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MA4: HIGH-ENERGY ASTROPHYSICS

MA4: HIGH-ENERGY ASTROPHYSICS. Critical situation of manpower : 1 person ! Only «free research » based in OAT. Big collaborations based elsewhere (Fermi, CTA, MAGIC). Competition / cooperation with INFN. Collaborations : local : F. Longo ( Trieste U. )

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MA4: HIGH-ENERGY ASTROPHYSICS

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  1. MA4: HIGH-ENERGY ASTROPHYSICS • Critical situation of manpower : 1 person! • Only «free research» based in OAT. • Big collaborationsbasedelsewhere (Fermi, CTA, MAGIC). • Competition/cooperation with INFN. • Collaborations: local: F. Longo (Trieste U.) A. De Angelis et al. (Udine U.) int’l: Y. Rephaeli(Tel Aviv, UCSD) MAGIC, CTA, Fermi/LAT NT particles, SF gal’s

  2. MacroArea 4: High Energy Astrophysics& Astroparticles Particle Acceleration Massimo Persic

  3. Radiation Processes synchrotron bremsstrahlung Inverse Compton

  4. energy gains / losses diffusion rate of particles production per unit volume of coordspace by definition: energyloss for particles of energy E Diffusion-LossEquation

  5. MP, Rephaeli & Arieli 2008, A&A, 486, 143 Rephaeli, Arieli & MP 2010, MNRAS, 401, 473 MP & Rephaeli 2010, MNRAS, 403, 1569 MP & Rephaeli 2013, A&A, to be submitted CosmicRays in Galaxies Up from g-rays … directly from protons!  Do electrons trace protons? Ne(g) = Ne,0g-qg1£g £g2 electron spectrum synchro-Compton Coulomb bremsstrahlung

  6. p/e ratios e.g., Schlickeiser 2002 MP & Rephaeli 2013 particle/field energy density equipartition

  7. Magneticfield Up from electrons

  8. Energy gain timescale ~ ~ Energy losstimescale~ ~ SF timescale Equipartition + theor motivated p/e ratio ok electrons trace protons Application to high-z gal’s?

  9. Ground Based γ-ray Astronomy

  10. Current Status of VHE Ap • The current generation of telescopes (H.E.S.S. / MAGIC / VERITAS) have detected >100 sources. • Several more with HESS2 / MAGIC2 / upgraded VERITAS • Stellar Winds • Supernova Remnants • Pulsar Wind Nebulae • Binary Systems • Molecular Clouds • Galactic Centre • No Counterpart/Dark Sources • AGN • Constraints on EBL • Constraints on QG • CR Electron Spectrum Regular observations made between 70 GeV-20 TeV with few % Crab sensitivity

  11. Science Potential Distance kpcMpcGpc Blazars (~60) Starbursts (2) SNR/PWN (~30) Radio Gals. (4) Binaries (4) Pulsed (1) Current CTA Sensitivity Flux Clusters DM Colliding Winds GRBs DM Current instruments have passed the critical sensitivity threshold and reveal a rich panorama, but this is clearly only the tip of the iceberg. What big science questions remain?

  12. Big Science Questions Left to Next-Generation Instruments • Determining • Origin of galactic cosmic-rays • Whether γ-ray binaries emit via wind/jet • Studying • Star formation regions • Pulsars and PWN • Studying Physics of AGN Jets • Galaxy clusters: the dark side of structure formation • Constraining • Extragalactic Background Light • Quantum Gravity Energy Scale • May detect WIMP annihilation • Dark sources / New source classes

  13. CTA tech wish list • Higher Sensitivity at TeV energies (x10) Deep Observations  More Sources • Higher Detection Area Greater Detection Rates  Transient Phenomena • Better Angular Resolution Improved morphology studies  Structure of Extended Sources • Lower Threshold (some 10 GeV) Pulsars, distant AGN, source mechanisms • Higher Energy Reach (PeV and beyond) Cutoff region of galactic accelerators Sources of UHECRs? • Wide Field of View Extended Sources, Surveys

  14. CTA sensitivity tyuujunas hjv

  15. Expected Design Study Results CTA Design started ! • Detailed knowledge of characteristics, availability of a few good site candidates. • Array layout which optimises physics performance for a given cost (and which is about 1 order of magnitude better than we have now). • Detailed design and industrial cost estimates for telescopes and associated equipment • Plan how to organise, produce, install commission, operate the facility; estimate for operating cost • Model and prototype how to handle and analyse the data • Small prototype series of common components, to ensure that production issues and costs are understood.

  16. Possible CTA sites

  17. 1 eV 1 keV 1 MeV 1 GeV 1 TeV 1 PeV 10-11 10-12 10-13 10-14 10-15 10-16 CTA: In Context Space-based instruments only optical UV | X-ray | g-ray | VHE g-ray Integral Fermi GST nFn (erg cm-2 s-1) Current Instruments More sensitive XMM HST Energy

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