Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC...

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Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005

Transcript of Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC...

Page 1: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Performance of CRTNT forSub-EeV Cosmoc Ray Measurement

Zhen Cao IHEP, Beijing & Univ. of Utah, SLC

Aspen, CO, 04/2005

Page 2: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Outline

• Motivation of CRTNT project

• Design of CRTNT

• Status of prototype detector construction

• Simulation

• Aperture and event rate

• Conclusion

Page 3: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Motivation

• UHEτneutrinos

(Z.Cao et al., J. Phys. G: 31 (2005) 571-582)

• Sub-EeV Cosmic Rays

Page 4: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

UHECR Energy Spectrum Structure

Page 5: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

No Absolute Calibration

Page 6: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Poor Measurement on Composition

Page 7: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

HiRes/MIA, HeverahPark,Cerenkov etc

Page 8: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

CR arrival direction: Anisotropy

Page 9: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Millard CountyUtah/USA

~600 Scintillators(1.2 km spacing)

AGASA x 9

3 x Fluorescence StationsAGASA x 4

phase-1 TA Detector Configuration

Exp Res.

AGASA

1.60

TA SD ~1.00

TA FD 0.60

TA Hyb.

0.40

Low Energy ExtensionOf TA in Hybrid

TALETALE

TA

Page 10: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

UHECR Research Strategyco-site, cross-calibration ,dedicate

TA/AugerTALECRTNT X

access?

Page 11: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

CRTNT Detector Design& Prototype

• Mobile

• High sensitivity

• Big dynamic range

Page 12: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

CRTNT DetectorCRTNT Detector

2.3m

2.3m

3.0m

•Shower imaging camera:

16x16 40mm hexagonal

Photonis PMT array

•A half of Connex box

•20 Φ600mm spherical

mirror, reflectivity 82%

Page 13: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Detector Structure

• Remote control door

• 256 pixels

• On board FADC electronics

• UV filter

• ~5m2 spherical Al reflector

Page 14: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Main tower detector12 telescopes

64º

21º 35º

10m 7m

Page 15: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

F/C light Detector

Linux box

Page 16: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Detector Design: OpticsSpherical mirror: R=4490mmFocal plane camera: D=2305mmHexagonal pixel size: A=40mmMirror reflectivity: R=82%UV filter transmission: T=80%Physical optical spot: about the size of the pixel

Page 17: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Trigger/read out Electronics

50 MHz 10 bit FADC: High gain: 3 count/peLow gain: 0.3 count/pe

FPGA: single channel trigger 3.5σ

Digital adjustable HV supply 4 pole filter, x 30 Amp (H) x 3 Amp (L)

Page 18: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Detector Design: Electronics

848 pe440 ns

160 pe240 ns

• sky noise background: 40 photon/μsec/m2

• single channel trigger: signal/noise ratio>3.5σ• 320 ns running widow• 3 histories of 6μsec per event stored

320 ns window320 ns window

Page 19: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Characteristics of pulses

1000 events: 6X107GeV <E< 3X109GeV

Pulse Width (ns) # of pe’s per 20 ns bin

LG

HG

Page 20: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Status of Prototype Construction

• $0.3M for two prototype telescopes• 512 PMT’s calibration by Aug., • 2 modified connext boxes by June• 40 Φ600mm mirrors mounted by Aug.• Analog electronics by July.• Single channel trigger digital board by Sept.• 10 m2 UV filter by Sept.• Event trigger board & I/O by Nov.

Page 21: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Simulation & Performance

Page 22: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Simulation for CRTNT

• Detector configuration (3 site stereo)

• Proton primary

• Corsika+QGSJet based parameterization

• Single channel (tube) trigger: 3.5σ

• Telescope trigger: any 6 channels

• Event trigger: main tower && (one of sides)

• Cuts: edge events, Cerenkov light events

Page 23: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

CRTNT Configuration

• Portable fluorescence detectors

• 3 site stereo

(12+2+2)

8km

3km

1-12

W1,2 E1,2

Page 24: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Cerenkov/edge events

Page 25: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Aperture of CRTNT

Page 26: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Impact Parameter

to the Tower Detector

Page 27: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

AzimuthAngle

distribution

Page 28: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Zenith angle

distribution

Page 29: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Event distribution

Page 30: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Event Rate

Page 31: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Shower angular resolution

Page 32: Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005.

Conclusion

• The CRTNT is dedicated to the “second knee”

• All components for prototype are ordered

• Constr. /Testing in lab until the end of this year

• On-site testing/calibration/background next year

• Simulated aperture ~ 30 km2 sr @ 0.1EeV

• 20k events per year (>0.1EeV, flat aperture)

• 550 events per yr (>1EeV, full aperture) for cross-calibration with TALE