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          Institute: MPI für Kernphysik     Collection: High-Energy Astrophysics     Display Documents

ID: 318244.0, MPI für Kernphysik / High-Energy Astrophysics
Milagro constraints on very high energy emission from short
duration gamma ray bursts
Authors:Abdo, A.; Allen, B. T.; Berley, D.; Blaufuss, E.; Casanova, S.; Chen, C.; Coyne, D.; Delay, R. S.; Dingus, B. L.; Ellsworth, R. W.; Gonzalez, M. M.; Goodman, J. A.; Hays, E.; Hoffmann, C.; Landsell, C. P.; Linnemann, J. T.; McEnery, J. E.; Nemethy, P.; Noyes, D.; Ryan, J. M.; Samuelson, F. W.; Saz Parkinson, P. M.; Shoup, A.; Sinnis, G.; Smith, A. J.; Sullivan, G. W.; Vasileiou, V.; Walker, G. P.; Williams, D. A.; Xu, X. W.; Yodh, G. B.
Date of Publication (YYYY-MM-DD):2007-09-01
Title of Journal:Astrophysical Journal, Part 1
Issue / Number:1
Start Page:361
End Page:367
Review Status:not specified
Audience:Experts Only
Abstract / Description:Recent rapid localizations of short, hard gamma-ray bursts (GRBs) by the Swift and HETE satellites have led to the observation of the first afterglows and the measurement of the first redshifts from this type of burst. Detection of >> 100 GeV counterparts would place powerful constraints on GRB mechanisms. Seventeen short duration (< 5 s) GRBs detected by satellites occurred within the field of view of the Milagro gamma-ray observatory between 2000 January and 2006 December.
We have searched the Milagro data for >100 GeV counterparts to these GRBs and find no significant emission correlated with these bursts. Due to the absorption of high-energy gamma rays by the extragalactic background light (EBL), detections are only expected for redshifts less than ~0.5. While most long duration GRBs occur at redshifts higher than 0.5, the opposite is thought to be true of short GRBs. Lack of a detected VHE signal thus allows setting meaningful fluence limits. One GRB in the sample (050509b) has a likely association with a galaxy at a redshift of 0.225, while another (051103) has been tentatively linked to the nearby galaxy M81. Fluence limits are corrected for EBL absorption, either using the known measured redshift, or computing the corresponding absorption for a redshift of 0.1 and 0.5, as well as for the case of z=0.
External Publication Status:published
Document Type:Article
Version Comment:Automatic journal name synchronization
Affiliations:MPI für Kernphysik/Group of W. Hofmann/High Energy Astrophysics (F. Aharonian)
External Affiliations:Department of Physics and Astronomy, Michigan State, USA University, 3245 BioMedical Physical Sciences Building, East Lansing, MI 48824, USA
Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA
Department of Physics, University of Maryland, College Park, MD 20742, USA
Group P-23, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545, USA
Department of Physics and Astronomy, George Mason University, 4400 University Drive, Fairfax, VA 22030, USA
Instituto de Astronomía, Universidad Nacional Autónoma de México, D.F., México, 04510, Mexico
High Energy Physics Division, Argonne National Laboratory, Argonne, IL 60439 and Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA
Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA
NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
Department of Physics, University of New Hampshire, Morse Hall, Durham, NH 03824-3525, USA
Office of Science and Engineering Laboratories, Center for Devices and Radiological Health, U.S. Food and Drug Administration, USA
Santa Cruz Institute for Particle Physics, University of California, 1156 High Street, Santa Cruz, CA 95064 Ohio State University, Lima, OH 45804, USA
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