|
Dr. Kael HANSON Chargé de cours Université Libre de Bruxelles Service de Physique des particules élémentaires Boulevard du Triomphe, CP-230 B-1050 Brussels, Belgium Office: VUB Campus Building G Locale 0G125 Email: khanson@ulb.ac.be Tel: +32-2-629-35-82 Fax: +32-2-629-38-16 |
Following are the lecture notes which accompany several of the lectures.
| Introduction | ||
| The computational framework: particle physics and cosmology | ||
| Exercises #1 and #2 | ||
| Exercises #3 | ||
| Cosmic Rays | ||
| Underground Muons and Neutrinos | ||
| PPTX | Neutrino Oscillations and Neutrino Astrophysics | |
| Dark Matter / Dark Energy and VHE Gamma Ray Astronomy | ||
| PDF Printable | Data analysis using IceCube Data | |
IceCube is a neutrino telescope
currently under construction at the geographic South Pole. It is a
joint collaboration between over 300 physicists
from Europe, USA, Japan, Canada, and New Zealand. It consists
of a deep array of 5000 10" photomultipler tubes deployed between 1450 m
and 2450 m in the glacial ice and 160 frozen IceTop tanks at the surface
which form an airshower detector. IceCube has been optimized for the
detection of astrophysical diffuse and point sources of high-energy (> 1 TeV) neutrinos,
however its scientific reach extends into several areas including
cosmic ray composition around the knee, dark matter, gamma ray bursts,
and MeV neutrinos from galactic supernova explosions.
However, IceCube is unlike anything ever built and
it is likely that in the coming years we will find entirely different uses
for this powerful tool.
I manage the IceCube data acquisition system, conventionally known as the DAQ. The DAQ is the combined package of in-ice hardware, data transmission over cables, and counting-house hardware and software that is responsible for the collection of some 300 MB/sec of data coming out of the ice of which 10 MB/sec is written to disk file for later analysis.
The 86 string IceCube detector (IC86) was completed on Dec 18, 2010. The project will switch to 86-string data collection sometime in May 2011 following a transition of the commissioning and software systems to the new configuration. Before this there were the following science runs: IC79 (May 2010 - May 2011); IC59 (June 2009 - May 2010); IC40 (May 2008 - June 2009). IC22 data was taken beginning March 2007 until May 2008 and produced several science papers even though the detector itself was not officially in operational mode.
| Powerpoint PDF | Slides from the Nov 17th 2010 DAQ review |
The mission of ARA is to probe the EHE end (> 100's of PeV) of the neutrino energy spectrum, hoping to capture particles resulting from the GZK interaction of protons on the CMBR. The detector technology is premised on antennas sensitive to the electromagnetic Askar'yan pulse radiated when high energy EM cascades dissipate in dense RF transparent media.