LHAASO @ TeV 物理工作组会议
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Transcript of LHAASO @ TeV 物理工作组会议
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LHAASO @ TeV 物理工作组会议
曹臻, IHEP,北京
泰达学院,塘沽, 2009
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CRs at TeV
TeV γray astronomy
Ultra High Energy Cosmic Rays GZK cut-off related physics
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“conventional” model
• Propagation effects• Fermi acceleration• Astro-accelerators?
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Out line
• TeV γray astronomy (introduction)
• CR observational focus @ TeV region
• What can LHAASO contribute
• Status of the project
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In our galaxy
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All interesting objects
• PWN: Crab, Vela …
• SNR: RXJ1713, Cas A …
• XRB: Cygnus X-1, LS 5039
• ….
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Models for γray emission• Electron origin model: synchrotron+IC• Synchrotron photons could be scattered again b
y electrons (SSC model)• Multi wavelength observation
lg10 (E/eV)
???
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Hadronic model
ASCA data:
(synchrotron X rays)• Fine structures in the radiation
morphology points to B>100µG• If leptonic, X/TeV ratio requires
B~10µG (with IC/Sync B-2 )
Hadronic model favored
Difficulties:RXJ1713.7-3946 Leptonic model
Still pending: Hadronic model to be confirmed Occurence of such objects? (cf scan)
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We are looking for good astro-accelerator lab in the sky
SN1006:γ ray observation still needs to be improved
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The other example: PSR B1259-63• XRB: TeV emission occurs as the compact
object is far away from the Be Star?!
Could be an effect of absorption by photons from the B-star, however, is it really against the SSC model?
LSI+61 303 is Another example which does not Show difference Of spectral index
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EarthEarth
LS I +61 303LS I +61 303
P~26.5 dayP~26.5 dayBH/NSBH/NS
Be StarBe Star
Radio OutburstsRadio Outburstsnear apastron,near apastron,
~4yr modulation~4yr modulation
High X-ray activityHigh X-ray activitythroughout orbit throughout orbit
(strongest at apastron,(strongest at apastron,secondary near secondary near
periastron)periastron)
TeV Activity detected TeV Activity detected by MAGIC/VERITAS by MAGIC/VERITAS around apastron around apastron
passagepassage
By Andy Smith at TeVPA 2009, SLAC
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All Data 2006-2009All Data 2006-2009
Prel
imin
ary
Prel
imin
ary
Prel
imin
ary
Prel
imin
ary
Prelim
inary
Prelim
inary
1010σσ ~4.5~4.5σσ(pre-trial) (pre-trial)
ApastronApastron
Phases 0.9-0.5Phases 0.9-0.5Phases 0.5-0.9Phases 0.5-0.9
By Andy Smith at TeVPA 2009, SLAC
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Almost isotropic and from z=0.0044(M87) to z=0.536(3c 279)
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Many varying sources > 0.05ICrab at base states≥10 ICrab during flares
Very far sources:EBL absorption is severe above 10TeV
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γastronomy: Mrk421flares
• 2006/7~8: 5.9σ• 2007: very calm• 2008/1~4: ~5.7σ
ASM of RXTE
2006/07-08
2006/09
2006/10
2006/09
2006/11
5.9σ
RXTE
ARGO
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Mrk421single flare: 10ICrab
• ARGO has seen a 4σeffect
for 2008/05/02 transition.
Whipple
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ARGO
2008 June 11-13day163-165
RXTE/ASM
Multi-wave-length Observation of Flares of Mrk421For LHAASO, only 1 minute is needed
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Multi-wavelength observation:does SSC model work perfectly?
More sensitive observation with much larger exposureis essential in TeV regime
VERITASCollaboration
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Mrk 501 Longterm Variability
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There are many samples“Personality” seems very strong between transient events and objectsMany “guesses” with lacks of strong evidences. Strong demanding on population study: full sky survey!
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Or some big pieces “dropped” into BH/NS and triggered an outburst??
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TeV γRay Astronomy
• γRay Burst Search & Exotic phenomena– Yet successfully observed any GRB– Dark matter search– Quantum gravity effect search
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Focus of CR observation @ TeV
• Knee and second knee
• Absolute energy scale at UHECR experiments
• Forward region behavior
• μ content in a shower
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1017 eV Energy Spectrum: second knee: where is it? w
hy?
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UHECR Research (experiment)
YBJ
access?
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What can LHAASO help?
• All sky source survey
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Scientific Problems and Possible Solutions
• TeVγray observation has an opportunity of finding CR origin: 80+ sources discovered– 50+ galactic sources: γat high energy (>30TeV) is crucial
(high sensitivity and high energy resolution)
– All-sky survey forγsource population is necessary
(full duty cycle, wide FOV and sufficient sensitivity)
• PeV CR spectra of individual composition– Bridge between space/balloon borne measurements and g
round based UHECR measurements
• Searching for Dark Matter galactic sub-structures
?
Hadronic model
Leptonic model
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Large High Altitude Air Shower Observatory
Charge Particle
Arrayμdetector
Array
Water CArray
LHAASO Project: γastronomy and origin of CR
Wide FOVC-Telescope
Array&
Core DetectorArray
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Forγastronomy
ARGO
?
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Resolution for light and heavy composition
μ-content, Xmax and HE (>30TeV) shower particles
Proton Iron
For Proton and Helium:
1.5 m spacing
Nb>100 , any 5
(> 30 GeV)
For Iron:
3.75m spacing
Nb>100 , any 21
( > 30 GeV)
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The keys are to lower threshold, making connections with direct measurements & measure spectra up to 100PeV
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A bridge between balloon measurements and ground base UHECR experimentcovering both “knees” with absolute energy scale
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An unique location
knee
Sec
ond
knee
We are here
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Prototyping• R/D budget: ~$1M
• Detector unit prototype @ IHEP
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On Site Prototype Exp.
• 1% of the final configuration of LHAASO
ARGO Hall
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预先研究进展
• 1% 规模实验计划
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From S. P. SWORDY, Space Science Reviews 99: 85–94, 2001.
CR Energy Spectrum
(160k events)
resolution < 10%With bias<3%Core resolution <1m
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Conclusion• √s ~ 1TeV for CRs is a very important region ass
ociated with a transition from galactic origins to extra-galactic origins
• Elab~ 1TeV for γrays is one of the most active astro-particle physics fields. Many sources have been discovered in the last two decades
• LHAASO will boost all sky source survey power for population study, also have strong power for galactic CR source discovery
• Currently, the R/D for the project goes smoothly