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Detailed timetable
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3-11 July 2007
Merida, Mexico
Mexico/General timezone
- icrc2007@icrc2007.unam.mx
Support
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In conjunction with a having a key associated with your account, to have the possibility of exporting private event information necessitates the creation of a persistent key. This new key is also associated with your account and whilst it is active the data which can be obtained through using this key can be obtained by anyone in possession of the link provided. Due to this reason, it is extremely important that you keep links generated with this key private and for your use only. If you think someone else may have acquired access to a link using this key in the future, you must immediately remove it from 'My Profile' under the 'HTTP API' tab and generate a new key before regenerating iCalendar links.
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HE 1.5
Place
Location: Merida, Mexico
Room: Yucatan II+III+IV (Fiesta Americana)
Date:
from 5 Jul 09:20 to 10 Jul 13:30
Timetable | Contribution List
The IceCube neutrino detector is built into the Antarctic ice sheet at the South Pole to measure high energy
neutrinos. For this, 4800 PMTs are being deployed at depths between 1,450 and 2,450 meters into the ice to
measure neutrino induced charged particles like muons. IceTop is a surface air shower detector consisting of 160
Cherenkov ice tanks located on top of IceCube. To extend IceTop,
... More
Presented by Dr. Timo KARG
on
10/7/2007
at
17:53
The fluorescence detection of ultra high energy ($\gtrsim 10^{18}$ eV) cosmic rays
requires a detailed knowledge of the fluorescence light emission from nitrogen
molecules, which are excited by the cosmic ray shower particles along their path in
the atmosphere. We have made a precise measurement of the fluorescence light spectrum
excited by MeV electrons in dry air. We measured the relative i
... More
Presented by Dr. Gonzalo RODRIGUEZ FERNANDEZ
on
10/7/2007
at
16:18
The surface detector of Telescope Array(TA) experiment are deployed in desert of
western utah,USA. The detector consists of two layers of plastic
scintillators of 3m2 area with wave length shifter fiber(WLSfiber).
And at each layer,PMT are connected with WLS fibers.
At each layer ,2 LEDs are also equipped to check PMT linearity.
To estimate number of shower particles with good accuracy, it
... More
Presented by Dr. Toshiyuki NONAKA
on
10/7/2007
at
16:06
GRAPES-3 experiment employs a high-density array of scintillators and a
large area tracking muon telescope. The GRAPES collaboration is being
expanded with addition of several major facilities. These include a
Cerenkov telescope and low frequency dipole array for the measurement of
shower energy. Addition of several modules of muon telescopes to cover a
larger area, expansion of the scintilla
... More
Presented by Prof. Sunil GUPTA
on
10/7/2007
at
17:29
In the fluorescence detection of ultra high energy ($\gtrsim 10^{18}$ eV) cosmic
rays, it is assumed that the number of emitted fluorescence photons is proportional
to the energy deposited in air by shower particles. We have performed measurements of
the fluorescence yield in atmospheric gases excited by electrons over a wide energy
range. AIRFLY has collected data between 1 and 3 MeV at a Va
... More
Presented by Dr. Lorenzo CAZON
on
10/7/2007
at
17:17
The Cern Neutrinos to Gran Sasso (CNGS) project aims to produce a high
energy, wide band muon neutrino beam at Cern and send it towards the INFN
Gran Sasso National Laboratory (LNGS). Its main goal is the observation of the
tau neutrino appearance.
The beam started its operation in August 2006: a total amount of $7.6~10^
{17}$ protons were delivered to the target.
The LVD detector, instal
... More
Presented by Gabriella SARTORELLI
on
10/7/2007
at
15:30
The yield of fluorescence photons in an extensive air shower allows
the observer to determine the number of shower particles by measuring
the number of photons produced. As the systematic uncertainties in
both ground array and fluorescence detectors improve our need to
better understand this calibration is required. Additionally, as more
sensitive fluorescence detectors observe further into t
... More
Presented by Dr. Kevin REIL, Dr. Petra HUENTEMEYER
on
10/7/2007
at
14:06
Radio receivers (RICE, AURA) have been deployed to detect impulsive emissions from
neutrino interactions in ice at South Pole. An alternative source of pulses is the
cores of cosmic ray induced air showers. AIRES and CORSIKA simulations suggest that
>10% of the primary cosmic ray energy enters the ice within 20 cm of the primary axis
impact point. The resulting 5-10 m cascade will make Askarya
... More
Presented by Dr. David SECKEL
on
10/7/2007
at
15:54
JEM-EUSO with a large and wide-angle telescope mounted on ISS has been
planed as a space mission to explore extremes of the universe through the
investigation of ultra-high-energy cosmic rays by detecting photons which
accompany air showers developed in the earth's atmosphere. JEM-EUSO will
be launched by Japanese H-II Transfer Vehicle(HTV) and mounted at the
Exposed Facility of Japanes
... More
Presented by Prof. Fumiyoshi KAJINO
on
10/7/2007
at
14:30
The surface air-shower array above the IceCube neutrino telescope now
consists of 52 ice Cherenkov tanks at 26 stations spread over an area of 0.22
square kilometer. This paper reports on experience with deployment and
operation of IceTop and describes data that verify the performance, threshold
and energy response of the array.
