Toni Carlson of Fairbury Jr. Sr. High School. Research center located in Los Angeles, California Caltech, Cal State Northridge, and UC Irvine collaborate.

Slides:



Advertisements
Similar presentations
1 Korean Ultra High Energy Cosmic Ray School Array Experiment Global Hands-On Universe 2007 National Astronomical Observatory, Mitaka, Tokyo, Japan 2007.
Advertisements

Testing of a Cellphone-based Cosmic-ray Detector Network Steven Wright, Zach Irwin, Charlie Steingard, Max Caplow, David Olin, Jesse Silva Wildwood School,
Detecting Particles: The Spark Chamber Particle Physics Masterclass Stephen A. Bull Tuesday 24 th April 2007.
Shantanu Menon Thomas Irons Michael Jacoutot. Cosmic Rays  High energy particles (mainly protons) from outer space.  Have up to 10 million times more.
The Pierre Auger Observatory Nicolás G. Busca Fermilab-University of Chicago FNAL User’s Meeting, May 2006.
WATERLOO HIGH SCHOOL. COSMIC RAY OBSERVATORY PROJECT  Goal of the statewide project  Install cosmic ray detectors at high schools around the state of.
EUSO: Extreme Universe Space Observatory Jessica Cerny Bancroft-Rosalie School.
Searching for Small-Scale Anisotropies in the Arrival Directions of Ultra-High Energy Cosmic Rays with the Information Dimension Eli Visbal (Carnegie Mellon.
CRAnE: A JAS-based Data Acquisition System for Cosmic Rays Jennifer Docktor & Manuel Reyes Mentors Tom Glanzman & Willy Langeveld August 13, 2003 Department.
Large Magellanic Cloud, 1987 (51.4 kparsec) SN 1987a after before 2006 Hubble.
Detecting Cosmic Rays An inexpensive portable detector By: Danny Franke Quarknet 2004.
The Milagro Gamma-Ray Observatory By Timothy Willett CROP: Roncalli Division.
Solving the Mystery of the Ultra-High Energy Cosmic Rays The Pierre Auger Observatory Pablo Bauleo Physics Department Colorado State University Fort Collins.
The Highest Energy Cosmic Rays Two Large Air Shower Detectors
SPHERE PEG GAY FAIRBURY JR SR HIGH SCHOOL. PROJECT SPHERE  Cherenkov light: radiation which is emitted whenever charged particles pass through matter.
Lecture 2-Building a Detector George K. Parks Space Sciences Laboratory UC Berkeley, Berkeley, CA.
Dwight Johns / RONCALLI update on O.W.L. project for: CROP summer 2002 by: Dwight Johns RONCALLI date: August 6, 2002.
QuarkNet 2011 Mohamed Ali-Hussein Ayasha Jabber. Cosmic Rays Discovered by Victor Hess in 1912 High energy particles (atoms, protons, electrons) traveling.
LHC ~E -2.7 ~E -3 ankle 1 part km -2 yr -1 knee 1 part m -2 yr -1 T. Gaisser 2005 Nature accelerates particles 10 7 times the energy of LHC! where?how?
 Our energy efficient house is located in Los Angeles, California.  The 3 energy reducing features in our home are solar panels, Energy Star light bulbs,
Cosmic Ray Muon Detection Department of Physics and Space Sciences Florida Institute of Technology Georgia Karagiorgi Julie Slanker Advisor: Dr. M. Hohlmann.
§ 4.3 Scientific Notation. Angel, Elementary Algebra, 7ed 2 Scientific Notation A number written in scientific notation is written as a number greater.
Team 25 COSMICi Mechanical Engineers George Chakhtoura Brian Kirkland Electrical/Computer Engineers Aarmondas Walker Samad Nurideen Juan Calderin Michael.
COSMIC RAYS An Overview Dr. Darrel Smith Department of Physics Embry-Riddle Aeronautical University Prescott, AZ
Dominik Wermus (Virginia Military Institute, Lexington, VA 24450), Doug Higinbotham (Thomas Jefferson National Accelerator Facility, Newport News, VA,
QuarkNet Muon Data Analysis with Shower Array Studies J.L. FISCHER, A. CITATI, M. HOHLMANN Physics and Space Sciences Department, Florida Institute of.
Scintillators, DAQ boards, and PMTs Getting Familiarized With the Equipment By Melissa Sussmann and Alex Bonnifield.
Cosmic Rays: Ever Present and Useful Anthony Gillespie Denbigh High School Mentor: Dr. Douglas Higinbotham Cosmic Rays Using the Cosmic Rays Current Research.
Design and status of the Pierre Auger Observatory J. C. Arteaga Velázquez 1, Rebeca López 2, R. Pelayo 1 and Arnulfo Zepeda 1 1 Departamento de Física,
SCINTILLATION COUNTER. PRINCIPLE When light radiations strike fluorescent material it produces flashes of light called scintillations. These are detected.
A Cherenkov Radiation Detector for the Auger Project Katarzyna Oldak Research Adviser: Corbin Covault Department of Physics The purpose of this project.
OPTICON is funded by the European Commission under Contract no RII3-CT Site Characterization of the Canarian Observatories: Different activities.
GEOGRAPHIC LOCATION OF THE PIERRE AUGER OBSERVATORY Northern Hemisphere: Millard County, Utah Southern Hemisphere: Malargüe Mendoza Province Argentina.
, A possible origin of ultra-high energy cosmic rays: collisions of two galaxies The main goal of the Pierre Auger Project is a detailed study of the energy.
The HEAP-MM proposal P. Piattelli VLVnT The call  INFRA Research Infrastructures for astroparticle physics: High energy cosmic rays,
