1. Surveying the Galactic Plane with VERITAS and GLAST Amanda Weinstein, UCLA Getting Involved with GLAST workshop May 22, 2007 UCLA

2. The EGRET Sky The galaxy we used to know…

3. ParameterEGRETGLAST LAT VERITAS Energy Range35 MeV-30 GeV Energy Resolution<15%<10%15% Duty cycle100% 12% Field of View0.5 sr2.2 sr3.5 deg Angular Resolution 1.5 deg @ 1GeV 0.5deg @ 10GeV 0.1 deg @ 10 GeV 0.42 deg @ 1 GeV 0.1 deg Effective area~0.3m 2 ~1 m 2 ~10 5 m 2 Point source sensitivity 1.2  10 -8 cm 2 s -1 E>1 GeV 1.5  10 -10 cm 2 s -1 E>1 GeV 10 -11 cm 2 s -1 E>100 GeV ~100 GeV - 50 TeV 20 MeV -~300 GeV

4. GLAST and IACT Surveys HESS 4-IACT array Galactic plane survey ’04 → large catalog of new TeV sources VERITAS 4-IACT array Cygnus region survey (current)

5. VERITAS Sky Survey Survey with VERITAS-4 ~200 hours over a 2-yr period (07-8) Even coverage, sensitive to point sources at 5% of Crab flux Minimal time budgeted for follow-up Cygnus region: 52<l<82, -1<b<4

6. Survey Speculations/Expectations 2465 11 3932 18 5-11 Extrapolation Region 1HESS 5 11 8 18 EGRET (GeV) TeV Sources 8 10 14 18 EGRET (3EG) TeV Sources 22 5 82 18 SNR (Green) TeV Sources CygnusGal Center PWN: 3-4 high spindown loss-rate pulsars which meet HESS criterion for likely PWN detection 11-12 X-ray sources  5 HMXBs  7 LMXBs Confirmed TeV sources  MGRO sources  TeVJ2032 ROSAT TeV Sources

7. ParameterEGRETGLAST LAT VERITAS Energy Range35MeV-30GeV20MeV-~300GeV~100GeV-50TeV Energy Resolution<15%<10%15% Duty cycle100% 12% Field of View0.5 sr2.2 sr3.5 deg Angular Resolution 1.5 deg @ 1GeV 0.5deg @ 10GeV 0.1 deg @ 10 GeV 0.42 deg @ 1 GeV Effective area~0.3m 2 ~1 m 2 ~10 5 m 2 Point source sensitivity 1.2  10 -8 cm 2 s -1 E>1 GeV 1.5  10 -10 cm 2 s -1 E>1 GeV 10 -11 cm 2 s -1 E>100 GeV 0.1 deg

8. Implications Source identification  VERITAS angular resolution an advantage  TeV instruments less affected by diffuse background Modelling emissions process in SNR Microquasars (contemporaneous light curves) PWNe  TeV instruments powerful tool for detecting & mapping unpulsed emission from PWNe SNR RX J1713.7-3946 HESS data Simulated GLAST data

9. Cooperation VERITAS will provide a TeV survey of Cygnus region Joint source analysis, x-calibration valuable From VERITAS side, follow-up critical  Light curves  Spectra  Follow-up time in 2009 likely to be comparable to time spent on survey itself.  Limited time for follow-up in 07/08

10. Work with us! Multi-wavelength input  Valuable for extracting science  Enormous impact on follow-up strategy.  Not only GeV, but radio, x-ray, optical.  We want to work with you.  If interested, please contact: rene@astro.ucla.edu amandaw@astro.ucla.edu

11. Supporting Slide: VERITAS Survey Coverage 0.8° sep. in galactic latitude, 1° longitude