1. Sabrina Casanova Max Planck Institut fuer Kernphysik, Heidelberg TeV Diffuse Galactic Gamma-Ray Emission

3. Surveys of the sky at TeV energies Milagro: Northern sky H.E.S.S. : Southern sky

4. Outline 1. CR origin and propagation are not well known phenomena 2. Diffuse gamma-ray emission: a unique probe of CR origin and propagation 3. The origin of Galactic Cosmic Rays: searching for the Galactic Pevatron Sources 4. Cosmic Ray Propagation in the Galaxy Diffuse gamma rays from molecular clouds close to CR sources Large scale TeV diffuse emission 5. On the level of the CR background 6. Summary & Future experimental goals

5. 1. CR origin and propagation are not well known phenomena

6. The Cosmic Ray Spectrum at Earth Galactic Origin Extragalactic Origin δ = -2.7 δ = -3.0 Almost featureless spectrum Galactic accelerators have to inject particles up to at least PeV energies Isotropy up to very high energy: 1 TeV proton in B=1uG, Gyro-Radius = 200AU= 0.001pc Knee ~ 3 x10 15 eV

7. Standard Model of Cosmic Rays Acceleration : DSA in SNRs Energy dependent Escape

8. Key Questions in High Energy Astrophysics The origin of cosmic rays What are the cosmic ray accelerators ? How high in energy can galactic sources produce particles? Are CR accelerators different from electron sources? How are cosmic ray sources distributed in the Galaxy ? Is there a nearby (<10's of parsecs) source of cosmic rays ? The character of propagation of cosmic rays How do cosmic rays propagate in the Galaxy ? What is the production rate of protons and electrons ?

9. 2. Diffuse Gamma Ray Emission from the Galactic CR population : a unique probe of CR origin and propagation

10.  Electromagnetic Processes: Synchrotron Emission -important for e - energy losses - –E   (E e /m e c 2 ) 2 B Inverse Compton Scattering –E f ~ (E e /m e c 2 ) 2 E i Bremsstrahlung -more important at GeV energies- –E  ~ 0.5 E e  Hadronic Cascades. Gamma Rays are emitted through decay of neutral pions produced by CRs interacting with the ambient gas. Also secondary electrons and neutrinos are produced. p + p  ± +  o +…  e ± +  +  +…  -rays from electron and CR Galactic populations

11.  -rays travel rectilinearly through the Galactic magnetic fields and point back to the production locations The highest energy CR particles produce the highest energy  -rays. Hadronic and leptonic mechanisms produce different energy spectra and  -ray morphology. However it is experimentally not easy to detect such differences. Gamma ray spectrum and spatial distribution of the diffuse gamma ray emission provide spectra and density of hadrons and leptons in the different regions of the Galaxy Diffuse TeV  -rays from the Galaxy: unique probe of CR origin and propagation

12. 3. The origin of Galactic Cosmic Rays : searching for the Galactic Pevatron Sources

13. Are SNRs the Galactic PeVatron sources ? TeV  -rays and shell type morphology : acceleration of e - and protons There is a significant γ-ray flux (4.8 σ) above 30 TeV. In the hadronic scenario, this implies efficient proton acceleration up to 200 TeV with slope = -2 and energy in CRs of about 10 50 erg/s. In the leptonic scenario this implies acceleration up to 100 TeV because of KN losses. Not yet the knee. Correlation TeV/X-ray. IC and hadronic scenarios can both explain the  -ray emission. We do not have a conclusive proof of CR acceleration. Γ= 2.04±0.04 E 0 = 17.9 ± 3.3 TeV SNR RX J1713-3946 seen in TeVs (H.E.S.S. Collaboration)

14. Variability of X-rays on year timescales – witnessing particle acceleration in real time Uchiyama, Aharonian, Tanaka, Maeda, Takahashi, Nature 2007 flux increase - particle acceleration flux decrease - synchrotron cooling it requires B-field of order 1 mG in hot spots and, most likely, 100  G outside. This supports the idea of amplification of B-field by in strong nonlinear shocks through non-resonant streaming instability of charged energetic particles (Bell, 2000 Zirakashvili, Ptuskin Voelk 2007)

