The Experimental Status at TeV Energies Jim Hinton University of Leeds.
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Transcript of The Experimental Status at TeV Energies Jim Hinton University of Leeds.
![Page 1: The Experimental Status at TeV Energies Jim Hinton University of Leeds.](https://reader038.fdocuments.in/reader038/viewer/2022110322/56649d575503460f94a36ced/html5/thumbnails/1.jpg)
The Experimental Status at TeV
Energies
Jim HintonUniversity of Leeds
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Non-thermal radiationGround-based -ray TechniquesCurrent InstrumentsA quick introduction to the TeV source classes
Supernova remnantsPulsar wind nebulaeUnidentified galactic sourcesAGN
Outline
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Energy Flux (F)
Stars
Dust
Detectors?
Radio Infra-red X-rays -rays
Tracers for ultrarelativistic electrons and hadrons
Non-thermal windowsRadio (low energy electrons)Hard X-ray
-ray
SatellitesCherenkov Telescopes
Inverse Compton Scattering
Synchrotron Emission
0 decay
Energy
Optical, UV, Soft X-ray – Heavily absorbed
The ‘Non-Thermal Windows’
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Tracers
X-raysSoft X-rays still dominated by thermal emission2-10 keV band excellent resolution, very sensitive instruments
– but – Synchrotron emission gives information only on energetic electrons ( ×B2 )
Hard X-ray detectors not yet as sensitive
GeV -rays?Hard to launch large detectors, poor angular resolution (< a few GeV)
TeV Neutrinos?Small effective collection area, atmospheric background
TeV -rays?Large detection areas, better angular resolution
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Pair production→e+ e-
Bremsstrahlunge- + () → e- +
Cascade develops
~ 120 m
Primary -ray
ParticleShower
~ 10 km
Air Cherenkov Technique
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Pair production→e+ e-
Bremsstrahlunge- + () → e- +
Cascade develops
Charged relativistic particles emit Cherenkov light
1° angle at 10 km height → 100 m radius ‘light-pool’~10 ns light ‘flash’
~ 120 m
Primary -ray
ParticleShower
~ 100 m
~ 10 km
Air Cherenkov Technique
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Primary -ray
Air-shower...
Detecting Very High Energy Gamma-Rays with Cherenkov Light
~ 120 m
Focal Plane
ParticleShower
Image Analysis gives Shower Energy Background rejection Shower Direction
~ 100 m
~ 10 km
Air Cherenkov Technique
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Air-shower...
Detecting Very High Energy Gamma-Rays with Cherenkov Light
~ 120 m
Focal Plane
ParticleShower
Image Analysis gives Shower Energy Background rejection Shower Direction
Stereoscopic viewsImproved angular resolution and background rejection ~ 100 m
~ 10 km
Primary -ray
Air Cherenkov Technique
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~ 120 m
ParticleShower
Total amount of Cherenkov light produced (approx) Shower Energy
Arrival times at photosensors (approx) Shower Direction
Distribution of particles on ground
(some) background rejection
Primary -ray
WaterTank
Photosensors
Water Cherenkov Technique
+ ~100% duty cycle+ Wide FoV- Background Sensitivity- Angular resolution- Energy resolution
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IACT Systems
3 Major systems, all have~100 GeV energy threshold~0.1° angular resolution~4° Field of View1% Crab flux ( ~ 3 ×10-13 erg/cm2/s ) sensitivity
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Major VHE Instruments
STACEE
MILAGRO
TIBETARGO-YBJ
PACT
TACTIC
MAGIC
HESS
MILAGRO
VERITAS
UK + Ireland
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Four 13m diameter telescopes in the Khomas highlands of Namibia (southern Africa)
Latitude 23° south → galactic sources100 GeV – 100 TeV, 15% energy resolution5’ angular resolution, 5° field of view150 hours/year open to external observation proposals
e.g. HESS
completed early 2004
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Four 13m diameter telescopes in the Khomas highlands of Namibia (southern Africa)
Latitude 23° south → galactic sources100 GeV – 100 TeV, 15% energy resolution5’ angular resolution, 5° field of view150 hours/year open to external observation proposals
e.g. HESS
VERITASVery similar system in Arizona, completed early 2007
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Under Construction
MAGIC-IIA second 17 m tel.
HESS-IIA new 30 m tel.
Aiming at lower energies and better sensitivity
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Performance: Sensitivity
Funk,
Reim
er,
Torr
es,
Hin
ton 2
007
Milagro
(VERITAS)+
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Performance: Angular Resolution
Can reach 2 orders of magnitude better resolution than at 1 GeV
for much less money!
