cosmic accelerators astrophysics with high energy particles
DESCRIPTION
Cosmic Accelerators Astrophysics with High Energy Particles. Graduiertenkolleg “Physik an Hadronen-Beschleunigern” Klausurtagung, 17.10.2006. Thomas Lohse Humboldt University Berlin. The Cosmic Ray Spectrum. E 2.7 , mostly protons. Knee. solar modulation. transition to - PowerPoint PPT PresentationTRANSCRIPT
Cosmic AcceleratorsAstrophysics with High Energy Particles
Thomas LohseHumboldt University Berlin
Graduiertenkolleg “Physik an Hadronen-Beschleunigern” Klausurtagung, 17.10.2006
The Cosmic Ray Spectrum
Power Laws
Shock Accelerationpredicts FSource E2
Discovery Balloon Flight Victor Hess, 1912
sola
r m
odul
atio
n
E2.7, mostly protons
transition toheavier nuclei E3.1
mostly Fe?
Knee
?
Ankle
EAS DetectorsDirect Measurements
transition tolighter nuclei ?
Open questions after 90 years
What and where are the sources?
How do they work?
Are the particles really accelerated?...
…or due to new physics at large mass scales?
And how do cosmic rays manage to reach us?
Production in Cosmic Accelerators
protons/nucleielectrons/positrons
p
0
radiation fields and matter
p
e Inverse Compton(+Bremsstr.)
Experimental Techniques ( E 10 GeV )
InstrumentedWater / Ice
Scintillator or Water Č
Č-Telescope
Č
Fluorescence Detector
Hadron-Detector
Fluorescence
Primary (Hadron,Gamma)
Air Shower
Atmospheric (4)
Primary (4)
, e,
R&DRadio-Detection
Acoustic-Detection
1. Cosmic rays beyond the ankle
2. Neutrinos from cosmic ray sources
3. Gammas from cosmic ray sources
1. Cosmic rays beyond the ankle
2. Neutrinos from cosmic ray sources
3. Gammas from cosmic ray sources
OutlineOutline
p beyond ankle
Greisen-Zatsepin-Kuzmin Cut-Off:Energy loss in cosmic microwave
background (CMB)p(100 EeV) + (CMB) p + , n +
p(100 EeV)p
p below ankle isotropized in B-fields
E eV102010191018
E3
FE
cut-off
reprocessed p
no GZK cut-off?
triplet
model fit to HIRes data
AGASA
HIResFly’s Eye
AGASA
AGASA: surface detector array
HIRes: fluorescence light detector
Spectra consistent allowing for 30% systematic energy shift…
The Pierre Auger Project3000 km2 Hybrid Detector
1600 Water Č-Detectors 75% installed
4 Fluorescence Sites
AGASA
Energy Calibration of Surface Detectors
14% duty cycle
Present systematics:Calibration 12%Fluorescence yield 15%
Clean EeV Hybrid Events
contemporaneous atmospheric monitoring
statistically limited
up to now…statistically limited
up to now…
• calorimetric measurement independent of primary
composition independent of air shower details
First Look at 3 EeV Energy Spectrum( from surface detector array )
Data: Jan. 2004 – Jan 2005
Exposure: 1750 km2 sr yr AGASA + 7%
Events: 3525
Power Law Fit
2.4d.o.fχ
EEd
Id
2
03.084.2
systematic errors
AUGER best fit
preliminary Calibration uncertainty
1. Cosmic rays beyond the ankle
2. Neutrinos from cosmic ray sources
3. Gammas from cosmic ray sources
Amundsen-Scott South Pole Station
South PoleDome
Summer camp
AMANDA
1500 m
2000 m[not to scale]
IceCube(in construction)
The Main Players presently: • Amanda / IceCube, South Pole Ice• BAIKAL, Water of Lake Baikal
+ future Mediterranean detectors
upward (2 coverage)
preliminarypreliminary
horizontal
vertical
atmospheric
Search for Diffuse Cosmic Neutrinos
1:1:1 flavour flux ratio
E2-Flux Limit
add directional & temporal constraints …
IceCube 3 years
h24 h
90
90
Unbinned Search for Clusters
AMANDA 2000-2003
preliminary
AMANDA 2000-2003
preliminary
Significance Sky Map
Maximum Excess 3.4
max. excess from random
skymaps3.4
92%
AMANDA Search for Transient Sources
events
time
sliding window • time window: 40 / 20 days• angular bin: 2.25°-3.75°
fixed a priori
Source Events Backgr. window doublets Prob.
