The Pierre Auger Observatory Water Cherenkov Detectors Gamma Ray Bursts GRB detection by WCD

Cosmic Ray Detectors: Probes for the Highest Energies

Xavier Bertou

Centro Atómico Bariloche. Argentina

Mérida, Venezuela, August 27 – 31, 2007

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Water Cherenkov Detectors Gamma Ray Bursts GRB detection by WCD Outline

1 The Pierre Auger Observatory Ultra High Energy Cosmic Rays The Pierre Auger Observatory Auger South Ground Array First results 2 Water Cherenkov Detectors WCD Basics Calibration Some Specific Properties 3 Gamma Ray Bursts Discovery and Basic Understanding: Vela and BATSE To the Sources: Beppo-SAX Improving the Understanding: SWIFT... High Energy Detection 4 GRB detection by WCD The Pierre Auger Observatory The Large Aperture GRB Observatory Prototypes WCD LAGO status

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Outline

1 The Pierre Auger Observatory Ultra High Energy Cosmic Rays The Pierre Auger Observatory Auger South Ground Array First results 2 Water Cherenkov Detectors WCD Basics Calibration Some Specific Properties 3 Gamma Ray Bursts Discovery and Basic Understanding: Vela and BATSE To the Sources: Beppo-SAX Improving the Understanding: SWIFT... High Energy Detection 4 GRB detection by WCD The Pierre Auger Observatory The Large Aperture GRB Observatory Prototypes WCD LAGO status

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Spectrum

Power law with index 2.7 12 orders of magnitude in energy 32 orders of magnitude in flux only 2 (3?) features

At ankle: 1 event/km2/year At 1020 eV: 1 event/km2/century (or millennium?)

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Spectrum

Power law with index 2.7 12 orders of magnitude in energy 32 orders of magnitude in flux only 2 (3?) features

At ankle: 1 event/km2/year At 1020 eV: 1 event/km2/century (or millennium?)

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Spectrum

Power law with index 2.7 12 orders of magnitude in energy 32 orders of magnitude in flux only 2 (3?) features

At ankle: 1 event/km2/year At 1020 eV: 1 event/km2/century (or millennium?)

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results AGASA Spectrum (2002)

AGASA 111 scintillator detectors, over 100 km2 for 11 years

Exciting feature: harder slope at UHE

Even better: post-GZK events

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results AGASA Spectrum (2002)

AGASA 111 scintillator detectors, over 100 km2 for 11 years

Exciting feature: harder slope at UHE

Even better: post-GZK events

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results AGASA Spectrum (2002)

AGASA 111 scintillator detectors, over 100 km2 for 11 years

Exciting feature: harder slope at UHE

Even better: post-GZK events

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results GZK cut-off

At UHE, protons interact with CMB photons by photo production, and nuclei with CMB and IR photons through photo dissociation

UHECR should lose energy quickly on short distances (<100 Mpc)

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results GZK cut-off

At UHE, protons interact with CMB photons by photo production, and nuclei with CMB and IR photons through photo dissociation

UHECR should lose energy quickly on short distances (<100 Mpc)

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results GZK cut-off

At UHE, protons interact with CMB photons by photo production, and nuclei with CMB and IR photons through photo dissociation

UHECR should lose energy quickly on short distances (<100 Mpc)

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results UHECR Astronomy

Magnetic fields At low energies, CR are deflected by galactic and extra-galactic magnetic fields. UHECR should point to the source

1018 eV 1019 eV 1020 eV

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results UHECR Astronomy

Magnetic fields At low energies, CR are deflected by galactic and extra-galactic magnetic fields. UHECR should point to the source

1018 eV 1019 eV 1020 eV

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results AGASA sky

High Energy Low Energy > 40 EeV 1-3 EeV

1 triplet and 6 doublets Excess in GC direction

Exciting (new?) physics and astrophysics

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results AGASA sky

High Energy Low Energy > 40 EeV 1-3 EeV

1 triplet and 6 doublets Excess in GC direction

Exciting (new?) physics and astrophysics

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results AGASA sky

High Energy Low Energy > 40 EeV 1-3 EeV

1 triplet and 6 doublets Excess in GC direction

Exciting (new?) physics and astrophysics

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results UHECR Sources?

Bottom-Up Top/Down

Super massive particle Topological Defect

neutrinos photons

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results UHECR Sources?

Bottom-Up Top/Down

Super massive particle Topological Defect

neutrinos photons

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results UHECR Sources?

