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The Auger Observatory was built to find the origin of UHE Cosmic Rays. Interesting because it is a genuine high energy frontier. Detects UHECRs by Extensive Air Showers EAS. What can you measure with EAS ? :. Energy Spectrum. Arrival Directions. Composition.

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Presentation Transcript
slide1

The Auger Observatory was built to find the origin of UHE Cosmic Rays

Interesting because it is a genuine high energy frontier

Detects UHECRs by Extensive Air Showers EAS.

What can you measure with EAS ? :

Energy Spectrum

Arrival Directions

Composition

This is all we’ve got to work with to solve the problem of origins.

slide2

Scientific Progress Seems hopeless :

But look at the Cosmic Micro-wave Background

We are only able to measure the same three things for incoming MBR photons.

Spectrum - Thermal

Age of Universe

Composition - Photons

Geometry of the space

Directionality - Slight anisotropy

Baryon fraction

etc

What we know about CRs now.

Spectrum – Non-Thermal power law.

Isotropic – with a hint at some anisotropy at the highest energies

Composition - ????

Doesn’t tell us much without composition – at the moment.

slide3

The Auger Cosmic Ray Observatory

Surface Array

1600 detector stations

1.5 Km spacing

3000 Km2

Fluorescence Detectors

4 Telescope enclosures

6 Telescopes per

enclosure

24 Telescopes total

slide4

The Auger Hybrid Observatory

Fluorescence Detector

6 Telescopes – 30ox30o field of view

10 m2 water cherenkov tank

slide6

Typical flash ADC trace

at about 2 km

Detector signal (VEM) vs time (µs)

Lateral density distribution

PMT 1

PMT 2

PMT 3

θ~ 48º, ~ 70 EeV

18 detectors triggered

Flash ADC traces

Flash ADC traces

slide8

How can composition measurements help in our quest for cosmic ray origins?

Two Divisions in UHECR theories of origin

Top-Down

Bottom-up

(Z-BurstModel).

UHE ns annihilate on relic ns and produce a Z boson, which decays into UHE photons and light hadrons.

Stochastic acceleration

(shock acceleration)

(SHDM Models )

Decay of super-heavy dark matter particles. [relic metastable particles] (SHDM Models) . Berezinsky (1997)

Charged particle flux

Possibility of heavy nuclei

(TD models)

Decay of relic Topological Defects

Cosmic Strings decay into UHE photons

Large Photon flux at High Energies

slide9

Look for the photons predicted by the Top Down models.

Composition information is reflected in shower development behavior.

(Also Muon content)

Vertical 1019 eV Corsika Simulations

(Example)

Different primary particle types produce showers that maximize at different depths. (different “Xmax’s”.

For a fixed energy.

Look for showers with deep Xmax.

slide10

Can we do this with the much larger SD data set?

Surface Detector parameters that correlate with Xmax :

I. Tank signal Rise-time t1/2 (at 1000m from the core)

Shower size grows to ½ maximum

Shower size grows to ½ maximum

Xmax

b

b

Xmax

a

a

Surface Station

Surface Station

Deep Xmax, ta-tb ~ t1/2 large.

Shallow Xmax, t1/2small.

t1/2 is weakly correlated with Xmax

slide11

II. Shower Front Radius of Curvature rc.

Shower axis

Xmax

Xmax

rc

rc

Ground level

Shallow Xmax, Large rc

rc is anti-correlated with Xmax

Deep Xmax, Smaller rc

Plan : Use the much more prolific SD data to search for photons. 10x the data as FD but less accurate.

  • Look for photon-induced showers with
  • Large t1/2 and
  • Small rc
slide12

Use Data from 1January 2004 to 31 December 2006.

Energies above 10 EeV

Zenith Angles between 30o and 60o

Integrated Aperture = 3130 km2 sr yr

~ 1 full array year

2761 events pass the quality cuts.

Procedure :

For each event form the deviation from the expectation for a photon shower.

Is the average of an ensemble of simulated photon showers with the same S(1000) and q as the recordedd event.

(X is either t1/2 or Rc)

slide13

Apply this same procedure to a spectrum-generated set of Monte Carlo photon showers.

a = 2

You get the greatest separation between photons and nuclears along this axis.

Find principle axis using first 5% of the data.

slide14

Remaining 95% of data is projected on to the principle axis.

Mean of photon distribution

Photon candidates lie above the dashed line.

There are no Photon candidates in the events above 10 EeV..

10EeV 20 EeV 40EeV

Photon Flux Limits

3.8x10-3 2.5x10-3 2.2x10-3 km-2sr-1yr-1

2.0% 5.1% 31%

Photon Fraction

slide15

Limits on Photon Fraction -

Most Top Down Models are disfavored but not ruled out

slide16

Photon Flux Limits compared to Top Down Model estimates

Top Down models clearly disfavored at all measured energies.

slide17

Bottom up theories – share acceleration mechanism but differ on what gets accelerated and what makes it into our detectors.

1. If the acceleration/injection region is benign (low radiation density) we might expect a nearly solar composition of nuclei to be accelerated and propagated.

2. Otherwise we might have only protons.

Measurement of Nuclear composition might thus lead us to an understanding of the injection/acceleration process.

Both cases predict the same features in the energy spectrum!

slide18

“dip” due to changing source distribution

Cut-off due to

GZK effect and

Nuclear breakup

Extra-galactic flux must be mixed to match all the features.

(Allard et. Al.)

slide19

“Dip” due to pair production

Off the MBR.

Cut-off due to

GZK effect

(Berezinsky et al)

slide20

The separation between nuclear species is quite small compared with photons.

Requires the accuracy of the Hybrid detector and direct measurement of EAS development.

Plan : Look at the average Xmax as a function of energy. Compare with Monte Carlo estimates.

slide21

Use hybrid data from December 2004 through April 2007

FD showers with at least one triggered SD station.

Quality cuts :

Xmax in field of view

Profile fit c2 pdf. <= 2.5

DXmax < 40 gm cm-2

DE/E < 20%

Min Viewing Angle > 20o

Geometrical cuts – minimize composition biases due to different detection efficiencies for different species.

4329 events remain after the cuts.

slide22

Data compared to EPOS1.6 Pure Composition Predictions

[Getting Heavier]

[Constant]

Best fit : two linear regions with a break in slope at 1018.35 eV

Mixed composition everywhere.

Constant comp. low energy : At high energy , getting heavier

slide23

Data Compared to QGSJET pure composition predictions

[Getting lighter]

[Constant]

Mixed composition everywhere

Getting lighter at low energy : Constant at high energy.

slide24

Bad news : composition behavior depends on what interaction model you use, and the different models do not agree.

Will have to use some additional composition handle to sort this out.

eg Dispersion in Xmax or Average Muon content.

Good news : All interaction models agree on a mixed composition everywhere.

The pure proton model is disfavored – even at this early stage.

slide25

Summary

Scientific progress has been made on finding the origin of UHE cosmic rays by composition studies

Searches for photons have produced flux limits which disfavor most Top-Down theories.

An analysis of average Xmax has found a mixed composition which disfavors a class of pure proton source models.

Future studies have to be performed to establish the mixed composition conclusion in a model-indepentent way.