Highlights of the Poster Session

(just a short summary)

Christian Joram (CERN)

Trieste, 20 Oct 2007

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

Npo

ster

2004 2007 2010 2013

10

22

50

110data

most probable evolution

Conceptual / Experimental studies / Results

• Using Water Cherenkov Detectors at the Large Aperture GRB ObservatoryXavier Bertou

• TUNKA Cherenkov Extensive Air Shower Experiment in Tunka ValleyBayarto Lubsandorzhiev

• Study of a water Cherenkov detector for using in an air shower arrayFarzaneh Sheidaei

• Use of floating surface detector stations for the calibration of a deep-sea neutrino telescopeApostolos Tsirigotis

• Recent results from the MAGIC telescopeValeria Scapin

• A Magnetic Spectrometer RICH (MASRICH)Massimo Lenti

• The Barrel DIRC of the PANDA experimentCarsten Schwarz

• The Endcap DIRC of the PANDA experimentPeter Schönmeier

• Compact water cherenkov counterYuriy Bashmakov

AstroParticlePhysics

ParticlePhysics

Instrumentation / Technology

• A new Direction-Sensitive Optical module to be employed in Deep-sea neutrino TelescopesAndrea Bersani

• Quantum Efficiency Measurements of Hybrid Photon DetectorFranz Muheim

• The characterisation of the multianode photomultiplier tubes for the RICH-1 upgrade project at COMPASSAndreas Teufel

• Progress in Aerogel Synthesis in NovosibirskAlexander Danilyuk

• Remote alignment of large mirror array for RICH detectorsStefano Levorato

• Ageing Tests and Recovery Procedures of Silica AerogelDavide Luigi Perego

• Silicon photomultipliers as readout for the CEDAR counter of the K→πνν experiment P326 at CERNGianmaria Collazuol

• ArcaLux-a novel mass-producible flat-panel photon detector for homeland security and high-energy astrophysicsDaniel Ferenc

• COMPASS RICH-1 mirrors - towards an absolute alignment with CLAM by camera calibration and photogrammetryJean-Christophe Gayde

Software / History of science

• Likelihood analysis of patterns in a Time-of-propagation (TOP) counterPeter Križan

• Design optimization of the proximity focusing RICH with dual aerogel radiator using a maximum-likelihood analysis of Cherenkov ringsRok Pestotnik

• Hadron Finder, a novel method for gamma/hadron separation for Atmospheric Imaging Cherenkov TelescopesDaniel Ferenc

• Cherenkov radiation discovery historyElena Cherenkova

However… 4 No-shows!

Study of a water Cherenkov detector for using in an air shower arrayFarzaneh Sheidaei

Quantum Efficiency Measurements of Hybrid Photon DetectorFranz Muheim

Silicon photomultipliers as readout for the CEDAR counter of the K→πνν experiment P326 at CERNGianmaria 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

ApologiesSome 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)

A particularlynice poster!

Thanks to theTrieste team.

Cherenkov radiation discovery historyElena Cherenkova

Poster ps file576 Mb

Using Water Cherenkov Detectors at the Large Aperture GRB ObservatoryXavier 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 !?!?)

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.

Status: about 20 m2 of water Cherenkov detectors installed at 5 different (test) sites

After a couple of Months of operation nopositive event yet,but an upper fluencelimit could be set.

TUNKA Cherenkov Extensive Air Shower Experiment in Tunka ValleyBayarto Lubsandorzhiev

Seven optical detectors form a cluster (19 in total)

Watertank

Layout of Tunka-133 array1 km2

8-inch PMTs + concentrator conesFADC readout

Currently installation + comissioning

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 1015 – 1018 eV (around the ‘knee’)

Use of floating surface detector stations for the calibration of a deep-sea neutrino telescopeApostolos Tsirigotis

KM3NeTdetector

Scintillation counters + GPS Measure amplitude + arrival time

4000

m

An independent (complementary) method todetermine position and angular orientation of underwater telescope.

KM3NeT

E > 1014 eV

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

Recent results from the MAGIC telescopeValeria 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.

•A new Direction-Sensitive Optical module to be employed in Deep-sea neutrino TelescopesAndrea Bersani

NEMO / KM3NeT

Custom specific development by Hamamatsu: a 10” PMT with 4 indepdentAnodes.

17” pressure sphere

PlexiglassLight guide

Optical Module“OM”

Special light guide designWith aluminized side faces subdivideOM in 4 sectors.

Spatial resolution of PMT transformsIn a direction-sensitivity of the OM

MC model shows that effectivedetection area of a km3 detectorprofits from such a detector.

Compact water cherenkov counterYuriy Bashmakov (no file)

PMT1PMT2

A Luminometer for HERA, operated from 1992 – 2007

The simplest and cheapest detector presented at this conference. Gave L/L ~ 1% !

Synchrotron radiationfrom HERA machine

Be converter

e+ e- pairs

mirror

Tank filled with distilled water, d = 5cm

A Magnetic Spectrometer RICH (MASRICH)Massimo Lenti (published in NIM A)

Idea: One detector measures simultaneously thevelocity and the momentum of a chargedparticle and so its mass

Simulated setup:• 20 m long, 2.5 m diameter vessel• f = 20 m (spherical mirror)• pt 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)

Reminds us of CERES RICH ?

2 superconductive solenoids providean azimuthal momentum kick to the e+e- pairs

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

The characterisation of the multianode photomultiplier tubes for the RICH-1 upgrade project at COMPASSAndreas Teufel

Hamamatsu R7600-03-M16

576 MAPMTs2-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

(Re-)discovery: some photoelectronsmiss the first dynode

In the end…

The work has paid off!

COMPASS RICH-1 mirrors - towards an absolute alignment with CLAM by camera calibration and photogrammetryJean-Christophe Gayde

CLAM = Contiuous Line Alignment Method

Photogrammetry of GRID with presicion 0.2 mmLink 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

LHCb RICH1: 16 large tiles 200 x 200 x 50 mm3,Hygroscopic aerogelClarity 0.0050 m4/cm, refractive index n 1.03Producer: Boreskov Institute of Catalysis, Novosibirsk

• Irradiation tests (p,n,) up to some 1013 /cm2 (15 LHCb years) no evidence of ageing due to irradiation.

Ageing Tests and Recovery Procedures of Silica AerogelDavide 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 Npe, but recoverable by exposure to N2.

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.

Preliminary result for CF4

After • QE (CsI) measurement• Gain• Geom. Efficiency• etc.

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 astrophysicsDaniel Ferenc

~4 cm

Plexi glass model

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 (Nposter = 50) we will try to organize this properly.