1. Highlights of the Poster Session (just a short summary) Christian Joram (CERN) Trieste, 20 Oct 2007

2. Statistics: Number of posters RICH 2004: about <10 (as far as I remember) RICH 2007: 22 (According to the book of abstracts) x 2.2 Log N poster 2004 2007 2010 2013 10 22 50 110 data most probable evolution

3. Conceptual / Experimental studies / Results Using Water Cherenkov Detectors at the Large Aperture GRB Observatory Xavier Bertou TUNKA Cherenkov Extensive Air Shower Experiment in Tunka Valley Bayarto Lubsandorzhiev Study of a water Cherenkov detector for using in an air shower array Farzaneh Sheidaei Use of floating surface detector stations for the calibration of a deep-sea neutrino telescope Apostolos Tsirigotis Recent results from the MAGIC telescope Valeria Scapin A Magnetic Spectrometer RICH (MASRICH) Massimo Lenti The Barrel DIRC of the PANDA experiment Carsten Schwarz The Endcap DIRC of the PANDA experiment Peter Schönmeier Compact water cherenkov counter Yuriy Bashmakov Astro Particle Physics Particle Physics

4. Instrumentation / Technology A new Direction-Sensitive Optical module to be employed in Deep-sea neutrino Telescopes Andrea Bersani Quantum Efficiency Measurements of Hybrid Photon Detector Franz Muheim The characterisation of the multianode photomultiplier tubes for the RICH-1 upgrade project at COMPASS Andreas Teufel Progress in Aerogel Synthesis in Novosibirsk Alexander Danilyuk Remote alignment of large mirror array for RICH detectors Stefano Levorato Ageing Tests and Recovery Procedures of Silica Aerogel Davide Luigi Perego Silicon photomultipliers as readout for the CEDAR counter of the K→πνν experiment P326 at CERN Gianmaria Collazuol ArcaLux-a novel mass-producible flat-panel photon detector for homeland security and high-energy astrophysics Daniel Ferenc COMPASS RICH-1 mirrors - towards an absolute alignment with CLAM by camera calibration and photogrammetry Jean-Christophe Gayde

5. Software / History of science Likelihood analysis of patterns in a Time-of-propagation (TOP) counter Peter Križan Design optimization of the proximity focusing RICH with dual aerogel radiator using a maximum-likelihood analysis of Cherenkov rings Rok Pestotnik Hadron Finder, a novel method for gamma/hadron separation for Atmospheric Imaging Cherenkov Telescopes Daniel Ferenc Cherenkov radiation discovery history Elena Cherenkova

6. However… 4 No-shows! Study of a water Cherenkov detector for using in an air shower array Farzaneh Sheidaei Quantum Efficiency Measurements of Hybrid Photon Detector Franz Muheim Silicon photomultipliers as readout for the CEDAR counter of the K→πνν experiment P326 at CERN Gianmaria Collazuol Hadron Finder, a novel method for gamma/hadron separation for Atmospheric Imaging Cherenkov Telescopes Daniel Ferenc Instead… 1 extra-show: Scintillation yield of CF4 N. Smirnov Apologies Some posters will not be discussed in this talk -because no electronic file was available -or because the topic was already broadly covered in a talk -or because I felt unable to give an adequate summary (given the limited time and CPU resources)

7. A particularly nice poster! Thanks to the Trieste team.

8. Cherenkov radiation discovery history Elena Cherenkova Poster ps file 576 Mb

9. Using Water Cherenkov Detectors at the Large Aperture GRB Observatory Xavier Bertou LAGO = Large Aperture Grb (gamma ray bursts) Observatory Argentina (2x), Bolivia, France, Italy, Mexico (2), Venezuela GRB have not yet been detected with ground based detectors, only by satellites. Idea: Use Water Cherenkov Detectors in order to detect all secondaries (photons represent 80-90% of secondaries), but one needs to go to VERY high altitudes. Otherwise, LAGO is a real low cost project. Chacaltaya, Bolivia, 5300m a.s.l.. (Power, internet !?!?)

10. Wikipedia… Gamma-ray bursts (GRBs) are probably the most luminous events in the universe since the Big Bang. They are flashes of gamma rays coming from seemingly random places in deep space at random times. GRBs last from milliseconds to minutes, often followed by an afterglow emission at longer wavelengths (X-ray, UV, optical, IR, and radio). Gamma-ray bursts are detected by orbiting satellites about two to three times per week, as of 2007, though their actual rate of occurrence is much higher.luminousuniverseBig Banggamma raysX-rayUVopticalIRradio

11. Status: about 20 m 2 of water Cherenkov detectors installed at 5 different (test) sites After a couple of Months of operation no positive event yet, but an upper fluence limit could be set.

12. TUNKA Cherenkov Extensive Air Shower Experiment in Tunka Valley Bayarto Lubsandorzhiev Seven optical detectors form a cluster (19 in total) Water tank Layout of Tunka-133 array 1 km 2 8-inch PMTs + concentrator cones FADC readout Currently installation + comissioning

13. Preliminary integral energy spectrum taken with the first cluster of Tunka- 133 array. Energy threshold of 100% efficiency Usage both the amplitude and pulse FWHM in analysis makes it possible to estimate the EAS core distance and energy E0 even for distant events. TUNKA will study the cosmic rays energy spectrum and mass composition in the energy range 10 15 – 10 18 eV (around the ‘knee’)

14. Use of floating surface detector stations for the calibration of a deep-sea neutrino telescope Apostolos Tsirigotis KM3NeT detector Scintillation counters + GPS  Measure amplitude + arrival time 4000 m An independent (complementary) method to determine position and angular orientation of underwater telescope. KM3NeT E > 10 14 eV

15. Very detailed M.C. study (corsika  Geant4  data treatment …) Conclusions The operation of 3 stations (3x16 counters) for 10 days will provide: The determination of a possible angular offset of the KM3NeT with an accuracy ~ 0.05 deg The determination of the absolute position of the KM3NeT with an accuracy ~ 0.6 m

16. Recent results from the MAGIC telescope Valeria Scapin A very rich harvest ! Since its operation start in 2004 eight Galactic and eleven extragalactic sources have been detected. For experts… TeV source BL Lac, Supernova remnants Cas A, IC443 Quasar 3C 279 X-ray binaries  Numerous publications.

