1. The TeV view of the Galactic Centre R. Terrier APC

2. The TeV view of the Galactic Centre 2 point like sources: HESS J1745-290 compatible with GC Composite SNR G0.9+0.1 Extended source associated with unid 3EG J1744-3011 HESS > 380 GeV

3. SF2A 2004 The TeV emission from the Galactic Centre HESS J1745-290: data up to 2004 total of ~50h live time (Aharonian et al. 2004 & Aharonian et al 2006) Flux ~ 10% crab F(E>1TeV) = 1.87± 0.1 10 -12 cm -2 s -1 Luminosity: ~ 10 35 erg/s No significant variability detected Detection confirmed by MAGIC observations (Albert et al, 2005) Position and spectrum compatible

4. SF2A 2004 The TeV emission from the Galactic Centre HESS J1745-290: data up to 2004 total of ~50h live time (Aharonian et al. 2004 & Aharonian et al 2006) Flux ~ 10% crab F(E>1TeV) = 1.87± 0.1 10 -12 cm -2 s -1 Luminosity: ~ 10 35 erg/s Position compatible with Sgr A* (<7'') a = 17 h 45 m 39.44 s ± 0.6 s d = -29d00'30.3'' ± 9.7'' Statistical error: 10'' Systematic pointing error: 20''

5. SF2A 2004 The TeV emission from the Galactic Centre HESS J1745-290: data up to 2004 total of ~50h live time (Aharonian et al. 2004 & Aharonian et al 2006) Flux ~ 10% crab F(E>1TeV) = 1.87± 0.1 10 -12 cm -2 s -1 Luminosity: ~ 10 35 erg/s Spectrum: power-law:  ~2.25 ± 0.1 No indication of cut-off < 9 TeV  =2.25 +- 0.1

6. SF2A 2004 The TeV emission from the Galactic Centre Presence of underlying diffuse emission along Galactic plane 90% of total flux due to point-like source Once diffuse emission removed: Source size compatible with point source :  <1.2' (95%CL)

7. SF2A 2004 The TeV emission from the Galactic Centre HESS J1745-290: Origin of the emission?: Dark matter annihilation Non-thermal emission from SgrA east Pulsar Wind Nebula Emission from particles accelerated around SgrA*

8. SF2A 2004 Dark matter annihilation at the origin of the Galactic centre TeV emission? HESS J1745-290 spectrum inconsistent with DM annihilation (Aharonian et al. 2006, PRL) MSSM & KK models deviate from simple PL above a few TeV Contribution of DM < 10% of total HESS J1745-290 flux

9. SF2A 2004 The TeV emission from the Galactic Centre HESS J1745-290: Origin of the emission?: Dark matter annihilation: No spectral cut off Non-thermal emission from SgrA east Pulsar Wind Nebula Emission from particles accelerated around SgrA*

10. SF2A 2004 The TeV emission from the Galactic Centre HESS J1745-290: Origin of the emission?: Dark matter annihilation: No spectral cut off Non-thermal emission from SgrA east Position and size constraints Pulsar Wind Nebula Emission from particles accelerated around SgrA* 1.2' VLA 90cm

11. SF2A 2004 A PWN close to the Galactic Centre G359.95-0.04 : a candidate PWN at 7'' (0.3pc) of SgrA* (Wang et al 2006) Non-thermal cometary structure detected in X-rays (1-9 keV) Luminosity ~ 10 34 erg/sSpectral index  = 1.94 ± 0.2 10'' Chandra 1-9 keV Sgr A* IRS 13 G359.95-0.04

12. SF2A 2004 A PWN close to the Galactic Centre G359.95-0.04 : a candidate PWN at 7'' (0.3pc) of SgrA* (Wang et al 2006) Clear indication of spectral cooling of electrons Ram pressure confined pulsar wind nebula

13. SF2A 2004 G359.95-0.03 = HESS J1745-290? G359.95-0.04 as a TeV emitter (Wang et al 2006, Hinton & Aharonian, 2006) Position and extension compatible X-ray flux 1 order of magnitude lower than TeV flux Huge radiation field due to large number of massive stars in central pc up to U NIR ~ 5 10 3 eV.cm -3 IC losses are dominant ( L X << L  ) Lifetime of 50 TeV e - ~ 20 yr

14. SF2A 2004 The TeV emission from the Galactic Centre HESS J1745-290: Origin of the emission?: Dark matter annihilation: No spectral cut off Non-thermal emission from SgrA east Position and size constraints Pulsar Wind Nebula Emission from particles accelerated around SgrA* Hadrons, leptons?

