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MPI Kernphysik, Heidelberg Humboldt Univ. Berlin Ruhr-Univ. Bochum Univ. Hamburg LSW Heidelberg

MPI Kernphysik, Heidelberg Humboldt Univ. Berlin Ruhr-Univ. Bochum Univ. Hamburg LSW Heidelberg Univ. Tübingen Ecole Polytechnique, Palaiseau APC Paris Univ. Paris VI-VII Paris Observatory, Meudon LAPP Annecy LAOG Grenoble LPTA Montpellier CEA Saclay CESR Toulouse Durham Univ.

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MPI Kernphysik, Heidelberg Humboldt Univ. Berlin Ruhr-Univ. Bochum Univ. Hamburg LSW Heidelberg

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  1. MPI Kernphysik, Heidelberg Humboldt Univ. Berlin Ruhr-Univ. Bochum Univ. Hamburg LSW Heidelberg Univ. Tübingen Ecole Polytechnique, Palaiseau APC Paris Univ. Paris VI-VII Paris Observatory, Meudon LAPP Annecy LAOG Grenoble LPTA Montpellier CEA Saclay CESR Toulouse Durham Univ. Dublin Inst. for Adv. Studies Charles Univ., Prague Yerewan Physics Inst. North-West Univ., Potchefstroom Univ. of Namibia, Windhoek VHE Gamma Ray Astronomy with the HighEnergyStereoscopicSystem: Highlights W. Hofmann MPIK Heidelberg

  2. MPI Kernphysik, Heidelberg Humboldt Univ. Berlin Ruhr-Univ. Bochum Univ. Hamburg LSW Heidelberg Univ. Tübingen Ecole Polytechnique, Palaiseau APC Paris Univ. Paris VI-VII Paris Observatory, Meudon LAPP Annecy LAOG Grenoble LPTA Montpellier CEA Saclay CESR Toulouse Durham Univ. Dublin Inst. for Adv. Studies Charles Univ., Prague Yerewan Physics Inst. North-West Univ., Potchefstroom Univ. of Namibia, Windhoek September 28, 2004: Inauguration of the H.E.S.S. telescopes VHE Gamma Ray Astromony with the HighEnergyStereoscopicSystem: Highlights W. Hofmann MPIK Heidelberg

  3. Four telescopes, 107 m2 mirror area each 960 PMT cameras, field of view 5o Observation in moonless nights, ~1000 h / year Each night several objects are tracked and ~300 images recorded per second First analysis (almost) online in the same night on PC cluster in Namibia Final analysis and calibration in Europe Energy threshold: ~ 100 GeV Sensitivity: 1% Crab in 25 h

  4. H.E.S.S. Highlights • Galactic sources • Galactic plane survey • Supernova remnants • Pulsar wind nebulae • Binaries • The Galactic Center • Extragalactic sources • Details & physics discussion in parallel sections

  5. H.E.S.S. Highlight:Galactic Plane Survey

  6. Scale height: ≈ 0.3o rms ≈ molecular gas  S. Funk, OG 23  A. Lemiere, OG 23 H.E.S.S. Highlight:Galactic Plane Survey 15 new TeV sources + 3 known

  7. Ensemble characteristics Most sources are extended (size resolved if > 2…3’) Spectra measured for all sources; relatively hard , <G> = 2.3 Photon index Source size

  8. “beam size” What are they ? (smoothed image) 5 sources could be associated with SNR, e.g. HESS J1834-087 3 could be pulsar wind nebulae, typically displaced from the pulsar some coincide with EGRET, ASCA, … unidentified sources 3 have no counterpart known to us

  9. HESS J1813-178: now identified (smoothed image) HESS J1813-178 White et al. 2005 Brogan et al. 2005 20 cm VLA Ubertini et al., 2005 Integral Beam

  10. HESS J1614-518, J1708-410: no counterpart (yet) (smoothed image) (smoothed image)

  11. H.E.S.S. Highlight: Resolved Supernova-Remnants SNR as cosmic particle accelerators Predicted power law spectrum dN/dE ~ E-2…2.2 Efficiency 10-50% Imaged using secondary gamma rays created in interactions with ambient medium

  12.  D. Berge, OG 22 H.E.S.S. Highlight: Resolved Supernova-Remnants RX J1713-3946

  13. Spectra Preliminary  Acceleration of primary particles in SNR shock to well beyond 100 TeV • Index ~ 2.1 – 2.2 • Little variation across SNR • Cutoff or break at high energy

  14. H.E.S.S. Gamma rays ASCA X-rays NANTEN CO at ~1 kpc

  15. Primary population: e or p ? Electron model B ~ 10 mG • Need about 10 mG B field to match flux ratios • Simplest electronic models don’t work well

  16. RX J0852.0-4622 “Vela Junior” Flux ~ Crab Index 2.1 ± 0.1  N. Komin, OG 22 Feb. 2004 (3.2 h) New 04/05 data 3D-Analysis Preliminary ROSAT contours

