TeV Particle Astrophysics 2010 Results from the HiRes Experiment Gordon Thomson University of Utah

Outline Introduction Some recent results –Spectrum –Composition –Anisotropy Summary

High Resolution Fly’s Eye (HiRes) Collaboration J. Boyer, B. Connolly, C.B. Finley, B. Knapp, E.J. Mannel, A. O’Neill, M. Seman, S. Westerhoff Columbia University J.F. Amman, M.D. Cooper, C.M. Hoffman, M.H. Holzscheiter, C.A. Painter, J.S. Sarracino, G. Sinnis, T.N. Thompson, D. Tupa Los Alamos National Laboratory J. Belz, M. Kirn University of Montana J.A.J. Matthews, M. Roberts University of New Mexico D.R. Bergman, G. Hughes, D. Ivanov, S.R. Schnetzer, L. Scott, B.T. Stokes, S. Stratton, G.B. Thomson, A. Zech Rutgers University N. Manago, M. Sasaki University of Tokyo R.U. Abbasi, T. Abu-Zayyad, G. Archbold, K. Belov, J. Belz, D.R. Bergman, A. Blake, Z. Cao, W. Deng, W. Hanlon, P. Huentemeyer, C.C.H. Jui, E.C. Loh, K. Martens,J.N. Matthews, D. Rodriguez, J. Smith, P. Sokolsky, R.W. Springer, B.T. Stokes, J.R. Thomas, S.B. Thomas, G.B. Thomson, L. Wiencke University of Utah

The Two HiRes Fluorescence Detectors HiRes1: atop Five Mile Hill 21 mirrors, 1 ring (3<altitude<17 degrees). Sample-and-hold electronics (pulse height and trigger time). HiRes2: Atop Camel’s Back Ridge 12.6 km SW of HiRes1. 42 mirrors, 2 rings (3<altitude<31 degrees). FADC electronics (100 ns period).

Mirrors and Phototubes 4.2 m 2 spherical mirror 16 x 16 array of phototubes,.96 degree pixels.

Reconstruction The trajectory of the EAS can be determined in one of two ways: 1.Monocular reconstruction using the arrival time of light signal at the detector. 2.Stereo by intersecting the shower- detector planes (SDP) seen from the two detector sites. 2.) 1.)

Spectrum and Composition Method Spectrum: aperture varies with energy. Must calculate with Monte Carlo method. –Trigger and thresholds very important. –Excellent accuracy is achievable. Composition: Monte Carlo simulations are essential to understand Xmax studies.

Compare Data to Monte Carlo: Judge success of simulation and acceptance calculation. Inputs to Monte Carlo: Fly’s Eye stereo spectrum; HiRes/Mia and HiRes Stereo composition; Library of Corsika showers. Detailed nightly information on trigger logic and thresholds, live mirrors, etc. Result: excellent simulation of the data, and an accurate aperture calculation.

5σ Observation of the Break in the Spectrum Broken Power Law Fits –Two BP with extension to test hypothesis that a break is present. Expect 43 events Observe 13 events Poisson probability: P(13;43) = 7x10 -8, which is 5.3  –The break is statistically significant. Break is at (5.6 ± 0.5) x eV; GZK expected between 5 and 6 x eV. The break is the true GZK cutoff. E -5.1

Use Berezinsky’s E ½ Method to Test E ½ is the energy where the integral spectrum falls below the power-law extension by a factor of 2. Berezinsky et al.: log 10 E ½ = 19.72, for a wide range of spectral slopes. Use 2 Break Point Fit with Extension for the comparison. log 10 E ½ = ± 0.07 Passes the test.

Local Density of Sources Theoretical predictions for spectrum shape agree with HiRes measurements. Compare HiRes spectrum slope above the GZK energy to Berezinsky et al. predictions: –Line 1: constant density. –Line 5: no sources within 10 Mpc. –Line 2: double density within 30 Mpc. Berezinsky, Gazizov, and Grigorieva, Phys. Rev. D74, (2006) (uses older HiRes spectrum)

Local Density of Sources Compare HiRes spectrum slope above the GZK energy to Berezinsky et al. predictions: –Line 1: constant density. –Line 5: no sources within 10 Mpc. –Line 2: double density within 30 Mpc. –Line 3: triple density within 30 Mpc. –HiRes: E -5.1 fall-off. More work is needed to make a better comparison, but... Constant density of sources is favored. Berezinsky, Gazizov, and Grigorieva, Phys. Rev. D74, (2006) (uses older HiRes spectrum) E -5.1

HiRes/Auger Spectra Comparison Auger confirms all spectral features of HiRes spectrum

Spectrum Summary The GZK cutoff is present. The first observation was by the HiRes experiment. All details of the spectrum indicate the composition is protons. –The energy of the GZK cutoff is as expected for protons. –Highest energy extragalactic cosmic rays travel > 50 Mpc. –The fall-off above the cutoff is evidence for a constant density of sources. CR’s travel a long distance. Spallation breaks up all nuclei at high energies  proton flux results. –The ankle has been observed by HiRes, at eV. The spectral index changes from -3.2 to -2.8 –Shape and energy of the ankle are consistent with e + e - production in collisions between extragalactic protons and photons of the CMBR.

