73 research outputs found
Search for TeV emission from geminga by the VERITAS observatory
Journal ArticleDuring November/December 2007, we observed the region centered on the Geminga Pulsar for 10.4 hours using the VERITAS IACT Observatory. We find no evidence for either steady emission point source emission, or pulsed emission of a point source at the period of the Geminga pulsar (237 msec). The measured VHE y-ray flux limits for the impulsed search is Fy(> 300 GeV , 99% c.l) lOOGeV , 99%c.l.) < 0.8 - 1.0 x 10-8 m-2 s"1
Gamma-ray emission by the BL Lac Markarian 501
posterOptical astronomy is the study of the heavens as they emit light, or the visible portion of the electromagnetic spectrum. Gamma-ray astronomy is the study of astrophysical sources that emit the most energetic form of electromagnetic radiation (ie: gamma-rays). High Energy gamma-rays are much too faint to be directly seen with the human eye. Thus they are detected using arrays of large diameter (39 ft) mirrors and fast digitizing cameras which image the light emitted from the gamma-ray as it is absorbed in the Earth's atmosphere
Simulation of Near Horizontal Muons and Muon Bundles for the HAWC Observatory with CORSIKA
The HAWC (High Altitude Water Cerenkov) gamma ray observatory observes muons
with nearly-horizontal trajectories corresponding to zenith angles greater than
. HAWC is located at an altitude of 4100 meters a.s.l. (70 deg.
atmospheric depth of 2400 g/cm) on the extinct volcano, Sierra Negra in
Mexico. In this poster, we summarize the CORSIKA and GEANT4 as well as
toy-model based simulations performed to determine the effective area of HAWC
to muons from high zenith angle cosmic ray primaries. We are developing an
updated GEANT4 based detector response simulation that includes a model of the
volcanoes that are located near HAWC. These simulations are investigating the
capability to use muon multiplicity and rates to differentiate between the
primary particle composition (proton or iron) and measure the primary energy.Comment: Presented at the 35th International Cosmic Ray Conference (ICRC2017),
Bexco, Busan, Korea. See arXiv:1708.02572 for all HAWC contribution
Detection of Near Horizontal Muons with the HAWC Observatory
The HAWC (High Altitude Water Cherenkov) gamma ray observatory is able to
observe muons with nearly horizontal trajectories. HAWC is located at an
altitude of 4100 meters a.s.l. on the Sierra Negra volcano in Mexico. The HAWC
detector is composed of 300 water tanks, each 7.3 m in diameter and 4.5 m tall,
densely packed over a physical area of 22,000 m. Previous and current
experiments have observed high zenith angle (near horizontal) muons at or near
sea level. HAWC operates as a hodoscope able to observe multi-TeV muons at
zenith angles greater than 75 degrees. This is the first experiment to measure
near horizontal muons at high altitude and with large ( 10 m) separations
for multiple muons. These muons are distinguishable from extensive air showers
by observing near horizontal particles propagating with the speed of light. The
proximity of Sierra Negra and Pico de Orizaba volcanoes provides an additional
measurement of muons with rock overburdens of several km water equivalent. We
will present the angular distribution and rate at which HAWC observes these
muon eventsComment: Presented at the 35th International Cosmic Ray Conference (ICRC2017),
Bexco, Busan, Korea. See arXiv:1708.02572 for all HAWC contribution
Deployment of a pair of 3M telescopes in Utah
Journal ArticleTwo 3m telescopes are being installed in Grantsville Utah. They are intended for the testing of various approaches to the implementation of intensity interferometry using Cherenkov Telescopes in large arrays as receivers as well as for the testing of novel technology cameras and electronics for ground based gamma-ray astronomy
Search for γ rays above 1014 eV from Cygnus X-3 during the June and July 1989 radio outbursts
Journal ArticleWe have looked for γ-ray emission above 100 TeV from the binary x-ray source Cygnus X-3 during a period of intense radio emission in the summer of 1989. We find no evidence for excess air showers from the direction of the source and the muon content of air showers from this direction is the same as that of ordinary cosmic rays. The flux of γ rays from Cygnus X-3 with energies exceeding 2.1x10^14 eV is < 5.5x10^-13 cm-1 sec-1 (90% C.L.)
Observation of the shadows of the moon and sun using 100 TeV cosmic rays
Journal ArticleThe Chicago Air Shower Array (CASA) is a large ground-based scintillation detector [1-4]. It is located at the Dugway Proving Ground is west central Utah, latitude 40°N and mean atmospheric depth 870 g / c m 2. A schematic aerial view of CASA is shown in Fig. 1. Each dot represents one scintillation station of the array
Overview of the ANITA project
Journal ArticleThe ANITA project is designed to investigate ultra-high energy (>1017 eV) cosmic ray interactions throughout the universe by detecting the neutrinos created in those interactions. These high energy neutrinos are detectable through their interactions within the Antarctic ice sheet, which ANITA will use as a detector target that effectively converts the neutrino interactions to radio pulses. This paper will give an overview of the project including scientific objectives, detection description and mission design
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