1. CEA Saclay – Institute of research into the fundamental laws of the Universe KM3NeT Physics case Th. Stolarczyk CEA Irfu SSC open session meeting March 30 th, 2011 www.km3net.org

2. Contents Overview A KM3NeT detector Point like sources Other topics Considerations on the future Conclusion Note : Most of the results are from the KM3neT TDR. Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 2

3. The goals Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 3 p/A + p /             HE  HE    HE  HE     e e  e e e +  HE  e +  e +  HE  (inverse Compton) Pulsars Supernova remnants AGN Microquasars GRB Origin of cosmic rays Understanding of know sources Unknown phenomena Galactic Extra-Galactic

4. Atmospheric muons  10 8 per year.km 3 Atmospheric neutrinos  10 4 per year.km 3 Cosmic ray Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 4

5. Atmospheric Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 5 Log(E) Log(dN/dE) E -3.7 E -2 atm Cut 1 – 10 TeV Often shown as E 2 x dN/dE

6. HE telescopes Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 6 Mediterranean South Pole Lake Baïkal Mediterranean

7. Sky view Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 7 Mediterranean ~ 43 o North South Pole 0% 100 % North-South common sky : 0.5  sr instantaneous 1.5  sr per day Nothern hemisphere detectors : Galactic center seen 75% of the time Cover Hess and Auger skys

8. Searches for sources… VHE  -ray sources (107) detected by Cerenkov telescope Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 8 Galactic plane (61)  Many sources without counterpart (unidentified)

9. 380 d. 40 lines 36900 evts E>1 PeV above horizon Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 9 Antares IceCube Equatorial coord. 304 d.  7 lines 2040 evts 22779  14121 

10. A KM3NeT DETECTOR Outlook and performance of Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 10

11. The KM3NeT “ proposal ” Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 11 KM3NeT sensitivity 90% CL KM3NeT discovery 5  50% IceCube sensitivity 90%CL IceCube discovery 5  50% 2.5÷3.5 above sensitivity flux. (extrapol. from IC40) Declination 1 year

12. Detector configuration 310 DUs @ 180 m 20 floors @ 40 m / DU Active height = 760 m 2 Digital Optical Modules* / floor Hexagonal sea floor layout  50 DUs  1 km 3 instrumented volume Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 12 In the TDR, many studies made with 6 x 8’’ PM / floors.  Results checked to remain similar. Further studies on-going.

13. Energy response Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 13

14. DU-distance Optimisations made so far for E -2 spectrum. E spectrum with cut-off requires further optimisation of the distance between DUs Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 14 10 TeV logE Log(dN/dE) E -2 E-E-  =2.2  =2.0

15. Performance Selection optimized for E -2 sources (quality cut, number of hits, cone size). Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 15   Quality cut for 0.2° @30 TeV Antares 100 X Antares Effective area Below the size of some galactic sources Angular resolution

16. Performances (cont’d) Obtained with a binned method Use of (like in IceCube) unbinned method + energy estimator  40% better ? Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 16 Discovery 50% @ 5  Sensitivity 90% CL  =-60° Discovery 5  50% Sensitivity 90%

17. POINT-LIKE SOURCES Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 17

18. Point Like Sources Extra galactic Acceleration processes ? Transparent to TeV  ? EBL absorption  Uncertain predictions Galactic Transparent to TeV .  Upper limit on prediction (hadronic scenario) Challenging: Cut-off in E Extended (> angular resolution)  atm background Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 18

19. Galactic candidates SNR RXJ1713 and Vela Junior Most intense E>10 TeV sources PWNe (Pulsar Wind nebulae) Vela X Galactic centre Hess J1745-290 (=SMBH Sagittarius A*) SNR Sgr A East PWN G359.95-0.04 Microquasars (X-ray binary system with radio jets) GX 339-4, SS 433, LSI+61303, LS 5039 Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 19 Hess RXJ1713-39.43

20. The galactic source challenge Extended sources Discovery potential degrades as source size increases Energy cut-off Closer to the atm background Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 20 RXJ 1713 Discov. Pot. 5  Sensitivity 90% CL 5  Discov. Pot. Cut-off at 20 TeV 1 year

21. Some predictions Full Monte Carlo study  Evidence in less than 4 years. Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 21 RXJ 1713 Hess RXJ1713-39.43 RXJ 1713 IF protons are efficiently accelerated !