Markarian 421 6 5.58 40 days 0 Close to 1
1ES1959+650 5 3.71 40 days 1 0.34
3EG J1227+4302 6 4.37 40 days 1 0.43
QSO 0235+164 6 5.04 40 days 1 0.52
Cygnus X-3 6 5.04 20 days 0 Close to 1
GRS 1915+105 6 4.76 20 days 1 0.32
GRO J0422+32 5 5.12 20 days 0 Close to 1
12 Objects tested (over 4 years), no triplets found … BUT …
…
5 events
backgrounddublet window
66 day triplet
WHIPPLE E > 0.6 TeV
HEGRAE > 2 TeV
AMANDA – 1ES1959+650 – 2.25o search bin sizerevisited a posteriori
Orphan -flare (not seen in
X-rays)
Statistical significance hard to tell … but promising!Lessons learned: Multimessenger & multiwavelength
studies important. Use -ray flares (not only X-rays)…
The first cosmic ray neutrino ???
1. Cosmic rays beyond the ankle
2. Neutrinos from cosmic ray sources
3. Gammas from cosmic ray sources
H.E.S.S. CANGAROO III
MAGIC
Veritas
in construction
Cherenkov Telescopes (3rd Generation)
3.1. Supernovae
Synchrotron radiation
Pulsar Wind Nebula:Electron wind from central
pulsar heats the cloud
The Standard Candle for TeV -AstronomyCrab Supernova 1054 a.D. d = 2 kpc
optical
1 lig
htye
ar
But what about hadrons (protons and nuclei)?
Cassiopaeia A Supernova 1658 a.D. d = 2,8 kpc
X ray picture
“Shell Type” SNR:
• no electron wind from pulsar
• gamma signal from shell regions not totally drowned in that of electron wind
• good source class to observe hadron acceleration
resolution
H.E.S.S. 2004E 210 GeV
RX J1713.73946
resolution
H.E.S.S. 2004E 210 GeV
RX J1713.73946
First Resolved Supernova Shells in -Rays
H.E.S.S. 2005E 500 GeV
RX J0852.04622
Strong correlation with X-ray intensitiesStrong correlation with X-ray intensities
• SN-Shells are accelerating particles up to at least 100 TeV!• But are these particles protons/nuclei or electrons?
E2 d
N/d
E
log(E)
Stars
radio infrared visible light X-rays VHE -rays
CMB
Dust
CosmicElectron
Accelerators BEe
Electron or Hadron Accelerator?
Synchrotron Radiation Inverse Compton
e
e
EdNd
B, e
e
EdNd BEe
Cosmic Proton
Accelerators
, p
p
Ed
Nd Matter Density
0Synchrotron Radiation of Secondary Electrons
EGRET
2.0 2.0
B 7, 9, 11
GB 7, 9, 11
G
Electron accelerator fits for RX J1713.73946 :• Continuous electron injection over 1000 years• Injection spectrum: power law with cutoff
• IC peak not well described• B-field low for SNR shell
• large & injection rate bremsstrahlung important
• needs tuning at low E
αeE
B 10
G B 10
G
2.0, 2.25, 2.5 2.0, 2.25, 2.5H.E.S.S.H.E.S.S.
Continuous proton injection over 1000 years Injection spectrum: power law, index 2 Different cutoff shapes & diffusion parameters
Proton accelerator fit:
H.E.S.S. RX J1713.73946
3.2. Inner Glactic Plane30 ≲l ≲ 30
3 ≲ b ≲3
H.E.S.S. Scan of Inner Galactic Plane
Resolution
14 new sources, all extended! Possible counterparts: (plus previously known ones)
5 SNR3 Pulsar 3 ???
HESS J1837069
HESS J1834087
HESS J1825137
HESS J1813178
HESS J1804216
G0.90.1HESS J1747281
Galactic CentreHESS J1745290
HESS J1745290
HESS J1713381
RX J1713.73946HESS J1708410
HESS J1702420HESS J1640465
HESS J1634472
HESS J1632478HESS J1616508
HESS J1614518
HESS J1834-087
HESS J1804-216 HESS J1640-465
TeV-Gamma-RayRadioX-Ray
… a new source class: “Dark Accelerators”
Five sources known: TeV J20324130 (HEGRA)
HESS J1303631 HESS J1614518
HESS J1702420 HESS J1708410
What are these sources? Are they hadron accelerators?