More Direct Composition Measurement: use HiRes result on, and on σ(Xmax), indicate light composition. dependence is logarithmic: halfway is Be. Spallation at high energies breaks up light elements.  Composition is essentially all protons.

QGSJetII Protons Look Like Our Data ( points=data, histogram=MC) MC protons MC iron

Data (points) vs. QGSJet-II MC (histogram) Energy Bins: 18.3, 18.5

Energy Bins: 18.7, 18.9

Energy Bins: 19.1, 19.3

Energy Bins: 19.5, 19.7

Composition Summary The most direct indicator of composition is. Our data indicate a light composition, and favor protons. This is consistent with all of our spectrum information.

The Search for Anisotropy: Aim is to identify UHECR sources. Two methods: –Make a sky plot and look for bumps. –Look for correlations with known astronomical object types. All cosmic ray results are of marginal significance: –Sky plots: AGASA doublets/triplet at 40 EeV –Correlations: BL Lac’s at 10 EeV & AGN’s at 57 EeV

AGN Correlations Auger events’ correlations with AGN’s (south) –Early data set: scanned in (E min, θ, z max ) using Veron- Cetty+Veron catalog, found best correlations at (57 EeV, 3.1°,.018). –Tested correlation with later data set, found 8/13 events correlated, chance probability of (2.9σ). Not an “observation”: PRL requires 5 σ. Require confirmation. Auger test using later data: 42 events, 12 correlated, expect 8.8 random, 1 σ.  no effect.

HiRes Test of AGN Correlations (north) Choose Auger optimum point, same catalog. –2/13 events correlated (expect 3 randomly) –chance probability of 0.23  no effect. Scan the HiRes data –best point is (15.8 EeV, 2.5°, 0.016), 46/198 correlated. –chance probability of 0.29  no effect.

Test of Correlations with Local Large Scale Structure All results extragalactic, point source; energies of 10 (BL Lac), 40 (clusters), 57 EeV (AGN). Matter is not distributed uniformly within the horizon of 57 EeV protons  Search for correlations with local large scale structure for high energy events with relatively close horizons. A priori choice: 10, 40, 57 EeV. Also choose, a priori, to quote 95% CL.

HiRes Stereo Data HiRes complete stereo data set, angular resolution ~0.8° Events not within 10° of galactic plane: –10 above 57 EeV –27 above 40 EeV –310 above 10 EeV 6636 events in all

Local LSS Model Based on 2 Micron All-Sky Redshift Survey (2MRS) 1, a flux-limited sample of galaxies with m ≤ –Remove galactic plane (|b| < 10°) and objects within 5 Mpc. –Transform to a volume-limited sample by weighting. –Result is 15,508 galaxies between 5 and 250 Mpc. –Assume distribution is isotropic beyond 250 Mpc. 1. J. Huchra, L. Macri, T. Jarrett, et al., in preparation.

Procedure: set of MC events coming from LSS Start with local LSS model. Modify using HiRes aperture. Simulate the data set; find average predicted event density. Two parameters: –Minimum energy –Angular smearing to simulate magnetic fields Expect ~1°, extragalactic fields, for E≥40 EeV 1 Expect 2°-4°, galactic fields. Perform K-S test between data and expectation from LSS. Repeat starting with an isotropic galaxy distribution. 1. T. Kashti and E. Waxman, JCAP 0805, 006 (2008). 57 EeV 40 EeV 10 EeV Smearing angle of 6°

Sky Plots 10 EeV 40 EeV 57 EeV

Results Choose 95% c.l. exclusion to quote, a priori. For isotropic model, get good agreement. For local LSS model get poor agreement. Exclude correlation at 95% c.l. for θ s < 10°, E ≥ 40 EeV

LSS Conclusions We have searched for correlations between the pointing directions of HiRes stereo high energy events and local large scale structure. There are none at the 95% confidence level for magnetic smearing angles < 10°. This is very surprising. –One expects to see correlations. –One expects magnetic field smearing at the 4°-5° level. –With limited statistics we are able to place very significant limits. –Are the sources not in galaxies? Are magnetic field estimates wrong? This result should be confirmed by a future experiment (north). The Telescope Array Experiment is now collecting data. It has statistics equal to HiRes stereo (see TA talk, Yuichiro Tameda).

Summary HiRes made the first observation of the GZK cutoff. –It occurs at (5.6 ± 0.5 ± 0.9) x eV. –Flux α E -5.1 ± 0.7 above the cutoff. We see the “ankle” at eV. –E -3.3 below and E -2.8 above. The composition is very light, probably protons No AGN correlations are observed. Correlations with local large scale structure are very weak; magnetic fields may be larger than previously thought.