17. A new Direction-Sensitive Optical module to be employed in Deep-sea neutrino Telescopes Andrea Bersani NEMO / KM3NeT Custom specific development by Hamamatsu: a 10” PMT with 4 indepdent Anodes. 17” pressure sphere Plexiglass Light guide Optical Module “OM”

18. Special light guide design With aluminized side faces  subdivide OM in 4 sectors. Spatial resolution of PMT transforms In a direction-sensitivity of the OM MC model shows that effective detection area of a km3 detector profits from such a detector.

19. Compact water cherenkov counter Yuriy Bashmakov (no file) PMT1 PMT2 A Luminometer for HERA, operated from 1992 – 2007 The simplest and cheapest detector presented at this conference. Gave  L/L ~ 1% ! Synchrotron radiation from HERA machine Be converter e+ e- pairs mirror Tank filled with distilled water, d = 5cm

20. A Magnetic Spectrometer RICH (MASRICH) Massimo Lenti (published in NIM A) Idea: One detector measures simultaneously the velocity and the momentum of a charged particle and so its mass Simulated setup: 20 m long, 2.5 m diameter vessel f = 20 m (spherical mirror) p t kick: 360 MeV/c (  B = 1.5 T ?) Magnetic field longitudinal spread: 0.88 m radiator: Neon at atm.pressure photon detectors: Hamamatsu R7400U-04 PM granularity: 18 mm (hex packing)

21. Reminds us of CERES RICH ? 2 superconductive solenoids provide an azimuthal momentum kick to the e + e - pairs

22. Good particle ID and momentum resolution (dominated by size of photodetectors (18 mm) In real life … (my personal concerns) Design requires large aperture magnet  Expensive + high stray field

23. The characterisation of the multianode photomultiplier tubes for the RICH-1 upgrade project at COMPASS Andreas Teufel Hamamatsu R7600-03-M16 576 MAPMTs 2-hour procedure visual inspection of cathode surface measurement of dc of all channel recording of ADC spectra at five different high voltage values ( 850V / 880V / 910V / 940V / 970V ) and two different wavelength values (360 nm / 480nm) Digital oscilloscope recording of all channels Uniformity / rel. QE. / Gain High voltage as function of charge

24. (Re-)discovery: some photoelectrons miss the first dynode In the end… The work has paid off!

25. COMPASS RICH-1 mirrors - towards an absolute alignment with CLAM by camera calibration and photogrammetry Jean-Christophe Gayde CLAM = Contiuous Line Alignment Method

26. Photogrammetry of GRID with presicion 0.2 mm Link to global coord. System: 0.5 mm A related poster by Stefano Levorato (unfortunately too large to be opened (120 Mb pdf)) shows a nice technical study of a motorized adjustment system for each individual mirror, based on piezo actuators

27. LHCb RICH1: 16 large tiles 200 x 200 x 50 mm 3, Hygroscopic aerogel Clarity 0.0050  m 4 /cm, refractive index n 1.03 Producer: Boreskov Institute of Catalysis, Novosibirsk Irradiation tests (p,n,  ) up to some 10 13 /cm 2 (15 LHCb years)  no evidence of ageing due to irradiation. Ageing Tests and Recovery Procedures of Silica Aerogel Davide Luigi Perego Natural aging ( 4years)  small effects on n and C Hygroscopic sample exposed to humidity  degradation of its optical properties as expected, but in a reversible way! Aging in presence of C4F10. 10- 20% on N pe, but recoverable by exposure to N 2.

28. Scintillation yield of CF4 Nikolai Smirnov Use of triple GEM with CsI to re-measure CF4 scintillation production Signal: SBD  -trigger Signal: GEM pulse HV: Mesh/GEM HV: SBD CF4 Flow control SS Cubical Vessel Gas Analyzer Scintillation Light Collimated  -source (Am-241) Surface Barrier Det. (SBD) (  -trigger) Bubbler 3x3 cm Mesh &Triple GEM Stack/ 7 electrode volt. divider Plunger (y) Plunger (x) Fe55 (GEM abs. gain) Pressure Gauge CsI Photocathode CF4 scintillation data, from NIM 354, (1995), 262; Pansky, Breskin,… Va’vra.

29. Preliminary result for CF4 After QE (CsI) measurement Gain Geom. Efficiency etc.

30. Hope to use mass production technologies a la flat panel TV ArcaLux-a novel mass-producible flat-panel photon detector for homeland security and high-energy astrophysics Daniel Ferenc ~4 cm Plexi glass model

31. No summary of the summary ! Thanks to all poster-authors for producing nice and informative posters. Conclusions: Posters are a good way - to increase the number of contributions to the workshop - to display information in a graphically attractive way - to explain details and complicated relations However… - The value of a poster is much increased if the author is available to explain and answers questions In RICH 2010 (N poster = 50) we will try to organize this properly.