Gus SinnisCTA Workshop, Paris, March 2007

Synoptic TeV Telescopes:Recent Results & Future Plans

Gus Sinnis

Los Alamos National Laboratory

Gus SinnisCTA Workshop, Paris, March 2007

Detectors in Gamma-Ray AstrophysicsHigh Sensitivity

HESS, MAGIC, CANGAROO, VERITAS

Large Aperture/High Duty Cycle

Milagro, Tibet, ARGO, HAWC

Low Energy Threshold

EGRET/GLAST

Energy Range .05-50 TeVArea > 104 m2

Background Rejection > 99%Angular Resolution 0.05o

Aperture 0.003 srDuty Cycle 10%

Energy Range 0.1-100 GeVArea: 1 m2

Background FreeAngular Resolution 0.1o - 0.3o

Aperture 2.4 srDuty Cycle > 90%

Energy Range 0.1-100 TeVArea > 104 m2

Background Rejection > 95%Angular Resolution 0.3o - 0.7o

Aperture > 2 srDuty Cycle > 90%

High Resolution Energy SpectraStudies of known sourcesSurveys of limited regions of sky

Unbiased Sky Survey (<100 GeV)Extended SourcesTransients (AGN, GRBs) <100 GeVSimultaneous Observations

Unbiased Sky Survey Extended SourcesTransients (GRB’s) Simultaneous Observations

Gus SinnisCTA Workshop, Paris, March 2007

Current Generation EAS ArraysT

ibet

III

Mila

gro

Gus SinnisCTA Workshop, Paris, March 2007

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 SinnisCTA 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 m2/3.4x104 m2 (phys. area)• 2-12 TeV median energy• 1700 Hz trigger rate• 0.3o-0.5o resolution• 99% background rejection

Milagro

Gus SinnisCTA Workshop, Paris, March 2007

Background Rejection in Milagro

Proton MC Proton MC

Data Data MC 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

Gus SinnisCTA Workshop, Paris, March 2007

Background Rejection (Cont’d)

( )mxPE

nFitfOut+fTop=A

∗4

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: A4New 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

Gus SinnisCTA Workshop, Paris, March 2007

Analysis Example: The Crab Nebula

Weight each eventby Expected S/B

Excess Signal = 2,074Background = 60,637S/B = 3.4%

Excess Signal = 44Background = 74S/B = 60%

A4 > 3.0

A4 > 12.0

Gus SinnisCTA 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 regionExcess from the Cygnus region Energy dependence to anisotropyAnisotropy fade away ~ 300 TeV

(Statistics?)

Gus SinnisCTA Workshop, Paris, March 2007

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 SinnisCTA Workshop, Paris, March 2007

Galactic Longitude Flux Profile

• Flux calculations assume a Crab spectrum (-2.62)• 3 sources detected, MGRO J1909+06, 1MGRO 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

Gus SinnisCTA 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

Gus SinnisCTA Workshop, Paris, March 2007

MGRO J2019+37MGRO 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 ± 0.1o

stat ± 0.3osys

b = 0.3o ± 0.1ostat ± 0.3o

sys

MGRO J2019+37

Gus SinnisCTA Workshop, Paris, March 2007

MGRO J2033+42

Will put in Galactic coordinates and change color scale

Prelim

inary

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 ± 0.3o

sys

b = 1.0o ± 0.3ostat ± 0.3o

sys

Gus SinnisCTA Workshop, Paris, March 2007

MGRO J1909+06

MGRO J1909+06 Statistical Sig. 8.2 σ Flux @ 12 TeV ~850 mCrab Location:

l = 40.5o ± 0.1ostat ± 0.3o

sys

b = -1.0o ± 0.1ostat ± 0.3o

sys

Will put in Galactic coordinates and change color scale

Prelim

inary

Gus SinnisCTA 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/cm2/s) and 3EG J2033+4118

2.4±0.4stat11.3 75.1±0.1stat , 0.3±0.1statMGRO J2019+37

4.8±0.5stat15.2-175.4±0.1stat , -5.7±0.1statCrab

1.0±0.4stat4.5106.4±0.5stat , 1.7±0.8stat

34.1±0.3stat , 0.0±0.2stat

77.2±0.2stat , -4.0±0.2stat

76.3±0.1stat , -1.9±0.2stat

80.4±0.4stat , 1.0±0.3stat

40.5±0.1stat , -1.0±0.1stat

1Position (l, b)

