The Pierre Auger Observatory
An Overview
Review Agenda
Observatory Goals
Timeline
Design
Construction
Operation
Collaboration
Outreach
Agenda
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8:30 Executive session 9:00 Welcome 9:05 Overview (Paul Mantsch/Peter Mazur)
Auger Observatory Science Program and Run Plan 9:55 The energy spectrum (Carlos Escobar/Carlos Hojvat)10:20 Break10:35 Composition (Eun-Joo Ahn)11:25 Anisotropy (Peter Kasper)
12:05 Lunch break Fermilab Participation 1:05 Data analysis, detector characterization and data integrity (Paul Lebrun)1:55 Detector R&D (Peter Mazur)2:10 Project Management (Hank Glass)2:25 Auger Foundation (Carlos Hojvat)
The Future of UHECR Physics
2:40 R&D and the future of UHECR physics (Paolo Privitera) 3:20 Summary (Paul Mantsch)
Pierre Auger Observatory
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GoalsProbe the source and nature of
the highest energy cosmic rays.Study particle interactions
at extreme energy.
Interesting ResultsStrong suppression in the of
the spectrum at GZK thresholdTentative evidence for anisotropy
in arrival directions above 55 EeV.Proton-Air cross-section at 57 TeV cm Surprising features in the air- shower development with energy.
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Results: Air-Shower Development
Depth of shower maximum (Xmax) and the fluctuation in Xmax appear to suggest either a transition to a composition dominated by heavy primaries or else require major changes to the particle interaction models at high energies.
Either explanation would be unexpected and further investigation with improved statistics is high priority.
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Auger Timeline1991 – Concept of a Giant Array Project
ICRC Dublin, Ireland February-July 1995 - Design Workshop15 March 1999 - Signing of the
International Agreement, Mendoza, ArgentinaNovember 1995 – Collaboration formed, UNESCO, Paris
18 March 1999 - Inauguration of the Auger Site, Malargüe, Argentina 23 May 2001 - First Fluorescence Detector event 31 July 2001 - First Surface Array event 9 December 2001 - First hybrid event August 2005 – First results at conferences
November 2007 – First major publications June 2008 – The Observatory is complete
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Design of the Auger Observatory
Surface detector array + Air fluorescence detectors
Fluorescence Eye
Particle Detector Array
Combines strength of
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Design of the Auger Observatory Surface detector array + Air fluorescence detectors
Fluorescence Eye
Particle Detector
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Design of the Auger Observatory
Surface Array1600 Water Cerenkov Detectorsover 3000 Km2
Features 100% duty cycleUniform apertureSimple robust detectors
Fluorescence Detector24 telescopes in four enclosures
FeaturesCalorimetric energy
measurementDirect measurement of
shower development
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The Fluorescence Detector Telescope
11 square meter segmented mirror
Aperture stop and optical filter
440 pixel camera
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The Surface Detector Station
Communications antenna
Electronics enclosure
3 – nine inchphotomultipliertubes
Solar panels
Plastic tank with 12 tons of water
Battery box
GPS antenna
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The Auger Observatory
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Atmospheric Monitoring and Calibration
Lidar at each fluorescence eye
Central Laser Facility
Drum for uniform camera illumination – end to end calibration .
Camera Calibration
Atmospheric Monitoring
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Observatory Complete!(On budget - $54M)
Last Surface Detector – June 2008
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14 November 2008
Inauguration!
Goal-20 (~1%)
Performance
Black tanks
(average no of tanks weighted by live time)/(nominal tanks)
Efficiency
Goal-98%
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90%
100%
100
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Funding
ConstructionCompleted under the budget of $54.6M
Contributions from counties - 80% in-kind - 20% common fund – nominally for photomultiplier tubes
No contribution exceeded 25%
OperatingContributions to operating costs based on the number of authors
on scientific papers (excluding students)
Operating budget (2012 - $1.9M) is <3.5% of the construction cost
The US operating cost share for calendar 2012 is $373K
split equally between DOE and NSF
The Auger Collaboration19 Countries, 93 Institutions, 463 Collaborators
Argentina NetherlandsAustralia PolandBolivia* PortugalBrazil RomaniaCroatia Slovenia Czech Republic SpainFrance United Kingdom Germany USAItaly Vietnam*
Mexico
* associate
True International Partnership
by non-binding agreement -
No country, region or institution dominates
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International AgreementInitial signing March 16, 1999
Defines a framework for the organization, management and funding required for the construction, commissioning and operation of the Pierre Auger Observatory
The Parties to the Agreement are the funding agencies or their designates.