Bottom-Up Top/Down

Super massive particle Topological Defect

neutrinos photons

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Model Killer

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results UHECR Extended Air Shower

EAS at 1020 eV 50 W light bulb at speed of light 1012 particles spread over >20 km2

Detector Fluorescence Telescope Ground Array

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results UHECR Extended Air Shower

EAS at 1020 eV 50 W light bulb at speed of light 1012 particles spread over >20 km2

Detector Fluorescence Telescope Ground Array

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results UHECR Extended Air Shower

EAS at 1020 eV 50 W light bulb at speed of light 1012 particles spread over >20 km2

Detector Fluorescence Telescope Ground Array

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Japan ICRC 2003

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results The Pierre Auger Observatory

A Giant Hybrid Observatory

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Pierre Auger

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Auger Design

An Hybrid Giant 2 sites, in USA and Argentina Performance (Auger South) Southern site: 3000 km2 fully efficient > 10 EeV 1600 SD WCD: 100% duty cycle (SD) 1.5 km triangular grid 4 FD buildings: 10% duty cycle (FD) 24 telescopes 20% energy resolution Northern site: 10000 km2? 1◦ above 10 EeV 4000 SD WCD: 0.5◦ Hybrid 1 mile square grid 3 FD buildings: cross-calibration 18 telescopes

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Auger Design

An Hybrid Giant 2 sites, in USA and Argentina Performance (Auger South) Southern site: 3000 km2 fully efficient > 10 EeV 1600 SD WCD: 100% duty cycle (SD) 1.5 km triangular grid 4 FD buildings: 10% duty cycle (FD) 24 telescopes 20% energy resolution Northern site: 10000 km2? 1◦ above 10 EeV 4000 SD WCD: 0.5◦ Hybrid 1 mile square grid 3 FD buildings: cross-calibration 18 telescopes

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Parenthesis: Neutrinos

Earth crust 200 km ντ interaction length 50 km Auger size 60 km ντ decay length 30 km

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Parenthesis: Neutrinos

Earth crust 200 km ντ interaction length 50 km Auger size 60 km ντ decay length 30 km

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Auger South layout

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Auger Water Cherenkov Detector

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Pictures

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Auger South Status (August 2006)

Thursday August 31th 1186 tanks deployed 1167 with water 986 with electronics

SD Data 510405 events <60◦ 363071 for analysis 2.7× AGASA

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Auger South Status

Thursday August 23rd 1480 tanks deployed 1433 with water 1376 with electronics

SD Data 882473 events <60◦ 648079 for analysis 4.6× AGASA

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Data status

All detectors are constantly monitored Towards 1M Events

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Data status

All detectors are constantly monitored Towards 1M Events

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Auger Spectrum

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Galactic Center

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Photon Limit

No photons: Top-Down models strongly constrained

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Neutrino Limit

Still no Neutrino

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Ultra High Energy Cosmic Rays Water Cherenkov Detectors The Pierre Auger Observatory Gamma Ray Bursts Auger South Ground Array GRB detection by WCD First results Neutrino Limit

Still no Neutrino

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Outline

1 The Pierre Auger Observatory Ultra High Energy Cosmic Rays The Pierre Auger Observatory Auger South Ground Array First results 2 Water Cherenkov Detectors WCD Basics Calibration Some Specific Properties 3 Gamma Ray Bursts Discovery and Basic Understanding: Vela and BATSE To the Sources: Beppo-SAX Improving the Understanding: SWIFT... High Energy Detection 4 GRB detection by WCD The Pierre Auger Observatory The Large Aperture GRB Observatory Prototypes WCD LAGO status

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Auger Water Cherenkov Detector

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Cherenkov Light

Particle crossing a medium at a speed higher than speed of light in that medium produce coherent Cherenkov light

2 2   d N = q − 1 dxdλ k λ2 1 β2n2

Light mainly in UV and Blue

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Water

Cherenkov Photons propagate in Water and get absorbed

Difference between absorption and scattering (and attenuation) dN N = a(λ) + b(λ) = c(λ)

In Auger Water Absorption Length is about 60 m

(and highly depends on wavelength, 100× more for red than blue)

=⇒ Cherenkov photons will bounce many times before reaching the PMTs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Water

Cherenkov Photons propagate in Water and get absorbed

Difference between absorption and scattering (and attenuation) dN N = a(λ) + b(λ) = c(λ)

In Auger Water Absorption Length is about 60 m

(and highly depends on wavelength, 100× more for red than blue)

=⇒ Cherenkov photons will bounce many times before reaching the PMTs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Water

Cherenkov Photons propagate in Water and get absorbed

Difference between absorption and scattering (and attenuation) dN N = a(λ) + b(λ) = c(λ)

In Auger Water Absorption Length is about 60 m

(and highly depends on wavelength, 100× more for red than blue)

=⇒ Cherenkov photons will bounce many times before reaching the PMTs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Water

Cherenkov Photons propagate in Water and get absorbed

Difference between absorption and scattering (and attenuation) dN N = a(λ) + b(λ) = c(λ)

