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Synoptic TeV Telescopes: Recent Results & Future Plans

Synoptic TeV Telescopes: Recent Results & Future Plans. Gus Sinnis Los Alamos National Laboratory. Low Energy Threshold EGRET/GLAST. Large Aperture/High Duty Cycle Milagro, Tibet, ARGO, HAWC. High Sensitivity HESS, MAGIC, CANGAROO, VERITAS. Detectors in Gamma-Ray Astrophysics.

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Synoptic TeV Telescopes: Recent Results & Future Plans

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  1. Synoptic TeV Telescopes:Recent Results & Future Plans Gus Sinnis Los Alamos National Laboratory Gus Sinnis CTA Workshop, Paris, March 2007

  2. Low Energy Threshold EGRET/GLAST Large Aperture/High Duty Cycle Milagro, Tibet, ARGO, HAWC High Sensitivity HESS, MAGIC, CANGAROO, VERITAS Detectors in Gamma-Ray Astrophysics Energy Range 0.1-100 GeV Area: 1 m2 Background Free Angular Resolution 0.1o - 0.3o Aperture 2.4 sr Duty Cycle > 90% Energy Range 0.1-100 TeV Area > 104 m2 Background Rejection > 95% Angular Resolution 0.3o - 0.7o Aperture > 2 sr Duty Cycle > 90% Energy Range .05-50 TeV Area > 104 m2 Background Rejection > 99% Angular Resolution 0.05o Aperture 0.003 sr Duty Cycle 10% Unbiased Sky Survey Extended Sources Transients (GRB’s) Simultaneous  Observations Unbiased Sky Survey (<100 GeV) Extended Sources Transients (AGN, GRBs) <100 GeV Simultaneous  Observations High Resolution Energy Spectra Studies of known sources Surveys of limited regions of sky Gus Sinnis CTA Workshop, Paris, March 2007

  3. Current Generation EAS Arrays Tibet III Milagro Gus Sinnis CTA Workshop, Paris, March 2007

  4. The Tibet Air Shower Array • 4300m asl • Scintillator array • 497 detectors • 0.5m2 each • 5mm lead on each • 5.3x104 m2 (phys. area) • 3 TeV median energy • 680 Hz trigger rate • 0.9o resolution Gus Sinnis CTA Workshop, Paris, March 2007

  5. e m g 8 meters 50 meters 80 meters 10 m Milagro • 2600m asl • Water Cherenkov Detector • 898 detectors • 450(t)/273(b) in pond • 175 water tanks • 4000 m2/3.4x104 m2 (phys. area) • 2-12 TeV median energy • 1700 Hz trigger rate • 0.3o-0.5o resolution • 99% background rejection Gus Sinnis CTA Workshop, Paris, March 2007

  6. Proton MC Proton MC g MC g MC Data Data Background Rejection in Milagro • Hadronic showers contain penetrating component: ’s & hadrons • Cosmic-ray showers lead to clumpier bottom layer hit distributions • Gamma-ray showers give smooth hit distributions Gus Sinnis CTA Workshop, Paris, March 2007

  7. New Rejection Parameter: A4 Apply a cut on A4 to reject hadrons:A4 > 3 rejects 99% of Hadrons retains 18% of Gammas S/B increases with increasing A4 Background Rejection (Cont’d) mxPE: maximum # PEs in bottom layer PMT fTop: fraction of hit PMTs in Top layer fOut: fraction of hit PMTs in Outriggers nFit: # PMTs used in the angle reconstruction Gus Sinnis CTA Workshop, Paris, March 2007

  8. Analysis Example: The Crab Nebula A4 > 3.0 A4 > 12.0 Weight each event by Expected S/B Excess Signal = 2,074 Background = 60,637 S/B = 3.4% Excess Signal = 44 Background = 74 S/B = 60% Gus Sinnis CTA Workshop, Paris, March 2007

  9. Cosmic-Ray Anisotropy: Tibet Array 4.0 TeV 6.2 TeV 12 TeV 50 TeV 300 TeV Excess from the Cygnus region Energy dependence to anisotropy Anisotropy fade away ~ 300 TeV (Statistics?) From Science, V314, pp.439 – 443 (2006), by the analysis method (I) (slide from C.T. Yan, Texas in Australia) Gus Sinnis CTA Workshop, Paris, March 2007

