The Third Fermi GBM Gamma-Ray Burst Catalog: The First Six Years

Bhat, P. N.; Meegan, C.; Kienlin, A. von; Pačiesas, W. S.; Briggs, M. S.; Burgess, J. Michael; Burns, E.; Chaplin, V.; Cleveland, W. H.; Collazzi, A. C.; Connaughton, V.; Diekmann, A.; Fitzpatrick, G.; Gibby, M. H.; Giles, M. M.; Goldstein, A.; Greiner, J.; Jenke, P.; Kippen, R. M.; Kouveliotou, C.; Mailyan, B.; McBreen, S.; Pelassa, V.; Preece, R. D.; Roberts, O. J.; Sparke, Linda S.; Stanbro, M.; Vereš, P.; Wilson-Hodge, C.; Xiong, S. L.; Younes, George; Yu, H. F.; Zhang, Bin-Bin

doi:10.3847/0067-0049/223/2/28

Cited by 245 publications

(184 citation statements)

References 39 publications

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“…The GBM is used to study gamma-ray bursts; the data received by its 14 detectors (12 NaI and 2 BGO) are collected by a central Data Processing Unit (DPU) [17]. The database from the Fermi GBM detectors, the FERMIGBRST 1 catalog [18,19] contains more than 2000 GRBs with several parameters such as position, durations, flux, fluences and spectral properties. These parameters were calculated from the light curves and spectral fitting.…”

Section: Data and Mathematical Summarymentioning

confidence: 99%

Spectral classification and variation of Fermi GRBs

Rácz¹,

Balázs²,

Toth³

et al. 2017

Proceedings of 7th International Fermi Symposium — PoS(IFS2017)

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The Fermi GBM catalog contains general physical quantities of the observed objects and also estimated parameters (peak energy, spectral indices, intensity) from four fitted spectral models (Band, smoothly broken power law, Comptonized, power law) for the peak flux and the fluence. We studied the nature of the errors of the peak flux, the fluence, and duration parameters. We have found a linear correlation between the logarithm of the measured quantities and their error bars. We interpret our results as an indication that the peak flux, fluence and duration follow a Poissonic distribution.

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Section: Data and Mathematical Summarymentioning

confidence: 99%

Spectral classification and variation of Fermi GRBs

Rácz¹,

Balázs²,

Toth³

et al. 2017

Proceedings of 7th International Fermi Symposium — PoS(IFS2017)

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“…Spectral models commonly applied to GRB prompt spectra include a single power law (PL), a power law with an exponential cutoff (CPL), and a Band function (Preece et al 2000;Kaneko et al 2006;Nava et al 2011;Goldstein et al 2012;Gruber et al 2014;Bhat et al 2016;Lien et al 2016). These empirical models usually return a satisfactory fit to most spectra.…”

Section: Spectral Modelsmentioning

confidence: 99%

Detection of Low-energy Breaks in Gamma-Ray Burst Prompt Emission Spectra

Oganesyan

Nava

Ghirlanda

et al. 2017

ApJ

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The radiative process responsible for gamma-Ray Burst (GRB) prompt emission has not been identified yet. If dominated by fast-cooling synchrotron radiation, the part of the spectrum immediately below the νF ν peak energy should display a power-law behavior with slope α 2 = −3/2, which breaks to a higher value α 1 = −2/3 (i.e. to a harder spectral shape) at lower energies. Prompt emission spectral data (usually available down to ∼ 10−20 keV) are consistent with one single power-law behavior below the peak, with typical slope α = −1, higher than (and then inconsistent with) the expected value α 2 = −3/2. To better characterize the spectral shape at low energy, we analyzed 14 GRBs for which the Swift X-ray Telescope started observations during the prompt. When available, Fermi-GBM observations have been included in the analysis. For 67% of the spectra, models that usually give a satisfactory description of the prompt (e.g., the Band model) fail in reproducing the 0.5 − 1000 keV spectra: low-energy data outline the presence of a spectral break around a few keV. We then introduce an empirical fitting function that includes a low-energy power law α 1 , a break energy E break , a second power law α 2 , and a peak energy E peak . We find α 1 = −0.66 (σ = 0.35), log(E break /keV) = 0.63 (σ = 0.20), α 2 = −1.46 (σ = 0.31), and log(E peak /keV) = 2.1 (σ = 0.56). The values α 1 and α 2 are very close to expectations from synchrotron radiation. In this context, E break corresponds to the cooling break frequency. The relatively small ratio E peak /E break ∼ 30 suggests a regime of moderately fast cooling, which might solve the long-lasting problem of the apparent inconsistency between measured and predicted low-energy spectral index.

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“…In Figure 10, we compare the distribution of sGRB 1 s fluence measurements from the 3rd GBM GRB catalog (Bhat et al 2016) to our upper bounds for LVT151012 and GW151226, as well as the fluence measurement described in Connaughton et al (2016). The fluences from the GBMdetected sGRBs span´-2.5 10 8 to´-1.1 10 5 erg cm −2 , with GW150914-GBM around the 40th percentile.…”

Section: Comparison To the Sgrbsmentioning

confidence: 96%

Searching the Gamma-Ray Sky for Counterparts to Gravitational Wave Sources: Fermi Gamma-Ray Burst Monitor and Large Area Telescope Observations of Lvt151012 and Gw151226

Racusin¹,

Burns²,

Goldstein³

et al. 2017

ApJ

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We present the Fermi Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) observations of the LIGO binary black hole merger event GW151226 and candidate LVT151012. At the time of the LIGO triggers on LVT151012 and GW151226, GBM was observing 68% and 83% of the localization regions, and LAT was observing 47% and 32%, respectively. No candidate electromagnetic counterparts were detected by either the GBM or LAT. We present a detailed analysis of the GBM and LAT data over a range of timescales from seconds to years, using automated pipelines and new techniques for characterizing the flux upper bounds across large areas of the sky. Due to the partial GBM and LAT coverage of the large LIGO localization regions at the trigger times for both events, differences in source distances and masses, as well as the uncertain degree to which emission from these sources could be beamed, these non-detections cannot be used to constrain the variety of theoretical models recently applied to explain the candidate GBM counterpart to GW150914.

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The Third Fermi GBM Gamma-Ray Burst Catalog: The First Six Years

Cited by 245 publications

References 39 publications

Spectral classification and variation of Fermi GRBs

Spectral classification and variation of Fermi GRBs

Detection of Low-energy Breaks in Gamma-Ray Burst Prompt Emission Spectra

Searching the Gamma-Ray Sky for Counterparts to Gravitational Wave Sources: Fermi Gamma-Ray Burst Monitor and Large Area Telescope Observations of Lvt151012 and Gw151226

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