In Auger Water Absorption Length is about 60 m

(and highly depends on wavelength, 100× more for red than blue)

=⇒ Cherenkov photons will bounce many times before reaching the PMTs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD TyvekTM Liner

Water in enclosed in a light-tight bag

Tyvek is a highly reflective and diffusive material

Allows light to reach PMT well after 100 ns (i.e. more than 10 reflections) Makes light in a tank uniform

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD TyvekTM Liner

Water in enclosed in a light-tight bag

Tyvek is a highly reflective and diffusive material

Allows light to reach PMT well after 100 ns (i.e. more than 10 reflections) Makes light in a tank uniform

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD TyvekTM Liner

Water in enclosed in a light-tight bag

Tyvek is a highly reflective and diffusive material

Allows light to reach PMT well after 100 ns (i.e. more than 10 reflections) Makes light in a tank uniform

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD PMT basics

Vacuum-tight glass envelope Photon knock on photocathode and produce electron (photoelectric effect) Each Dynode is a multiplication stage Last step is Anode, for a cleaned signal Magnetic field influences PMT collection efficiency Afterpulses: nuclei knocked and accelerated

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Response to Particles

Muon Photon Electron Typical energy: Typical energy: Typical energy: 1 - 50 GeV few MeV few 10 MeV Represent 1% Represent 90% Represent 10% of secondaries of secondaries of secondaries Usually too 1.2 m is deep Simple calorimeter: energetic to be enough to provoke leaves a signal stopped in a WCD. pair creation. proportional to its Leaves a signal The e+ e− pair then energy proportional to track radiates its energy length

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Response to Particles

Muon Photon Electron Typical energy: Typical energy: Typical energy: 1 - 50 GeV few MeV few 10 MeV Represent 1% Represent 90% Represent 10% of secondaries of secondaries of secondaries Usually too 1.2 m is deep Simple calorimeter: energetic to be enough to provoke leaves a signal stopped in a WCD. pair creation. proportional to its Leaves a signal The e+ e− pair then energy proportional to track radiates its energy length

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Response to Particles

Muon Photon Electron Typical energy: Typical energy: Typical energy: 1 - 50 GeV few MeV few 10 MeV Represent 1% Represent 90% Represent 10% of secondaries of secondaries of secondaries Usually too 1.2 m is deep Simple calorimeter: energetic to be enough to provoke leaves a signal stopped in a WCD. pair creation. proportional to its Leaves a signal The e+ e− pair then energy proportional to track radiates its energy length

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Response to Particles

Muon Photon Electron Typical energy: Typical energy: Typical energy: 1 - 50 GeV few MeV few 10 MeV Represent 1% Represent 90% Represent 10% of secondaries of secondaries of secondaries Usually too 1.2 m is deep Simple calorimeter: energetic to be enough to provoke leaves a signal stopped in a WCD. pair creation. proportional to its Leaves a signal The e+ e− pair then energy proportional to track radiates its energy length

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Response to Particles

Muon Photon Electron Typical energy: Typical energy: Typical energy: 1 - 50 GeV few MeV few 10 MeV Represent 1% Represent 90% Represent 10% of secondaries of secondaries of secondaries Usually too 1.2 m is deep Simple calorimeter: energetic to be enough to provoke leaves a signal stopped in a WCD. pair creation. proportional to its Leaves a signal The e+ e− pair then energy proportional to track radiates its energy length

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Response to Particles

Muon Photon Electron Typical energy: Typical energy: Typical energy: 1 - 50 GeV few MeV few 10 MeV Represent 1% Represent 90% Represent 10% of secondaries of secondaries of secondaries Usually too 1.2 m is deep Simple calorimeter: energetic to be enough to provoke leaves a signal stopped in a WCD. pair creation. proportional to its Leaves a signal The e+ e− pair then energy proportional to track radiates its energy length

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Flux to Charge Histogram

Flux Charge Histogram

Electrons

Energy Charge

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Flux to Charge Histogram

Flux Charge Histogram

Electrons

Energy Charge

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Flux to Charge Histogram

Flux Charge Histogram

Electrons Photons

Energy Charge

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Flux to Charge Histogram

Flux Charge Histogram

Electrons Photons

Energy Charge

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Flux to Charge Histogram

Flux Charge Histogram

Electrons Photons Muons

Energy Charge

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Flux to Charge Histogram

Flux Charge Histogram

Electrons Photons Muons

Energy Charge

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Flux to Charge Histogram

Flux Charge Histogram

Electrons Photons Muons

Energy Charge

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Hump to VEM

VEM: Vertical Equivalent Muon. The average charge deposited by a vertical and central muon

