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TACTIC & MACE gamma-ray telescopes

TACTIC & MACE gamma-ray telescopes. Kuldeep Yadav ( For HIGRO collaboration ) Astrophysical Sciences Division Bhabha Atomic Research Centre Mumbai- 400 085, India. TACTIC telescope (TeV Atmospheric Cherenkov Telescope With Imaging Camera). Control room. TACTIC console.

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TACTIC & MACE gamma-ray telescopes

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  1. TACTIC & MACE gamma-ray telescopes Kuldeep Yadav ( For HIGRO collaboration) Astrophysical Sciences Division Bhabha Atomic Research Centre Mumbai- 400 085, India Rencontres de Moriond 2009

  2. TACTIC telescope(TeV Atmospheric Cherenkov Telescope With Imaging Camera) Control room TACTIC console Rencontres de Moriond 2009

  3. TACTICParameters • Location : Mt. Abu, Rajasthan (72.7dE,24.6dN, 1400m asl) • Light collector : ~9.5 sq. meter • Camera FoV : 5.9d x 5.9d (349 pixels) • Trigger FoV : 3.4d x 3.4d • Trigger Criteria : 3NCT (Fast RAM based) • SPE threshold : 7pe • Energy threshold : ~1 TeV • Distributed 4-node DAS using RTOS • Drive Control : SM based (120Ncm) • Observations time : 1170 hr/year( Oct-June) • NIM & CAMAC R.Koul et. al., Nucl. Instrum. and meth. A., 578(2007) 548 Rencontres de Moriond 2009

  4. Multi-node DA & CS of TACTIC G A I N C O N T R O L N O D E C D C D A T A N O D E SCALER Test Q X NODE #3 Q X NODE # 1 N N HV Test PCR CDC DATA CCR Semaphore - EVENT Manager - CALIBRATION - SKY-NOISE GAIN SHARED CONTROL MEMORY LED CAMAC LED HV Driver Driver Driver CAMAC DRIVER Driver CAMAC HV LED CAMAC TTG` CAMAC CDC SCALER TCP - IP Linux NODE # 4 Linux NODE #5 Q X NODE # 2 Linux NODE # 4 N INTERRUPT HANDLER --- Data Processing --- Data Processing - Master Process --- Display --- Display - Display Manager --- Data quality check --- Data quality check - Data Storage --- Archiving --- Archiving Calibration Chance Event Event ACE Event ( From TTG ) Multi-node Data Acquisition System Rencontres de Moriond 2009

  5. Mrk 501 observations 1997 Rencontres de Moriond 2009

  6. Crab Nebula Observations (2003-04) Rencontres de Moriond 2009

  7. Rencontres de Moriond 2009

  8. TACTIC observation of MrK 421 (2005-06) Rencontres de Moriond 2009

  9. TACTIC light curve of Mrk 421 (2005-06) Rencontres de Moriond 2009

  10. Crab & Mrk 421 concurrent Energy Spectra (2005-06) K.K.Yadav et. al., Astroparticle Physics, 27(2007) 447 Rencontres de Moriond 2009

  11. On-source alpha plot of 1ES2344 + 514 (60 h data during 2004-05) I(≥1.5 TeV) ≤ 3.84 x 10 -12 ph cm-2s-1 S.V.Godambe et. al., J.Phys.G:Nucl.Part.Phys. 34(2007) 1683 Rencontres de Moriond 2009

  12. Mrk 501 observations (2006) 7.5 sigma in 69 h 2005 observation ~46h I(≥1 TeV) ≤ 4.62 x 10 -12 ph cm-2s-1 2006 observation ~69h Rencontres de Moriond 2009

  13. Mrk 501 energy spectrum (2006) f0=1.66±0.52 x 10-11cm-2s-1TeV-1 ſ = 2.8 ± 0.27 S.V.Godambe et. al., J.Phys.G:Nucl.Part.Phys. 34(2008) 065202 Rencontres de Moriond 2009

  14. H1426+428 observations (2004,06,07) ~150 h K.K.Yadav et. al., submitted to J.Phys.G:Nucl.Part.Phys. Rencontres de Moriond 2009

  15. TACTIC & ASM light curves of H1426 Rencontres de Moriond 2009

  16. Project HIGRO anintroduction A New Indian initiative in g- ray astronomy Project HIGRO ( Himalayan g-Ray Observatory) Collaborators --- IIA, TIFR and BARC ………………….. 7 Element HAGAR wavefront sampling telescope + 21m dia. Stereo MACE ( Major Atmospheric Cerenkov Experiment) Each telescope element will use a cluster of ~1408 PMTs with a pixel resolution of 0.10 ; FoV ~ 40 x 40. Aim : Study the sky in theunexplored energy range Eγ > 20 GeV to bridge the gap between the space-based and the ground based detectors. Rencontres de Moriond 2009

  17. Hanle, Ladakh (32.7d N, 79d E, 4200m asl) Rencontres de Moriond 2009

  18. Telescope site IIA Campus , Hanle 4200 m asl (~ 600 g cm -2 ) Site Characteristics Observatory site Location IIA Campus, HANLE Lat. And Long 32.7 0 N, 78.90 E Altitude 4200 m asl (~ 600 g cm -2 ) Nearest town 260 Km Leh- Hanle travel 8 hrs Accessibility full year Med. Temp. -20 C (at night) Min. Temp -240 C (at night) 2m HCT HAGAR (1/7) Med. Rel. Humidity 30% Med. Wind speed • kmph Time for out door work May - Oct High altitude related difficulties Rencontres de Moriond 2009

