Journal
ASTROPARTICLE PHYSICS
Volume 62, Issue -, Pages 125-133Publisher
ELSEVIER
DOI: 10.1016/j.astropartphys.2014.08.004
Keywords
Detector prototype; Scientific verification; TeV cosmic rays
Funding
- National Science Foundation
- US Department of Energy Office of High-Energy Physics
- LDRD program of Los Alamos National Laboratory
- Consejo Nacional de Ciencia y Tecnologia [55155, 103520, 105033, 105666, 122331, 194116, 132197, 179588]
- Red de Fisica de Altas Energias
- DGAPA-UNAM [IN110212, IN105211, IN108713, IN121309, IN115409, IN111612, IN112412, IG100414-3]
- VIEP-BUAP [161-EXC-2011]
- Luc-Binette Foundation UNAM Postdoctoral Fellowship
- University of Wisconsin Alumni Research Foundation
- Institute of Geophysics and Planetary Physics at Los Alamos National Lab
- Division Of Physics
- Direct For Mathematical & Physical Scien [1002546] Funding Source: National Science Foundation
- Division Of Physics
- Direct For Mathematical & Physical Scien [1308033, 1308127, 1002542] Funding Source: National Science Foundation
- STFC [ST/H00081X/2] Funding Source: UKRI
Ask authors/readers for more resources
VAMOS(1) was a prototype detector built in 2011 at an altitude of 4100 m a.s.l. in the state of Puebla, Mexico. The aim of VAMOS was to finalize the design, construction techniques and data acquisition system of the HAWC observatory. HAWC is an air-shower array currently under construction at the same site of VAMOS with the purpose to study the TeV sky. The VAMOS setup included six water Cherenkov detectors and two different data acquisition systems. It was in operation between October 2011 and May 2012 with an average live time of 30%. Besides the scientific verification purposes, the eight months of data were used to obtain the results presented in this paper: the detector response to the Forbush decrease of March 2012, and the analysis of possible emission, at energies above 30 GeV, for long gamma-ray bursts GRB111016B and GRB120328B. (C) 2014 Elsevier B.V. All rights reserved.
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