15. DSA in SNRs accelerates electrons -> DSA is likely to accelerate protons. However : Quantify the electron vs proton content in SNRs : is VHE emission from SNRs leptonic or hadronic in nature ? What is the max proton energy achieved ? How do CRs escape SNRs and diffuse in the ISM ? Are SNRs the Galactic PeVatron sources? – PeV particles are accelerated at the beginning of Sedov phase (~200yrs), when the shock speed is high. PeV particles quickly escape as the shock slows down. Lower energy particles are released later. – Even if a SNR accelerates particles up to PeV energies, a SNR is a PeVatron for a very short time – There is still no evidence for the existence of escaping CRs

16. 4. Cosmic Ray Propagation in the Galaxy Diffuse gamma rays from molecular clouds close to CR sources

17. Gamma Rays from Molecular Clouds close to CR sources  MCs are ideal targets to amplify the emission produced by CRs accelerated by nearby sources (Aharonian & Atoyan, 1996, Aharonian, 2001)  Highest energy protons quickly escape the accelerator and therefore do not significantly contribute to gamma-ray production inside the proton accelerator-PeVatron. Gamma rays from nearby MCs are therefore crucial to probe the highest energy protons.

18. Cosmic ray flux in MCs close to a SNR: dependence on SNR age and location Gabici et al, 2009 1 = 500 yr 2 = 2000 yr 3 = 8000 yr 4 = 32000 yr Power in CRs: E CR = 3 X 10 50 erg, Diffusion coefficient: D = D 0 E 0.5

19. GeV versus TeV emission spectra in MC Gabici et al 2009 M=10 5 solar masses; R=20pc ;n =120 cm -3 ; B=20  G; D=1kpc ;D =10 28 cm 2 /s GeV steady CR sea TeV t-dependent SNR CRs Concave shape Steep spectrum at GeV energies and hard at TeV 1 = 500 yr 2 = 2000 yr 3 = 8000 yr 4 = 32000 yr

20. MWL implications GeV-TeV connection...and PeV-hard X connection (pp interactions produce secondary electrons) Ee = 100 TeV

21. Multiwavelength emission close to MCs M=10 5 solar mass; R=20pc ;n=120cm -3 ; B=20G ; d (SNR/MC)=100pc ; D=1kpc X-RAYS GAMMA RAYS RADIO t = 500 yr t = 2000 yr t = 8000 yr t = 32000 yr t = ∞ yr Synchrotron of secondaries and primary e - The gamma-ray emission is an order of magnitude higher than the emission at other wavelengths. So far unidentified TeV sources (dark sources) could be MCs illuminated by CRs from a nearby SNR. Gabici et al, 2009

22. CLOUD CRs Assumptions : Energy in CRs: E CR = 3 X 10 50 erg Injection spectrum: f(E) = K E -2 Diffusion coefficient: D = D 0 E 0.5 Source age and location t= 1600 yr, d = 1kpc gammas Modeling particle escape from RXJ1713-3946 SNR CRs gammas CRs of about 150 TeV are escaping from the shell now Zirakashvili & Aharonian, 2010

23. Variety of CR spectra close to RXJ1713 c TeV position dependent GeV steady

24. Casanova et al, 2010 Constraints on diffusion regime Variety of  -ray spectra close to RXJ1713

25. D = 10 26 E 0.5 cm 2 /s at 10 GeV SNR RXJ1713 CR sea (Runaway CRs + sea CRs) /sea CRs 6 TeV The emission from the environment of RX J1713 provides clues concerning the SNR accel history.

26. Morphological studies of the emission close to CR sources: constraining CR diffusion regime D 0 = 10 28 E 0.5 cm 2 /s at 10 GeV D = 10 27 E 0.5 cm 2 /s at 10 GeV Casanova et al, 2010

27. Molecular Clouds close to the SNR W 28 H.E.S.S. collaboration, F. Aharonian et al., and Y. Moriguchi, Y. Fukui, NANTEN, 2008 W28 : an old SNR and nearby molecular clouds.The VHE/molecular cloud association could indicate a hadronic origin for HESS J1801-233 and HESS J1800-240

28. (Aharonian et al, 2006) Spectral index 2.29 ± 0.07 ± 0.20 implies harder CR spectrum than in solar neighborhood  Proximity of accelerator and target HESS observations of the diffuse emission from the GC

