1. TeV 物理工作组会议
曹臻，IHEP，北京
泰达学院，塘沽，2009

2. CRs at TeV Ultra High Energy Cosmic Rays GZK cut-off related physics
TeV γray astronomy

3. “conventional” model Propagation effects Fermi acceleration
Astro-accelerators?

4. Out line TeV γray astronomy (introduction)
CR observational TeV region
What can LHAASO contribute
Status of the project

6. In our galaxy

7. All interesting objects
PWN: Crab, Vela …
SNR: RXJ1713, Cas A …
XRB: Cygnus X-1, LS 5039 ….

8. Models for γray emission
Electron origin model: synchrotron+IC
Synchrotron photons could be scattered again by electrons (SSC model)
Multi wavelength observation
???
lg10 (E/eV)

9. Difficulties: RXJ1713.7-3946 ASCA data: (synchrotron X rays)
Leptonic 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 sIC/sSync a B-2 )
Hadronic model favored
Hadronic model
Still pending:
Hadronic model to be confirmed
Occurence of such objects? (cf scan)

10. We are looking for good astro-accelerator lab in the sky
SN1006:
γ ray observation
still needs to be
improved

11. 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 is
Another example
which does not
Show difference
Of spectral index

12. LS I +61 303 Radio Outbursts near apastron, ~4yr modulation Be Star
TeV Activity detected by MAGIC/VERITAS around apastron passage
High X-ray activity
throughout orbit (strongest at apastron,
secondary near periastron)
Be Star
BH/NS
P~26.5 day
Earth
By Andy Smith at TeVPA 2009, SLAC

13. All Data 2006-2009 Preliminary Apastron Preliminary Preliminary
By Andy Smith at TeVPA 2009, SLAC
Apastron
Preliminary
Phases
Phases
~4.5σ(pre-trial)
10σ
Preliminary
Preliminary

14. Almost isotropic and from z=0.0044(M87) to z=0.536(3c 279)

15. Many varying sources
> 0.05ICrab at base states
≥10 ICrab during flares
Very far sources:
EBL absorption is severe
above 10TeV

16. γastronomy: Mrk421flares
5.9σ
2006/07-08
2006/09
2006/10
2006/11
2006/09
ASM of RXTE
ARGO
2006/7~8：5.9σ
2007：very calm
2008/1~4：~5.7σ
RXTE

17. Mrk421single flare: 10ICrab
Whipple
ARGO has seen a 4σeffect
for 2008/05/02 transition.

18. Multi-wave-length Observation of Flares of Mrk421 For LHAASO, only
ARGO
RXTE/ASM
2008 June 11-13
day
Multi-wave-length
Observation of
Flares of Mrk421
For LHAASO, only
1 minute is needed

19. Multi-wavelength observation: does SSC model work perfectly?
More sensitive
observation with
much larger
exposure
is essential in
TeV regime
VERITAS
Collaboration

20. Mrk 501 Longterm Variability

21. There are many samples
“Personality” seems very strong between
transient events and objects
Many “guesses” with lacks of strong evidences.
Strong demanding on population study: full sky survey！

22. Or some big pieces “dropped” into BH/NS and
triggered an outburst??

23. TeV γRay Astronomy γRay Burst Search & Exotic phenomena
Yet successfully observed any GRB
Dark matter search
Quantum gravity effect search

24. Focus of CR observation @ TeV
Knee and second knee
Absolute energy scale at UHECR experiments
Forward region behavior
μ content in a shower

25. 1017 eV Energy Spectrum: second knee: where is it? why?

26. UHECR Research (experiment)
access?
YBJ

30. What can LHAASO help?
All sky source survey

31. Scientific Problems and Possible Solutions
Hadronic model
Leptonic model ？
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 ground based UHECR measurements
Searching for Dark Matter galactic sub-structures

32. Large High Altitude Air Shower Observatory
LHAASO Project: γastronomy and origin of CR
Wide FOV
C-Telescope
Array
&
Core Detector
μdetector
Array
Water C
Array
Charge
Particle
Array
Large High Altitude Air Shower Observatory

33. Forγastronomy ？
ARGO

34. 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)

35. The keys are to lower threshold, making connections with direct measurements & measure spectra up to 100PeV

36. A bridge between balloon measurements and ground base UHECR experiment covering both “knees” with absolute energy scale

37. An unique location
knee
Second knee
We are here

38. R/D budget: ~$1M
Detector unit IHEP
Prototyping

39. On Site Prototype Exp. 1% of the final configuration of LHAASO
ARGO Hall
1% of the final configuration of LHAASO

41. 预先研究进展
1%规模实验计划

42. CR Energy Spectrum (160k events) resolution < 10% With bias<3%
Core resolution <1m
From S. P. SWORDY, Space Science
Reviews 99: 85–94, 2001.

43. Conclusion
√s ~ 1TeV for CRs is a very important region associated 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