Presented by Prof. Tom GAISSER
on
5/7/2007
at
14:20
The Telescope Array Low Energy Extension (TALE) Experiment consists of
three detectors which will extend the sensitivity in energy of the
Telescope Array (TA) experiment by two orders of magnitude, from
18.5<log(E)<20.5 (in eV) to 16.5<log(E)<20.5. In addition it will
increase the aperture of the TA experiment at all energies, and double
it at the highest energies. The aim of the experiment
... More
Presented by Prof. Gordon THOMSON
on
10/7/2007
at
18:17
JEM-EUSO space observatory will have a very large exposure factor in several years, which is far exceeding the
critical exposure factor required for observation of most of the sources within a few hundred Mpc. The main
science objective is the source identifying atsronomy in particle channel. Quasi-linear tracking of the sources
becomes feasible at energy > 10^20 eV for all-sky. Acceleration
... More
Presented by Prof. Yoshiyuki TAKAHASHI
on
10/7/2007
at
14:18
SiPM is the novel solid state photodetector which can be operated
in the single photon counting mode. It has excellent features,
high quantum efficiency, good charge resolution, fast response,
very compact, high gain of 10^6, very low power consumption,
immune to the magnetic field and low bias voltage, typically 60V.
Drawbacks of this device are currently the large dark current,
cross
... More
Presented by Prof. Masahiro TESHIMA
on
10/7/2007
at
17:41
The uncertainty of hadron interaction models of Monte Carlo simulations have caused
some systematic errors of energy reconstruction and the determination of composition
in ultra high energy cosmic ray measurements. The uncertainty is due to the lack of
the experimental data on the nuclear interactions in the energy region over
2x10^14eV. The LHCf experiment will provide crucial calibration poi
... More
Presented by Mr. Hiroaki MENJO
on
10/7/2007
at
14:42
The space TUS detector of UV fluorescence light radiated by EAS of Ultra
High Energy Cosmic Rays (UHECR) is under preparation for the launch in 2009-
2010. The TUS instrument will have ~2 sq. m. mirror - concentrator area and
256 PMT pixels in the photo receiver at the mirror focal surface. The TUS mission
is now planned for operation at the Small Space Apparatus separated from the
main
... More
Presented by Dr. LEONID TKACHEV
on
10/7/2007
at
13:54
The EEE (/Extreme Energy Event/) Project is an experiment for the study of very
high-energy extensive air showers, actually starting in Italy. It is based on the
detection of the shower muon component by means of a network of tracking detectors,
installed in Italian High Schools.
The Project, supported by the Ministero dell’Università e della Ricerca (MIUR),
Istituto Nazionale di Fisica
... More
Presented by C. SBARRA
on
10/7/2007
at
18:05
JEM-EUSO is a science mission to explore extremes of the Universe. It
observes the dark-side of the Earth and detects UV photons emitted from
the giant air shower caused by an extremely high energy particle (about
10^20 eV). Such a particle arrives almost straightly through our Milky
Way Galaxy and is expected to allow us to trace the source location by
its arrival direction. This will open
... More
Presented by Dr. Toshikazu EBISUZAKI
on
10/7/2007
at
13:42
The Pierre Auger Observatory is a multi-national project for research on ultra-high
energy cosmic rays. The Southern Auger Observatory in Mendoza province, Argentina,
is approaching completion in 2007 with an instrumented area of 3,000 square
kilometers. It will accurately measure the spectrum and composition of ultra-high
energy cosmic rays up to and beyond the predicted GZK feature. We ha
... More
Presented by Prof. David NITZ
on
10/7/2007
at
16:42
Near UV detector on-board the “Universitetsky-Tatiana” satellite has observed
the atmosphere glow at night side of the Earth. Digital oscilloscopes help to
select transient luminous events and to measure their temporal profiles in time
scale of 1-64 ms. Data from those detectors were analyzed for prediction the
duty cycle of future space detectors of ultra high energy cosmic rays.
Presented by Mr. Pavel KLIMOV
on
10/7/2007
at
15:42
Ultra High Energy Cosmic Rays and Neutrinos, with energies from a few 10^18 eV to
beyond the decade of 10^20 eV, and Cosmic Rays with E >= 5 10^19 eV appear to be the
only suitable messengers to explore the Universe at frontier energies, where
radiation is expected to be produced under the most extreme physical conditions.
Observations of these UHE particles will certainly provide new informa
... More
Presented by Dr. Andrea SANTANGELO
on
10/7/2007
at
16:30
In the framework of LOPES (LOFAR PrototypE Station), a Self-Triggered Array of Radio
detectors (STAR) is developed. The challenge of LOPES^STAR is to provide an
independent self-trigger on radio emission of extensive air showers with primary
energy above approximate 5*10^17 eV.
Measurements are done both with an external and self-trigger in radio loud and quiet
areas. Based on these data the
... More
Presented by Mr. Thomas ASCH
on
10/7/2007
at
17:05
