ASTROPARTICLE PHYSICS in SWEDEN ASTROPARTICLE PHYSICS in SWEDEN experiments experiments lm univ., Royal Inst. of Technology (KTH), Uppsala univ., Kal -PhD researchers + 12 PhD students + 2 engineers lly financed by ish Research Council (SRC/VR) investments, salaries, run. costs and Alice Wallenberg Foundation (KAW) investments ish National Space Board (SNSB) investments, salaries, run. costs ish Polar Research Secretariat drillers at the South Pole nternational collaborations in ~ 1990 Olga Botner, Uppsala ECFA meeting, May 9, 2008
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 - PowerPoint PPT Presentation
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
ASTROPARTICLE PHYSICS in SWEDENASTROPARTICLE PHYSICS in SWEDENexperimentsexperiments
• 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
Scientific ScopeScientific 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 BurstsActive Galactic Nuclei
COMMON SCIENTIFIC THEME IUnderstanding processes
generating immense energy outflows in the Universe.
COMMON SCIENTIFIC THEME IUnderstanding processes
generating immense energy outflows in the Universe.
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
Status of AMANDA/IceCubeStatus 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 1018 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 1018 eV are from AMANDA
• 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
AMANDA – examplesAMANDA – examples
use the Earth as a filter to remove atmospheric ’s
4282 ’spredominantly atmospheric
map of Northern sky
Point source searches 2000 - 2004
Off-Source
On-Source
cc ,bb ,tt , ,W,Z 0,HH 0
HZW
ll
qq
,,
~~
WIMP search
Swedish groups in AMANDA/IceCubeSwedish 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
• 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 ’s, search, (GRB)• ice model, geometry calibration with downgoing ’s
• 8 post-PhD researchers + 5 PhD students
• 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 IceCubeExtensions of IceCube
UHE: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.Low energy Deep Core ext.
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
>109 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)
Scientific goalsScientific 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
Anticoincidence reduces out of acceptance background
Sign of charge, rigidity, dE/dx
Electron energy, dE/dx, lepton-hadron
separation
e- p _
e+ p (He,...)
Trigger, ToF, dE/dx
- +
~470 kg
~360 W
~1.
3 m
21.5 cm2sr
Si-W
0.45 T magnet + silicon tracker
Sweden’s contribution
Energy range Particles/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
1 HEAT-PBAR flight ~ 22.4 days PAMELA data1 CAPRICE98 flight ~ 3.9 days PAMELA data
Design performanceDesign performance
• unprecedented statistics and new energy range for CR physics e.g. contemporary antiproton & positron energy, Emax 50 GeV• simultaneous measurements of many species
• constrain secondary production models
Secondary production
Primary production
annihilation m() = 964 GeV
Secondary production (CAPRICE94-based)
Secondary production ‘C94 model’ + primary
distortion
Secondary productionMoskalenko&Strong
Secondary production
Secondary production ‘M+S model’ + primary distortion
Primary production
annihilation m() = 336 GeV
anti-protonsanti-protonspositronspositrons
1. Simon et al., ApJ 499 (1998) 2502. Ullio , astro-ph/99040863. Bergström et al., ApJ 526 (1999) 215
• order of magnitude more data that all previous measurements • significant new data at high energies
PAMELA summaryPAMELA 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, ~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!
The Gamma-ray The Gamma-ray Large Area Space Large Area Space
• 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
GLAST StatusGLAST 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 EGRETField 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.
COMPARISON WITH EGRETField 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
e.g. G L A S T
trE ,ˆ,
PtrE ˆ,,ˆ,
[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.
PoGOLite payloadPoGOLite payload
PoGOLite SummaryPoGOLite 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.
Primary production from annihilation (m() = 964 GeV)
Secondary production ‘C94 model’ +
primary distortion
PAMELA
Ullio : astro-ph/9904086
PositronsPositrons
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
PAMELA
Baltz + Edsjö, Phys Rev D59 (1999) 023511.
84 GV interacting antiproton
candidate
92 GV positron candidate
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 groupActive role in GRB working groupMulti-wavelength observations of AGN Partipation in instrument analysis and beam testParticipation 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%)