29. Molecular Clouds close to the SNR IC 443 seen by MAGIC & VERITAS 12 CO emission line intensity by Dame et al, 2001 (cyan line) contours of 20 cm VLA radio data from Condon et al. (1998) (green) 1720 MHz OH maser indication for a shock in a high matter density environment (black point) Xray contours from Rosat (purple) (Asaoka & Aschenbach 1994) Gamma –ray contours from EGR-ET (Hartman et al. 1999) (black) gamma-ray excess coincides with cloud and masers soft spectrum: Γ = 3.1 ± 0.3 [ Albert et al. ApJ 664L 87A 2007

30. 4. Cosmic Ray Propagation in the Galaxy Large scale TeV diffuse emission

31. Milagro analysis of Galactic TeV diffuse emission Flux profiles ← Source subtraction + offset/base

32. GALPROP Model hadronic leptonic total (Abdo et al, 2008) Galactic Latitude Profile The narrow distributions of Milagro data points agrees better with a dominant hadronic component.

33. Below Horizon Cygnus Region GALPROP (optimized) Sources Subtracted Abdo et al, 2008 2.7x GP 1.5x GP Longitude Profile |b|<2° Galactic Longitude Flux Profile There is an excess of diffuse TeV gamma rays from the Galactic plane Additional unresolved sources (Casanova & Dingus, 2008)? Cosmic-ray acceleration sites? Most significant discrepancy between data and model predictions in the Cygnus region.

34. Diffuse Emission from the Cygnus Region Cygnus Region: Matter Density Contours overlaying Milagro Obs. Strong & Moskalenko GALPROP model of Cygnus Region standard optimized Inverse Compton Pin bremsstrahlung Abdo et al, 2007

35. Pevatrons in the Cygnus Region ? 100 pc MGRO J2031+41 The extension of the entire Cygnus region is about 300 pc, and thus a single accelerator might influence strongly the entire region In fact only one or at most a few strong young accelerators in the Cygnus region are needed to explain the excess emission measured by Milagro with respect to GALPROP

36. 5. On the level of the cosmic ray background

37.  Average CR flux (“CR sea”) is produced by the effective mixture of CRs from individual sources diffusing in the Galaxy for times of 10 7 years  CR at Earth is representative of the average CR flux ?  Observational test : MCs as cosmic ray barometers Assuming CR sea = CR at Earth An observed gamma-ray flux from MC less than predicted would imply a CR density less than that observed at Earth On the level of the cosmic ray background

38. The level of the CR background 100 GeV only one or at most few massive MCs many low mass MCs sr -1 cm -2 s -1 TeV -1 Casanova et al, 2010 CLOUDS CR sea gammas

39. Flux >1 Gev Localisation of the peak emission along the line of sight DENSITY MASS Casanova et al, 2010

40.  CR =   M H2 /d H2 2 The emission from MCs constrains the CR flux in specific regions of the Galaxy Mass and integral flux as a function of the distance for the region 345.3<l<346 and 1<b<1.7 Casanova et al, 2010 85% of the emission for the region 345.3<l<346 and 1<b<1.7 is produced between 0.5 and 3 kpc

41.  The CR origin and propagation are still uncertain.  TeV diffuse gamma-ray emission is a unique probe of CR origin and propagation  TeV diffuse emission has been observed from MCs close to CR sources by HESS,MAGIC and Veritas and on a larger scale by Milagro  MCs close to CR sources are ideal targets to amplify the emission produced by CRs penetrating the cloud and to produce very specific observable features in the gamma-ray emission  Diffuse gamma-ray from MCs far away from known CR sources can help constraining the level of the CR sea. Summary

42. Future experimental goals Detect large (>>10  G) magnetic field : x-ray telescopes such as Chandra and Astro-H Observe  -ray at hundreds TeV : CTA, AGIS, HAWC Observed X-rays produced by secondary electrons Observe neutrinos : Icecube and KM3NET Image the spectrum and spatial distribution of the Galactic diffuse emission Compare the source  -ray images, spectra, and variability with those from other wavelengths (for instance with radio) Detect many sources of many different classes : population studies with CTA, AGIS, HAWC

43. Thanks for the invitation !