Resolution Science
source IDs, resolved systems…
Simulation: 36x 18m telescopes
Funk,
Reim
er,
Torr
es,
Hin
ton 2
007
1’
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Source number versus time
Adapted from T. Kifune by R. White
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The TeV Sky in 2007
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TeV Source Populations
ExtragalacticActive galactic nuclei 20
( point-like emission, variability seen in all strong sources)
GalacticSupernova remnants ~10Pulsar wind nebulae ~20Unidentified galactic plane sources ~20
( all typically extended on 0.1-1 degree scales ) +Gamma-ray binaries 3 (4)
( all showing variable/periodic emission)
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- 85°
+65°
Galactic Centre
~6°
Significance of -ray excess
2004-07, 40 sources, scale saturated at 20 σ
HESS Galactic Plane Survey
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Milagro Northern Sky Survey
7 year exposure~20 TeV median energy0.5° angular resolution~0.5 Crab sensitivity3 significant new sources (all on galactic plane)
Abdo et al ICRC 2007
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Milagro Northern Sky Survey
7 year exposure~20 TeV median energy0.5° angular resolution~0.5 Crab sensitivity3 significant new sources (all on galactic plane)
Abdo et al ICRC 2007
HESS ICRC 2007
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Milagro Northern Sky Survey
7 year exposure~20 TeV median energy0.5° angular resolution~0.5 Crab sensitivity3 significant new sources (all on galactic plane)
Abdo et al ICRC 2007
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Supernova remnants
Best candidates for acceleration of the bulk of the galactic cosmic rays
Well established mechanism (diffusive shock acceleration)Energetics are OK (10% kinetic energy into cosmic-rays)
Evidence for ultrarelativisitic electrons in young SNR
X-ray synchrotron emission:
x2 x2 x2
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ROSAT – X-ray HESS – TeV -ray
Purely non-thermal X-ray source1000 year old, Distance ~ 1 kpc, dense environment?First TeV gamma-ray SNR (and first image, Nature 432, 75)Closely correlated keV/TeV morphology…
MoonFor Scale
ASCAcontours
TeV Shells e.g. RX J1713.7-3946
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Close correlation with X-rays [+electrons]Spectral shape [+protons]IC interpretation implies (too) low B-field [+protons]No correlation with molecular material [+electrons]
Not yet clear…Need data at lower energies to be sure, e.g. GLAST
protons
electrons
Energy Spectrum
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SNR/cloud interactions?
Correlations with available target materialIC 443 and W 28, Old (>104 yr) SNRs near mol. CloudsBoth have associated GeV sources pp → π0 → ?
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Relativistic e-/e+ plasma wind driven by pulsar - confined by SNR of pulsar progenitor
Efficient conversion of rotation power into relativistic particlesAssociated with young pulsars - high ‘spin-down power’Expansion in non-uniform medium may lead to complex morphol.
High ISMdensity
Low ISMdensity
Reverse shock crushes PWN
Blondin et al. ApJ 563 (2001) 806
G21.5-0.9 Chandra / H.Matheson & S.Safi-Harb
Pulsar Wind Nebulae
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Many known X-ray PWN now identified as TeV emitters and almost all of the highest spin-down power radio pulsars have associated TeV emission
Efficient particle accelerators
May be easier to detect in TeV than keV ?Integration over pulsar lifetime for TeV electrons (less cooling)TeV instruments sensitive to more extended objects no confusion with thermal emissionMany of our unidentified sources may be PWN
The PWN Population
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Random Catalogues
Implied efficiency Spin-down → TeV
~ 1%
-ray PWN can be large, asymmetric and offset from the pulsar Need to assess chance coincidence HESS scan analysis shows that 70% of Edot/d2 > 1035 erg/s/kpc2 are TeV sources
Search for TeV PWN
HESS
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PSR J1826-133431036 erg/s spin-down power, ~2104 years old
5’ X-ray PWNG 18.0-0.7 (Gaensler et al 2002)
1° TeV -ray sourceHESS J1825-137 (Aharonian et al 2005)
Energy dependent morphologyA first at TeV energies
Cooling of electrons away from pulsar? (tcool 1/E)
[ 2 keV synchrotron emission comes from 200 TeV electrons (if B 10 G)…, -rays come from lower energy electrons ]
HESS
HESS J1825-137
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Gamma-ray binaries
Three (4) systems, two basic scenariosPSR B1259-63 / SS 2883, LSI +61 303, LS 5039 + (Cyg X-1)
Mirabel 2007
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Gamma-ray binaries
High mass companions
O and B stars
PSR B1259-63 = NSLS 5039/LS I +61 303
Nature of compact object not clearBoth appear to have relativistic radio jets Gamma-ray spectral modulation (LS 5039), absorption, variation of acceleration with phase ??
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Gamma-ray binaries
High mass companions
O and B stars
PSR B1259-63 = NSLS 5039/LS I +61 303
Nature of compact object not clearBoth appear to have relativistic radio jets Gamma-ray spectral modulation (LS 5039), absorption, variation of acceleration with phase ??
