Document Type

Article

Publication Date

3-10-2011

Abstract

Of all the observable quantities for gamma-ray bursts (GRBs), one of the most important is E peak. E peak is defined as the peak of the νF ν power spectrum from the prompt emission. While E peak has been extensively used in the past, for example with luminosity indicators, it has not been thoroughly examined for possible sources of scatter. In the literature, the reported error bars for E peak are the simple Poisson statistical errors. Additional uncertainties arise due to the choices made by analysts in determining E peak (e.g., the start and stop times of integration), imperfect knowledge of the response of the detector, different energy ranges for various detectors, and differences in models used to fit the spectra. We examine the size of these individual sources of scatter by comparing many independent pairs of published E peak values for the same bursts. Indeed, the observed scatter in multiple reports of the same burst (often with the same data) is greatly larger than the published statistical error bars. We measure that the 1σ uncertainty associated with the analyst's choices is 28%, i.e., 0.12 in log10(E peak), with the resultant errors always being present. The errors associated with the detector response are negligibly small. The variations caused by commonly used alternative definitions of E peak (such as present in all papers and in all compiled burst lists) are typically 23%-46%, although this varies substantially with the application. The implications of this are: (1) Even the very best measured E peak values will have systematic uncertainties of 28%. (2) Thus, GRBs have a limitation in accuracy for a single event, with this being reducible by averaging many bursts. (3) The typical 1σ total uncertainty for collections of bursts is 55%. (4) We also find that the width of the distribution for E peak in the burst frame must be near zero, implying that some mechanism must exist to thermostat GRBs. (5) Our community can only improve on this situation by using collections of bursts which all have identical definitions for the E peak calculation. © 2011. The American Astronomical Society. All rights reserved.

Publication Source (Journal or Book title)

Astrophysical Journal

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