1. 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 - 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 Olga Botner, UppsalaECFA meeting, May 9, 2008

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

3. Scientific scope COMMON SCIENTIFIC THEME II Investigation of the possible particle composition of DM. COMMON SCIENTIFIC THEME II Investigation of the possible particle composition 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.  p cosmic accelerator Atmospheric neutrinos are isotropic Atmospheric muons come from above      CMB we believe that sources producing CRs also produce ’s ’s propagate through space with little hindrance and point back to their sources Neutrino Observations with IceCube

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

6. Detection principle  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 Digital Optical Module

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 fluxes below 10 18 eV are from AMANDA AMANDA  proof of concept final configuration 2000  taking data, now integral part of IceCube almost all relevant limits on cosmic fluxes below 10 18 eV are from AMANDA IceCube deployed successfully  now 50% complete - 1 string (2005)+8 strings (2006) + 13 strings (2007) + 18 strings (2008) installed strings are immediately operational mainly funded through an MRE grant from the NSF  242.1 MUSD - and Sweden, Belgium, Germany  34.5 MUSD int’l collaboration: USA (12 inst)+Europe (15 inst)+Japan+New Zealand from Sweden: Stockholm univ., Uppsala univ. first analyses already published analysis techniques are continually refined as we gain operational knowledge  improved analysis sensitivity IceCube deployed successfully  now 50% complete - 1 string (2005)+8 strings (2006) + 13 strings (2007) + 18 strings (2008) installed strings are immediately operational mainly funded through an MRE grant from the NSF  242.1 MUSD - and Sweden, Belgium, Germany  34.5 MUSD int’l collaboration: USA (12 inst)+Europe (15 inst)+Japan+New Zealand from Sweden: Stockholm univ., Uppsala univ. first analyses already published analysis techniques are continually refined as we gain operational knowledge  improved analysis sensitivity

8. AMANDA – examples  use the Earth as a filter to remove atmospheric  ’s 4282 ’s predominantly atmospheric map of Northern sky Point source searches 2000 - 2004 Off-Source On-Source    scatt  capture  annihilation int.   WIMP search

9. Swedish groups in AMANDA/IceCube thanks to early support from SRC, KAW and the Swedish Polar Research substantial contribution to the investment costs and development  large impact and influence 1 st 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 ’s,   search, (GRB) ice model, geometry calibration with downgoing  ’s 8 post-PhD researchers + 5 PhD students

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

11.    km  km a satellite based powerful charged particle identifier launched June 15, 2006 from Baikonur, Kazakhstan elliptical orbit: altitude 350 – 610 km, inclination 70  continuous data-taking > 600 days >10 9 triggers recorded and under analysis int’l collaboration: 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. Anticoincidence reduces out of acceptance background Sign of charge, rigidity, dE/dx Electron energy, dE/dx, lepton-hadron separation e-e- p _ e+e+ p (He,...) Trigger, ToF, dE/dx - + ~470 kg ~360 W ~1.3 m 21.5 cm 2 sr Si-W 0.45 T magnet + silicon tracker Sweden’s contribution

14. Energy range Particles/3 years Antiproton flux 80 MeV - 190 GeV O(10 4 ) Positron flux50 MeV – 270 GeVO(10 5 ) Electron/positron fluxup to 2 TeV (from calorimeter) Electron flux up to 400 GeVO(10 6 ) Proton flux up to 700 GeVO(10 8 ) Light nuclei (up to Z=6) up to 200 GeV/n He/Be/C:O(10 7/4/5 ) Antinuclei search Sensitivity of O(10 -8 ) in He-bar/He 1 HEAT-PBAR flight ~ 22.4 days PAMELA data 1 CAPRICE98 flight ~ 3.9 days PAMELA data Design performance unprecedented statistics and new energy range for CR physics e.g. contemporary antiproton & positron energy, E max  50 GeV simultaneous measurements of many species constrain secondary production models

15. Secondary production Primary production  annihilation m(  ) = 964 GeV Secondary production (CAPRICE94-based ) Secondary production ‘C94 model’ + primary  distortion Secondary production Moskalenko&Strong Secondary production Secondary production ‘M+S model’ + primary  distortion Primary production  annihilation m(  ) = 336 GeV anti-protons positrons 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 backgrounds:

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

17. PAMELA summary PAMELA has been in orbit and studying charged cosmic rays for almost 2 years (3 year nominal mission) Sweden participates in the governing bodies of Pamela PAMELA is routinely collecting data, ~ 10 9 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-ray Large Area Space Telescope 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) GLAST

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

20. Sweden in GLAST physics interest focuses on DM searches prime candidates SUSY , UED, inert Higgs sources galactic centre galactic halo galactic satellites/ dwarf galaxies extra-galactic diffuse ”smoking gun”  DM annihilation into  or  Z backgrounds CR induced diffuse galactic  -rays extra-galactic diffuse  -rays (superposed AGN) charged particles leading role in Dark Matter working group active role in GRB working group multi-wavelength observations of AGN participation in instrument analysis and beam test participation in governing bodies of GLAST leading role in Dark Matter working group active role in GRB working group multi-wavelength observations of AGN participation in instrument analysis and beam test participation in governing bodies of GLAST MC 5  signal at 200 GeV

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 100 at higher energies. COMPARISON WITH EGRET Field of View factor ~ 4 Point Spread function factor > 3 Effective area factor > 5 A factor > 30 improvement in sensitivity below 100 at higher energies. expected launch: 2008

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

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 polarised photon, 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. Hot-water drilling Hose reel Drill tower IceTop tanks 5 MW Hot water generator

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

29. Proposed : 91 holes, 1 km spacing 5 radio+3 acoustic sensors/hole note the scale! radio acoustic particle shower  heating  sudden thermal expansion  acoustic pulse both methods in exploratory phase: - assess South Pole ice properties - develop hardware both methods in exploratory phase: - assess South Pole ice properties - develop hardware to catch ’s at the highest energies … listen particle shower  moving charge excess  radio pulse sudden energy deposit of ~10 9 GeV

30. Expected rates from astrophysical sources per square km 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)

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

32. Positrons Secondary production ‘Leaky box model’ R. Protheroe, ApJ 254 (1982) 391. Secondary production ‘Moskalenko + Strong model’ without reacceleration. ApJ 493 (1998) 694. Primary production from  annihilation (m(  ) = 336 GeV) Secondary production ‘M+S model’ + primary  distortion PAMEL A Baltz + Edsjö, Phys Rev D59 (1999) 023511.

33. 84 GV interacting antiproton candidate

34. 92 GV positron candidate

35. 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%)

36. Crab nebula, 1054

37. Compton scattering 100 keV 10 keV Compton scatter Photoelectric absorption  Incident  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) Array of plastic scintillators

38. Measuring polarisation Compton scattering: Klein-Nishina formula 0 when  =90 o Max when  =90 o  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 Azimuthal scattering angle,  Polarisation plane Polar scatterin g angle,  k k0k0 E

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

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

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

42. 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 1.11x10 6 m 3 balloon; target altitude ~40 km Pulsar / SNR High-mass X-ray binary