From The Pierre Auger Observatory to AugerPrime

6th School on Cosmic Rays and Astrophysics

Parra, Alejandra^1,2 ; Bravo, Oscar Martínez^1,2

Avenida San Claudio y 18 sur, Colonia San Manuel, Ciudad Universitaria, Edificio FM1-101B, Puebla

C.P. 72570, Mexico^1

Observatorio Pierre Auger, Av. San Martin Norte 304, Malargüe

5613, Argentina^2

关键词: Atmospheric showers;    Extensive air showers;    Pierre Auger observatory;    Primary particles;    Scintillator detector;    Surface detectors;    Three parameters;    Water Cherenkov detectors;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/866/1/012001/pdf
DOI  :  10.1088/1742-6596/866/1/012001

来源: IOP

【 摘 要 】

In the present work we report the principal motivation and reasons for the new stage of the Pierre Auger Observatory, AugerPrime. This upgrade has as its principal goal to clarify the origin of the highest energy cosmic rays through improvement in studies of the mass composition. To accomplished this goal, AugerPrime will use air shower universality, which states that extensive air showers can be completely described by three parameters: the primary energy E0, the atmospheric shower depth of maximum Xmax, and the number of muons, Nμ. The Auger Collaboration has planned to complement its surface array (SD), based on water-Cherenkov detectors (WCD) with scintillator detectors, calls SSD (Scintillator Surface Detector). These will be placed at the top of each WCD station. The SSD will allow a shower to shower analysis, instead of the statistical analysis that the Observatory has previously done, to determine the mass composition of the primary particle by the electromagnetic to muonic ratio.