Performance of CRTNT forSub-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

Motivation

• UHEτneutrinos

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

• Sub-EeV Cosmic Rays

UHECR Energy Spectrum Structure

No Absolute Calibration

Poor Measurement on Composition

HiRes/MIA, HeverahPark,Cerenkov etc

CR arrival direction: Anisotropy

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

UHECR Research Strategyco-site, cross-calibration ,dedicate

TA/AugerTALECRTNT X

access?

CRTNT Detector Design& Prototype

• Mobile

• High sensitivity

• Big dynamic range

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%

Detector Structure

• Remote control door

• 256 pixels

• On board FADC electronics

• UV filter

• ~5m2 spherical Al reflector

Main tower detector12 telescopes

64º

21º 35º

10m 7m

F/C light Detector

Linux box

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

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)

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

Characteristics of pulses

1000 events: 6X107GeV <E< 3X109GeV

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

LG

HG

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.

Simulation & Performance

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

CRTNT Configuration

• Portable fluorescence detectors

• 3 site stereo

(12+2+2)

8km

3km

1-12

W1,2 E1,2

Cerenkov/edge events

Aperture of CRTNT

Impact Parameter

to the Tower Detector

AzimuthAngle

distribution

Zenith angle

distribution

Event distribution

Event Rate

Shower angular resolution

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