15. SF2A 2004 Particles accelerated in the vicinity of the SMBH? Several mechanisms of particle acceleration in the central pc have been proposed: Stochastic acceleration around Sgr A* (Liu et al 2006) Massive stars wind collisions (Quataert & Loeb 2005) Others... Electrons radiate their energy very quickly in high ambient field Hadrons accelerated in the vicinity of Sgr A* can diffuse away Will be confined by stronger mag field in circum-nuclear disk 1.5 pc radius, height ~ 0.5 pc density ~ 10 5 cm -3 5 10 45 erg can account for TeV luminosity ( Ballantyne et al 2006)

16. SF2A 2004 The TeV emission from the Galactic Centre HESS J1745-290: Origin of the emission?: Dark matter annihilation: No spectral cut off Non-thermal emission from SgrA east Position and size constraints Pulsar Wind Nebula Emission from particles accelerated around SgrA* Stochastic acceleration of p Massive stars wind collisions  production in the dense CND : 1’ extended source And many other possibilities...

17. SF2A 2004 TeV and hard X-ray sources at the Galactic Centre IGR J17456-2901: Luminosity: 5 10 35 erg/s (20-200 keV) Spectral index: 3.04 ± 0.08 HESS J1745-290: Luminosity: 10 35 erg/s Spectral index: 2.25 XMM integrated over 5' IGR J17456-2901 is not due to: Sgr A* emission from binaries close to the GC hot plasma emission G359.95-0.04 (Belanger et al, 2006) Maybe due to: superposition of large number of faint X-ray sources in central 30pc (Krivonos et al 2006) non-thermal diffuse emission (~10pc) (Belanger et al, 2006)

18. The TeV view of the Galactic Centre

19. Diffuse emission in the Central Molecular Zone (CMZ): after subtraction of point sources

20. Diffuse emission from the CMZ CS emission (49 Ghz) traces dense cores of massive molecular clouds ~ 5 10 7 M o of molecular matter in the CMZ Tsuboi et al 1998

21. Diffuse emission from the CMZ CS emission (49 Ghz) traces dense cores of massive molecular clouds TeV diffuse emission well correlated with giant molecular clouds  produced through p-p collisions Tsuboi et al 1998

22. SF2A 2004 Diffuse  emission from CMZ supermassive clouds Diffuse emission spectrum similar to HESS J1745-290:  = 2.29 ± 0.1 Not compatible with spectrum expected from local CR spectral distribution (  ~ 2.7) Existence of a local cosmic-ray accelerator 10 49 erg in CR protons in 4-40 TeV band

23. SF2A 2004 Diffuse  emission from CMZ supermassive clouds Origin of the CR producing the TeV diffuse emission? Deficit at l=1.3° suggests propagation effect CS distribution Expected profile for 0.8°gaussian CR distrib Diffusion of CR injected by young (<10 kyr) accelerator (e.g. Sgr A east)? (Aharonian et al 2006)

24. SF2A 2004 Diffuse  emission from CMZ supermassive clouds Origin of the CR producing the TeV diffuse emission? Deficit at l=1.3° suggests propagation effect CS distribution Expected profile for 0.8°gaussian CR distrib Diffusion of CR injected by young (<10 kyr) accelerator (e.g. Sgr A east)? (Aharonian et al 2006) Diffusion of CR injected by central source HESS J1745-290 (spectral index similarity) (Ballantyne et al. 2007) In situ CR production in the molecular clouds (Yusef-Zadeh et al, 2006)

25. SF2A 2004 Diffuse TeV  & hard X-ray emission from CMZ 60-80 keV 6.4 keV Ka Fe line VHE

26. SF2A 2004 Diffuse TeV  & hard X-ray emission from CMZ 6.4 keV line and hard X-ray cloud emission usually interpreted as: - fluorescence & Compton echo of a 10 39 erg/s flare 300 yr ago - low energy cosmic-rays electrons (LECRE) Can a single CR population explain TeV & hard X-ray emissions? Sgr B (Crocker et al 2007) CR hadrons secondaries LECRE

27. SF2A 2004 Conclusions & future prospects HESS J1745-290: a point-like stable source compatible with Sgr A* (<7'') Position error due to pointing systematics (~20'') Extension < 1.2‘ radius Nature still unclear (PWN, accelerated particles around Sgr A*)? Link with hard X-ray source unclear Diffuse emission from the CMZ: Evidence of active CR accelerator in th GC region Compatible with CR injected by a single SNR 10 kyr ago Single CR population cannot reproduce hard X-ray and TeV spectra Future: Currently improving pointing accuracy CTA (>2012) with better PSF and 10 times better sensitivity: significantly improved size and position constraints improved diffuse emission imaging and morphology

28. G0.9+0.1 Composite SNR I 0 = 5.7 ± 0.7 ± 1.2 10 -12 cm -2 s -1 (>0.2 TeV) Γ = 2.29 ± 0.14 Assuming distance of 8.5 kpc: L γ = 2 10 34 erg/s L X = 5 10 34 erg/s (PWN) TeV emission most likely due to PWN SED well explained by: 6 μG field strong starlight component