Cosmic RaysGammas, Hadrons, Neutrinos

Thomas LohseHumboldt University Berlin

HEP2005 International Europhysics Conference on High Energy Physics

July 27th 2005Lisboa, Portugal

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

Outline

1. The nature of the knee

2. Cosmic rays beyond the ankle

3. Neutrinos from cosmic ray sources

4. Gammas from cosmic ray sources

1. The nature of the knee

2. Cosmic rays beyond the ankle

3. Neutrinos from cosmic ray sources

4. Gammas from cosmic ray sources

Outline

log E

log

E

2.5

F

pSi

Fe

Knee

Interpretation of the Knee

EKnee ZEKnee Z

New physics in air shower development

new strong interaction

new strong interaction

EKnee AEKnee A

Diffusive escape from galactic B-field

Maximum acceleration energy

KASCADE: Unfolding for individual mass groups

Input:

measured ne vs. n

hadronic interaction models

• large model dependence

• no model describes all data

• more experimental input for hadronic interaction models needed

1. The nature of the knee

2. Cosmic rays beyond the ankle

3. Neutrinos from cosmic ray sources

4. Gammas from cosmic ray sources

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 50% installed

4 Fluorescence Sites3 fully operational

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

Search for Localized Excess Fluxes with AUGER

Exposure Map

Event Map

Example:1 EeV E 5 EeV5 Smoothing

30548 events

AGASA evidence for small scale anisotropies NOT confirmed!

Excess significance distribution

1. The nature of the knee

2. Cosmic rays beyond the ankle

3. Neutrinos from cosmic ray sources

4. 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

Point Source Search in Northern Hemisphere

test region (MC-optimised)

background estimation from

real data

AMANDA 2000-2003

preliminary

AMANDA 2000-2003

preliminary

Selected: 3329 clean

Expected: 3438 atmosph.

Selected: 3329 clean

Expected: 3438 atmosph.

• Hemisphere averaged• 33 pre-selected point-source candidates• Source stacking (11 samples)

Typical limits

No significant excess

.l.c %90scm10GeV 10 1298ν

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. The nature of the knee

2. Cosmic rays beyond the ankle

3. Neutrinos from cosmic ray sources

4. Gammas from cosmic ray sources

H.E.S.S. CANGAROO III

MAGIC

Veritas

in construction

Cherenkov Telescopes (3rd Generation)

resolution

H.E.S.S. 2004E 210 GeV

RX J1713.73946

resolution

H.E.S.S. 2004E 210 GeV

RX J1713.73946

1) Supernova Shells: Cosmic Ray Accelerators?

H.E.S.S. 2005 preliminary

preliminary

E 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

ln(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. preliminarymodels: F. AharonianH.E.S.S. preliminarymodels: F. Aharonian

Continuous proton injection over 1000 years Injection spectrum: power law, index 2 Different cutoff shapes & diffusion parameters

Proton accelerator fit:

H.E.S.S. preliminary

RX J1713.73946

models: F. Aharonian

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

2) Galactic Centre: A TeV- Point Source

H.E.S.S. (95%)

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. (preliminary)

3) H.E.S.S. Scan of Inner Galactic Plane

HESS J1834-087

HESS J1804-216

HESS J1640-465

Resolution

8 new sources, all extended! Possible counterparts: 7 SNR/PWN1 ???

TeV-Gamma-RayRadioX-Ray

… a new source class: “Dark Accelerators”

Three sources known: TeV J20324130 (HEGRA)

HESS J1303631

HESS J1616508

What are these sources? Are they hadron accelerators?

• extended• hard spectra, • steady emission

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

4) Extragalactic Sources: 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

Mrk421Mrk501

1ES 19596501ES 2344514

PKS 2155304H1426428

PKS 2005489

EBL models

adapted from Blanch & Martinez 2004

more on ICRC‘05

CANGAROO H.E.S.S. VERITAS

MAGIC

5) X-Ray Binary LS 5039: The first TeV Micro-Quasar-Candidate

Accretion from normal star on stellar-mass black hole scaled-down AGN in our Galaxy

• Dynamics of accretion

• Jet production

• Acceleration of electrons vs. hadrons

H.E.S.S.-Discovery in Summer 2004 Galactic Plane Scan:

• 10.5 hours live time spread over 4 months

7 E 0.2 … 4 TeV

• point-like

• steady at 15% c.l.

• hard spectrum 2.12 0.15

Acceleration of particles to ≳ 10 TeV established !

Sciencexpress, July 7th, 2005

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-candidate established as TeV accelerator diffuse galactic TeV emission (Milagro water Č-telescope) TeV- from Active Galactic Nuclei at large red-shifts, …

AGN

Black Holes

Microquasars

Gamma Ray Bursts

Pulsars

Dark Accelerators

Supernovae

The Cosmic Ray Source Cocktail ?