The system of DAQ for TA surface array

Shunsuke Ozawa; H. Ohoka; M. Takeda; N. Sakurai; S. Yoshida; S. Kawakami; H. Tanaka

The system of DAQ for TA surface array

Shunsuke Ozawa, H. Ohoka, M. Takeda, N. Sakurai, S. Yoshida, S. Kawakami, H. Tanaka

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

The installation of The Telescope Array experiment started in earnest. Since observation by combine two different type air shower detector, we aim to search super GZK cosmic ray and determine accurately the energy of these CRs. In past, extensive air shower observations using scintillation detector array give many good results Utilize these experience, we combine scintillator array and fluorescence detectors for determination for EAS energy scale, core position and incoming direction. In this paper, we introduce the electronics and data acquisition system for our scintillator array; call Surface Detector (SD). The engineering array that constituted 18 scintillation detectors was installed on December 2004. We have tested our electronics and DAQ on this small array. Complete SD will have 576 detectors, around 900 km². This will be about 9 times larger than AGASA.

Original language	English
Title of host publication	29th International Cosmic Ray Conference, ICRC 2005
Publisher	Tata Institute of Fundamental Research
Pages	177-180
Number of pages	4
Volume	8
Publication status	Published - 2005
Externally published	Yes
Event	29th International Cosmic Ray Conference, ICRC 2005 - Pune, India Duration: 2005 Aug 3 → 2005 Aug 10

Other

Other	29th International Cosmic Ray Conference, ICRC 2005
Country/Territory	India
City	Pune
Period	05/8/3 → 05/8/10

ASJC Scopus subject areas

Nuclear and High Energy Physics

Cite this

@inproceedings{c696bec71e914528a5890d18605d0bff,

title = "The system of DAQ for TA surface array",

abstract = "The installation of The Telescope Array experiment started in earnest. Since observation by combine two different type air shower detector, we aim to search super GZK cosmic ray and determine accurately the energy of these CRs. In past, extensive air shower observations using scintillation detector array give many good results Utilize these experience, we combine scintillator array and fluorescence detectors for determination for EAS energy scale, core position and incoming direction. In this paper, we introduce the electronics and data acquisition system for our scintillator array; call Surface Detector (SD). The engineering array that constituted 18 scintillation detectors was installed on December 2004. We have tested our electronics and DAQ on this small array. Complete SD will have 576 detectors, around 900 km2. This will be about 9 times larger than AGASA.",

author = "Shunsuke Ozawa and H. Ohoka and M. Takeda and N. Sakurai and S. Yoshida and S. Kawakami and H. Tanaka",

year = "2005",

language = "English",

volume = "8",

pages = "177--180",

booktitle = "29th International Cosmic Ray Conference, ICRC 2005",

publisher = "Tata Institute of Fundamental Research",

note = "29th International Cosmic Ray Conference, ICRC 2005 ; Conference date: 03-08-2005 Through 10-08-2005",

}

TY - GEN

T1 - The system of DAQ for TA surface array

AU - Ozawa, Shunsuke

AU - Ohoka, H.

AU - Takeda, M.

AU - Sakurai, N.

AU - Yoshida, S.

AU - Kawakami, S.

AU - Tanaka, H.

PY - 2005

Y1 - 2005

N2 - The installation of The Telescope Array experiment started in earnest. Since observation by combine two different type air shower detector, we aim to search super GZK cosmic ray and determine accurately the energy of these CRs. In past, extensive air shower observations using scintillation detector array give many good results Utilize these experience, we combine scintillator array and fluorescence detectors for determination for EAS energy scale, core position and incoming direction. In this paper, we introduce the electronics and data acquisition system for our scintillator array; call Surface Detector (SD). The engineering array that constituted 18 scintillation detectors was installed on December 2004. We have tested our electronics and DAQ on this small array. Complete SD will have 576 detectors, around 900 km2. This will be about 9 times larger than AGASA.

AB - The installation of The Telescope Array experiment started in earnest. Since observation by combine two different type air shower detector, we aim to search super GZK cosmic ray and determine accurately the energy of these CRs. In past, extensive air shower observations using scintillation detector array give many good results Utilize these experience, we combine scintillator array and fluorescence detectors for determination for EAS energy scale, core position and incoming direction. In this paper, we introduce the electronics and data acquisition system for our scintillator array; call Surface Detector (SD). The engineering array that constituted 18 scintillation detectors was installed on December 2004. We have tested our electronics and DAQ on this small array. Complete SD will have 576 detectors, around 900 km2. This will be about 9 times larger than AGASA.

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M3 - Conference contribution

AN - SCOPUS:71749111501

VL - 8

SP - 177

EP - 180

BT - 29th International Cosmic Ray Conference, ICRC 2005

PB - Tata Institute of Fundamental Research

T2 - 29th International Cosmic Ray Conference, ICRC 2005

Y2 - 3 August 2005 through 10 August 2005

ER -

The system of DAQ for TA surface array

Abstract

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ASJC Scopus subject areas

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