  17. High ISM density Reverse shock crushes PWN Pulsar wind termination shock Low ISM density Blondin et al. • Asymmetric PWN due to • collimated wind • SNR reverse shock crushing into PWN Pulsar wind creates void H.E.S.S. Highlight:Pulsar Wind Nebulae Blondin et al. ApJ 563 (2001) 806 • Pulsar winds have modest energetics • compared to SN ejecta, but … • most of the energy is in electrons • radiative loss time scales for e± are a few 1000 y, versus 107 y for p

  18. H.E.S.S. Highlight:Pulsar Wind Nebulae  B. Khelifi, OG 22 Vela X hard spectrum G ≈1.9 or G ≈1.5  cutoff extends to 50 TeV no emission from vela pulsar detected Vela pulsar ROSAT contours Preliminary

  19. Photon index 2.27 ± 0.03 ± 0.20  B. Khelifi, OG 22 Another pulsar wind: MSH 15-52 Contours: Rosat Greyscale: Radio

  20. HESS J1825-137 X-rays Gaensler et al. TeV  O. de Jager, OG 22

  21. March 04 Pulsar eclipsed PSR B1259-63 3.4 year highly eccentric orbit around ~10 M Be star closest approach ~1013 cm or ~20 stellar radii H.E.S.S. Highlight:Distant and Close Binaries Mar 04 Douglas Gies (CHARA, GSU) William Pounds

  22.  S. Schlenker, OG 22 PSR B1259-63first variable galactic TeV source HESS J1303-631 PSR B1259-63 Feb. 04 early March 04 Apr./May 04

  23. with more data … Distant and Close Binaries  M. de Naurois, OG 22

  24. Paredes J. M. et al., A&A 2002 RA (mas) Microquasar LS 5039first detection of TeV emission from a microquasar • compact 4 (?) M object in eccentric 4 day orbit around 20-30 M star • closest approach ~1012 cm or ~2 stellar radii fueled by wind accretion(?)

  25. Spectral energy distribution • Expect strong attenuation of gammas in photon field of massive star • Hadronic component ? • Orbital modulation ?? Index 2.12 ± 0.15

  26. SNR G0.9+0.1 PWN The centerof ourGalaxy Sgr A East SNR ? Black hole ? DM Annihilation ? GC

  27. Point-like core Extended tail Similar to NFW profile Colors: H.E.S.S. Contours: Radio Angular distribution Sagittarius A syst. error

  28. Gamma ray spectrum  L. Rolland, OG 22 Preliminary • Power law, index 2.3 • No significant variability • on year scale • on month scale • on day scale • on hour scale • on minute scale (in ~40 h obs. time distributed over 2 years) Preliminary

  29. 20 TeV Neutralino 20 TeV KK particle Dark matter annihilation ? Preliminary proposed based on early H.E.S.S. data proposed before H.E.S.S. data  J. Ripken, OG 22

  30. H.E.S.S. Highlight:Galactic center region

  31. GC molecular clouds Tsuboi et al. 1999 H.E.S.S. Highlight:Galactic center region

  32. H.E.S.S. Highlight:Galactic center region  J. Hinton, OG 21

  33. Diffuse emission from the GC ridge Spectral index 2.29 ± 0.07 ± 0.20 Implies harder CR spectrum than in solar neighborhood  Proximity of accelerator and target

  34. (subtracted) gamma rays CS

  35. x x x gVHEgEBL e+e- Extragalactic TeV astronomy • Physics of AGN jets • Density of cosmological extragalactic background light (EBL) EBL

  36. Costamante & Ghisellini, 2002 501 421 2155 1101 1426 2344 2356 2005 H.E.S.S. Highlight:New distant blazar sources 1ES 1101-232 z = 0.186 ~12 s Preliminary H 2356-309 z = 0.165 ~10 s  S. Pita, OG 23  M. Tluczykont, OG 23

  37. Source spectrum G = 1.5 EBL Spectra & ExtragalacticBackgroundLight 1 ES 1101 G = 2.9±0.2 H 2356 (x 0.1) G = 3.1±0.2 Preliminary

  38. Spectra & ExtragalacticBackgroundLight Source spectrum  Upper limit on EBL too much EBL 1 ES 1101 G = 2.9±0.2 H 2356 (x 0.1) G = 3.1±0.2 Preliminary

  39. Spectra & ExtragalacticBackgroundLight UV EBL Not really a solution: add huge amount of UV photons to EBL  problems with source energetics, X-ray/gamma-ray SED ratio too much EBL 1 ES 1101 G = 2.9±0.2 H 2356 (x 0.1) G = 3.1±0.2 Preliminary

  40. X X X   X

  41. Reference shape HESS limits Spectra & ExtragalacticBackgroundLight • EBL resolved • Universe more • transparent X measure- ments upper limits X lower limits from galaxy counts

  42. Conclusion • First H.E.S.S. results demonstrate that latest generation Cherenkov instruments have reached the critical sensitivity threshold • Lots of interesting stuff out there – hard spectra and extended sources • We’re looking forward to explore this domain further, together with CANGAROO, MAGIC, VERITAS, … MACE • See talks and posters (OG 21, OG 22, OG 23, OG 27) for details on H.E.S.S. results, also • M87 detection, PSK 2005, 2155 spectra, Crab, Mkn 421, … • SNR, pulsar, microquasar, NGC253, … limits, …

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