2000AIPC..526..751D
Milagro: A TeV observatory for gamma-ray bursts
Dingus, B. L. ( University of Utah, Salt Lake City, Utah 84112 ); Atkins, R. ( University of Utah, Salt Lake City, Utah 84112 ); Benbow, W. ( University of California, Santa Cruz, California 95064 ); Berley, D. ( University of Maryland, College Park, Maryland 20742 ); Chen, M. L. ( University of Maryland, College Park, Maryland 20742 ); Coyne, D. G. ( University of California, Santa Cruz, California 95064 ); Ellsworth, R. W. ( George Mason University, Fairfax, Virginia 22030 ); Evans, D. ( University of Maryland, College Park, Maryland 20742 ); Falcone, A. ( University of New Hampshire, Durham, New Hampshire 03824 ); Fleysher, L. ( New York University, New York, New York 10003 ); Fleysher, R. ( New York University, New York, New York 10003 ); Gisler, G. ( Los Alamos National Laboratory, Los Alamos, New Mexico 87545 ); Goodman, J. A. ( University of Maryland, College Park, Maryland 20742 ); Haines, T. J. ( Los Alamos National Laboratory, Los Alamos, New Mexico 87545 ); Hoffman, C. M. ( Los Alamos National Laboratory, Los Alamos, New Mexico 87545 ); Hugenberger, S. ( University of California, Irvine, California 92697 ); Kelley, L. A. ( University of California, Santa Cruz, California 95064 ); Leonor, I. ( University of California, Irvine, California 92697 ); McConnell, M. ( University of New Hampshire, Durham, New Hampshire 03824 ); McCullough, J. F. ( University of California, Santa Cruz, California 95064 ); McEnery, J. E. ( University of Utah, Salt Lake City, Utah 84112 ); Miller, R. S. ( Los Alamos National Laboratory, Los Alamos, New Mexico 87545; University of New Hampshire, Durham, New Hampshire 03824 ); Mincer, A. I. ( New York University, New York, New York 10003 ); Morales, M. F. ( University of California, Santa Cruz, California 95064 ); Nemethy, P. ( New York University, New York, New York 10003 ); Ryan, J. M. ( University of New Hampshire, Durham, New Hampshire 03824 ); Shen, B. ( University of California, Riverside, California 92521 ); Shoup, A. ( University of California, Irvine, California 92697 ); Sinnis, C. ( Los Alamos National Laboratory, Los Alamos, New Mexico 87545 ); Smith, A. J. ( University of California, Riverside, California 92521; University of Maryland, College Park, Maryland 20742 ); Sullivan, G. W. ( University of Maryland, College Park, Maryland 20742 ); Tumer, T. ( University of California, Riverside, California 92521 ); Wang, K. ( University of California, Riverside, California 92521 ); Wascko, M. O. ( University of California, Riverside, California 92521 ); Westerhoff, S. ( University of California, Santa Cruz, California 95064 ); Williams, D. A. ( University of California, Santa Cruz, California 95064 ); Yang, T. ( University of California, Santa Cruz, California 95064 ); Yodh, G. B. ( University of California, Irvine, California 92697 ) and 28 coauthors show affiliations
GAMMA-RAY BURSTS: 5th Huntsville Symposium. AIP Conference Proceedings, Volume 526, pp. 751-755 (2000).
Published in Sep 2000
Observation of prompt TeV γ-rays from GRBs requires a new type of detector to overcome the low duty factor and small field of view of current TeV observatories. Milagro is such a new type of very high energy (> a few 100 GeV) gamma-ray observatory, which has a large field of view of >1 steradian and 24 hours/day operation. Milagrito, a prototype for Milagro, was operated from February 1997 to May 1998. During the summer of 1998, Milagrito was dismantled and Milagro was built. Both detectors use a 80 m×60 m×8 m pond of water in which a 3 m×3 m grid of photomultiplier tubes detects the Cherenkov light produced in the water by the relativistic particles in extensive air showers. Milagrito was smaller and had only one layer of photomultipliers, but allowed the technique to be tested. Milagrito observations of the Moon's shadow and Mrk 501 are consistent with the Monte Carlo prediction of the telescope's parameters, such as effective area and angular resolution. Milagro will have improved flux sensitivity over Milagrito due to larger effective area, better angular resolution and cosmic-ray background rejection. .
Keywords:
Free Keywords: 95.75.Fg; 95.85.Pw; 98.62.Nx; Jets and bursts; Spectroscopy and spectrophotometry; galactic winds and fountains; gamma-ray
PACS Codes: 95.75.Fg; 95.85.Pw; 98.62.Nx
PACS: Jets and bursts; Spectroscopy and spectrophotometry; galactic winds and fountains; gamma-ray
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