: (inkl. overhead) Swedish Space Board: 1.1 MSEK (2007), 1.0 MSEK (2008) (increase expected post-launch) Swedish Space Board: 1.2 MSEK (2007-2009) (50 % Researcher Position, assoc. prof level) Swedish Science Council: 1.1 MSEK (2006-2009) (50 % Researcher Position, assist. prof. Level). Personell: Permanent: 0.25 FTE Prof. (all male) 0.75 FTE Assoc. Prof (all male) (all active in Astroparticle Physics, 100%) Non-permanent: 0.9 FTE Assist. Prof. (all male) 2 FTE PostDoc (all female) 1.8 FTE PhD students (all male) 0.25 Technical personell (all male) (all active in Astroparticle Physics, 100%)

  35. Crab nebula, 1054

  36. 10 keV 100 keV Compton scattering • Incident g deposits little energy at Compton site • ‘Large’ energy deposited at photoelectric absorption site •  large energy difference • Can be distinguished by simple plastic scintillators (despite intrinsic poor energy resolution) Photoelectric absorption Array of plastic scintillators g Compton scatter

  37. Polarisation plane E k k0 Polarscattering angle, q Azimuthal scattering angle, f Measuring polarisation 0 when f=90o Compton scattering: Klein-Nishina formula Max when f=90o • g from a polarised source undergo Compton scattering in a suitable detector material • Higher probability of being scattered perpendicular to the electric field vector (polarisation direction) • Observed azimuthal scattering angles are therefore modulated by polarisation

  38. 0.9cm overlap 4.0cm 20cm 60cm 19cm PMT Assembly BGO Bottom Veto Fast Scintillator Detector Section Slow Scintillator Hexagonal Tube Active Collimator PoGOLite instrument schematic BGO BGO [NB: simplified! 217 wells in reality] BGO anticoincidence

  39. Crab Pulsar emission models [Outer gap] [Slot gap caustic] [Polar cap]

  40. Testing emission models with PoGOLite (OSO-8 assumed) Slot gap caustic Polar cap Outer gap

  41. Maiden flight: 2010 • Reduced volume ‘pathfinder’ flight planned from Esrange facility in North of Sweden. • 6 – 24 hour long flight expected • Assess backgrounds, study Crab nebula and Cygnus X-1 • Total payload weight ~1000 kg • 1.11x106 m3 balloon; target altitude ~40 km High-mass X-ray binary Pulsar / SNR

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