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FPI for the CTA project Razmick Mirzoyan for the FPI WP J. Bolmont, P. Espigat, D. Fink, D. Gascon, G. Hermann, B. Khelifi, E. Lorenz, P. Manigot, M. Punch,

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Presentation on theme: "FPI for the CTA project Razmick Mirzoyan for the FPI WP J. Bolmont, P. Espigat, D. Fink, D. Gascon, G. Hermann, B. Khelifi, E. Lorenz, P. Manigot, M. Punch,"— Presentation transcript:

1 FPI for the CTA project Razmick Mirzoyan for the FPI WP J. Bolmont, P. Espigat, D. Fink, D. Gascon, G. Hermann, B. Khelifi, E. Lorenz, P. Manigot, M. Punch, M. Shayduk, T. Schweizer, H. Sol, K.-H. Sulanke, P. Tavernet, M. Teshima, P. Vincent, H. Wetteskind, V. Zimmer, et al.,

2 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Camera Mechanics H.E.S.S.-II camera under construction in Paris

3 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Camera Mechanics: Cost Estimate Example: MAGIC-2, 1039-pixel camera

4 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Camera Sealing NamibiaTenerife Arizona Australia

5 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Camera Sealing One needs to reduce the back-reflection from the surface (apply anti-reflective coating)

6 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Cooling – temperature stabilisation It makes sense to split the imaging camera design into 2 parts: 1. T° sensitive sealed part (PMT, ampl., FADC,…) and 2. not sensitive to T° „open“ part (power supplies, e.t.c….) To cool and stabilize the T° only inside the sensitive part

7 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Cooling – temperature stabilisation An interesting idea is to consider a distributed system of cooling for a cluster of nearby telescopes. Say every 4 telescopes share 1 system This may reduce the cost for the cooling system

8 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Pop-up reflective target for miror reflectivity and pointing calibration

9 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Light Guide System: Experience of H.E.S.S.

10 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Light Guide System: Experience of H.E.S.S.

11 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland MAGIC: Optimization hex input – hex output Exit rad. [mm] Photo eff. [%] Noise eff. [%] old91.421.8 1192.216.9 10.591.513.4 1090.810.3 9.589.97.7 Masaaki Hayashida

12 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Light Guide System: Experience of MAGIC

13 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Where the differences between H.E.S.S. & MAGIC Light Guide efficiencies are coming from ? One possible explanation: –H.E.S.S. is using flat window PMTs that are touching the edge of the LG. Incident light hits the PMT input window under very large angles, light polarisation plays a big role –MAGIC is using hemi-spherical window PMTs that „enter“ into the LG. Light hits the photo cathode mostly under relatively small angles, providing higher efficiency (also, double hits; the photo cathode is semi-transparent) The above needs to be checked soon: affects the selection of PMT

14 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland HV system: Cockroft-Walton ? Typical power consumption of a „classical“ resistive type voltage divider circuit (active or passive) is ~500 mW. 1000 PMTs dividers will dissipate 500 W heat Cockroft-Walton type consumes ~ 15 mW 1000 PMTs will dissipate 15 W heat Ideal solution could be: feed with 1 Cockroft-Walton a cluster of 10-20 PMTs Need additional stabilisation of the photo-cathode to 1st dynode voltage @ ~300 V

15 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Low Noise Power Supplies

16 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Bandwidth The bandwidth of MAGIC-I (from PMT to FADC, all included) is about 230 MHz. We are really profiting from the parabolic shape and the ultra-fast readout of this telescope –Reduced 2-3 times hadron background –Much lower pile-up of LONS photons, almost get rid of it –Analysis at lower thresholds possible (sum-trigger, pulsar studies) H.E.S.S. 28m telescope shall have a comparable ultra-fast design. We believe that the entire signal chain for the large telescopes shall provide ≥ 200 MHz bandwidth. The mid-size telescopes known to work well with ≤ 80-100 MHz bandwidths

