UHE Cosmic Rays in the Auger Era UHE Cosmic Rays in the Auger Era - - PowerPoint PPT Presentation

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UHE Cosmic Rays in the Auger Era UHE Cosmic Rays in the Auger Era - - PowerPoint PPT Presentation

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Vulcano Workshop 2010 - May, 23-29, 2010 UHE Cosmic Rays in the Auger Era UHE Cosmic Rays in the Auger Era Sergio Petrera, L'Aquila University email: sergio.petrera@aquila.infn.it Vulcano Workshop 2010 - May, 23-29, 2010 UHE Cosmic Rays in the

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Vulcano Workshop 2010 - May, 23-29, 2010

UHE Cosmic Rays in the Auger Era UHE Cosmic Rays in the Auger Era

Sergio Petrera, L'Aquila University email: sergio.petrera@aquila.infn.it

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Vulcano Workshop 2010 - May, 23-29, 2010

UHE Cosmic Rays in the Auger Era UHE Cosmic Rays in the Auger Era

Sergio Petrera, L'Aquila University email: sergio.petrera@aquila.infn.it

Motivations Present status of the Pierre Auger Observatory The physics items: energy spectrum CR composition arrival directions Summary and outlook

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The interest for UHECRs in three points

transition galactic/extragalactic origin GZK effect pointing to the sources (particle astronomy !?) E > 1018 eV

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The interest for UHECRs in three points

transition galactic/extragalactic origin GZK effect pointing to the sources (particle astronomy !?) E > 1018 eV

The interest for UHECRs in three points

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The interest for UHECRs in three points

transition galactic/extragalactic origin GZK effect pointing to the sources (particle astronomy !?) E > 1018 eV

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The interest for UHECRs in three points

transition galactic/extragalactic origin GZK effect pointing to the sources (particle astronomy !?) E > 1018 eV

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The interest for UHECRs in three points

transition galactic/extragalactic origin GZK effect pointing to the sources (particle astronomy !?) E > 1018 eV

+ GZK  reduces the horizon

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AGASA: stopped Jan. 2004 HiRes: stopped Apr 2006 Auger: operating Telescope Array: starting

UHE UHE ankle GZK few/km sq per century

the all-particle spectrum

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AGASA: stopped Jan. 2004 HiRes: stopped Apr 2006 Auger: operating Telescope Array: starting

Exposures Exposures

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The Pierre Auger Observatory

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Auger South: the plan Auger South: the plan

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3000 km 3000 km2

2 area

area

Vulcano Workshop

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Nitrogen fluorescence detected as shower develops Particles detected as they reach ground

Fluorescence

Fluorescence (50 W light bulb @ c) (50 W light bulb @ c)

 nearly calorimetric  direct view of shower evolution  10% duty cycle  Acceptance depends on energy +

atmosphere

 Surface

Surface (10 (1012

12 particles over 20 km

particles over 20 km2

2)

)

 100% duty cycle  Flat acceptance above threshold  Indirect measurements of primary

energy and mass (relies on simulation)

Hybrid = surface + fluorescence Hybrid = surface + fluorescence

Auger detection techniques

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Observables at Auger

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Observables at Auger

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Observables at Auger

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SD energy calibration based on FD profiles “golden hybrid” events (independently detected) energy systematic error ~22 % mostly from systematics

  • f the FD detector

(fluorescence yield, atmospheric transparency...)

Energy Calibration

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Water Cherenkov tank

Rotomolded polyethylene tank 10 m2 x 1.2 m of ultrapure water in a light diffusing Tyvek liner, 3 PMTs Photonis (9’’ diameter); Autonomous unit: solar panel+battery, GPS timing, communication antenna, electronics Max 10 W power consumption

the Surface Detector

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Camera with 440 PMTs

(Photonis XP 3062)

Schmidt Telescope using 11 m2 mirrors UV optical filter (also: provide protection from outside dust)

the Fluorescence Detector

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Camera with 440 PMTs

(Photonis XP 3062)

UV optical filter (also: provide protection from outside dust) Schmidt Telescope using 11 m2 mirrors

the Fluorescence Detector

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Construction ended Apr. 2008 Enhancements for Detection @ Low Energies: HEAT (High Elevation Auger Telescopes) AMIGA (Auger Muon and Infill Array) + AERA array of radio detectors

Auger 2010

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Construction ended Apr. 2008 Enhancements for Detection @ Low Energies: HEAT (High Elevation Auger Telescopes) AMIGA (Auger Muon and Infill Array) + AERA array of radio detectors New R&D: MW fluorescence detection [after Gorham et al., PR D 78 (2008) 032007] Towards an FD with 100% duty cycle?