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Global Organization
Auger US Members Case Western Reserve University Corbin Covault – two PhD students Colorado School of Mines Fred Sarazin, Lawrence Wiencke - two Masters students Colorado State University, Fort Collins Jeffrey Brack, Alexei Dorofeev (PostDoc), John Harton, Miguel
Mostafá, Francisco Salesa Greus (PostDoc) - four PhD students Colorado State University, Pueblo William C. Brown Fermilab Eun-Joo Ahn (PostDoc), Henry Glass, Carlos Hojvat, Peter Kasper, Paul Lebrun, Paul Mantsch,
Peter Mazur, Hal Spinka (at ANL) Los Alamos National Laboratory Patrick Younk Louisiana State University James Matthews (also at Southern University), Michael Sutherland (PostDoc) -
three PhD students Michigan Technological University Johana Chirinos Diaz (PostDoc), Brian Fick, Roger Kieckhafer, Dave
Nitz - two PhD students New York University Jeff Allen (PostDoc), Glennys Farrar, Jonathan Roberts (PostDoc), Ingyin Zaw Northeastern University Thomas Paul, Yogendra N. Srivastava, John Swain, Allan Widom Ohio State University Patrick Allison (PostDoc), Jim Beatty, Eric Grashorn (PostDoc) - two PhD students Pennsylvania State University Karen S. Caballero-Mora (PostDoc), Stephane Coutu, Paul Sommers - two
PhD students University of Chicago James Cronin, Pedro Facal San Luis, Maria Monasor (PostDoc), Angela Olinto, Paolo Privitera, Benjamin Rouillé-d'Orfeuil (PostDoc), Tokonatsu Yamamoto (at Konan University) - three PhD students University of Nebraska Gregory Snow - one PhD student University of New Mexico Michael S. Gold, Robert Lauer (PostDoc), John A.J. Matthews University of Wisconsin-Madison Markus Ahlers, Segev BenZvi (PostDoc), Stefan Westerhoff – one PhD
student University of Wisconsin-Milwaukee Luis Anchordoqui
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Auger at FermilabPhysicists
Eun-Joo Ahn (Postdoc 100%)
Hank Glass (40%)
Carlos Hojvat (100%)
Peter Kasper (25%)
Paul Lebrun (50%)
Paul Mantsch (50%)
Peter Mazur (Scientist Emeritus)
Carlos Escobar
(International Fellow)
Our participation:
Project Management
Surface detector design and operation
Data analysis
Detector performance
FD/SD shifts
Data mirror/calibration database
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The Observatory and Staff
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Site ManagerGualberto Avila
FD Scientific OperationsCoordinator
Julio Rodriguez
SD Scientific OperationsCoordinatorRicardo Sato
Technical SystemAdministrator
Ruben Squatini
Maintenance ServicesRicardo Perez
Secretary of ManagementRosa Pacheco
Health, Safety & Environment
Jose Luis Escalona
Accounting AuxiliaryAdriana Cuartara
Visitor CenterAnalia Caceres
FD ObserverMariano Del Rio (IFN)
FD ElectronicsPrimo Vitale
FD ObserverJorge Rodriguez
FD/HEAT TechnicianLeandro Gomez
SD ObserverFernando Contreras (PT)
SD ObserverJavier Marin
SDE TechnicianMauro Gajardo
SDE TechnicianOscar Saez
SD TechnicianMiguel SalvadoresSDE TechnicianPablo Gongora
SDE Luis GonzalasSD Technician
Raul VidalPMS DBSDECo
OperatorJesica Velazquez (PT)SD Technician (WP)
Pedro Barraza
CDAS OperatorFernando Contreras (PT)
Electrical TechnicianRoberto Moyano
Mechanical TechnicianMario Rodríguez
Truck TechnicianJavier Salinas
NightwatchersSerafin Vidal
Alexis RodriguezIvan Munoz
HelpersJuan Blanco
Jorge Alcalde
CleaningEstela MansillaIsabel Farias
Auger Site Organization
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Impact and Diffusion of Auger Publications
Full Author List papersAnother 8 papers in the pipeline
In 2012, expect to prepare ~30 physics papers~10 detector papers
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Total Papers - 83 (1800 Citations)
Conference talks this year (to Sept) - 110
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Outreach
Malargüe Planetarium
Auger Office BuildingAnd Visitor Center>9000 visitors/yr
Auger collaboration on parade
James Cronin School
Beatriz Garcia (UTN,
Mendoza) and
Carlos Hojvat
A planetarium for the blind
Brightness represented by size of the
LEDs
Carlos Hojvat, Director’s Review, Fermilab, 15 December, 2011
Open top
Reaching for the stars Happy visitors!
At Tecnopolis, Buenos Aires
Back up
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Impact and Diffusion of Auger Publications
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Composition vs Hadronic Interactions
Inclined events
N ~ E095
No anisotropy at lower energies from Cen A region
A proton/iron model does not explain simultaneously the <Xmax > and σ (Xmax) data
The Nb of observed muons is quite above the expectations
The Nb of muons grows like what is expected for a single component composition
Composition vs Hadronic Interactions
<Xmax>
σ (Xmax)
: iron ; (1-): proton G. Wilk, Z. Wlodarczyk(J.Matthews, V.Serrini)
Operating Costs(2011 Budget)
The operating cost is 3.1% of the construction cost
The Observatory has always operated under budget.
The US part of the operating cost is shared equally between DOE and NSF
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Operating Costs(2011 Budget)
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Operating Costs(2012 Budget)
The operating cost is 3.5% of the construction cost
The Observatory has always operated within budget.
The US part of the operating cost is shared equally between DOE and NSF
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Operating Costs(2012 Budget)
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