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Title:
Milagro Constraints on Very High Energy Emission from Short-Duration Gamma-Ray Bursts
Authors:
Abdo, A. A.; Allen, B. T.; Berley, D.; Blaufuss, E.; Casanova, S.; Dingus, B. L.; Ellsworth, R. W.; Gonzalez, M. M.; Goodman, J. A.; Hays, E.; Hoffman, C. M.; Kolterman, B. E.; Lansdell, C. P.; Linnemann, J. T.; McEnery, J. E.; Mincer, A. I.; Nemethy, P.; Noyes, D.; Ryan, J. M.; Samuelson, F. W.; Parkinson, P. M. Saz; Shoup, A.; Sinnis, G.; Smith, A. J.; Sullivan, G. W.; Vasileiou, V.; Walker, G. P.; Williams, D. A.; Xu, X. W.; Yodh, G. B.
Affiliation:
AA(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824.), AB(Department of Physics and Astronomy, University of California, Irvine, CA 92697.), AC(Department of Physics, University of Maryland, College Park, MD 20742.), AD(Department of Physics, University of Maryland, College Park, MD 20742.), AE(Group P-23, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545.), AF(Group P-23, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545.), AG(Department of Physics and Astronomy, George Mason University, Fairfax, VA 22030.), AH(Instituto de Astronomía, Universidad Nacional Autónoma de México, D.F., Mexico, 04510.), AI(Department of Physics, University of Maryland, College Park, MD 20742.), AJ(Department of Physics, University of Maryland, College Park, MD 20742.; Current address: High Energy Physics Division, Argonne National Laboratory, Argonne, IL 60439.; Current address: Enrico Fermi Institute, University of Chicago, Chicago, IL 60637.), AK(Group P-23, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545.), AL(Department of Physics, New York University, New York, NY 10003.), AM(Department of Physics, University of Maryland, College Park, MD 20742.), AN(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824.), AO(NASA Goddard Space Flight Center, Greenbelt, MD 20771.), AP(Department of Physics, New York University, New York, NY 10003.), AQ(Department of Physics, New York University, New York, NY 10003.), AR(Department of Physics, University of Maryland, College Park, MD 20742.), AS(Department of Physics, University of New Hampshire, Durham, NH 03824.), AT(Office of Science and Engineering Laboratories, Center for Devices and Radiological Health, US Food and Drug Administration.), AU(Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, CA 95064.), AV(Ohio State University, Lima, OH 45804.), AW(Group P-23, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545.), AX(Department of Physics, University of Maryland, College Park, MD 20742.), AY(Department of Physics, University of Maryland, College Park, MD 20742.), AZ(Department of Physics, University of Maryland, College Park, MD 20742.), BA(Group P-23, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545.), BB(Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, CA 95064.), BC(Group P-23, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545.), BD(Department of Physics and Astronomy, University of California, Irvine, CA 92697.)
Publication:
The Astrophysical Journal, Volume 666, Issue 1, pp. 361-367. (ApJ Homepage)
Publication Date:
09/2007
Origin:
UCP
ApJ Keywords:
Gamma Rays: Bursts, Gamma Rays: Observations
DOI:
10.1086/519763
Bibliographic Code:
2007ApJ...666..361A

Abstract

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 (Fox et al. 2005; Gehrels et al. 2005; Villasenor et al. 2005; Berger et al. 2005; Barthelmy et al. 2005). 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.
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