Improved PMTs for the Cherenkov Telescope Array project Razmik Mirzoyan for the Focal Plane Instrumentation WG Max-Planck-Institute for Physics Munich,
Design and optimization of Electromagnetic particle Detectors (EDs) in LHAASO-KM2A Xiangdong Sheng, Jia Liu, Jing Zhao on behalf of the LHAASO collaboration.
Experiment Design SCIPP Teacher Workshop Mary Jo Nordyke August 2010.
SKALTA experiment SlovaKiAn Large-area Time coincidence Array.
Position sensitive scintillation detectors for the trigger system in the space experiment NUCLEON Supervisors: Anatoliy I. Kalinin a Students: Irina Cioara.
MINERvA Main INjector ExpeRiment for -A is the symbol for the neutrino. The beam that is sent to MINERvA is made out of neutrinos. In chemistry, an A stands.
THE GAMMA-400 PROJECT Direct measurements of the primary gamma- radiation in the energy range 30 GeV – 1 TeV GAMMA-400 COLLABORATION: Lebedev Physical.
A Cherenkov Radiation Detector Design for the Observation and Measurement of High Energy Cosmic Rays Yvette Cendes, Research Adviser: Corbin Covault Department.
Programmable logic device Time-to-digital converters 5 Volt DC power To PC serial port Four analog PMT inputs Discriminator threshold adjust GPS input.
Brian Lowery July 11,  Primary  From space ▪ Lower energy cosmic rays come from sun ▪ Higher energy cosmic rays come from other places in the.
IEAP CTU Project CZELTA Karel Smolek IEAP CTU
P.Auger, a major step: Need high statistics large detection area : 2 x3000 km² Uniform sky coverage 2 sites located in each hemisphere Argentina and USA.
MUONS!. What are we going to talk about? How muons are created Detecting methods Muon half life and decay rate Muon decay data Problems with the data.
QuarkNet and Cosmic Ray Muon Flux Experiments Florida Academy of Sciences Spring Conference 2009 Alfred Menendez and Michael Abercrombie with Dr. Marcus.
LA ACES Neutron Detector (NeD)
The Cosmic Ray Observatory Project in Nebraska Conference on Teacher Research Experiences University of Rhode Island April 2005 An education and.
The Auger Observatory for High-Energy Cosmic Rays G.Matthiae University of Roma II and INFN For the Pierre Auger Collaboration The physics case Pierre.
Where do ultra-high energy cosmic rays come from? No one knows the origin of ultra-high energy cosmic rays. The majority of low-energy cosmic ray particles.
Victor Hess in his balloon (1912). Cosmic Rays Produce Muons in the Atmosphere.
5 June 2002DAQ System Engineering Requirements 1 DAQ System Requirements DOM Main Board Engineering Requirements Review David Nygren.
E. W. Grashorn and A. Habig, UMD, for the MINOS Collaboration The Detectors of The Main Injector Neutrino Oscillation Search (MINOS) Experiment The MINOS.
What we do know about cosmic rays at energies above eV? A.A.Petrukhin Contents 4 th Round Table, December , Introduction. 2. How these.
Telescopes and The Sky Katherine Rawlins University of Wisconsin- Madison Presented by Jim Madsen UW-RF.
November 2007Infrasound Technology Workshop, Tokyo, JapanPage 1 Presented to: Infrasound Technology Workshop Tokyo, Japan PTS Experimental Infrasound Array.
UC Open Access Policy Presentation to CORCL October 17, /17/2013University of California Irvine1.
Pacific Earthquake Engineering Research Center HAWAII WASHINGTON CALIFORNIA OREGON Core University Partners: UC Berkeley, Davis, Irvine, Los Angeles, San.
GTL manages these industries:
QuarkNet and Cosmic Ray Muon Flux Experiments
Flying Radioactive Intergalactic Bunnies
Hadron Production Measurements
Detecting Particles: The Spark Chamber
The Laser Interferometer Gravitational-Wave Observatory
Detecting Cosmic Rays An inexpensive portable detector
Sci Formation of the Universe
ICRC2011, 32ND INTERNATIONAL COSMIC RAY CONFERENCE, BEIJING 2011
Presentation transcript:

Toni Carlson of Fairbury Jr. Sr. High School

Research center located in Los Angeles, California Caltech, Cal State Northridge, and UC Irvine collaborate with high school students L.A. Location and Collaboration

Potential CHICOS installation sites in L.A. Sites operating as of June 2002 Operating Sites

Array began in Fall 2001 Plans to continue deployment in the next 2 years ( ) Operate it as a major research facility. These are two students from Westridge School working on their supply boxes. Future Plans

To the right is a scintillation panel with special doping which turns cosmic rays into light. On the left is a Global Positioning System (GPS) receiver. Project Materials

This is a Photo Multiplier Tube (PMT). More Project Materials

Detect the highest energy elementary particles ever observed Primary goal is to collect more events at ultra-high energies and characterize that energy and locate apparent direction of origin

CHICOS is California High school Cosmic ray ObServatory The research center is in Los Angeles They plan to continue the deployment of new operating sites Primary goal is to find the origin of cosmic rays and characterize them

If you have any questions further regarding CHICOS, contact Dr. Michelle Larson, CHICOS project coordinator, at