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Unidentified Sources
Some sources have been (rather rapidly) identified through multiwavelength work
e.g HESS J1813-178 new radio SNR and new X-ray PWN
Some objects with compelling association but …E.g. Sgr A*, Stellar cluster Westerlund 2
Several rather extended objects where ID is difficultNeed more MWL work, and perhaps more sensitive TeV instruments (substructure, spectral clues, E-dep. morph. …)
Funk, Hinton et al 2007
XMM H.E.S.S. / VLA
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The Galactic Centre
TeV source in Sgr A discovered using Whipple 10mConfirmed by CANGAROO, HESS + MAGICGravitational centre of our galaxy – dark matter annihilation?
Deep HESS observationsPrecise (10”) localisation of sourceSpectrum measured over two decades in energyDiscovery of diffuse emission in the central 200 pc
HESS
SNR/PWNG 0.9+0.1
Sgr A Sgr A
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Supernova remnant Sgr A EastPulsar wind nebula G359.95-0.04Supermassive Black Hole Sgr A*Dark matter cusp?
H.E.S.S. 2005Contours - VLA radio
Sgr A East
100''
Sgr A*
Pulsar? - G359.95-0.04
Sagittarius A
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Sagittarius AH.E.S.S. 2005preliminary
Contours - VLA radio
Sgr A East
100''
Sgr A*
Pulsar? - G359.95-0.04
Supernova remnant Sgr A EastPulsar wind nebula G359.95-0.04Supermassive Black Hole Sgr A*Dark matter cusp? 10''
Sag A*
G359.95
Chandra – X-ray
HESS2007
stat. +sys.
10''
G359.95
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1 degree
CS Line Emission (dense clouds)smoothed to match H.E.S.S. PSF
HESS
pp → π0 → ?
Diffuse Emission
Point-source subtracted
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TeV emission from Westerlund 2?
Extended TeV source coincident with the massive stellar cluster Westerlund 2 discovered using HESS in 2006
Collective effect of stellar winds?
Radio
PSF
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TeV emission from Westerlund 2?
Extended TeV source coincident with the massive stellar cluster Westerlund 2 discovered using HESS in 2006
Collective effect of stellar winds?
Radio
PSF
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All 20 known extragalactic VHE gamma-ray sources are active galactic nucleiAll but one (M 87) are blazars
Particle acceleration in relativistic jetsBeaming allows us to see distant objects… but,
The gamma-ray horizon is limited by absorption via pair-production on the extragalactic background light (EBL)
Lower gamma-ray energies → more distant objectsThe spectral shapes of VHE sources can be used to place limits on the EBL – important cosmologically
Extragalactic Sources
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Relativistic AGN jet aligned within a few deg. of the line-of-sightHighly variable broad-band emission
typically correlated TeV/keV emission
keV TeV
Mrk 421
Whipple 10m tel.
Synchrotron Self Compton Fits
TeV Blazars
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2-3 minute variability timescales Very constraining for models, implies Г > 50 can be used to probe Quantum Gravity
>2 order of magnitude flare, July 2006
Crab Nebula Flux
HESS28th July 2006
MAGIC30th June 2005
Crab Nebula Flux
×10
-9
Quiescent Flux
Mrk 501 (MAGIC), PKS 2155-304 (HESS)
e.g. Begelmann, Fabian, Rees 2007
e.g. Albert et al 2007
TeV Blazar Flares
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New HESS and MAGIC AGN
xxx
VHEEBL e+e-
EBL
Approx.`Gamma-ray horizon’
3C 279(z=0.54)
RGB J0152+017
20 known TeV AGN
1ES 1011+496
TeV Blazars and the EBL
Absorption signature
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EBL constraints
Mazin+Raue 2007
Combined limits from all VHE blazars
Galaxy Counts
Direct limits
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M 87
Famous nearby radio galaxy16 Mpc, Jet angle ~30°
HESS 2 day variabilityEmission region
< 5 RS
Multi-year observations from HEGRA, HESS, VERITAS
Long timescale variability
Emission site?Knot HST1?Very close to SMBH?
HESS source pos.
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M 87 - Variability
Colin et al 2007
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M 87 – X-ray connection
2-10 keV emission (core dominated?) correlates well with TeV emission on long (6 month) timescales
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04 05 0607 08 09 10 11 12 13
HESS
MAGIC
VERITAS
CTA
GLAST
AGILE
Phase 1
Phase 1 Phase 2
Phase 2
Move to permanent site
Design Study Construction
We may be entering the golden age of (>GeV) gamma-ray astronomy
GeV - TeV -Ray Projects
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Conclusions
Enormous progress in the last few yearsLots of activity on new instrumentsGreat scientific potentialThe UK and Ireland have been involved since the beginning – and could play substantial roles in the future
Need new people / institutes
Funding?