  10. Milagro Sky Survey • Cygnus region shows two new TeV gamma-ray sources • Diffuse emission from Cygnus region: ~ 2 x Fcrab (120 square degrees) l (65,85), b (-3,3) • A new TeV source at low declinations Gus Sinnis CTA Workshop, Paris, March 2007

  11. MGRO J1909+06 Longitude Profile |b|<2° MGRO J2019+37 MGRO J2033+42 GALPROP optimized to fit EGRET below horizon Cygnus Region Galactic Longitude Flux Profile • Flux calculations assume a Crab spectrum (-2.62) • 3 sources detected, MGRO J1909+06,1MGRO J2019+37, andMGRO J2033+42 1Abdo et al., arXiv:astro-ph/0611691, to appear ApJ Letters Gus Sinnis CTA Workshop, Paris, March 2007

  12. Strong & Moskalenko GALPROP model of Cygnus Region Pion standard optimized bremsstrahlung Inverse Compton Diffuse Emission from Cygnus Region • Exclude an area of 3x3 degree square bin around MGRO J2019+37 • Strong & Moskalenko optimized model • Fit to EGRET • Increase 0 and IC component throughout Galaxy • Milagro flux ~2.5x prediction • Hard spectrum cosmic ray sources? • Unresolved point sources? Gus Sinnis CTA Workshop, Paris, March 2007

  13. MGRO J2019+37 MGRO J2019+37 MGRO J2019+37 • Statistical Sig. 11.3 σ • Coincident with 2 EGRET sources (unidentified)3EG J2016+36573EG J2021+3716 (PWN G75.2+0.1?) • Flux @ 12 TeV ~500 mCrab • Width = 0.32o ± 0.12o • Location: l = 75.1o± 0.1ostat ± 0.3osys b = 0.3o ± 0.1ostat ± 0.3osys Gus Sinnis CTA Workshop, Paris, March 2007

  14. MGRO J2033+42 MGRO J2033+42 MGRO J2033+42 • Statistical Sig. 7.1 σ • Coincident with:HEGRA TeV J2032+4130 EGRET 3EG J2033+4118 • Flux @ 12 TeV ~ 350 mCrab • Location: l = 80.4o± 0.4ostat ± 0.3osys b = 1.0o ± 0.3ostat ± 0.3osys Will put in Galactic coordinates and change color scale Preliminary Gus Sinnis CTA Workshop, Paris, March 2007

  15. MGRO J1909+06 MGRO J1909+06 • Statistical Sig. 8.2 σ • Flux @ 12 TeV ~850 mCrab • Location: l = 40.5o± 0.1ostat ± 0.3osys b = -1.0o ± 0.1ostat ± 0.3osys Will put in Galactic coordinates and change color scale Preliminary Gus Sinnis CTA Workshop, Paris, March 2007

  16. Object 1Position (l, b) Significance (pre-trials) Flux (x10-14) (/TeV/cm2/s) Crab -175.4±0.1stat , -5.7±0.1stat 15.2 4.8±0.5stat >5 post-trials MGRO J2019+37 75.1±0.1stat , 0.3±0.1stat 11.3 2.4±0.4stat MGRO J1909+06 40.5±0.1stat , -1.0±0.1stat 8.2 4.1±0.9stat MGRO J2033+42 80.4±0.4stat , 1.0±0.3stat 7.1 1.7±0.4stat 76.3±0.1stat , -1.9±0.2stat 5.8 0.9±0.2stat 77.2±0.2stat , -4.0±0.2stat 5.6 1.2±0.2stat 34.1±0.3stat , 0.0±0.2stat 5.1 5.5±1.4stat 106.4±0.5stat , 1.7±0.8stat 4.5 1.0±0.4stat 2 30% systematic error on flux 1 0.3° systematic error on position Galactic Plane Survey Summary • MGRO J2019+37 is coincident with 3EG J2016+3657 and 3EG J2021+3716 • MGRO J2033+42 is coincident with TeV 2032+4130 (dN/dE = (0.5±0.2)x10-14 /TeV/cm2/s) and 3EG J2033+4118 Gus Sinnis CTA Workshop, Paris, March 2007