1.2±0.2stat5.6

0.9±0.2stat5.8

5.5±1.4stat5.1

1.7±0.4stat7.1MGRO J2033+42

4.1±0.9stat8.2MGRO J1909+06

Flux (x10-14)

(/TeV/cm2/s)

Significance

(pre-trials)Object

2 30% systematic error on flux1 0.3° systematic error on position

>5σ

p ost

-tr i

als

Gus SinnisCTA Workshop, Paris, March 2007

The Multi-Wavelength Sky

TeV gamma rayHESS

Milagro

Gus SinnisCTA Workshop, Paris, March 2007

Future Synoptic TeV Telescopes

ARGOComplete summer 2007Chinese-Italian collaboration4300m asl (YBJ, Tibet)RPC carpet10-15σ /√year on Crab

Tibet w/Muon DetectorsProposal submittedChina-Japan collaboration4300m asl (YBJ, Tibet)Tibet w/buried water tanksEmphasis 10-1000 TeV

HAWCProposal submitted>4100m asl (Tibet or Mexico)Water Cherenkov100 σ /√year on Crab

Gus SinnisCTA Workshop, Paris, March 2007

ARGO

ScheduleEnd 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 m2) in DAQ No Pb installed 24 Cluster with AnalogRO

Gus SinnisCTA Workshop, Paris, March 2007

Tibet w/Muon Detector

Future AS+MD Array (Type 2)

7.2m x 7.2m x 1.5m depth 　 Water pool20”PMT x 2 　 　 (HAMAMATSU R3600)Underground 2.5m ( ~515g/cm2~19X0)

Material:Concrete poolWhite epoxy resin paint184 detectorsTotal muon area 　 9540 m2

Gus SinnisCTA Workshop, Paris, March 2007

Tibet MD: Sensitivity10 TeV:Cut value NPE=~40Background: ~99% 　RejectionGamma rays: ~60% SurvivalSensitivity: ~6 times Improved

100 TeV:Cut value NPE=~600Background: >99.8% 　RejectionGamma rays: ~100% SurvivalSensitivity: >20 times Improved Almost background free!

1000 TeV:Cut value NPE=~8000Background: >>99.8% RejectionGamma rays: ~100% SurvivalSensitivity: Background free!

Gus SinnisCTA Workshop, Paris, March 2007

High　Altitude　Water　Cherenkov　Telescope

HAWC

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 SinnisCTA Workshop, Paris, March 2007

Detector Layout

Milagro:450　PMT　　(25x18)　shallow　(1.4m)　layer273　PMT　(19x13)　deep　(5.5m)　layer175　PMT　outriggers

Instrumented　Area:　 ~40,000m2

PMT　spacing:　 2.8mTotal　Area: 3500m2

　det　Area: 2200m2

HAWC:900　PMTs　(30x30)5.0m　spacingSingle　layer　with　4m　depth

Instrumented　Area:　 22,500m2

PMT　spacing:　 5.0mTotal　Area: 22,500m2

　det　Area: 22,500m2

HAWCMilagro

Gus SinnisCTA Workshop, Paris, March 2007

Gamma/Hadron Separation

Circles are EM particles > 1 GeV Circles are ’s & hadrons > 1 GeVCircles are 30m radius (~area of Milagro layer)

prot

ons

gam

mas

nHit/cxPE>5.0Eff = 34%Eff CR = 3%

nHit/cxPE>5.0Eff = 56%Eff CR = 1.5%

Gus SinnisCTA Workshop, Paris, March 2007

Sensitivity vs. Source Size

Gus SinnisCTA Workshop, Paris, March 2007

HAWC Sky Survey

Gus SinnisCTA Workshop, Paris, March 2007

Sensitivity of Synoptic TeV Telescopes

Tibet

Milagro

HAWC

sHAWC

TibetMD

Whipple

ARGO

Crab

HESS/VERITAS

GLAST

Gus SinnisCTA 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