VEM - Hump shift due to muon track distribution and photostatistic

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Hump to VEM

VEM: Vertical Equivalent Muon. The average charge deposited by a vertical and central muon

VEM - Hump shift due to muon track distribution and photostatistic

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Hump to VEM

VEM: Vertical Equivalent Muon. The average charge deposited by a vertical and central muon

VEM - Hump shift due to muon track distribution and photostatistic

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Decay

Muon decay rate is proportional to the volume of the WCD. Signal is a first peak (muon) then another one (electron). Time difference is µ lifetime, ∼ 2.2µs.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Decay

Muon decay rate is proportional to the volume of the WCD. Signal is a first peak (muon) then another one (electron). Time difference is µ lifetime, ∼ 2.2µs.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Decay

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Decay

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Decay

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Incoming Zenith angle

Muon Each muon gives a signal proportional to track length: RR SVEM ∝ TL(θ, x, y)dS SVEM ∝ V

Electrons

SVEM ∝ S(θ)

Photons More complex (pair production probability) but more like electrons.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Incoming Zenith angle

Muon Each muon gives a signal proportional to track length: RR SVEM ∝ TL(θ, x, y)dS SVEM ∝ V

Electrons

SVEM ∝ S(θ)

Photons More complex (pair production probability) but more like electrons.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Incoming Zenith angle

Muon Each muon gives a signal proportional to track length: RR SVEM ∝ TL(θ, x, y)dS SVEM ∝ V

Electrons

SVEM ∝ S(θ)

Photons More complex (pair production probability) but more like electrons.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Azimuth and Entry point

With 3 PMTs, Auger WCD offer uniform response

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Azimuth and Entry point

With 3 PMTs, Auger WCD offer uniform response

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Azimuth and Entry point

With 3 PMTs, Auger WCD offer uniform response

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Water Quality

A better Water/Tyvek increases chance of late light to reach PMT With equivalent gain, the same intensity peak would be observed but more late charge would be collected.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Water Quality

A better Water/Tyvek increases chance of late light to reach PMT With equivalent gain, the same intensity peak would be observed but more late charge would be collected.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Introduction to Saturation

Many items may saturate: Numeric saturation: ADC Electronic saturation: Base PMT Non Linearity

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Introduction to Saturation

Many items may saturate: Numeric saturation: ADC Electronic saturation: Base PMT Non Linearity

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Saturation Recovery

Undershoot is proportional to integrated signal =⇒ Signal can be extracted from Undershoot

One can fit signal with a proper signal shape. Check by artificially cutting unsaturated signals.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Saturation Recovery

Undershoot is proportional to integrated signal =⇒ Signal can be extracted from Undershoot

One can fit signal with a proper signal shape. Check by artificially cutting unsaturated signals.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Saturation Recovery

Undershoot is proportional to integrated signal =⇒ Signal can be extracted from Undershoot

One can fit signal with a proper signal shape. Check by artificially cutting unsaturated signals.

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Extras

Many extra quantities can be studied with a WCD.

Water Level Muon Histogram gives water level PMT Glass Sometimes a particle can hit directly a PMT

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Extras

Many extra quantities can be studied with a WCD.

Water Level Muon Histogram gives water level PMT Glass Sometimes a particle can hit directly a PMT

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Extras

Many extra quantities can be studied with a WCD.

Water Level Muon Histogram gives water level PMT Glass Sometimes a particle can hit directly a PMT

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Extras

Many extra quantities can be studied with a WCD.

Water Level Muon Histogram gives water level PMT Glass Sometimes a particle can hit directly a PMT

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Extras

Many extra quantities can be studied with a WCD.

Water Level Muon Histogram gives water level PMT Glass Sometimes a particle can hit directly a PMT

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Charge-Peak Histograms

X. Bertou Cosmic Ray Detectors Through PMT 3

Showers (PMT 1>2 VEM) Glass (difference)

The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Telescope

VEM (central)

X. Bertou Cosmic Ray Detectors Showers (PMT 1>2 VEM) Glass (difference)

The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Telescope

VEM (central) Through PMT 3

X. Bertou Cosmic Ray Detectors Glass (difference)

The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Telescope

VEM (central) Through PMT 3

Showers (PMT 1>2 VEM)

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory WCD Basics Water Cherenkov Detectors Calibration Gamma Ray Bursts Some Specific Properties GRB detection by WCD Muon Telescope

VEM (central) Through PMT 3

Showers (PMT 1>2 VEM) Glass (difference)

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Outline

1 The Pierre Auger Observatory Ultra High Energy Cosmic Rays The Pierre Auger Observatory Auger South Ground Array First results 2 Water Cherenkov Detectors WCD Basics Calibration Some Specific Properties 3 Gamma Ray Bursts Discovery and Basic Understanding: Vela and BATSE To the Sources: Beppo-SAX Improving the Understanding: SWIFT... High Energy Detection 4 GRB detection by WCD The Pierre Auger Observatory The Large Aperture GRB Observatory Prototypes WCD LAGO status

