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Wide Field of View surveying in Next Generation GeV/TeV Observatories

Wide Field of View surveying in Next Generation GeV/TeV Observatories. D. Kieda University of Utah. Milagro Cygnus Arm Detection. Significance is 5.5  (Crab is 5.9) Source extent is ~5 o Implied source flux is several Crab.

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Wide Field of View surveying in Next Generation GeV/TeV Observatories

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  1. Wide Field of View surveying in Next Generation GeV/TeV Observatories D. Kieda University of Utah UCLA Gamma Ray Workshop

  2. Milagro Cygnus Arm Detection • Significance is 5.5  (Crab is 5.9) • Source extent is ~5o • Implied source flux is several Crab R. Atkins et al, 22nd Texas Symposiumon Astrophysics, Stanford (2004) UCLA Gamma Ray Workshop

  3. Whipple Follow-up • No Strong point source evident (given # of trials) • Typical point source flux limit~300 mCrab • Quoted for E > 400 GeV , angular resolution ~ 0.05o. • Milagro source diameter >> f.o.v. of Whipple camera G. Walker, Ph.D Thesis, U of Utah (2004) UCLA Gamma Ray Workshop

  4. Source Detectability Source Size < Angular resolution = Point Sources: Crab AGN M87 constant UCLA Gamma Ray Workshop

  5. Source Detectability Source Size > Angular Resolution = Diffuse Sources: SNR Tibet-Milagro UID Molecular Cloud n.b. if Source has internal structure you will do better UCLA Gamma Ray Workshop

  6. HESS Diffuse Sources Many sources appear to have internal structure: Ability to resolve a diffuse source is a key to determining its astrophysical processes (HESS , 2005) UCLA Gamma Ray Workshop

  7. Source Resolvability Source Size > Angular Resolution Just need some factor >1 more S/N to resolve internal source structure UCLA Gamma Ray Workshop

  8. Source Resolvability Source Size < Angular resolution As F increases, tails of Gaussian become detectable->resolve source size UCLA Gamma Ray Workshop

  9. Source Detect/Resolve • Increased Milagro sensitivity • for extended source • longer exposure • Wider fov • Excellent Point Source sensitivity • of IACT does not help here • Note that this plot neglects energy • threshold benefits of IACTs X Detected Milagro only Detected (both) Whipple UCLA Gamma Ray Workshop

  10. Newer Arrays Extended Sources: Molecular clouds SNR Point Sources: AGN Pulsar Diffuse Sources: Galactic Plane Galactic Arm Next Gen is 1 km2 IACT, 5 deg f.o.v, 1 mCrab/50 hours UCLA Gamma Ray Workshop

  11. Larger Sources Imaging Source diameters > IACT f.o.v requires multiple pointing 4 pointings: 200 hours: about the most one can do per year Larger areas require reduced time/pointing, thereby reducing sensitivity Intersect at (Fx, x) UCLA Gamma Ray Workshop

  12. Larger Sources vs. Wider f.o.v IACTs H=Hawk N=Next Gen Typical UCLA Gamma Ray Workshop

  13. Summary • Source sensitivity depends on source diameter • If Cyg Arm is truly diffuse source, it is barely accessible to current IACT • Next Gen area 100 x HAWC can compensate for 10% on-time efficiency • Next Gen ( 1 km2) IACT superior for • Next Gen needs fov > 100 in order to resolve 250 diffuse sources • Next Gen better for resolving sources, point sources, looking deeper • HAWC-type better for large diffuse sources (ignoring energy threshold differences) UCLA Gamma Ray Workshop

  14. Strategy • HAWC All-sky: Monitor + large scale structure • Large IACT Next Gen looks deep, low E (followup), spectral/time evolution • Limited energy range above 10 TeV-200 TeV: probe with km2 array of small (1 m class) dedicated imagers • Study/design phase: Next year? • Pursue Modular design: • quick test/low cost • allow deploy/test subsystem at high altitude? • Site testing? • Easy final deployment, cheaper fabrication/maintenence UCLA Gamma Ray Workshop

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