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Title: Probing Galactic Diffuse TeV Gamma-Ray Emission with the HAWC Observatory

ORCiD logo [1];  [2];  [3]
  1. Los Alamos National Laboratory
  2. University of Rochester
  3. Stanford University
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE Laboratory Directed Research and Development (LDRD) Program
OSTI Identifier:
Report Number(s):
DOE Contract Number:
Resource Type:
Resource Relation:
Conference: International Cosmic Ray Conference ; 2017-07-12 - 2017-07-20 ; Busan, Korea, South
Country of Publication:
United States
Astronomy and Astrophysics

Citation Formats

Zhou, Hao, Rho, Chang Dong, and Vianello, Giacomo. Probing Galactic Diffuse TeV Gamma-Ray Emission with the HAWC Observatory. United States: N. p., 2017. Web.
Zhou, Hao, Rho, Chang Dong, & Vianello, Giacomo. Probing Galactic Diffuse TeV Gamma-Ray Emission with the HAWC Observatory. United States.
Zhou, Hao, Rho, Chang Dong, and Vianello, Giacomo. 2017. "Probing Galactic Diffuse TeV Gamma-Ray Emission with the HAWC Observatory". United States. doi:.
title = {Probing Galactic Diffuse TeV Gamma-Ray Emission with the HAWC Observatory},
author = {Zhou, Hao and Rho, Chang Dong and Vianello, Giacomo},
abstractNote = {},
doi = {},
journal = {},
number = ,
volume = ,
place = {United States},
year = 2017,
month = 8

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  • We discuss uncertainties and possible sources of errors associated with the determination of the diffuse Galactic {gamma}-ray emission using the EGRET data. Most of the issues will be relevant also in the GLAST era. The focus here is on issues that impact evaluation of dark matter annihilation signals against the diffuse {gamma}-ray emission of the Milky Way.
  • Diffuse emission from the Milky Way dominates the gamma-ray sky. About 80% of the high-energy luminosity of the Milky Way comes from processes in the interstellar medium. The Galactic diffuse emission traces interactions of energetic particles, primarily protons and electrons, with the interstellar gas and radiation field, thus delivering information about cosmic-ray spectra and interstellar mass in distant locations. Additionally, the Galactic diffuse emission is the celestial foreground for the study of gamma-ray point sources and the extragalactic diffuse gamma-ray emission. We will report on the latest developments in the modeling of the Galactic diffuse emission, which will be usedmore » for the Gamma Ray Large Area Space Telescope (GLAST) investigations.« less
  • No abstract prepared.
  • Gamma-rays represent the most energetic electromagnetic window for the study of the Universe. They are studied both from space at MeV and GeV energies, with instruments like the Fermi{gamma}-ray Space Telescope, and at TeV energies with ground based instruments profiting of particle cascades in the atmosphere and of the Cerenkov radiation of charged particles in the air or in water. The Milagro gamma-ray observatory represented the first instrument to successfully implement the water Cerenkov technique for {gamma}-ray astronomy, opening the ground for the more sensitive HAWC {gamma}-ray observatory, currently under development in the Sierra Negra site and already providing earlymore » science results.« less
  • The first limits on the prompt emission from the long gamma-ray burst (GRB) 130427A in the >100 GeV energy band are reported. GRB 130427A was the most powerful burst ever detected with a redshift z ≲ 0.5 and featured the longest lasting emission above 100 MeV. The energy spectrum extends at least up to 95 GeV, clearly in the range observable by the High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory, a new extensive air shower detector currently under construction in central Mexico. The burst occurred under unfavorable observation conditions, low in the sky and when HAWC was running 10% ofmore » the final detector. Based on the observed light curve at MeV-GeV energies, eight different time periods have been searched for prompt and delayed emission from this GRB. In all cases, no statistically significant excess of counts has been found and upper limits have been placed. It is shown that a similar GRB close to zenith would be easily detected by the full HAWC detector, which will be completed soon. The detection rate of the full HAWC detector may be as high as one to two GRBs per year. A detection could provide important information regarding the high energy processes at work and the observation of a possible cut-off beyond the Fermi Large Area Telescope energy range could be the signature of gamma-ray absorption, either in the GRB or along the line of sight due to the extragalactic background light.« less