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Discovery of GRBs: Vela 5

GRBs - Vela 5 Discovered accidentally in the 60’s by US military satellites

GRB ∆t ≈ 0.01 s - 100 s E > 100 keV

Enigma for 30 years origin distance luminosity

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Discovery of GRBs: Vela 5

GRBs - Vela 5 Discovered accidentally in the 60’s by US military satellites

GRB ∆t ≈ 0.01 s - 100 s E > 100 keV

Enigma for 30 years origin distance luminosity

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Discovery of GRBs: Vela 5

GRBs - Vela 5 Discovered accidentally in the 60’s by US military satellites

GRB ∆t ≈ 0.01 s - 100 s E > 100 keV

Enigma for 30 years origin distance luminosity

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection BATSE: 1991 - 2000

Compton Gamma Ray Observatory BATSE OSSE 50 keV - 10 MeV Field of view: 4 π sr BATSE 20 keV - 20 MeV Flux > 0.1 γ cm−2 s−1 COMPTEL 800 keV - 30 MeV Angular resolution > 4◦ EGRET 20 MeV - 30 GeV

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection BATSE: 1991 - 2000

Compton Gamma Ray Observatory BATSE OSSE 50 keV - 10 MeV Field of view: 4 π sr BATSE 20 keV - 20 MeV Flux > 0.1 γ cm−2 s−1 COMPTEL 800 keV - 30 MeV Angular resolution > 4◦ EGRET 20 MeV - 30 GeV

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection BATSE Signals

1 GRB per day (30% efficiency) Duration

2 distinct populations

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection BATSE Signals

1 GRB per day (30% efficiency) Duration

2 distinct populations

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection BATSE Signals

1 GRB per day (30% efficiency) Duration

2 distinct populations

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection BATSE Signals

1 GRB per day (30% efficiency) Duration

Short < 2 s

Long > 2 s

2 distinct populations

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Before BATSE

GRB were supposed to be born in our galaxy (neutron stars explosion?)

In such a case, an anisotropy was expected

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Before BATSE

GRB were supposed to be born in our galaxy (neutron stars explosion?)

In such a case, an anisotropy was expected

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Before BATSE

GRB were supposed to be born in our galaxy (neutron stars explosion?)

In such a case, an anisotropy was expected

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection BATSE sky

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Luminosity distribution

Deficit at low luminosity Galactic halo Cosmological distribution

BATSE showed GRBs are isotropes GRBs are not homogenous

Need to measure the distance to GRBs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Luminosity distribution

Deficit at low luminosity Galactic halo Cosmological distribution

BATSE showed GRBs are isotropes GRBs are not homogenous

Need to measure the distance to GRBs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Luminosity distribution

Deficit at low luminosity Galactic halo Cosmological distribution

BATSE showed GRBs are isotropes GRBs are not homogenous

Need to measure the distance to GRBs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Luminosity distribution

Deficit at low luminosity Galactic halo Cosmological distribution

BATSE showed GRBs are isotropes GRBs are not homogenous

Need to measure the distance to GRBs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Luminosity distribution

Deficit at low luminosity Galactic halo Cosmological distribution

BATSE showed GRBs are isotropes GRBs are not homogenous

Need to measure the distance to GRBs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Luminosity distribution

Deficit at low luminosity Galactic halo Cosmological distribution

BATSE showed GRBs are isotropes GRBs are not homogenous

Need to measure the distance to GRBs

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Beppo-SAX - 1996-2002

GRB 40-700 keV monitor Various X-rays detectors Angular resolution: 50”