  19. Advantages of setting up MACE at HANLE Reduction in threshold energy by a factor of ~ 2.5-3.5 at Hanle ( ~ 4200m asl ) compared to lower Altitudes sites like Gurushikhar ( ~1700m asl). Cloud free sky --- Spectroscopic Nights : ~260 nights / yr Photometric Nights : ~190 night /yr Year round sky coverage -- Quite a few important sources cannot be observed at Gurushikhar during June-Sept due to Monsoon. Concurrent observations with HAGAR telescope (>60GeV) & Coordinated multi-wavelength observations with the HCT at Hanle. Improvement in sensitivity because of being closer to shower maximum ( images become broader at higher altitudes). Rencontres de Moriond 2009

  20. Broad guide lines for designing the MACE telescope Lower the energy threshold to ~20GeV (Observation altitude, Large light collection area, small coin. gate width, appropriate pixel size, CPCs, Intelligent trigger generation scheme) Employ GHz signal processing using Analog Ring Sampler Install MACE in the close vicinity of the HAGAR array Improve detection sensitivity by using coincident HAGAR data Use central pixel for used for optical monitoring of the source ---- photometric observations Fast repositioning of the telescope --- high energy tails of GRBs. Operate PMTs at a gain of ~20,000 --- ( use partially moon lit nights) Improve detection sensitivity – employ a stereo system in a phased manner Rencontres de Moriond 2009

  21. Increase in Cherenkov Photon density with altitude . Rencontres de Moriond 2009

  22. Telescope structure material -- Steel – SA-333 Gr 6 (suitable for low temp. applications) Mirror basket structure Aluminum Honey comb panels for mounting mirror facets Active Miror control (AMC) alignment system Camera vessel for housing focal plane instrumentation Drive control system ( DC servo motors with 17 bit encoders) Track and wheel design concept for azimuth motion (27 m dia) Camera handling and maintenance structure Total weight ~ 150 MT Overall height of the telescope ~ 45m Operational/ Survival wind speed ~ 45 km/h // 150 km/h Operating temp. ~ -300C to 050C ( Winter) ~ 050C to 300 C (Summer) Major mechanical sub-systems of the telescope Rencontres de Moriond 2009

  23. MACE telescope --- Light collector design Rencontres de Moriond 2009

  24. Expected PSF of the light collector Plate scale : 43.6mm =0.10 Rencontres de Moriond 2009

  25. Imaging camera Imaging camera specifications: Imaging camera Vessel Size : 2m x 2m x 2.5m Mass : 1200 kg Rencontres de Moriond 2009

  26. Signal Processing Hardware • 16 channel module • GHz Sampling • Integrated Camera (all signal processing instrumentation housed within the camera structure of 2mx2mx1.2m size) • Temperature control of the Camera during operation and standby condition. Rencontres de Moriond 2009

  27. CORSIKA air shower simulation code Energy range -- 1 - 1000 GeV for gamma-rays & e; 10 - 10000 GeV for p & alpha Observatory altitude : 4200 m asl ( Hanle) LONS background : 3.0 x 10 12 photons m-2 s-1 sr-1 No. of showers generated : 8 x 106 each for γ, p , α & e Zenith angle : Vertical incidence Impact parameter : 0-400 m for gamma -rays, e & p ; 0-500 m for alpha Mirror reflectivity, CPC collection efficiency, : Taken into account Atmospheric extinction Trigger FoV : 2.40 x 2.40 Single pixel threshold ~ 4 pe Trigger generation logic : NNQ Monte Carlo simulation studies Rencontres de Moriond 2009

  28. Monte Carlo simulation studies– Effective collection area Rencontres de Moriond 2009

  29. Monte Carlo simulation studies – Threshold energy estimates Rencontres de Moriond 2009

  30. Standard image cleaning procedure picture threshold =4.4pe & Boundary threshold= 2.2pe. Hillas parameters ( Length, Width, Frac2, Distance, Alpha ) ( Dynamic supercuts with Alpha<80 .) Preliminary calculations using Hillas parameters Detection sensitivity for Crab Nebula @ 5σ significance Tmin ~ 13 mins ( @ Size> 530pe -- Eγ > 200 GeV) Tmin ~ 43 mins ( @ Size>50 pe -- Eγ > 55 GeV) Rencontres de Moriond 2009

  31. Funding for 1 MACE element already approved (~ 40 crores ) $ 8 M Telescope mechanical design (~ DDR is completed ) First Light --- 2010 (Single MACE element ) Agenda for ongoing work Prototype 256 pixel camera with ARS –based instrumentation being developed at BARC Camera design optimization (~ FOV and Pixel size --- arrive at the most optimum configuration) Use of WLS dyes for improving the QE of PMTs Include PMT temporal response in MC simulations. Use pulse profile information also for improving γ /hsegregation Achieve Tmin ~ <2 min @ E γ>100 GeV using conventional analysis and simultaneously use alternative γ/hsegregation methodologies for improving the sensitivity @ E γ< 100 GeV Simulation for stereo MACE Repeat simulations at different zenith angles & also at lower altitude (~1600 m) for quantifying the quantum of sensitivity improvement at higher altitude. Implementation status Rencontres de Moriond 2009

  32. . THANK YOU Rencontres de Moriond 2009

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