• extended• hard spectra, • steady emission
3.3. Galactic Centre
HESS J1837069
HESS J1834087
HESS J1825137
HESS J1813178
HESS J1804216
G0.90.1HESS J1747281
Galactic CentreHESS J1745290
HESS J1745290
HESS J1713381
RX J1713.73946HESS J1708410
HESS J1702420HESS J1640465
HESS J1634472
HESS J1632478HESS J1616508
HESS J1614518
Chandra GC surveyNASA/UMass/D.Wang et al.
CANGAROO (80%)
Whipple
(95%)
H.E.S.S.
Chandra GC surveyNASA/UMass/D.Wang et al.
CANGAROO (80%)
Whipple(95%)
Contours from Hooper et al. 2004
Galactic Centre: A pointlike TeV- source
H.E.S.S. (95%); MAGIC similar
Astrophysical Source Candidates:
• 3106 M⊙ black hole Sgr A
─ EMF close to rotating black hole─ Accretion shocks
• Supernova Remnant Sgr A East─ Expanding shock waves
Radio
H.E.S.S.
Systematicpointing error
Radio Contour
Sgr A*
Sgr A EastSNR
no visible cut-off rather large mass
measured flux large cross-section and/or DM density
… or maybe dark matter annihilation ?
10-13
10-12
10-11
0,1 1 10
E2 F
(E)
[Te
V/c
m2 s]
E [TeV]
20 TeV Neutralino20 TeV Kaluza Klein particle
… unlikely !
H.E.S.S. MAGICGC
Crab
Galactic Centre Neighbourhood
~150 pc
Galactic CentreHESS J1745290
SNR G0.90.1HESS J1747281
EGRET GeV--sources
...point sources subtracted
first resolved detection of diffuse TeV--radiation cosmic rays (hadrons) interacting with molecular clouds
~150 pc
Galactic Centre Neighbourhood
molecular clouds density profiles
HESS J1745290
Cosmic Ray Spectrum at the GC...
diffuse radiation
expected flux for CR spectrum
observed on earth
Cosmic rays are much harder and have 3
larger density around the GC
Cosmic rays are much harder and have 3
larger density around the GC
is very different from the one at earth
Possible reason:
Close-by source population
Possibly single SN-explosion
3.3. Active Galaxies
General Active Galactic Nuclei (AGN):• Supermassive black holes, M 109 M
• accretion disk and relativistic jets
Blazar-Typ: Jet points towards the earth• Doppler-boost TeV -radiation
Blazars
E
dN/d
E
Measurement of EBL ( Cosmology )
Physics of compact objects,acceleration/absorption in jets,…
EdN
/dE
Absorption in (infrared) extragalactic background light (EBL)
(TeV) + (EBL) e+e-
e+
e-
Cut-off Energy and -Ray Horizon
PG 1553113
H 2356 (x 0.1) = 3.1±0.2 Preliminary
EBL Unfolding of Measured Spectra
1 ES 1101 = 2.9±0.2
EBL
H 2356 (x0.1) = 3.1±0.2
Hardest plausiblesource spectrum = 1.5
Hardest plausiblesource spectrum = 1.5
Too muchEBL
Lower Limits(Galaxy Counts)
New Upper Bound on EBL Density
Direct IRTSMeasurements
Assumed shape for rescaling
H.E.S.S. upper boundfrom spectral shapes of
1ES 1101-232 (z = 0.186) H 2356-309 (z = 0.165)
EBL density seems 2 smaller than expected! Little room for EBL sources other than galaxies (early stars…)
Upper Limits
excluded by H.E.S.S.
Summary• Cosmic ray puzzle persists…but is under pressure by
massive attack from EAS-arrays, - and -telescopes
• Progress in understanding knee, ankle and GZK-region AUGER data disfavour small scale anisotropies
• Cosmic -detection in multi-messenger campaigns ?Neutrino astronomy might start sooner than expected !
• Major break-through in TeV--astronomy supernova shells are 100 TeV accelerators large population of extended galactic TeV sources discovered first microquasar-candidates established as TeV accelerator diffuse galactic TeV emission (Milagro, H.E.S.S.) TeV- from Active Galactic Nuclei at large red-shifts, …
AGN
Black Holes
Microquasars
Gamma Ray Bursts
Pulsars
Dark Accelerators
Supernovae
The Cosmic Accelerator Cocktail ?