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Results from the Telescope Array Experiment Charlie Jui University - - PowerPoint PPT Presentation

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Results from the Telescope Array Experiment Charlie Jui University of Utah TeVPA 2013 Irvine, CA Aug. 27, 2013 http://www.physics.utah.edu/~jui/ta-tevpa2013.pdf TA, TeVPA2013 1 Telescope Array Collaboration T. Abu-Zayyad a , M. Allen a , R.

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Results from the Telescope

Array Experiment

Charlie Jui

University of Utah TeVPA 2013 Irvine, CA

  • Aug. 27, 2013

http://www.physics.utah.edu/~jui/ta-tevpa2013.pdf

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aaHiroshima City University, abAdvanced Science Institute, RIKEN, acNational Institute of Radiological Science, adEhime University

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  • T. Abu-Zayyada, M. Allena, R. Andersona, R. Azumab, E. Barcikowskia, J. W. Belza, D. R. Bergmana,
  • S. A. Blakea, R. Cadya, M. J. Chaec, B. G. Cheond, J. Chibae, M. Chikawaf, W. R. Chog, T. Fujiih, M. Fukushimah,i,
  • K. Gotoj, W. Hanlona， Y. Hayashij, N. Hayashidak, K. Hibinok, K. Hondal, D. Ikedah, N. Inouem, T. Ishiil,
  • R. Ishimorib, H. Iton, D. Ivanova,o, C. C. H. Juia, K. Kadotap, F. Kakimotob, O. Kalashevq, K. Kasaharar, H. Kawais,
  • S. Kawakamij, S. Kawanam, K. Kawatah, E. Kidoh, H. B. Kimd, J. H. Kima, J. H. Kimd, S. Kitamurab, Y. Kitamurab,
  • V. Kuzminq, Y. J. Kwong, J. Lana, J.P. Lundquista, K. Machidal, K. Martensi, T. Matsudat, T. Matsuyamaj,
  • J. N. Matthewsa, M. Minaminoj, K. Mukail, I. Myersa, K. Nagasawam, S. Nagatakin, T. Nakamurau, H. Nanpeij,
  • T. Nonakah, A. Nozatof, S. Ogioj, S. Ohc, M. Ohnishih, H. Ohokah, K. Okih, T. Okudav, M. Onon, A. Oshimaj,
  • S. Ozawar, I. H. Parkw, M. S. Pshirkovx, D. C. Rodrigueza, G. Rubtsovq, D. Ryuy, H. Sagawah, N. Sakuraij,
  • A. L. Sampsona, L. M. Scotto, P. D. Shaha, F. Shibatal, T. Shibatah, H. Shimodairah, B. K. Shind, T. Shirahamam,
  • J. D. Smitha, P. Sokolskya, R. W. Springera, B. T. Stokesa, S. R. Strattona,o, T. A. Stromana, M. Takamurae,
  • A. Taketaz, M. Takitah, Y. Tamedak, H. Tanakaj, K. Tanakaaa, M. Tanakat, S. B. Thomasa,
  • G. B. Thomsona, P. Tinyakovq,x, I. Tkachevq, H. Tokunob, T. Tomidaab, S. Troitskyq, Y. Tsunesadab, K. Tsutsumib,
  • Y. Uchihoriac, F. Urbanx, G. Vasiloffa, Y. Wadam, T. Wonga, H. Yamaokat, K. Yamazakij, J. Yangc,
  • K. Yashiroe, Y. Yonedaj, S. Yoshidas, H. Yoshiiad, R. Zollingera, Z. Zundela

aUniversity of Utah, bTokyo Institute of Technology, cEwha Womans University, dHanyang University, eTokyo University of Science, fKinki University, gYonsei University, hInstitute for Cosmic Ray Research, Univ. of Tokyo, iKavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, the University of Tokyo, jOsaka City University, kKanagawa University, lUniv. of Yamanashi, mSaitama University, nAstrophysical Big Bang Laboratory, RIKEN,

  • Rutgers University, pTokyo City University, qInstitute for Nuclear Research of the Russian Academy of Sciences, rWaseda University,

sChiba University, tInstitute of Particle and Nuclear Studies, KEK, uKochi University, vRitsumeikan University, wSungkyunkwan University, xUniversite Libre de Bruxelles, yChungnam National University, zEarthquake Research Institute, University of Tokyo,

Telescope Array Collaboration

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TA, TeVPA2013

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aaHiroshima City University, abAdvanced Science Institute, RIKEN, acNational Institute of Radiological Science, adEhime University

