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

2. Gus Sinnis CTA Workshop, Paris, March 2007 Detectors in Gamma-Ray Astrophysics High Sensitivity HESS, MAGIC, CANGAROO, VERITAS Large Aperture/High Duty Cycle Milagro, Tibet, ARGO, HAWC Low Energy Threshold EGRET/GLAST Energy Range.05-50 TeV Area > 10 4 m 2 Background Rejection > 99% Angular Resolution 0.05 o Aperture 0.003 sr Duty Cycle 10% Energy Range 0.1-100 GeV Area: 1 m 2 Background Free Angular Resolution 0.1 o - 0.3 o Aperture 2.4 sr Duty Cycle > 90% Energy Range 0.1-100 TeV Area > 10 4 m 2 Background Rejection > 95% Angular Resolution 0.3 o - 0.7 o Aperture > 2 sr Duty Cycle > 90% High Resolution Energy Spectra Studies of known sources Surveys of limited regions of sky Unbiased Sky Survey (<100 GeV) Extended Sources Transients (AGN, GRBs) <100 GeV Simultaneous Observations Unbiased Sky Survey Extended Sources Transients (GRB’s) Simultaneous Observations

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

4. Gus Sinnis CTA Workshop, Paris, March 2007 The Tibet Air Shower Array 4300m asl Scintillator array 497 detectors –0.5m 2 each –5mm lead on each 5.3x10 4 m 2 (phys. area) 3 TeV median energy 680 Hz trigger rate 0.9 o resolution

5. Gus Sinnis CTA Workshop, Paris, March 2007 8 meters e  80 meters 50 meters 10 m 2600m asl Water Cherenkov Detector 898 detectors – 450(t)/273(b) in pond – 175 water tanks 4000 m 2 /3.4x10 4 m 2 (phys. area) 2-12 TeV median energy 1700 Hz trigger rate 0.3 o -0.5 o resolution 99% background rejection Milagro

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

7. Gus Sinnis CTA Workshop, Paris, March 2007 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 New Rejection Parameter: A4 Apply a cut on A 4 to reject hadrons: A 4 > 3 rejects 99% of Hadrons retains 18% of Gammas S/B increases with increasing A 4

8. Gus Sinnis CTA Workshop, Paris, March 2007 Analysis Example: The Crab Nebula 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% A 4 > 3.0 A 4 > 12.0

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

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

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

12. Gus Sinnis CTA Workshop, Paris, March 2007 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? Strong & Moskalenko GALPROP model of Cygnus Region standard optimized Inverse Compton Pion bremsstrahlung

13. Gus Sinnis CTA Workshop, Paris, March 2007 MGRO J2019+37  Statistical Sig. 11.3   Coincident with 2 EGRET sources (unidentified) 3EG J2016+3657 3EG J2021+3716 (PWN G75.2+0.1?)  Flux @ 12 TeV ~500 mCrab  Width = 0.32 o ± 0.12 o  Location: l = 75.1 o ± 0.1 o stat ± 0.3 o sys b = 0.3 o ± 0.1 o stat ± 0.3 o sys MGRO J2019+37

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

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

16. Gus Sinnis CTA Workshop, Paris, March 2007 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/cm 2 /s) and 3EG J2033+4118 2.4±0.4 stat 11.3 75.1±0.1 stat, 0.3±0.1 stat MGRO J2019+37 4.8±0.5 stat 15.2-175.4±0.1 stat, - 5.7±0.1 stat Crab 1.0±0.4 stat 4.5106.4±0.5 stat, 1.7±0.8 stat 34.1±0.3 stat, 0.0±0.2 stat 77.2±0.2 stat, - 4.0±0.2 stat 76.3±0.1 stat, - 1.9±0.2 stat 80.4±0.4 stat, 1.0±0.3 stat 40.5±0.1 stat, - 1.0±0.1 stat 1 Position (l, b) 1.2±0.2 stat 5.6 0.9±0.2 stat 5.8 5.5±1.4 stat 5.1 1.7±0.4 stat 7.1MGRO J2033+42 4.1±0.9 stat 8.2MGRO J1909+06 Flux (x10 -14 ) (/TeV/cm 2 /s) Significance (pre-trials) Object 2 30% systematic error on flux 1 0.3° systematic error on position >5  post-trials

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

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

19. Gus Sinnis CTA Workshop, Paris, March 2007 ARGO Schedule End summer 2006 154 Cluster mounted Start data taking w/out Pb Early 2007 Install Pb Summer 2007 Fully operational with Pb + AnalogRO Central carpet (130 clusters/5800 m 2 ) in DAQ No Pb installed 24 Cluster with AnalogRO

20. Gus Sinnis CTA Workshop, Paris, March 2007 Tibet w/Muon Detector Future AS+MD Array (Type 2) 7.2m x 7.2m x 1.5m depth Water pool 20”  PMT x 2 (HAMAMATSU R3600) Underground 2.5m ( ~515g/cm 2 ~19X 0 ) Material:  Concrete pool  White epoxy resin paint  184 detectors  Total muon area 9540 m 2

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

22. Gus Sinnis CTA Workshop, Paris, March 2007 High Altitude Water Cherenkov Telescope  HAWC A proposal to redeploy the Milagro PMTs In a Large Reservoir (22,500 m 2 ) at Higher Altitude 10-15 times more sensitive than Milagro

23. Gus Sinnis CTA Workshop, Paris, March 2007 Detector Layout Milagro: 450 PMT (25x18) shallow (1.4m) layer 273 PMT (19x13) deep (5.5m) layer 175 PMT outriggers Instrumented Area: ~40,000m 2 PMT spacing: 2.8m Total Area:3500m 2  det Area:2200m 2 HAWC: 900 PMTs (30x30) 5.0m spacing Single layer with 4m depth Instrumented Area: 22,500m 2 PMT spacing: 5.0m Total Area:22,500m 2  det Area:22,500m 2 HAWC Milagro

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

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

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

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

28. Gus Sinnis CTA Workshop, Paris, March 2007 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 Conclusion