Transcript Highlights of the Poster Session

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)
x 2.2
RICH 2007: 22 (According to the book of abstracts)
110
Log Nposter
data
50
22
10
2004
most probable evolution
2007
2010
2013
Conceptual / Experimental studies / Results
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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
Instrumentation / Technology
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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
Software / History of science
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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
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)
A particularly
nice poster!
Thanks to the
Trieste team.
Cherenkov radiation discovery history
Elena Cherenkova
Poster ps file
576 Mb
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
!?!?)
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 no
positive event yet,
but an upper fluence
limit could be set.
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 km2
8-inch PMTs + concentrator cones
FADC readout
Currently installation + comissioning
TUNKA will study the cosmic rays energy spectrum and mass composition in
the energy range 1015 – 1018 eV (around the ‘knee’)
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.
Preliminary integral energy spectrum
taken with the first cluster of Tunka133 array.
Use of floating surface detector stations for the calibration of a deep-sea
neutrino telescope
Apostolos Tsirigotis
E > 1014 eV
Scintillation counters + GPS
 Measure amplitude + arrival time
4000 m
KM3NeT
An independent
(complementary) method to
KM3NeT
determine position and angular
detector
orientation of underwater
telescope.
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 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.
•A new Direction-Sensitive Optical module to be employed in Deep-sea
neutrino Telescopes
Andrea Bersani
NEMO / KM3NeT
Optical
Module
“OM”
17” pressure sphere
Plexiglass
Light guide
Custom specific development by Hamamatsu: a 10” PMT with 4 indepdent
Anodes.
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.
Compact water cherenkov counter
Yuriy Bashmakov (no file)
A Luminometer for HERA, operated from 1992 – 2007
The simplest and cheapest detector presented at this conference.
Gave DL/L ~ 1% !
mirror
Tank filled with
distilled water,
d = 5cm
PMT1
e+ e- pairs
Be converter
Synchrotron radiation
from HERA machine
PMT2
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)
• 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 provide
an 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 COMPASS
Andreas Teufel
576 MAPMTs
2-hour procedure
Hamamatsu R7600-03-M16
• 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 photoelectrons
miss 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
photogrammetry
Jean-Christophe Gayde
CLAM = Contiuous Line Alignment Method
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
Ageing Tests and Recovery Procedures of Silica Aerogel
Davide Luigi Perego
LHCb RICH1: 16 large tiles 200 x 200 x 50 mm3,
Hygroscopic aerogel
Clarity 0.0050 mm4/cm, refractive index n 1.03
Producer: Boreskov Institute of Catalysis, Novosibirsk
• Irradiation tests (p,n,g) up to some 1013 /cm2 (15
LHCb years)  no evidence of ageing due to
irradiation.
• 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. 1020% on Npe, but recoverable by
exposure to N2.
CF4 scintillation data, from NIM 354, (1995), 262; Pansky, Breskin,… Va’vra.
Scintillation yield of CF4
Nikolai Smirnov
Use of triple GEM with CsI to re-measure
CF4 scintillation production
Gas
Analyzer
Bubbler
SS Cubical Vessel
Collimated
a-source
(Am-241)
Signal: SBD a-trigger
Surface Barrier Det. (SBD
(a-trigger)
Scintillation
Light
Signal: GEM pulse
Plunger (x)
CsI Photocathode
Fe55 (GEM abs. gain)
HV: Mesh/GEM
HV: SBD
3x3 cm Mesh &Triple GEM Sta
7 electrode volt. divider
Pressure Gauge
Flow control
CF4
Plunger (y)
Preliminary result for CF4
After
• QE (CsI) measurement
• Gain
• Geom. Efficiency
• etc.
ArcaLux-a novel mass-producible flat-panel
photon detector for homeland security and
high-energy astrophysics
Daniel Ferenc
~4 cm
Plexi glass model
Hope to use mass
production
technologies a la flat
panel TV
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.