  17. HESS TeV gamma ray Milagro The Multi-Wavelength Sky Gus Sinnis CTA Workshop, Paris, March 2007

  18. Future Synoptic TeV Telescopes Tibet w/Muon Detectors Proposal submitted China-Japan collaboration 4300m asl (YBJ, Tibet) Tibet w/buried water tanks Emphasis 10-1000 TeV ARGO Complete summer 2007 Chinese-Italian collaboration 4300m asl (YBJ, Tibet) RPC carpet 10-15 /√year on Crab HAWC Proposal submitted >4100m asl (Tibet or Mexico) Water Cherenkov 100  /√year on Crab Gus Sinnis CTA Workshop, Paris, March 2007

  19. ARGO Central carpet (130 clusters/5800 m2) in DAQ No Pb installed 24 Cluster with AnalogRO Schedule End summer 2006 154 Cluster mounted Start data taking w/out Pb Early 2007 Install Pb Summer 2007 Fully operational with Pb + AnalogRO Gus Sinnis CTA Workshop, Paris, March 2007

  20. Future AS+MD Array (Type 2) Tibet w/Muon Detector • 7.2m x7.2m x 1.5m depthWater pool • 20”PMT x 2 (HAMAMATSU R3600) • Underground 2.5m ( ~515g/cm2~19X0) • Material: • Concrete pool • White epoxy resin paint • 184 detectors • Total muon area9540 m2 Gus Sinnis CTA Workshop, Paris, March 2007

  21. Tibet MD: Sensitivity 10 TeV: Cut value SNPE=~40 Background:~99%Rejection Gamma rays:~60% Survival Sensitivity:~6 times Improved 100 TeV: Cut value SNPE=~600 Background:>99.8%Rejection Gamma rays:~100% Survival Sensitivity:>20 times Improved Almost background free! 1000 TeV: Cut value SNPE=~8000 Background:>>99.8% Rejection Gamma rays:~100% Survival Sensitivity: Background free! Gus Sinnis CTA Workshop, Paris, March 2007

  22. g HAWC High Altitude Water Cherenkov Telescope A proposal to redeploy the Milagro PMTs In a Large Reservoir (22,500 m2) at Higher Altitude 10-15 times more sensitive than Milagro Gus Sinnis CTA Workshop, Paris, March 2007

  23. Detector Layout Milagro HAWC Milagro: 450 PMT (25x18) shallow (1.4m) layer 273 PMT (19x13) deep (5.5m) layer 175 PMT outriggers Instrumented Area: ~40,000m2 PMT spacing: 2.8m Total Area: 3500m2  det Area: 2200m2 HAWC: 900 PMTs (30x30) 5.0m spacing Single layer with 4m depth Instrumented Area: 22,500m2 PMT spacing: 5.0m Total Area: 22,500m2  det Area: 22,500m2 Gus Sinnis CTA Workshop, Paris, March 2007

  24. protons gammas Gamma/Hadron Separation nHit/cxPE>5.0 Eff g = 34% Eff CR = 3% nHit/cxPE>5.0 Eff g = 56% Eff CR = 1.5% Circles are EM particles > 1 GeV Circles are ’s & hadrons > 1 GeV Circles are 30m radius (~area of Milagro  layer) Gus Sinnis CTA Workshop, Paris, March 2007

  25. Sensitivity vs. Source Size Gus Sinnis CTA Workshop, Paris, March 2007

  26. HAWC Sky Survey Gus Sinnis CTA Workshop, Paris, March 2007

  27. Sensitivity of Synoptic TeV Telescopes Crab GLAST HESS/VERITAS Whipple Tibet Milagro ARGO HAWC TibetMD sHAWC Gus Sinnis CTA Workshop, Paris, March 2007

  28. Conclusion • Enormous progress has been made in the past decade in TeV survey technology • Measurement of cosmic-ray anisotropy • Discovery of diffuse TeV gamma rays from the Galactic plane • Discovery of diffuse TeV gamma rays from the Cygnus region • Discovery of a new extended TeV source in the Cygnus region • Discovery of at least 2 additional sources in the Galactic plane • HAWC can attain high sensitivity over an entire hemisphere • ~15 times the sensitivity of Milagro • ~5 sigma/√day on the Crab • 30 mCrab sensitivity over hemisphere • Unsurpassed sensitivity to extended sources • Unique TeV transient detector • (5x Crab in 10 minutes!) • Can be built quickly @ low cost Gus Sinnis CTA Workshop, Paris, March 2007

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