22. Is RXJ 1713 a proton accelerator ? Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 22 Hadronic model  0  e+   e+ 

23. Is RXJ 1713 a proton accelerator ? Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 23 Electromagnetic model e+   e+   0 

24. RX J1713 measured by Fermi-LAT Released today on arXiv:1103.5727 Presented by A.Kappes before lunch break Scanning mode data Aug. 2008 - Aug. 2010 Energy range: 500 keV - 300 GeV Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 24 Fermi-LAT count map after background subtraction RX J1713 detected at 8.6σ

25. RX J1713 measured by Fermi-LAT Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 25 From their summary: The spectral index in the Fermi-LAT band is very hard... which is well in agreement with emission scenarios in which the dominant source of emission is Inverse Compton scattering... the combination with H.E.S.S. data... strongly suggests a leptonic origin of the gamma-ray emission. From their summary: The spectral index in the Fermi-LAT band is very hard... which is well in agreement with emission scenarios in which the dominant source of emission is Inverse Compton scattering... the combination with H.E.S.S. data... strongly suggests a leptonic origin of the gamma-ray emission.

26. OTHER TOPICS A brief overview of Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 26

27. Transient sources (GRBs) Dramatic reduction of the atm. background 3  100 s / (2°)² is 4.10 -3 Two complementary strategies Use of the GCN system from Satellites (Swift, Fermi, SVOM…) All sky search (2  view) Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 27 GRB Expected Signal Backg. GRB080319B 2.65 x 10 -4 GRB080916C 2.75 x 10 -4 100 typical GRB (  1 yr) 126 x 10 -2 Neutrino flux hard to predict since mechanism largely unknown.

28. Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 28 Amanda Antares 07-09 WB limit KM3NeT 1yr Icecube 1 yr Atmospheric Baikal NT 200 Diffuse flux IC 40 preliminary

29. Dark matter search Wimps annihilation in the Sun 4.10 6 of models (DarkSusy) in the mSugra parameter space Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 29 ReachableUnreachable WMAP compatible

30. Other physics Galactic neutrinos Interaction of CR on ISM Cosmogenic neutrinos Interaction of CR on EBL (E > 1 PeV) Correlations with other messengers UHECR (Auger) Gravitational waves Classical physics Atmospheric neutrinos at high energies Atmospheric muons Particle physics (HE interaction, oscillations…) Exotic phenomena Monopole, nuclearites Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 30

31. THE UNKNOWN An illustration of what you expect from Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 31

32. Fermi Bubbles (Fermi LAT Observation ) Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 32 5 – 50 GeV 1 – 5 GeV Large extension (50° lat. 40° long.)

33. Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 33 Fermi Bubbles (Fermi LAT Observation ) 5 – 50 GeV 1 – 5 GeV Astrophys.J. 724 1044-1082 2010

34. Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 34 ~ 4 10 -7 Fermi Bubbles (Fermi LAT Observation )

35. Fermi Bubbles Discovery potential M. Crocker and F. Aharonian PRL106(2011)11102 Interpretation as a “saturated” reservoir of cosmic rays Related to the Star Formation rate in the center of the Galaxy  flux  10 -7 *E 2 GeV -1 cm -1 s -1 Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 35 Preliminary – 154 DU R. Coniglione

36. IMPLEMENTATION Strategic issues Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 36

37. Geopolitics in the Mediterranean Sea Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 37 Antares (1/50 km 3 ) Toulon, France -2475 m Nestor Pylos, Greece -3000 m to -5200 m Nemo Capo Passero, Italy -3500 m

38. Assume this is the money outlook Regional money (France, Italy, Greece): 3 x 50 M€ Other funds (agencies, Europe, whatever…): 100 M€  Total : 250 M€ would become available Constraints Regional money is not synchronised (comes in lump sums) Other funds are available relatively smoothly In this game, a staging strategy is mandatory Detector building block could be: 50 M€, 60 DUs  This could required considering physics issues. Considerations on the future Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 38

39. Performance versus DU number Effective areaAngular resolution Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 39 Effect of staging seems not dominant for the TDR detector Loose cuts X 3 0.40° 0.55°

40. Conclusion KM3NeT is a unique opportunity to investigate the Galaxy Galactic cosmic ray origin Galactic Centre (see Fermi bubbles) Complement ‘TeV-PeV’ Icecube sky Full sky coverage  Global Neutrino Observatory with Icecube ? Partner of the multi-messenger astronomy Auger, CTA, but also SVOM, Fermi… A very large European instrument for Sciences Including Earth and Sea Sciences Reliable Funding planning crucial for the time line and the staging strategy. Amsterdam - 30 March 2011 Th. Stolarczyk - CEA Irfu 40