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  • T. Abu-Zayyada, M. Allena, R. Andersona, R. Azumab, E. Barcikowskia, J. W. Belza, D. R. Bergmana,
  • S. A. Blakea, R. Cadya, M. J. Chaec, B. G. Cheond, J. Chibae, M. Chikawaf, W. R. Chog, T. Fujiih, M. Fukushimah,i,
  • K. Gotoj, W. Hanlona， Y. Hayashij, N. Hayashidak, K. Hibinok, K. Hondal, D. Ikedah, N. Inouem, T. Ishiil,
  • R. Ishimorib, H. Iton, D. Ivanova,o, C. C. H. Juia, K. Kadotap, F. Kakimotob, O. Kalashevq, K. Kasaharar, H. Kawais,
  • S. Kawakamij, S. Kawanam, K. Kawatah, E. Kidoh, H. B. Kimd, J. H. Kima, J. H. Kimd, S. Kitamurab, Y. Kitamurab,
  • V. Kuzminq, Y. J. Kwong, J. Lana, J.P. Lundquista, K. Machidal, K. Martensi, T. Matsudat, T. Matsuyamaj,
  • J. N. Matthewsa, M. Minaminoj, K. Mukail, I. Myersa, K. Nagasawam, S. Nagatakin, T. Nakamurau, H. Nanpeij,
  • T. Nonakah, A. Nozatof, S. Ogioj, S. Ohc, M. Ohnishih, H. Ohokah, K. Okih, T. Okudav, M. Onon, A. Oshimaj,
  • S. Ozawar, I. H. Parkw, M. S. Pshirkovx, D. C. Rodrigueza, G. Rubtsovq, D. Ryuy, H. Sagawah, N. Sakuraij,
  • A. L. Sampsona, L. M. Scotto, P. D. Shaha, F. Shibatal, T. Shibatah, H. Shimodairah, B. K. Shind, T. Shirahamam,
  • J. D. Smitha, P. Sokolskya, R. W. Springera, B. T. Stokesa, S. R. Strattona,o, T. A. Stromana, M. Takamurae,
  • A. Taketaz, M. Takitah, Y. Tamedak, H. Tanakaj, K. Tanakaaa, M. Tanakat, S. B. Thomasa,
  • G. B. Thomsona, P. Tinyakovq,x, I. Tkachevq, H. Tokunob, T. Tomidaab, S. Troitskyq, Y. Tsunesadab, K. Tsutsumib,
  • Y. Uchihoriac, F. Urbanx, G. Vasiloffa, Y. Wadam, T. Wonga, H. Yamaokat, K. Yamazakij, J. Yangc,
  • K. Yashiroe, Y. Yonedaj, S. Yoshidas, H. Yoshiiad, R. Zollingera, Z. Zundela

aUniversity of Utah, bTokyo Institute of Technology, cEwha Womans University, dHanyang University, eTokyo University of Science, fKinki University, gYonsei University, hInstitute for Cosmic Ray Research, Univ. of Tokyo, iKavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, the University of Tokyo, jOsaka City University, kKanagawa University, lUniv. of Yamanashi, mSaitama University, nAstrophysical Big Bang Laboratory, RIKEN,

  • Rutgers University, pTokyo City University, qInstitute for Nuclear Research of the Russian Academy of Sciences, rWaseda University,

sChiba University, tInstitute of Particle and Nuclear Studies, KEK, uKochi University, vRitsumeikan University, wSungkyunkwan University, xUniversite Libre de Bruxelles, yChungnam National University, zEarthquake Research Institute, University of Tokyo,

Telescope Array Collaboration

~120 collaborators in 5 countries Japan, USA, Korea, Russia, Belgium

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TA, TeVPA2013

Telescope Array Experiment

  • TA is a ultrahigh energy

(>1017 eV) cosmic ray

  • bservatory located in

the West Desert of Utah: largest in the northern hemisphere

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TARA (TA Radar)

  • An R&D project to observe radar reflections form cosmic

ray air showers

  • TARA1.5
  • April 2011 to July 2012
  • 54.1 MHz @ 1.5 kW
  • TARA40
  • Summer 2013~
  • 54.1 MHz @ 40 kW

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TARA Presentations at TeVPA2013:

  • Tue. Aug 27

14:24 Jordan HANSON 14:48: Samridha KUNWAR

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TA, TeVPA2013

  • 1. Introduction to Telescope Array
  • 2. Data Analysis Techniques
  • 3. Energy Spectrum
  • 4. Composition
  • 5. Photons and Neutrinos ???
  • 6. Anisotropy

Outline

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TA is a hybrid experiment

  • 507 scintillation

counters surface detector (SD)

– Covers 730 km2.

