1. Alexander Kappes UW-Madison 4 th TeVPA Workshop, Beijing (China) Sep. 24 – 28, 2008 The Hunt for the Sources of the Galactic Cosmic Rays — A multi-messenger approach

2. Outline  Energetics of Galactic CRs and source candidates  The missing PeVatrons and the Milagro skymap  Neutrino fluxes from Galactic CR source candidates Sep. 28, 20082Alexander Kappes, TeV Workshop, Beijing

3. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing3 Energetics of Cosmic Rays Galactic component: – GeV – PeV –   ≈ 10 -12 erg cm -3 # ≈ 4×10 -14 cm -3 – similar to energy density in light and magnetic field Transition: somewhere between 10 7 and 10 9 GeV Extra-Galactic component: – > EeV – ~10 -19 erg cm -3 extragalacticgalactic J.K. Becker

4. Even after 100 years sources of (Galactic) cosmic rays (CRs) unknown (CRs not back-traceable due to Galactic magnetic field) Multi-messenger astronomy is key: Neutrino telescopes: ✓ Unambiguous prove for CR acceleration ✗ Still under development ✗ No sources found yet  -Cherenkov telescopes: ✓ Very mature ✓ Discovered many (Galactic) sources ✗ Problem of synch/IC-pion ambiguity not overcome yet Multi-messenger Astronomy: Cosmic Rays,  -Rays and Neutrinos Sep. 28, 20084Alexander Kappes, TeV Workshop, Beijing p + p(  ) →   + X   +   e + e +  p + p(  ) →  0 + X    p  CRPhoton field p p CRIM Flux ratios (for E -2 ): (p+p) (p+  AND

5. Estimate of Gamma Flux from pp Interactions Sep. 28, 20085Alexander Kappes, TeV Workshop, Beijing Steady Galactic CR density (~10 -12 erg cm -3 ) requires 10 41 erg s -1 (finite CR containment time) Corresponds to release of 10 50 erg in CRs every 30 years Emissivity in  -rays for interaction of CRs with interstellar medium: energy released in CRs ≈ 10 -12 erg cm -3 F. Halzen, arXiv:0809.1874

6. Estimate of Gamma Flux from pp Interactions cont’d Sep. 28, 20086Alexander Kappes, TeV Workshop, Beijing Source candidates with known TeV  -ray emission: Supernovae (release ~10 51 erg every ~30 years): -n IM 100 – 1000 cm -3 in star-forming regions where SN typically occur -why don’t we see more SNe in TeV, why have all SNe cutoffs << 100 TeV? Binaries: only few observed up to now; again cutoffs << 100 TeV (absorption?) not visible in Milagro map Pulsar wind nebula: thought to accelerate (mainly) electrons Maybe something unknown!? The sources of the Galactic CR should have fluxes visible to current  -ray detector (in particular, they have to show up in the Milagro sky map)

7. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing7 The Missing PeVatrons SNRs generally considered as best candidates for Galactic cosmic ray accelerators But no SNR  spectrum extends above a few 10 TeV (“knee” corresponds to ~300 TeV) Possible reason: “Direct” high energy  -ray emission only in first few hundred years Detection still possible by observing secondary  -rays produced in nearby clouds Milagro-like experiments better suited than Cherenkov telescopes Gabici & Aharonian, arXiv:0705.3011 400 yr 2000 yr 8000 yr 32000 yr at 1 Kpc 2000 yr Cherenkov telescopes (e.g. HESS, Magic) Air shower arrays (Milagro) (10 4 solar masses) 8000 yr 10 TeV

8. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing8 2007 Milagro Sky Survey At 12 TeV Several sources along Galactic plane Large accumulation in the Cygnus region Additional small “cluster” at l = 40°

9. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing9 Milagro: Spectrum extends up to 100 TeV ! Strong indicator for proton acceleration in this source MGRO J1908+06 H.E.S.S.: E -2 spectrum without cutoff indication Flux  @ 1TeV: 3.2×10 -12 cm -2 s -1 TeV -1 (H.E.S.S. Coll., ICRC’07 proceedings)

10. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing10 MGRO J2031+41 Milagro: Flux @ 1TeV for E -2 : 2.4×10 -12 cm -2 s -1 TeV -1 MAGIC: E -2 spectrum Flux  @ 1TeV: 0.45×10 -12 cm -2 s -1 TeV -1 Lower flux probably due to high photon background in Cygnus region Milagro (Milagro Coll., ApJ 658:L33, 2007) (MAGIC Coll., ApJ 675:L25, 2008)

11. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing11 MGRO J2019+37 VERITAS: Not seen in first observation: F  < 30 mCrab (99% C.L.)  consistency with Milagro requires  < 2.2 VERITAS observation Milagro: Flux @ 1TeV for E -2 : 3.5×10 -12 cm -2 s -1 TeV -1 (VERITAS Coll., ICRC’07 proceedings) (Milagro Coll., ApJ 658:L33, 2007)

12. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing12 The Role of Neutrino Telescopes Several  -ray sources with hard spectra Photon production ambiguous Air-shower array currently only in Northern Hemisphere Cherenkov telescopes only small field of view (few deg 2 ) – cover only small part of sky (at a time) – large photon background in star-forming region (e.g. Cygnus) can hide sources Neutrinos unambiguous sign for hadronic acceleration Neutrino telescope properties very similar to air shower arrays – “all sky” sensitivity – increasing sensitivity with energy (fast decreasing background) – angular resolution O (1°)

13. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing13 Gamma and Neutrino Spectra Spectra for MGRO J1908+06 E -2 with Milagro normalization assumed (MGRO J1908+06 index = 2.1)  spectrum cutoff @ 180 TeV neutrino flux gamma flux 1 10 E (TeV) 1000 100 10 -13 10 -12 10 -11 10 -10 E 2  flux (TeV s -1 cm -2 ) Halzen etal, Phys.Rev. D78, 063004 (2008) J1852+01 MGRO J2019+37 MGRO J1908+06 MGRO J2031+41 C1 C2 Neutrino spectra for all sources

14. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing14 Significance for MGRO J1908+06 Source size and detector angular + energy resolution taken into account Milagro measurements favor lower sensitivity curve (dashed line) Individual sources probably hard to detect for IceCube IceCube with 80 strings observed events signal + atm. signal + atm. signal events 11 22 33 110 E thresh (TeV) 100 p value atm. atm. Halzen etal, Phys.Rev. D78, 063004 (2008) 10 years

15. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing15 Significance for stacked Sources p-value = 10 -4 after 5 years but large error band (not shown) Optimal threshold @ 30–40 TeV (determined by loss of signal events) Halzen etal, Phys.Rev. D78, 063004 (2008) 5 years 10 years

16. AMANDA II Search for muon neutrinos in 6 Milagro source regions in AMANDA II 7 year data set (3.8 years livetime) Per-source flux sensitivity improved by a factor of 4 compared to fixed-point search for any of the six sources Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing16 Shown by J. Braun @ COSMOS’08

17. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing17 Simulated Neutrino Skymap IC80 (5 years) J1852+01 MGRO J1908+06 Galactic Latitude (°) Galactic Longitude (°)

18. Conclusions Straight forward calculations show that sources of Galactic CR should show up in Milagro sky-map Sources might not be (easily) visible for Cherenkov telescopes – largest energy density might be at several 10 TeV (interactions of CR in molecular clouds) – large photon background in SN regions, e.g. Cygnus Several Milagro sources show indications for hard E -2 spectra with one (MGRO J1908+06) possibly extending to at least 100 TeV Hard to decide from  -ray signal alone whether  -ray sources are CR sources Neutrino telescopes can unambiguously identify sources of cosmic rays IceCube will be able to detect stacked Milagro sources after several years (individual sources difficult) Sep. 28, 200818Alexander Kappes, TeV Workshop, Beijing

19. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing19 Backup Slides

20. TeV Gamma-Ray Sky Map Sep. 28, 200820Alexander Kappes, TeV Workshop, Beijing

21. Sep. 28, 2008Alexander Kappes, TeV Workshop, Beijing21 Simulated Neutrino Skymaps IC80 (5 years) Galactic Latitude (°) Galactic Longitude (°)