Auger 2010

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ENERGY SPECTRUM ENERGY SPECTRUM

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PLB 685 (2010) 239

the Energy Spectrum

Cutoff at ~1019.6 eV significant with > 30

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PLB 685 (2010) 239

the Energy Spectrum

Cutoff at ~1019.6 eV significant with > 30

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the Energy Spectrum

Within the energy scale systematics

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Comparison to Source Models

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MASS COMPOSITION MASS COMPOSITION

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photons protons Fe Energy Xmax

Mass Composition: the principle

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photons protons Fe Data Energy Xmax Xmax

Mass Composition: the principle

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Elongation Rate Measurement

Auger and HiRes Xmax measurements are compatible within systematic uncertainties

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Comparison with Hadronic Models

⇒ Mass composition getting heavier HiRes PRL 2010 “proton dominance above 1.6 EeV” but... difficult to compare with HiRes due to different definitions

  • f observables.

PRL 104 (2010) 091101

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Comparison with Hadronic Models

PRL 104 (2010) 091101

More about Mass Composition by Analisa Mariazzi

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Photons: upper limits

Top down models strongly constrained

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Neutrinos: Earth skimming ντ

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ARRIVAL DIRECTIONS ARRIVAL DIRECTIONS

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Typical accuracy of reconstruction <1°

No significant emission from Galactic Centre No broadband signals – e.g. Dipole – at any energy above 1 EeV e.g 1 < E < 3 EeV, Amplitude < 0.7% No clustering of the type claimed by AGASA No signal from BL Lacs as possibly seen by HiRes Summary: Previous reports have not been confirmed Summary: Previous reports have not been confirmed ICRC 2007

Initial Anisotropy Searches

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Correlation with AGN's (2007)

Based on a Prescribed Anisotropy Test: Correlation with Veron-Cetty-Veron AGN Catalog

20 out of 27 events E>57 EeV correlating within 3.1 degrees with z<0.017 AGN's Isotropy rejected with >99% C.L.

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Update of the Prescribed Anisotropy Test (correlation with VCV catalog of AGNs) 38% (21/55) correlate (post exploration) vs. 21% expected from isotropy correlation decreased but still incompatible with isotropy at 99% C.L.

Correlation with AGN's (2010)

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More results on Correlations

New paper in preparation: new catalogs, autocorrelation, CenA preliminary

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Summary...

High quality results on all the observables of UHECR's A comprehensive interpretation of the whole data still missing

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Summary...

High quality results on all the observables of UHECR's A comprehensive interpretation of the whole data still missing

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Summary...

High quality results on all the observables of UHECR's A comprehensive interpretation of the whole data still missing

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Summary...

High quality results on all the observables of UHECR's A comprehensive interpretation of the whole data still missing Much work to do... many more data....

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… and Outlook

What's coming next?What's coming next?

A new observatory: TA (Telescope Array) Auger South: low energy extension HEAT (3 high elevation telescopes) AMIGA (SD infill + muon detectors) +... Auger North: at Lamar (CO) undergoing evaluation Go to space!

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… and Outlook

What's coming next?What's coming next?

A new observatory: TA (Telescope Array) TA (Telescope Array) Auger South: low energy extension HEAT (3 high elevation telescopes) AMIGA (SD infill + muon detectors) +... Auger North: at Lamar (CO) undergoing evaluation Go to space!

30 km

576 scintillator detectors 1.2 km interval

3 FD stations (atmospheric fluorescence telescopes) 3 (+2) Communication Towers ~2.5 hours from SLC

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… and Outlook

What's coming next?What's coming next?

A new observatory: TA (Telescope Array) TA (Telescope Array) Auger South Auger South: low energy extension HEAT (3 high elevation telescopes) AMIGA (SD infill + muon detectors) +... Auger North: at Lamar (CO) undergoing evaluation Go to space!

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… and Outlook

What's coming next?What's coming next?

A new observatory: TA (Telescope Array) TA (Telescope Array) Auger South Auger South: low energy extension HEAT (3 high elevation telescopes) AMIGA (SD infill + muon detectors) +... Auger North Auger North: at Lamar (CO) undergoing evaluation Go to space!

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Auger North

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Auger North: comparison with other expts

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Auger North: correlations above 60 EeV

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Photon search

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Auger North: Photon search

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… and Outlook

What's coming next?What's coming next?

A new observatory: TA (Telescope Array) TA (Telescope Array) Auger South Auger South: low energy extension HEAT (3 high elevation telescopes) AMIGA (SD infill + muon detectors) +... Auger North Auger North: at Lamar (CO) undergoing evaluation Go to space! Go to space!

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… and Outlook

What's coming next?What's coming next?

A new observatory: TA (Telescope Array) TA (Telescope Array) Auger South Auger South: low energy extension HEAT (3 high elevation telescopes) AMIGA (SD infill + muon detectors) +... Auger North Auger North: at Lamar (CO) undergoing evaluation Go to space! Go to space!

Thanks