  • 3 fluorescence

detector (FD) stations

– Located at the corners

  • f the SD array

TA Detectors

Middle Drum FD Black Rock FD Long Ridge FD

  • 1. Introduction
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Scintillation Counters

Pre-assembled in Japan, Final Assby/testing in Delta: 2 layers, 1.25 cm scintillator, 3m2 area

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Scintillator Detectors on a 1.2 km square grid

  • Power: Solar/Battery
  • Readout: Radio
  • Self-calibrated:

µ background

  • Operational: 3/2008
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Long Ridge Black Rock Mesa Middle Drum Refurbished from HiRes-I New FDs

6.8 m2 ~1 m2

14 telescopes@station 256 PMTs/camera

5.2 m2

TA Fluorescence Detectors

Observations since ~10/2007 Observation since ~11/2007 Observation since ~6/2007 12 telescopes/station 256 PMTs/camera Hamamatsu R9508 FOV~15x18deg

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TA, TeVPA2013

Example Event from 2008-10-26

MD LR BR SD

θ [o] φ [o] x[km] y[km] MD mono

51.43 73.76 7.83

  • 3.10

BR mono

51.50 77.09 7.67

  • 4.14

Stereo BR&LR

50.21 71.30 8.55

  • 4.88
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FD Geometrical Reconstruction

2. 1.

2 tan

i i

c R t t

P

θ + =

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. By intersecting the shower-detector

planes (SDP) seen from the two detector sites.

  • 2. Data Analysis
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Measurement of a fluorescence Event

Event Display

Black Rock Mesa

Monocular timing fit Reconstructed Shower Profile

Fluorescence Direct (Cerenkov) Rayleigh scatt. Aerosol scatt.

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Hybrid Reconstruction

Primary Cosmic Ray UV Fluorescence Photons Isotropic Emission Charged Particles Electromagnetic Shower

  • 3. Hybrid reconstruction:

Incorporating timing information

  • f SD into FD geometry fit

BLACK: Fluorescence Telescope PMT RED: Surface Detector “Virtual” PMT FD mono has ~5° ang. resolution Adding SD  ~0.5° resolution. ( Stereo FD resolution ~0.5° )

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r = 800m

Analyzing SD Event

Lateral Density Distribution Fit Geometry Fit (modified Linsley)

Fit with AGASA LDF

  • S(800): Primary Energy
  • Zenith attenuation by MC

2008/Jun/25 - 19:45:52.588670 UTC

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Surface Array Energy Measurement

  • Energy table is

constructed using the MC (CORSIKA)

  • Determination of

event energy by interpolating between S800 vs. sec(θ) lines

  • Uses novel “de-

thinning” of CORSIKA (paper draft in internal review)

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TA, TeVPA2013 Differential flux multiplied by E3 To highlight the subtle features in a steeply falling spectrum

AGASA: continuing spectrum seen HiRes: GZK suppression At 5σ significance

  • The TA Collaboration was in part a merger of the High Resolution

Fly’s Eye (HiRes) and the Akeno Giant Air Shower Array (AGASA)

AGASA flux systematically ~50% higher than HiRes

  • 3. Energy Spectrum of UHECR
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FD energy EFD SD energy ESD (scaled to FD energy) 𝐹𝐹𝑇𝑇𝑇𝑇 = 𝐹𝐹′𝑇𝑇𝑇𝑇/1.27 Hybrid events E > 1019 eV Angular resolution = 1.4o E > 1019 eV Energy resolution < 20%

Energy Scale Check and resolution

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TA data May, 2008 – May, 2013 Zenith angle < 45o 14787 ev. (E > 1018.2 eV) Exposure 4500 km2 sr yr

5 year TA SD spectrum

Broken power law fit

4-year TA surface detector spectrum Astrophysical Journal Letters 768 L1 (2013)

July, 2013

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Spectrum Summary

TA Monocular FD spectrum papers Astroparticle Physics 39–40 (2012) 109–119 Astroparticle Physics 48 (2013) 16–24 TA Hybrid Spectrum papers arXiv:1305.7273 [astro-ph.HE], submitted to Astroparticle Physics

Doug Bergman for the TA Colaboration: ICRC 2013 http://143.107.180. 38/indico/getFile.py /access?contribId=2 21&sessionId=3&res Id=0&materialId=sli des&confId=0

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Significance and energy of suppression

TA SD 5-year

Locations of the “ankle/dip” and of the suppression are consistent with interaction of protons with the CMBR

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HiRes: Phys.Rev.Lett.104:161101,2010 (with Xmax data suppl.)

consistent with predominately light (protons) composition

Hybrid Stereo

AUGER: Phys.Rev.Lett.104:091101,2010 Suggests shift to heavier composition at higher energies:

  • 4. Composition
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LR BR

Fluorescence Cherenkov

Camera images

Longitudinal Shower Profiles

TA Stereo Composition

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<Xmax> vs LogE

  • Y. Sunesada for the TA Collaboration

ICRC2013 http://143.107.180.38/indico/getFile.py /access?contribId=132&sessionId=3&re sId=0&materialId=slides&confId=0

5-year data (Nov., 2007 – Nov. 2012)