17 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Amplifier

18 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Amplifier

19 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Dynamic Range In order to see a single ph.e. event from a PMT in a given bandwidth its amplitude shall be ≥ 6 x amplifier noise For a good fast amplifier the 1  noise ~ 4000 ph.e. (equivalent)  For CTA we aim for x10 higher PMT gain ≥ 40000 (10x  noise ) A ~1´ PMT can deliver a linear dynamic range of ~ 5000 ph.e.  in the ideal case, by assuming 1ADC count = 1/6 ph.e. (1ADC count = 1  noise of the amplifier), one could cover a dynamic range of 6 x 5000 = 30000 (89.5 db) (15-bits = 32768) Usually the precision of single ph.e. calibration is believed to be ~10 %. Let us assume 1ADC count = 1/10 ph.e.  obtain a dynamic range even higher: 10 x 5000 = 50000 (94 db) (16-bits = 65536) A single ampifier could cover a dynamic range of ~3V/150µV = 20000 (86 db) (probably this is already good enough although again a 15 bit digitalisation necessary)

20 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland The above written is true when using a charge integrating ADC system. When using a fast FADC that produces sevaral samples for the minimum signal width of the PMT, the situation is somewhat better, effectively one may „recover“ ~1 bit. Alternative: if we abandon the option to measure the single ph.e. distributions from PMTs directly and assume that we could perform some alternative types of (ADC count/ph.e.) calibrations then one can set 1ph.e. = 1 ADC count and one needs to cover a dynamic range of only 5000 (74 db) (13 bits = 8192). A FADC system shall provide either –a) a very wide dynamic range or –b) double readout system for any given channel or –c) have some smart design feature allowing one to expand its dynamic range (active or passive multiplexing) to a larger bit number. We shall see how close can we come to the ideal Dynamic Range

21 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Example: pixel & cluster designs H.E.S.S.-II PMT cluster M-II cluster

22 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland SiPM: recent news Sometime during this year at least 2 new manufacturers will start producing SiPMs with UV sensitivity. We are evaluating the newest products that can find application in CTA H. Miyamoto TIPP-09

23 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Full-automatic QE measuring device @ MPI for Physics

24 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Photonis XP-52Y2 & XP-3060 Candidate PMTs from Photonis

25 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Photonis XP-29600

26 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Photonis XP-3102/FL & XP-31SF (hemi-spherical window)

27 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland 1´ Hamamatsu against 1´ ET PMT, both hemispherical ET PMT, coated with matt lacquer, Used in MAGIC-I Hamamatsu Superbialkali, used in MAGIC-II QE for the recent Hamamatsu 1´ hemispherical PMTs for the MAGIC-I upgrade camera

28 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland QE for 3 candidate PMTs from Hamamatsu: 1´, 1.5´, 2´ sizes

29 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland 1´ size Hamamatsu R8619

30 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland 2´ Hamamatsu R7724

31 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland 1.5´ Hamamatsu R9420

32 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Afterpulsing

33 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Electron Tubes Enterprises

34 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Conclusions-1 PMT candidates for the CTA telescopes are preliminarily selected from Hamamatsu (1.5´) and from ETE (1.5´ & 1 1/8 ´). The development work shall start very soon. Ideas about the camera mechanics are slowly crystallising. A critical comparison of the PMT HV system is underway. Low-noise power supplies are targeted. Probably the advantage shall be given to an amplifier that is integrated just behind the PMT. This may be very useful in future when alternative light sensors may become competitive with PMTs. This will make it relatively easy to upgrade with the new sensors the imaging cameras of the CTA telescopes.

35 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland The necessary dynamic range is still under discussions Low-noise, high bandwidth amplifiers are critically reviewed. A critical comparison of the LG systems is underway A camera of optimised sections is under study. A camera sealing, cooling & T° stabilisation systems are under study. Feasibility study of distributed system of T° stabilisation system is under discussion We are discussing to have the next joint FPI/ELEC meeting sometime in June or the beginning of July in some beautiful place in Bavaria Conclusions-2

36 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Hamamatsu R9420 socket 1,5-inch, active divider

37 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland HV system: Cockroft-Walton ?

38 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland Masaaki Hayashida MAGIC Light Guides: Possible loss of photons Gap between the side wall (hex type has 6 walls) –0.3 mm (x6) -> 2 % of loss in total Gap between the cone and the photo cathode (ex. hex-hex, exit r = 10mm) Gap [mm] 12345 Eff [%] 90.890.590.088.987.1

39 13th of May 2009 R. Mirzoyan, et al., FPI for CTA; General Meeting, Cracow, Poland QE for the recent Hamamatsu 1-inch hemispherical PMTs for the MAGIC-I upgrade camera

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