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970228

First coincidence Gamma - X

First afterglow, various days

Observation with other telescopes

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970228

First coincidence Gamma - X

First afterglow, various days

Observation with other telescopes 28 February 3 March

“Afterglow” in X-rays

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970228

First coincidence Gamma - X

First afterglow, various days

Observation with other telescopes 28 February 3 March

“Afterglow” in X-rays

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970228

First coincidence Gamma - X

First afterglow, various days

Observation with other telescopes

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970228

First coincidence Gamma - X

First afterglow, various days

Observation with other telescopes

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970228

First coincidence Gamma - X

First afterglow, various days

Observation with other telescopes

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970508

Observation of absorption lines in the optical spectrum of the afterglow

Redshift: Z ≈ 0.84

Cosmological origin

1 day 10 days 100 days

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970508

Observation of absorption lines in the optical spectrum of the afterglow

Redshift: Z ≈ 0.84

Cosmological origin

1 day 10 days 100 days

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970508

Observation of absorption lines in the optical spectrum of the afterglow

Redshift: Z ≈ 0.84

Cosmological origin

1 day 10 days 100 days

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection GRB 970508

Observation of absorption lines in the optical spectrum of the afterglow

Redshift: Z ≈ 0.84

Cosmological origin

1 day 10 days 100 days

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Redshifts

Luminosity Typically 1051-1054 erg

Sun Our galaxy 4 × 1033 erg 1044 erg

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Redshifts

Luminosity Typically 1051-1054 erg

Sun Our galaxy 4 × 1033 erg 1044 erg

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Redshifts

Luminosity Typically 1051-1054 erg

Sun Our galaxy 4 × 1033 erg 1044 erg

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Current Status

SWIFT (2004-) allowed detection of short GRB afterglows, early flares, high redshifts GRBs...

Long GRBs Short GRBs happen in star formation dimmer, but harder zone spectrum likely to be core-collapse of coalescence of a pair of massive stars compact objects ? connection with SN more data still needed

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Current Status

SWIFT (2004-) allowed detection of short GRB afterglows, early flares, high redshifts GRBs...

Long GRBs Short GRBs happen in star formation dimmer, but harder zone spectrum likely to be core-collapse of coalescence of a pair of massive stars compact objects ? connection with SN more data still needed

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Current Status

SWIFT (2004-) allowed detection of short GRB afterglows, early flares, high redshifts GRBs...

Long GRBs Short GRBs happen in star formation dimmer, but harder zone spectrum likely to be core-collapse of coalescence of a pair of massive stars compact objects ? connection with SN more data still needed

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection The Fireball model

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection At higher energy?

EGRET detected 16 GRBs spectrum with a power law of about ≈ 2.2

3 GRBs with photons of Eγ > 1 GeV maximum energy 18 GeV

Observation at higher energy could help

GLAST (early 2008) should give the answer

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection At higher energy?

EGRET detected 16 GRBs spectrum with a power law of about ≈ 2.2

3 GRBs with photons of Eγ > 1 GeV maximum energy 18 GeV

Observation at higher energy could help

GLAST (early 2008) should give the answer

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection At higher energy?

EGRET detected 16 GRBs spectrum with a power law of about ≈ 2.2

3 GRBs with photons of Eγ > 1 GeV maximum energy 18 GeV

Observation at higher energy could help

GLAST (early 2008) should give the answer

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection HECR Atmospheric Showers

What reaches ground Scintillator WCD Photons (90%) NO YES Electrons (9%) YES YES Muons (<1%) YES YES∗

If a GRB emits at high energies (> 1 GeV), HE photon flux is expected at the top of the atmosphere, Secondary photon flux is expected to increase during the burst

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection HECR Atmospheric Showers

What reaches ground Scintillator WCD Photons (90%) NO YES Electrons (9%) YES YES Muons (<1%) YES YES∗

If a GRB emits at high energies (> 1 GeV), HE photon flux is expected at the top of the atmosphere, Secondary photon flux is expected to increase during the burst

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection HECR Atmospheric Showers

What reaches ground Scintillator WCD Photons (90%) NO YES Electrons (9%) YES YES Muons (<1%) YES YES∗

If a GRB emits at high energies (> 1 GeV), HE photon flux is expected at the top of the atmosphere, Secondary photon flux is expected to increase during the burst

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection HECR Atmospheric Showers

What reaches ground Scintillator WCD Photons (90%) NO YES Electrons (9%) YES YES Muons (<1%) YES YES∗

If a GRB emits at high energies (> 1 GeV), HE photon flux is expected at the top of the atmosphere, Secondary photon flux is expected to increase during the burst

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Single Particle Technique

A different use of a ground array

Normal mode (shower) Single Particle Mode

With SPT, there is no direction and/or energy reconstruction

GRBs are detected as an excess of counts over background

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Single Particle Technique

A different use of a ground array

Normal mode (shower) Single Particle Mode

With SPT, there is no direction and/or energy reconstruction

GRBs are detected as an excess of counts over background

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Single Particle Technique

A different use of a ground array

Normal mode (shower) Single Particle Mode

With SPT, there is no direction and/or energy reconstruction

GRBs are detected as an excess of counts over background

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory Discovery and Basic Understanding: Vela and BATSE Water Cherenkov Detectors To the Sources: Beppo-SAX Gamma Ray Bursts Improving the Understanding: SWIFT... GRB detection by WCD High Energy Detection Single Particle Technique

