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.

• -

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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