TA data consistent with (QGSJET-II.3) protons

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Comparing Xmax Distribution with MC p/Fe expectations: Stereo

TA data consistent with (QGSJET-II.3) protons

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Comparing Xmax Distribution with MC p/Fe expectations: Stereo

TA data consistent with (QGSJET-II.3) protons

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Comparing Xmax Distribution with MC p/Fe expectations: Stereo

TA data consistent with (QGSJET-II.3) protons

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Hybrid Analysis <Xmax> vs LogE

4-year data (May, 2008 – May, 2012)

TA data consistent with (QGSJET-II.3) protons

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Comparing Xmax Distribution with MC p/Fe expectations: Hybrid

TA data consistent with (QGSJET-II.3) protons

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TA Surface Detector Photon Search

a = Linsley curvature parameter small a large a

  • G. Rubtsov for the TA Collaboration

ICRC 2013 http://143.107.180.38/indico/getFile. py/access?contribId=149&sessionId=3 &resId=0&materialId=slides&confId=0

  • 5. Photons and Neutrino Search
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γ MC

TA Data TA Data

γ MC γ MC

arXiv:1304.5614 [astro-ph.HE] Submitted to Phys Rev D

TA Data

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TA SD Neutrino Search

Surface Detector Recorded Waveforms Neutrinos primaries produce YOUNG (many peaks in waveform) but HIGHLY INCLINED showers

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TA PREIMINARY ICRC 2013

NO INCLINED YOUNG showers in TA data  ZERO neutrino candidates

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Search based on 3.3 year (May 2008-Sep 2011) data published: Astrophysical Journal, 757:26 (2012) zenith < 45 deg Results were consistent with Isotropic Source Model

E>10 EeV 988 events E>40 EeV 57 events E>57 EeV 25 events

Equatorial Coordinates

  • 6. Anisotropy
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TA Anisotrpy Update 2013

5 full years of Data: May 2008 – May 2013 Zenith < 55 deg E>10 EeV: 2130 events E>40 EeV: 132 events E>57 EeV: 52 events

Angular resolution better than 1.5 deg. Energy resolution ~20%

Results are still largely consistent with isotropy, but…

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E > 57 EeV, SuperGalactic coordinates

SuperGalactic Longitude (deg) SuperGalactic Latitude (deg)

Hot Spot?

K.S. p = 0.003 K.S. p = 0.06

  • P. Tinyakov for the TA

Collaboration ICRC 2013 http://143.107.180.38/in dico/getFile.py/access?c

  • ntribId=1033&sessionId

=3&resId=0&materialId= slides&confId=0

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P(δ) = Probability that the observed number

  • f pairs (at <δ) occurs

by chance from an isotropic distribution Small P(δ): Clustering at angular scale ~δ P(δ)~0.004 at δ~20o for E > 57 EeV

Separation angle

0.004

Clustering (autocorrelation)

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E > 10 EeV: 2130 events E > 40 EeV: 132 events E > 57 EeV: 52 events White dots: 5-year TA data with zenith angle < 55 deg. Gray patterns: expected flux density from proton LSS 2MASS Galaxy Redshift catalog (XSCz)

Comparison with Large-Scale Structure (LSS)

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E > 10 EeV E > 40 EeV E > 57 EeV

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Theta: deflection angle

Comparison with Large-Scale Structure (LSS) Need more data!

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  • TA Energy spectrum consistent with light composition

– ***TA surface scintillator array consistent with GZK cut-off

  • Preliminary <Xmax> composition result from both

stereo and hybrid analyses consistent with light (proton) composition

  • No UHE photon or neutrino
  • TA SD data largely consistent with isotropy

– Small Excess seen in SG – Hint of Clustering at ~20 deg – Marginally incompatible with isotropy at E>57 EeV but compatible with Large Scale Structure (LSS)

  • TA Low Energy Extension (TALE) nearly completed
  • Plans for TAx4 expansion

Conclusions

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Correlations with AGN

  • 472 AGN from 2006 Veron catalog with z < 0.018
  • E > 57 EeV, zenith angle < 45o, N = 42 (5 yr)
  • Separation angle = 3.1o
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Correlations with AGN

  • Probability to hit AGN with a single event po = 0.24
  • 17 events correlate out of 42 ⟹ p = 0.014

Astrophysical Journal, 757:26 (2012)

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  • A project to expand the TA

surface detector by a factor of 4 (~3000 km2)

  • 500 more scintillation counters

with 2.08 km spacing

  • A fluorescence detector of 10

telescopes from HiRes telescopes

  • The proposal is being prepared

for submission in fall, 2013.

  • Anisotropy studies with more

significance

  • By March, 2019
  • 20 TA years of SD data
  • 14 TA years of hybrid data

TA×4 Expansion

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