A different use of a ground array

Normal mode (shower) Single Particle Mode

With SPT, there is no direction and/or energy reconstruction

GRBs are detected as an excess of counts over background

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Outline

1 The Pierre Auger Observatory Ultra High Energy Cosmic Rays The Pierre Auger Observatory Auger South Ground Array First results 2 Water Cherenkov Detectors WCD Basics Calibration Some Specific Properties 3 Gamma Ray Bursts Discovery and Basic Understanding: Vela and BATSE To the Sources: Beppo-SAX Improving the Understanding: SWIFT... High Energy Detection 4 GRB detection by WCD The Pierre Auger Observatory The Large Aperture GRB Observatory Prototypes WCD LAGO status

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status The Pierre Auger Observatory

Located in Malargüe, Mendoza, at 1400 m asl 1600 Water Cherenkov Detectors (1300 in operation) (fluorescence telecopes)

Scalers Low (3 ADC ≈ 6 pe ≈ 15 MeV) scaler count, Muon (20 ADC ≈ 100 MeV) scaler count, Send to central DAQ difference of both every second

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status The Pierre Auger Observatory

Located in Malargüe, Mendoza, at 1400 m asl 1600 Water Cherenkov Detectors (1300 in operation) (fluorescence telecopes)

Scalers Low (3 ADC ≈ 6 pe ≈ 15 MeV) scaler count, Muon (20 ADC ≈ 100 MeV) scaler count, Send to central DAQ difference of both every second

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Simulation of Auger WCD Response

1.4 billion showers simulated with CORSIKA (no thinning) between 10 MeV and 10 TeV, 0 and 30 degrees Detector response with G4FastSim (Auger fast version of G4)

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Comparison of Auger Response with Scintillator array

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Auger Data

Scalers since September 2005 Rate vs Time

Rate vs Station Id

Sensitivity ≈ 2 particles/m2

Only Ligthning Events

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Auger Data

Scalers since September 2005 Rate vs Time

Rate vs Station Id

Sensitivity ≈ 2 particles/m2

Only Ligthning Events

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Auger Data

Scalers since September 2005 Rate vs Time

Rate vs Station Id

Sensitivity ≈ 2 particles/m2

Only Ligthning Events

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Auger Data

Scalers since September 2005 Rate vs Time

Rate vs Station Id

Sensitivity ≈ 2 particles/m2

Only Ligthning Events

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Auger Results for 18 months of data

No GRB detected: limit on GRB high energy fluence

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Auger Results for 18 months of data

No GRB detected: limit on GRB high energy fluence

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO

LAGO Large Aperture GRB Observatory

Idea Detect GRB at high energy from the ground

Who? How? Where? Argentina Using WCD: In high altitude Bolivia Easy to calibrate mountain sites Mexico (> 4000 m) + France, Venezuela, Italy Detect Photons

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO

LAGO Large Aperture GRB Observatory

Idea Detect GRB at high energy from the ground

Who? How? Where? Argentina Using WCD: In high altitude Bolivia Easy to calibrate mountain sites Mexico (> 4000 m) + France, Venezuela, Italy Detect Photons

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO

LAGO Large Aperture GRB Observatory

Idea Detect GRB at high energy from the ground

Who? How? Where? Argentina Using WCD: In high altitude Bolivia Easy to calibrate mountain sites Mexico (> 4000 m) + France, Venezuela, Italy Detect Photons

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO

LAGO Large Aperture GRB Observatory

Idea Detect GRB at high energy from the ground

Who? How? Where? Argentina Using WCD: In high altitude Bolivia Easy to calibrate mountain sites Mexico (> 4000 m) + France, Venezuela, Italy Detect Photons

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO

LAGO Large Aperture GRB Observatory

Idea Detect GRB at high energy from the ground

Who? How? Where? Argentina Using WCD: In high altitude Bolivia Easy to calibrate mountain sites Mexico (> 4000 m) + France, Venezuela, Italy Detect Photons

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Why going in altitude

Particles at ground level At 5200 m 100 × more signal 8 × more noise √ √ S/ N ≈ 35 ≈ 1600

1 detector at 5200 m ≈ 1600 Auger detectors at 1400 m

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Why going in altitude

Particles at ground level At 5200 m 100 × more signal 5200 m 8 × more noise √ √ S/ N ≈ 35 ≈ 1600

1400 m 1 detector at 5200 m ≈ 1600 Auger detectors at 1400 m

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Why going in altitude

Particles at ground level At 5200 m 100 × more signal 5200 m 8 × more noise √ √ S/ N ≈ 35 ≈ 1600

1400 m 1 detector at 5200 m ≈ 1600 Auger detectors at 1400 m

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Why going in altitude

Particles at ground level At 5200 m 100 × more signal 5200 m 8 × more noise √ √ S/ N ≈ 35 ≈ 1600

1400 m 1 detector at 5200 m ≈ 1600 Auger detectors at 1400 m

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Sensitivity vs Altitude and Size

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO Sites

Various sites Sierra Negra, Mexico Chacaltaya, Bolivia Auger South, Argentina

Detection in coincidence ◦ ∆Ω[Auger,Chacaltaya] ≈ 15

Other sites in Argentina and/or Venezuela?

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO Sites

Various sites Sierra Negra, Mexico Chacaltaya, Bolivia Auger South, Argentina

Detection in coincidence ◦ ∆Ω[Auger,Chacaltaya] ≈ 15

Other sites in Argentina and/or Venezuela?

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO Sites

Various sites Sierra Negra, Mexico Chacaltaya, Bolivia Auger South, Argentina

Detection in coincidence ◦ ∆Ω[Auger,Chacaltaya] ≈ 15

Other sites in Argentina and/or Venezuela?

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO Sites

Various sites Sierra Negra, Mexico Chacaltaya, Bolivia Auger South, Argentina

Detection in coincidence ◦ ∆Ω[Auger,Chacaltaya] ≈ 15

Other sites in Argentina and/or Venezuela?

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status LAGO Sites

Various sites Sierra Negra, Mexico Chacaltaya, Bolivia Auger South, Argentina

Detection in coincidence ◦ ∆Ω[Auger,Chacaltaya] ≈ 15

Other sites in Argentina and/or Venezuela?

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Pictures

Chacaltaya - 5300 m asl Sierra Negra - 4600 m asl

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Pictures

Chacaltaya - 5300 m asl Sierra Negra - 4600 m asl

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Pictures

Chacaltaya - 5300 m asl Sierra Negra - 4600 m asl

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Pictures II: Sierra Negra

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Prototype Detectors

Prototypes for Chacaltaya

Old prototype equipment from La Paz prototype Auger (EA): Electronics PMTs Commercial water tanks: 1 PMT per tank 6 tanks per electronic Software rewritten: 4 scalers per PMT 5 ms time sampling

Low cost

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Prototype Detectors

Prototypes for Chacaltaya

Old prototype equipment from La Paz prototype Auger (EA): Electronics PMTs Commercial water tanks: 1 PMT per tank 6 tanks per electronic Software rewritten: 4 scalers per PMT 5 ms time sampling

Low cost

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Prototype Detectors

Prototypes for Chacaltaya

Old prototype equipment from La Paz prototype Auger (EA): Electronics PMTs Commercial water tanks: 1 PMT per tank 6 tanks per electronic Software rewritten: 4 scalers per PMT 5 ms time sampling

Low cost

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Prototype Detectors

Prototypes for Chacaltaya

Old prototype equipment from La Paz prototype Auger (EA): Electronics PMTs Commercial water tanks: 1 PMT per tank 6 tanks per electronic Software rewritten: 4 scalers per PMT 5 ms time sampling

Low cost

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Prototype Detectors

Prototypes for Chacaltaya

Old prototype equipment from La Paz prototype Auger (EA): Electronics PMTs Commercial water tanks: 1 PMT per tank 6 tanks per electronic Software rewritten: 4 scalers per PMT 5 ms time sampling

Low cost

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Building Bariloche prototype: Nahuelito

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Current Status

Bariloche Sierra Negra Running 1 m2 prototype detector 14 m2 with runnning DAQ 2 × 1 m2 detectors Chacaltaya 3 × 4 m2 detectors 2 Running 1 m prototype detector More than 3 months of 2 4 m fiberglass tank in construction accumulated data

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Current Status

Bariloche Sierra Negra Running 1 m2 prototype detector 14 m2 with runnning DAQ 2 × 1 m2 detectors Chacaltaya 3 × 4 m2 detectors 2 Running 1 m prototype detector More than 3 months of 2 4 m fiberglass tank in construction accumulated data

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Current Status

Bariloche Sierra Negra Running 1 m2 prototype detector 14 m2 with runnning DAQ 2 × 1 m2 detectors Chacaltaya 3 × 4 m2 detectors 2 Running 1 m prototype detector More than 3 months of 2 4 m fiberglass tank in construction accumulated data

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Issues

Calibration at high altitude Light leaks

Use muon "shoulder" Lightning No muon decay Use one scaler below baseline

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Issues

Calibration at high altitude Light leaks

Use muon "shoulder" Lightning No muon decay Use one scaler below baseline

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Issues

Calibration at high altitude Light leaks

Use muon "shoulder" Lightning No muon decay Use one scaler below baseline

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Results for SN site

X. Bertou Cosmic Ray Detectors The Pierre Auger Observatory The Pierre Auger Observatory Water Cherenkov Detectors The Large Aperture GRB Observatory Gamma Ray Bursts Prototypes WCD GRB detection by WCD LAGO status Conclusion

Let’s start LAGO – Pico Espejo !

X. Bertou Cosmic Ray Detectors